FN Thomson Reuters Web of Science™ VR 1.0 PT B AU Hsu, F AF Hsu, F BE Spitzer, C Schmocker, U Dang, VN TI Defining the group importance measures (GIM) with applications in space shuttle PRA SO PROBABILISTIC SAFETY ASSESSMENT AND MANAGEMENT, VOL 1- 6 LA English DT Proceedings Paper CT Joint Meeting of the 7th International Conference on Probabilistic Safety Assessment and Management/European Safety and Reliability Conference CY JUN 14-18, 2004 CL Berlin, GERMANY SP TUV Suddeutschland, Swiss Fed Nucl Safety Inspectorate, Paul Scherrer Inst, AREVA, Basler & Hofmann, Gottlieb Daimler & Karl Benz Fdn, Swissnucl, VGB PowerTech, ABS Consulting, European Commiss, Joint Res Ctr, European Safety, Reliabil & Data Assoc, US Fed Aviat Adm, Idaho Natl Engn & Environm Lab, Risknowlogy, Scientech Inc, VDI, Assoc Engineers AB In order to address some technical challenges raised in the Space Shuttle PRA development, we introduce in this paper, a definition of Group (or Gate-level) Importance Measure (GIM). The GIM measures defined here are extensions of Fussel-Vesely (FV) type importances, and can also be extended to other type of importance measures. Algorithms are also developed for extended SAPHIRE implementations. Examples are given to show that the GIMs can be obtained for every level of contributors modeled in a PRA. Such measure can be easily used to produce PRA risk ranking at all level of details, such as by phase, element, sequence bins, failure type or any combinations of specific group of event type and failure mode. C1 NASA, Lyndon B Johnson Space Ctr, SAIC, Houston, TX 77058 USA. RP Hsu, F (reprint author), NASA, Lyndon B Johnson Space Ctr, SAIC, NC62, Houston, TX 77058 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG LONDON LTD PI GODALMING PA SWEETAPPLE HOUSE CATTESHALL RD FARNCOMBE, GODALMING GU7 1NH, SURREY, ENGLAND BN 1-85233-827-X PY 2004 BP 3583 EP 3590 PG 8 WC Engineering, Multidisciplinary; Operations Research & Management Science SC Engineering; Operations Research & Management Science GA BAU29 UT WOS:000223579900573 ER PT B AU Frank, J Gross, MAK Kurklu, E AF Frank, J Gross, MAK Kurklu, E GP AAAI TI SOFIA's choice: An AIl approach to scheduling airborne astronomy observations SO PROCEEDING OF THE NINETEENTH NATIONAL CONFERENCE ON ARTIFICIAL INTELLIGENCE AND THE SIXTEENTH CONFERENCE ON INNOVATIVE APPLICATIONS OF ARTIFICIAL INTELLIGENCE LA English DT Proceedings Paper CT 19th National Conference on Artificial Intelligence/16th Conference on Innovative Applications of Artificial Intelligence CY JUL 25-29, 2004 CL San Jose, CA SP Amer Assoc Artificial Intelligence AB We describe an innovative solution to the problem of scheduling astronomy observations for the Stratospheric Observatory for Infrared Astronomy, an airborne observatory. The problem contains complex constraints relating the feasibility of an astronomical observation to the position and time at which the observation begins, telescope elevation limits and available fuel. Solving the problem requires making discrete choices (e.g. selection and sequencing of observations) and continuous ones (e.g. takeoff time and setting up observations by repositioning the aircraft). The problem also includes optimization criteria such as maximizing observing time while simultaneously minimizing total flight time. We describe a method to search for good flight plans that satisfy all constraints. This novel approach combines heuristic search, biased stochastic sampling, continuous optimization techniques, and well-founded approximations that eliminate feasible solutions but greatly reduce computation time. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Frank, J (reprint author), NASA, Ames Res Ctr, Mail Stop N269-3, Moffett Field, CA 94035 USA. NR 8 TC 3 Z9 3 U1 0 U2 1 PU AMER ASSOC ARTIFICIAL INTELLIGENCE PI MENLO PK PA 445 BURGESS DR, MENLO PK, CA 94025 USA BN 0-262-51183-5 PY 2004 BP 828 EP 835 PG 8 WC Computer Science, Artificial Intelligence SC Computer Science GA BBP85 UT WOS:000226971400129 ER PT B AU Globus, A Crawford, J Lohn, J Pryor, A AF Globus, A Crawford, J Lohn, J Pryor, A GP AAAI TI A comparison of techniques for scheduling Earth observing satellites SO PROCEEDING OF THE NINETEENTH NATIONAL CONFERENCE ON ARTIFICIAL INTELLIGENCE AND THE SIXTEENTH CONFERENCE ON INNOVATIVE APPLICATIONS OF ARTIFICIAL INTELLIGENCE LA English DT Proceedings Paper CT 19th National Conference on Artificial Intelligence/16th Conference on Innovative Applications of Artificial Intelligence CY JUL 25-29, 2004 CL San Jose, CA SP Amer Assoc Artificial Intelligence AB Scheduling observations by coordinated fleets of Earth Observing Satellites (EOS) involves large search spaces, complex constraints and poorly understood bottlenecks; conditions where stochastic algorithms are often effective. However, there are many such algorithms and the best one to use is not obvious. Here we compare multiple variants of the genetic algorithm, hill climbing, simulated annealing, squeaky wheel optimization and iterated sampling on ten realistically-sized model EOS scheduling problems. Schedules are represented by a permutation (non-temperal ordering) of the observation requests. A simple, greedy, deterministic scheduler assigns times and resources to each observation request in the order indicated by the permutation, discarding those that violate the constraints created by previously scheduled observations. Simulated annealing performs best and random mutation outperforms a more 'intelligent' imitator. Furthermore, the best imitator, by a small margin, was a novel approach we call 'temperature-dependent swap' that makes large changes in the early stages of the search and smaller changes towards the end. C1 NASA, CSC, Ames, IA USA. RP Globus, A (reprint author), NASA, CSC, Ames, IA USA. NR 21 TC 17 Z9 32 U1 1 U2 4 PU AMER ASSOC ARTIFICIAL INTELLIGENCE PI MENLO PK PA 445 BURGESS DR, MENLO PK, CA 94025 USA BN 0-262-51183-5 PY 2004 BP 836 EP 843 PG 8 WC Computer Science, Artificial Intelligence SC Computer Science GA BBP85 UT WOS:000226971400130 ER PT B AU Tran, D Chien, S Sherwood, R Castano, R Cichy, B Davies, A Rabideau, G AF Tran, D Chien, S Sherwood, R Castano, R Cichy, B Davies, A Rabideau, G GP AAAI TI The autonomous sciencecraft experiment onboard the EO-1 spacecraft SO PROCEEDING OF THE NINETEENTH NATIONAL CONFERENCE ON ARTIFICIAL INTELLIGENCE AND THE SIXTEENTH CONFERENCE ON INNOVATIVE APPLICATIONS OF ARTIFICIAL INTELLIGENCE LA English DT Proceedings Paper CT 19th National Conference on Artificial Intelligence/16th Conference on Innovative Applications of Artificial Intelligence CY JUL 25-29, 2004 CL San Jose, CA SP Amer Assoc Artificial Intelligence AB The Autonomous Sciencecraft Experiment (ASE), currently flying onboard the Earth Observing-1 (EO-1) spacecraft, integrates several autonomy software technologies enabling autonomous science analysis and mission planning. The experiment demonstrates the potential for future space missions to use onboard decision-making to respond autonomously to capture short-lived science phenomena. The AAAI software demonstration will consist of two sections: a real-time display of an ASE-commanded ground contact from the EO-1 spacecraft, and a simulation of the full ASE autonomous science-response scenario. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tran, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 4 TC 1 Z9 1 U1 0 U2 1 PU AMER ASSOC ARTIFICIAL INTELLIGENCE PI MENLO PK PA 445 BURGESS DR, MENLO PK, CA 94025 USA BN 0-262-51183-5 PY 2004 BP 1040 EP 1041 PG 2 WC Computer Science, Artificial Intelligence SC Computer Science GA BBP85 UT WOS:000226971400192 ER PT S AU Naasz, BJ Burns, RD Gaylor, D Higinbotham, J AF Naasz, BJ Burns, RD Gaylor, D Higinbotham, J BE Montenbruck, O Battrick, B TI Hardware-in-the-loop testing of continuous control algorithms for a precision formation flying demonstration mission SO PROCEEDINGS OF THE 18TH INTERNATIONAL SYMPOSIUM ON SPACE FLIGHT DYNAMICS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 18th International Symposium on Space Flight Dynamics CY OCT 11-15, 2004 CL Munich, GERMANY SP DLR German Space Operat Ctr, ESA European Space Operat Ctr ID SPACECRAFT FORMATIONS; ORBITS AB A sample mission sequence is defined for a low earth orbit demonstration of Precision Formation Flying (PFF). Various guidance navigation and control strategies are discussed for use in the PFF experiment phases. A sample PFF experiment is implemented and tested in a realistic Hardware-in-the-Loop (HWIL) simulation using the Formation Flying Test Bed (FFTB) at NASA's Goddard Space Flight Center. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Naasz, BJ (reprint author), NASA, Goddard Space Flight Ctr, Code 595, Greenbelt, MD 20771 USA. NR 13 TC 2 Z9 2 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-859-X J9 ESA SP PUBL PY 2004 VL 548 BP 53 EP 58 PG 6 WC Engineering, Aerospace SC Engineering GA BBV58 UT WOS:000228033000009 ER PT S AU O'Donnell, JR Hsu, OC Hanson, J Hruby, V AF O'Donnell, JR Hsu, OC Hanson, J Hruby, V BE Montenbruck, O Battrick, B TI The space technology-7 disturbance reduction system SO PROCEEDINGS OF THE 18TH INTERNATIONAL SYMPOSIUM ON SPACE FLIGHT DYNAMICS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 18th International Symposium on Space Flight Dynamics CY OCT 11-15, 2004 CL Munich, GERMANY SP DLR German Space Operat Ctr, ESA European Space Operat Ctr AB The Space Technology 7 Disturbance Reduction System (DRS) is an in-space technology demonstration designed to validate technologies that are required for future missions such as the Laser Interferometer Space Antenna (LISA) and the Micro-Arcsecond X-ray Imaging Mission (MAXIM). The primary sensors that will be used by DRS are two Gravitational Reference Sensors (GRSs) being developed by Stanford University. DRS will control the spacecraft so that it flies about one of the freely-floating Gravitational Reference Sensor test masses, keeping it centered within its housing. The other GRS serves as a cross-reference for the first as well as being used as a reference for the spacecraft's attitude control. Colloidal MicroNewton Thrusters being developed by the Busek Co. will be used to control the spacecraft's position and attitude using a six degree-of-freedom Dynamic Control System being developed by Goddard Space Flight Center. A laser interferometer being built by the Jet Propulsion Laboratory will be used to help validate the results of the experiment. The DRS will be launched in 2008 on the European Space Agency (ESA) LISA Pathfinder spacecraft along with a similar ESA experiment, the LISA Test Package. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP O'Donnell, JR (reprint author), NASA, Goddard Space Flight Ctr, Code 595, Greenbelt, MD 20771 USA. NR 10 TC 3 Z9 3 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-859-X J9 ESA SP PUBL PY 2004 VL 548 BP 105 EP 110 PG 6 WC Engineering, Aerospace SC Engineering GA BBV58 UT WOS:000228033000017 ER PT S AU Han, D Highsmith, D Jah, M Craig, D Border, J Kroger, P AF Han, D Highsmith, D Jah, M Craig, D Border, J Kroger, P BE Montenbruck, O Battrick, B TI Mars express interplanetary navigation from launch to mars orbit insertion: The JPL experience SO PROCEEDINGS OF THE 18TH INTERNATIONAL SYMPOSIUM ON SPACE FLIGHT DYNAMICS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 18th International Symposium on Space Flight Dynamics CY OCT 11-15, 2004 CL Munich, GERMANY SP DLR German Space Operat Ctr, ESA European Space Operat Ctr AB The Jet Propulsion Laboratory (JPL), California Institute of Technology and the National Aeronautics and Space Administration have played a significant role in supporting the safe arrival of the European Space Agency (ESA) Mars Express (MEX) orbiter to Mars on 25 December 2003. MEX mission is an international collaboration between member nations of the ESA and NASA, where NASA is supporting partner. JPL ' s involvement included providing commanding and tracking service with JPL ' s Deep Space Network (DSN), in addition to navigation assurance. The collaborative navigation effort between European Space Operations Centre (ESOC) and JPL is the first since ESA ' s last deep space mission, Giotto, and began many years before the MEX launch. This paper discusses the navigational experience during the cruise and final approach phase of the mission from JPL ' s perspective. Topics include technical challenges such as orbit determination using non-DSN tracking data and media calibrations, and modelling of spacecraft physical properties for accurate representation of non-gravitational dynamics. Also mentioned in this paper is preparation and usage of DSN Delta Differential One-way Range (Delta DOR) measurements, a key element to the accuracy of the orbit determination. C1 CALTECH, Jet Prop Lab, Tech Staff, Pasadena, CA 91109 USA. RP Han, D (reprint author), CALTECH, Jet Prop Lab, Tech Staff, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Jah, Moriba/0000-0003-1109-0374 NR 6 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-859-X J9 ESA SP PUBL PY 2004 VL 548 BP 195 EP 200 PG 6 WC Engineering, Aerospace SC Engineering GA BBV58 UT WOS:000228033000031 ER PT S AU Highsmith, DE Konopliv, AS Han, D Jah, MK Craig, DE AF Highsmith, DE Konopliv, AS Han, D Jah, MK Craig, DE BE Montenbruck, O Battrick, B TI Mars atmospheric variability above 250 km altitude SO PROCEEDINGS OF THE 18TH INTERNATIONAL SYMPOSIUM ON SPACE FLIGHT DYNAMICS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 18th International Symposium on Space Flight Dynamics CY OCT 11-15, 2004 CL Munich, GERMANY SP DLR German Space Operat Ctr, ESA European Space Operat Ctr AB This paper describes the orbit reconstruction of Mars Express (MEX) with the specific goal of estimating the atmospheric density near periapsis and evaluating its variability and predictability. The goal is to validate the covariance analysis assumption of atmospheric variability for the 2005 NASA Mars Reconnaissance Orbiter (MRO). Topics covered include the MRO atmosphere model, MEX orbit determination and post-fit Doppler residuals, and atmosphere trending statistics gleaned from the orbit reconstructions. C1 Jet Prop Lab, Tech Staff, Pasadena, CA 91109 USA. RP Highsmith, DE (reprint author), Jet Prop Lab, Tech Staff, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Jah, Moriba/0000-0003-1109-0374 NR 4 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-859-X J9 ESA SP PUBL PY 2004 VL 548 BP 207 EP 212 PG 6 WC Engineering, Aerospace SC Engineering GA BBV58 UT WOS:000228033000033 ER PT S AU Cangahuala, LA Minett, G AF Cangahuala, LA Minett, G BE Montenbruck, O Battrick, B TI An orbit design method to support small body interior radar studies SO PROCEEDINGS OF THE 18TH INTERNATIONAL SYMPOSIUM ON SPACE FLIGHT DYNAMICS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 18th International Symposium on Space Flight Dynamics CY OCT 11-15, 2004 CL Munich, GERMANY SP DLR German Space Operat Ctr, ESA European Space Operat Ctr AB Consider a spacecraft equipped with a radar system that can generate signal returns from both the front and back ends of, as well as any significant voids or composition transitions in, a small body. For the purpose of determining the internal structure and inferring the composition of the body, it is necessary to collect returns from directions that encompass the whole body. Operational constraints include minimization of the survey duration and costs, and an unfamiliarity of the target shape, spin period and direction before arrival. This paper describes an approach that is robust for a variety of small body shapes and spin directions. The first part of this strategy uses orbits that are stable with respect to solar radiation pressure, at distances where the irregular shape is not a significant consideration. The second part uses orbit orientations that provide coverage at high latitudes not reached in the first part. One forces the eccentricity to evolve from an initial value through zero and back up, typically stretching out the useful time period over a couple of weeks, allowing for safe polar observations. This secular orbit evolution in the second part of the strategy is shown through averaging of the perturbing potential due to the solar radiation pressure force, as well as through numerical simulations. This paper shows orbit selections and coverage metrics for various small bodies, with masses, spin directions and rates that are representative of the observed subset of the total population. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cangahuala, LA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-859-X J9 ESA SP PUBL PY 2004 VL 548 BP 233 EP 238 PG 6 WC Engineering, Aerospace SC Engineering GA BBV58 UT WOS:000228033000037 ER PT S AU McElrath, TP Mottinger, NA Portock, BM Baird, DT Wawrzyniak, GG Graat, EJ AF McElrath, TP Mottinger, NA Portock, BM Baird, DT Wawrzyniak, GG Graat, EJ BE Montenbruck, O Battrick, B TI Differenced doppler applications for mars exploration rover navigation SO PROCEEDINGS OF THE 18TH INTERNATIONAL SYMPOSIUM ON SPACE FLIGHT DYNAMICS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 18th International Symposium on Space Flight Dynamics CY OCT 11-15, 2004 CL Munich, GERMANY SP DLR German Space Operat Ctr, ESA European Space Operat Ctr AB One of the navigation benefits of the twin-spacecraft Mars Exploration Rover (MER) project was the opportunity to learn from the first vehicle in order to improve the results for the second. In particular, differenced-Doppler data were collected and analyzed after the operational support of launch and Mars atmospheric entry for the MER-A spacecraft, with the results incorporated into realtime support of launch and atmospheric entry for the MER-B spacecraft. In the case of launch, differenced Doppler from two stations within the same tracking complex proved to be as useful as angle data in improving the post-launch single-complex orbit solutions. For atmospheric entry, differenced Doppler with intercontinental baselines proved useful in measuring the atmospheric accelerations, such that the landing site location could be significantly improved over the a priori results. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP McElrath, TP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-859-X J9 ESA SP PUBL PY 2004 VL 548 BP 277 EP 282 PG 6 WC Engineering, Aerospace SC Engineering GA BBV58 UT WOS:000228033000044 ER PT S AU Maghami, PG Hyde, TT Kim, J AF Maghami, PG Hyde, TT Kim, J BE Montenbruck, O Battrick, B TI Control of the Laser Interferometer Space Antenna SO PROCEEDINGS OF THE 18TH INTERNATIONAL SYMPOSIUM ON SPACE FLIGHT DYNAMICS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 18th International Symposium on Space Flight Dynamics CY OCT 11-15, 2004 CL Munich, GERMANY SP DLR German Space Operat Ctr, ESA European Space Operat Ctr AB The Laser Interferometer Space Antenna mission is a planned gravitational wave detector consisting of three spacecraft in heliocentric orbit. Laser interferometry is used to measure distance fluctuations between test masses aboard each spacecraft to the picometer level over a 5 million kilometer separation. The Disturbance Reduction System comprises the pointing and positioning control of the spacecraft, electrostatic suspension control of the test masses, and point-ahead and acquisition control. This paper presents a control architecture and design for the Disturbance Reduction System to meet the stringent pointing and positioning requirements. Simulations are performed to demonstrate the feasibility of the proposed architecture. C1 NASA, Goddard Space Flight Ctr, Guidance Navigat & Control Div, Greenbelt, MD 20771 USA. RP Maghami, PG (reprint author), NASA, Goddard Space Flight Ctr, Guidance Navigat & Control Div, Greenbelt, MD 20771 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-859-X J9 ESA SP PUBL PY 2004 VL 548 BP 411 EP 416 PG 6 WC Engineering, Aerospace SC Engineering GA BBV58 UT WOS:000228033000065 ER PT S AU Gramling, C Carpenter, R Lee, T Long, A AF Gramling, C Carpenter, R Lee, T Long, A BE Montenbruck, O Battrick, B TI Relative navigation strategies for the magnetospheric multiscale mission SO PROCEEDINGS OF THE 18TH INTERNATIONAL SYMPOSIUM ON SPACE FLIGHT DYNAMICS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 18th International Symposium on Space Flight Dynamics CY OCT 11-15, 2004 CL Munich, GERMANY SP DLR German Space Operat Ctr, ESA European Space Operat Ctr AB This paper evaluates several navigation approaches for the Magnetospheric Multiscale (MMS) mission, which consists of a tetrahedral formation of satellites flying in highly eccentric Earth orbits. For this investigation, inter-satellite separations of approximately 10 kilometers near apogee are used for the first two phases of the MMS mission. Navigation approaches were studied using ground station two-way Doppler measurements, Global Positioning System (GPS) pseudorange measurements, and cross-link range measurements between the members of the formation. An absolute position accuracy of 15 kilometers or better can be achieved with most of the approaches studied, and a relative position accuracy of 100 meters or better can be achieved at apogee in several cases. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gramling, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 NR 3 TC 1 Z9 1 U1 0 U2 1 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-859-X J9 ESA SP PUBL PY 2004 VL 548 BP 435 EP 440 PG 6 WC Engineering, Aerospace SC Engineering GA BBV58 UT WOS:000228033000069 ER PT S AU Bhaskaran, S Mastrodemos, N Riedel, JE Synnott, SP AF Bhaskaran, S Mastrodemos, N Riedel, JE Synnott, SP BE Montenbruck, O Battrick, B TI Optical navigation for the STARDUST wild 2 encounter SO PROCEEDINGS OF THE 18TH INTERNATIONAL SYMPOSIUM ON SPACE FLIGHT DYNAMICS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 18th International Symposium on Space Flight Dynamics CY OCT 11-15, 2004 CL Munich, GERMANY SP DLR German Space Operat Ctr, ESA European Space Operat Ctr AB On January 2, 2004, the STARDUST spacecraft flew by the short period comet P/Wild 2 at a distance of 237 km. The primary goal of the flyby was to collect samples of the coma and return them to Earth on January, 2006. An additional goal was to shutter images of the nucleus during the flyby. In order to meet these goals, the spacecraft had to be guided to a flyby about 250 km from the center of the nucleus with an accuracy of better than 50 km. This was accomplished by the use of standard radio navigation techniques, augmented by optical images of the comet using the onboard camera. This paper describes the optical navigation techniques used on approach to target the desired encounter conditions. The optical navigation phase of the mission began about a month prior to encounter when the first images of the comet were seen. Because of the dimness of the comet, plus unexpected problems with the camera due to contamination of the optics, individual frames could not be properly processed to get good navigation data. Techniques such as multiple frame co-addition were employed to boost the signal. The data was used to design a series of maneuvers to guide the spacecraft to its flyby target. At about 7 days prior to encounter, efforts to clean the camera paid off, and better signal to noise ratios were achieved. The final images for targeting were taken roughly 14 hours prior to encounter. These images indicated the previous targeting maneuver done at 2 days prior to encounter achieved the desired accuracy. The final flyby reconstruction showed the accuracy to have been better than 10 km. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Bhaskaran, S (reprint author), CALTECH, Jet Prop Lab, MS 264-280,4800 Oak Grove Dr, Pasadena, CA 91125 USA. NR 3 TC 6 Z9 6 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-859-X J9 ESA SP PUBL PY 2004 VL 548 BP 455 EP 460 PG 6 WC Engineering, Aerospace SC Engineering GA BBV58 UT WOS:000228033000072 ER PT S AU Martin-Mur, T Berry, D Flores-Amaya, F Folliard, J Kiehling, R Ogawa, M Pallaschke, S AF Martin-Mur, T Berry, D Flores-Amaya, F Folliard, J Kiehling, R Ogawa, M Pallaschke, S BE Montenbruck, O Battrick, B TI Exchange of standarized flight dynamics data SO PROCEEDINGS OF THE 18TH INTERNATIONAL SYMPOSIUM ON SPACE FLIGHT DYNAMICS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 18th International Symposium on Space Flight Dynamics CY OCT 11-15, 2004 CL Munich, GERMANY SP DLR German Space Operat Ctr, ESA European Space Operat Ctr AB Spacecraft operations require the knowledge of the vehicle trajectory and attitude and also that of other spacecraft or natural bodies. This knowledge is normally provided by the Flight Dynamics teams of the different space organizations and, as very often spacecraft operations involve more than one organization, this information needs to be exchanged between Agencies. This is why the Navigation Working Group within the CCSDS (Consultative Committee for Space Data Systems) has been instituted with the task of establishing standards for the exchange of Flight Dynamics data. This exchange encompasses trajectory data, attitude data, and tracking data. The Navigation Working Group includes regular members and observers representing the participating Space Agencies. Currently the group includes representatives from CNES, DLR, ESA, NASA and JAXA. This Working Group meets twice per year in order to devise standardized language, methods, and formats for the description and exchange of Navigation data. Early versions of some of these standards have been used to support mutual tracking of ESA and NASA interplanetary spacecraft, especially during the arrival of the 2003 missions to Mars. This paper provides a summary of the activities carried out by the group, briefly outlines the current and envisioned standards, describes the tests and operational activities that have been performed using the standards, and lists and discusses the lessons learned from these activities. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91104 USA. RP Martin-Mur, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91104 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-859-X J9 ESA SP PUBL PY 2004 VL 548 BP 537 EP 542 PG 6 WC Engineering, Aerospace SC Engineering GA BBV58 UT WOS:000228033000085 ER PT S AU Scharf, DP Hadaegh, FY Ploen, SR AF Scharf, DP Hadaegh, FY Ploen, SR GP acc TI A survey of spacecraft formation flying guidance and control (Part II): Control SO PROCEEDINGS OF THE 2004 AMERICAN CONTROL CONFERENCE, VOLS 1-6 SE PROCEEDINGS OF THE AMERICAN CONTROL CONFERENCE LA English DT Proceedings Paper CT American Control Conference CY JUN 30-JUL 02, 2004 CL Boston, MA SP Amer Automat Control Council, Int Federat Automat Control ID NONHOLONOMIC MOBILE ROBOTS; MEAN ORBIT ELEMENTS; RULE-BASED CONTROLS; MULTIPLE SPACECRAFT; INTERCONNECTED SYSTEMS; COORDINATED CONTROL; SATELLITES; STABILIZATION; STABILITY; ROTATION AB Formation flying is defined as a set of more than one spacecraft whose states are coupled through a common control law. This paper provides a comprehensive survey of spacecraft formation flying control (FFC), which encompasses design techniques and stability results for these coupled-state control laws. We divide the FFC literature into five FFC architectures: (i) Multiple-Input Multiple-Output, in which the formation is treated as a single multiple-input, multiple-output plant, (ii) Leader/Follower, in which individual spacecraft controllers are connected hierarchically, (iii) Virtual Structure, in which spacecraft are treated as rigid bodies embedded in an overall virtual rigid body, (iv) Cyclic, in which individual spacecraft controllers are connected non-hierarchically, and (v) Behavioral, in which multiple controllers for achieving different (and possibly competing) objectives are combined. This survey significantly extends an overview of the FFC literature provided by Lawton, which discussed the L/F, Virtual Structure and Behavioral architectures. We also include a brief history of the formation flying literature, and discuss connections between spacecraft FFC and other multi-vehicle control problems in the robotics and Automated Highway System literatures. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Scharf, DP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 137 TC 130 Z9 143 U1 3 U2 14 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0743-1619 BN 0-7803-8335-4 J9 P AMER CONTR CONF PY 2004 BP 2976 EP 2985 PG 10 WC Automation & Control Systems SC Automation & Control Systems GA BBC09 UT WOS:000224688300507 ER PT S AU Ploen, SR Hadaegh, FY Scharf, DP AF Ploen, SR Hadaegh, FY Scharf, DP GP acc TI Rigid body equations of motion for modeling and control of spacecraft formations - Part 1: Absolute equations of motion. SO PROCEEDINGS OF THE 2004 AMERICAN CONTROL CONFERENCE, VOLS 1-6 SE Proceedings of the American Control Conference LA English DT Proceedings Paper CT American Control Conference CY JUN 30-JUL 02, 2004 CL Boston, MA SP Amer Automat Control Council, Int Federat Automat Control AB In this paper, we present a tensorial (i.e., coordinate-free) derivation of the equations of motion of a formation consisting of N spacecraft each modeled as a rigid body. Specifically, using spatial velocities and spatial forces we demonstrate that the equations of motion for a single free rigid body (i.e., a single spacecraft) can be naturally expressed in four fundamental forms. The four forms of the dynamic equations include (1) motion about the system center-of-mass in terms of absolute rates-of-change, (2) motion about the system center-of-mass in terms of body rates of change, (3) motion about an arbitrary point fixed on the rigid body in terms of absolute rates-of-change, and (4) motion about an arbitrary point fixed on the rigid body in terms of body rates-of-change. We then introduce the spatial Coriolis dyadic and discuss how a proper choice of this non-unique tensor leads to dynamic models of formations satisfying the skew-symmetry property required by an important class of nonlinear tracking control laws. Next, we demonstrate that the equations of motion of the entire formation have the same structure as the equations of motion of an individual spacecraft. The results presented in this paper form the cornerstone of a coordinate-free modeling environment for developing dynamic models for various formation flying applications. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 13 TC 3 Z9 3 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0743-1619 BN 0-7803-8335-4 J9 P AMER CONTR CONF PY 2004 BP 3646 EP 3653 PG 8 WC Automation & Control Systems SC Automation & Control Systems GA BBC09 UT WOS:000224688300620 ER PT B AU Frederickson, AR AF Frederickson, AR GP IEEE TI Laboratory tests for spacecraft charging and discharging: From Hertz, Millikan and de Broglie to today's questions SO PROCEEDINGS OF THE 2004 IEEE INTERNATIONAL CONFERENCE ON SOLID DIELECTRICS, VOLS 1 AND 2 LA English DT Proceedings Paper CT 8th IEEE International Conference on Solid Dielectrics CY JUL 05-09, 2004 CL Toulouse, FRANCE SP IEEE Dielect & Elect Insulat Soc, Lab Genie Elect Toulouse, Alstom, CNRS, Univ Paul Sabatier, Toulouse III, DEIS, LGET C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Frederickson, AR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-8348-6 PY 2004 BP 916 EP 916 PG 1 WC Physics, Condensed Matter SC Physics GA BAS36 UT WOS:000223357100228 ER PT B AU Calle, CI Buhler, CR Mantovani, JG AF Calle, CI Buhler, CR Mantovani, JG GP IEEE TI Electrostatic charge generation on dielectric surfaces at low pressures SO PROCEEDINGS OF THE 2004 IEEE INTERNATIONAL CONFERENCE ON SOLID DIELECTRICS, VOLS 1 AND 2 LA English DT Proceedings Paper CT 8th IEEE International Conference on Solid Dielectrics CY JUL 05-09, 2004 CL Toulouse, FRANCE SP IEEE Dielect & Elect Insulat Soc, Lab Genie Elect Toulouse, Alstom, CNRS, Univ Paul Sabatier, Toulouse III, DEIS, LGET AB The surface charge generated on solid dielectrics placed in contact with granular materials at low gas pressures has been measured for several solid dielectrics. Induction sensors embedded in the dielectrics were used to measure the amount of charge that was induced on a metal electrode that had been exposed to some external distribution of electrostatic charge. These sensors have sensitivities in the picocoulomb per cm(2) range, achieved by adjusting circuit component values as well as the total electrode area. Environments such as the one described for these experiments are encountered on the surface of Mars. These studies serve to characterize the response of different dielectrics to the Martian environment, with applications to the near future exploration of the planet. C1 NASA, Kennedy Space Ctr, Electrostat & Surface Phys Lab, Kennedy Space Ctr, FL 32899 USA. RP Calle, CI (reprint author), NASA, Kennedy Space Ctr, Electrostat & Surface Phys Lab, Mail Code YA-C2-T, Kennedy Space Ctr, FL 32899 USA. NR 10 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-8348-6 PY 2004 BP 932 EP 935 PG 4 WC Physics, Condensed Matter SC Physics GA BAS36 UT WOS:000223357100231 ER PT B AU Liu, AK Zhao, YH Tang, TY Hsu, MK AF Liu, AK Zhao, YH Tang, TY Hsu, MK GP IEEE TI Nonlinear internal wave study during ASIAEX SO PROCEEDINGS OF THE 2004 INTERNATIONAL SYMPOSIUM ON UNDERWATER TECHNOLOGY LA English DT Proceedings Paper CT 4th International Symposium on Underwater Technology CY APR 20-23, 2004 CL Taipei, TAIWAN SP IEEE OES, Natl Taiwan Univ, Dept Engn Sci & Ocean Engn, IEEE OES Taipei Chapter, Univ Tokyo, Inst Ind Sci, Natl Sci Council ROC, Minist Educ ROC, Off Naval Res Int Field Off DE remote sensing; internal waves; shallow water acoustics ID CHINA SEAS; SULU SEA; EVOLUTION AB In recent Asian Seas International Acoustics Experiment (ASIAEX), extensive moorings have been deployed around the continental shelf break area in (lie northeast of South China Sea In May 2001. Simultaneous RADARSAT SAR images have been collected during the field test to integrate with the in-situ measurements front moorings, ship-board sensors, and CTD castings. Besides it provides synoptic Information, satellite imagery Is very useful for tracking the Internal waves, and locating surface fronts and mesoscale features. During ASIAEX In May 2001, many large internal waves were observed at the test area and were the major oceanic features for acoustic volume interaction. Based on the internal wave distribution maps compiled from satellite data, the wave crest can be as long as 200 km with amplitude of 100 in. Environmental parameters have been calculated based on extensive CTD casts data near the ASIAEX area. Nonlinear internal wave models have been applied to integrate and assimilate both SAR and mooring data. The shoaling, turning, and dissipation of large internal waves on the shelf break, elevation solitons, and wave-wave interaction have been studied and are very important issues for acoustic propagation. The internal wave effects on acoustic modal coupling has been implicated and discussed. C1 NASA, Goddard Space Flight Ctr, Oceans & Ice Branch, Greenbelt, MD 20771 USA. RP Liu, AK (reprint author), NASA, Goddard Space Flight Ctr, Oceans & Ice Branch, Greenbelt, MD 20771 USA. NR 16 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-8541-1 PY 2004 BP 231 EP 238 DI 10.1109/UT.2004.1405557 PG 8 WC Engineering, Ocean SC Engineering GA BBR41 UT WOS:000227356400033 ER PT B AU Goebel, M AF Goebel, M GP IEEE TI Breakdown characteristics and conditioning of carbon and refractory metal electrodes SO PROCEEDINGS OF THE 26TH INTERNATIONAL POWER MODULATOR SYMPOSIUM AND 2004 HIGH VOLTAGE WORKSHOP, CONFERENCE RECORD LA English DT Proceedings Paper CT 26th International Power Modulator Symposium/High Voltage Workshop CY MAY 23-26, 2004 CL San Francisco, CA SP IEEE Dielect & Elect Insulat Soc, IEEE Electron Devices Soc AB High voltage carbon and refractory metal electrodes employed in devices used in space, such as ion thrusters and traveling wave tubes, can be easily damaged by electrical breakdown and arcing events. Modification of the electrode surfaces due to these events can impact the voltage hold off capability of the surfaces, which could lead to additional arcing, further damage, and the potential for device failure. On the cathode-potential surface, the arc energy is deposited by all of the processes at the surface ultimately responsible for net electron emission, such as melting, vapor and particulate formation, sputtering, ion bombardment, etc. On the anode-potential surface, the energy is deposited from the plasma or electron stream that crosses the gap, which causes surface damage by local heating. In spite of this energy dependence on the damage, many systems that use arc discharges characterize the amount of material removed from the surfaces and the lifetime of the device for voltage hold-off by the amount of current that passes through the arc, or the "Coulomb-rating". The results of a series of tests that were per-formed on the voltage hold off capability and damage to carbon-carbon composite surfaces and molybdenum surfaces due to induced arcing will be presented and discussed. Damage to the surfaces was characterized by the field emission performance after the arc initiation and SEM photographs for the different energy and coulomb-transfer arc conditions. Both conditioning and damage to the surfaces were observed, and will be related to the characteristics of the electrical breakdown. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Goebel, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM dan.m.goebel@jpl.nasa.gov NR 3 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-8586-1 PY 2004 BP 1 EP 4 PG 4 WC Energy & Fuels; Engineering, Electrical & Electronic SC Energy & Fuels; Engineering GA BBZ41 UT WOS:000228358100001 ER PT S AU Howell, JT O'Neill, MJ Fork, RL AF Howell, JT O'Neill, MJ Fork, RL BE Lacoste, H Ouwehand, L TI Advanced receiver/converter experiments for laser wireless power transmission SO Proceedings of the 4th International Conference on Solar Power from Space - SPS '04, Together with the 5th International Conference on Wireless Power Transmission - WPT 5 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 4th International Conference on Solar Power from Space (SPS 04)/5th International Conference on Wireless Power Transmission (WPT 5) CY JUN 30-JUL 02, 2004 CL Granada, SPAIN SP European Space Agcy, Minist Ciencia & Tecnol, Ciemat, USEF, CDTI, EADS Space Transportat, DLR AB yFor several years NASA, ENTECH, and UAH have been working on various aspects of space solar power systems, some of which include four process elements: (1) space solar radiation collection and conversion to electrical power (2) conversion of this electrical power to laser radiation (3) wireless power transmission of this laser radiation to an end-use location (4) collection of the laser radiation and conversion to electrical power For the first element above, photovoltaic concentrator systems using ultra-light Fresnel lenses to focus space sunlight onto small solar cells have demonstrated significant performance, mass, and cost advantages over competing solar arrays. Recently, the photovoltaic concentrator approach has also been proposed for the fourth element, to provide similar performance, mass, and cost advantages over competing laser receiver/converters. This paper describes the new laser receiver/converter approach, including very encouraging test results on early-stage proof-of-concept prototype hardware. C1 NASA, George C Marshall Space Flight Ctr, Flight Projects Directorate, Huntsville, AL 35812 USA. RP Howell, JT (reprint author), NASA, George C Marshall Space Flight Ctr, Flight Projects Directorate, FD02, Huntsville, AL 35812 USA. NR 12 TC 10 Z9 10 U1 0 U2 2 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-878-6 J9 ESA SP PUBL PY 2004 VL 567 BP 187 EP 194 PG 8 WC Engineering, Aerospace; Energy & Fuels SC Engineering; Energy & Fuels GA BCI84 UT WOS:000229609600027 ER PT S AU Howell, J Carrington, C Day, G AF Howell, J Carrington, C Day, G BE Lacoste, H Ouwehand, L TI A 100 KW-class technology demonstrator for space solar power SO Proceedings of the 4th International Conference on Solar Power from Space - SPS '04, Together with the 5th International Conference on Wireless Power Transmission - WPT 5 SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 4th International Conference on Solar Power from Space (SPS 04)/5th International Conference on Wireless Power Transmission (WPT 5) CY JUN 30-JUL 02, 2004 CL Granada, SPAIN SP European Space Agcy, Minist Ciencia & Tecnol, Ciemat, USEF, CDTI, EADS Space Transportat, DLR AB A first step in the development of solar power from space is the flight demonstration of critical technologies. These fundamental technologies include efficient solar power collection and generation, power management and distribution, and thermal management. In addition, the integration and utilization of these technologies into a viable satellite bus could provide an energy-rich platform for a portfolio of payload experiments such as wireless power transmission (WPT). This paper presents the preliminary design of a concept for a 100 kW-class free-flying platform suitable for flight demonstration of Space Solar Power (SSP) technology experiments. C1 NASA, George C Marshall Space Flight Ctr, Adv Projects Off, Flight Projects Directorate, Huntsville, AL 35805 USA. RP Howell, J (reprint author), NASA, George C Marshall Space Flight Ctr, Adv Projects Off, Flight Projects Directorate, FD02,320 Sparkman Dr, Huntsville, AL 35805 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-878-6 J9 ESA SP PUBL PY 2004 VL 567 BP 225 EP 230 PG 6 WC Engineering, Aerospace; Energy & Fuels SC Engineering; Energy & Fuels GA BCI84 UT WOS:000229609600032 ER PT S AU Shrader, CR Titarchuk, LG AF Shrader, CR Titarchuk, LG BE Battrick, B TI Effects of comptonization by outflowing plasma in compact X-ray sources SO PROCEEDINGS OF THE 5TH INTEGRAL WORKSHOP ON THE INTEGRAL UNIVERSE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 5th INTEGRAL Workshop on The INTEGRAL Universe CY FEB 16-20, 2004 CL Bavarian Acad Sci, Munich, GERMANY SP European Space Acgy, DLR, MPE, INTA, NASA HO Bavarian Acad Sci ID REFLECTION; RADIATION AB We consider possible of effects of out-flowing plasma on the high-energy continuum spectra of accretion powered compact objects. We have developed an analytical formulation for the emergent spectrum of such systems, and performed model fitting on several Galactic X-ray binaries. Notably, Cyg X-3, is which is widely believed to be characterized by hot, dense circumstellar winds, provides a useful test case. Data from INTEGRAL and RXTE are included in our analysis. We further consider the possibility that the distortion of the power-law continuum above 10 keV may in some cases be explained by these spectral softening effects. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Shrader, CR (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 661, Greenbelt, MD 20771 USA. NR 12 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-863-8 J9 ESA SP PUBL PY 2004 VL 552 BP 381 EP 384 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR77 UT WOS:000227471700067 ER PT S AU Sturner, SJ Forot, M Laurent, P AF Sturner, SJ Forot, M Laurent, P BE Battrick, B TI Observations of PSR B1509-58 using integral core program data SO PROCEEDINGS OF THE 5TH INTEGRAL WORKSHOP ON THE INTEGRAL UNIVERSE SE ESA Special Publications LA English DT Proceedings Paper CT 5th INTEGRAL Workshop on The INTEGRAL Universe CY FEB 16-20, 2004 CL Bavarian Acad Sci, Munich, GERMANY SP European Space Acgy, DLR, MPE, INTA, NASA HO Bavarian Acad Sci DE pulsars; individual; PSR; B1509-58; Gamma rays; observations ID GAMMA-RAY PULSARS; SPECTRUM; SPECTROMETER; TELESCOPE; CASCADES; EMISSION; CATALOG; SPI AB We present spectral and imaging results from the analysis of the first year of INTEGRAL Core Program Data for the pulsar PSR B1509-58 and its associated supernova remnant MSH 15-52. PSR B1509-58 is a gamma-ray emitting, rotation-powered pulsar with a period of congruent to 150 ms and a characteristic age of roughly 1600 years. This pulsar is unusual among the gamma-ray pulsars in that its gamma-ray spectrum is cutoff at the lowest energy (similar to 10-30 MeV) and it has the highest surface magnetic field strength (1.54 x 10(13) G). We find that IBIS/ISGRI and SPI detect PSR B1509-58/MSH 15-52 up to similar to 200 keV. The spectral shape and flux level are in agreement with previous results C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sturner, SJ (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. RI laurent, philippe/E-6211-2013 NR 24 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-863-8 J9 ESA SPEC PUBL PY 2004 VL 552 BP 479 EP 482 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR77 UT WOS:000227471700088 ER PT S AU Sturner, SJ Beckmann, V Bykov, A Lebrun, F Terrier, R AF Sturner, SJ Beckmann, V Bykov, A Lebrun, F Terrier, R BE Battrick, B TI Integral studies of nonthermal emission from the supernova remnants Cassiopeia Aa, CTA 1, and MSH 11-61A SO PROCEEDINGS OF THE 5TH INTEGRAL WORKSHOP ON THE INTEGRAL UNIVERSE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 5th INTEGRAL Workshop on The INTEGRAL Universe CY FEB 16-20, 2004 CL Bavarian Acad Sci, Munich, GERMANY SP European Space Acgy, DLR, MPE, INTA, NASA HO Bavarian Acad Sci DE ISM; supernova remnants; gamma rays; observations ID X-RAY-EMISSION; ACCELERATION; PULSARS; SEARCH; SHELL AB We present the initial results from our study of the nonthermal continuum emission from the supernova remnants Cassiopeia A, MSH 11-61A, and CTA 1. We used the INTEGRAL Core Program data to conduct this study. During the INTEGRAL mission a significant fraction of the total observing time (e.g. 35% in year one) is allocated to the Core Program and is analyzed under the auspices of the INTEGRAL Science Working Team. We report no statistically significant detections thus far but we will continue to analyze the data as more is taken. The results so far are consistent with previous measurements from e.g. RXTE and ASCA. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sturner, SJ (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. RI Bykov, Andrei/E-3131-2014 NR 22 TC 1 Z9 1 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-863-8 J9 ESA SP PUBL PY 2004 VL 552 BP 497 EP 500 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR77 UT WOS:000227471700090 ER PT S AU Beckmann, V Gehrels, N Favre, P Courvoisier, TJL Walter, R Malzac, J Petrucci, PO AF Beckmann, V Gehrels, N Favre, P Courvoisier, TJL Walter, R Malzac, J Petrucci, PO BE Battrick, B TI NGC 4388 - Spectral studies of the first Seyfert 2 seen by integral SO PROCEEDINGS OF THE 5TH INTEGRAL WORKSHOP ON THE INTEGRAL UNIVERSE SE ESA Special Publications LA English DT Proceedings Paper CT 5th INTEGRAL Workshop on The INTEGRAL Universe CY FEB 16-20, 2004 CL Bavarian Acad Sci, Munich, GERMANY SP European Space Acgy, DLR, MPE, INTA, NASA HO Bavarian Acad Sci DE galaxies : active; galaxies : individual (NGC 4388); gamma rays : observations; X-rays : galaxies ID X-RAY ASTRONOMY; GALAXY NGC 4388; VIRGO CLUSTER; XMM-NEWTON; BEPPOSAX; REFLECTION; SPECTROMETER; VARIABILITY; SOFTWARE; MISSION AB We present first INTEGRAL and XMM-Newton observations of a Seyfert galaxy, the type 2 AGN NGC 4388. Several INTEGRAL observations performed in 2003 allow us to study the spectrum in the 20 - 300 keV range. In addition two XMM-Newton observations give detailed insight into the 0.2 - 10 keV emission. Comparison with previous observations by BeppoSAX, SIGMA and CGRO/OSSE show that the overall spectrum from soft X-rays up to the gamma-rays can be described by a highly absorbed (N-H similar or equal to 2.7 x 10(23) cm(-2)) and variable nonthermal component in addition to constant nonabsorbed thermal emission (T similar or equal to 0.8keV) of low abundance (Z similar to 7% Z(circle dot)), plus a constant Fe K alpha and K beta line. The hard X-ray component is well described by a simple power law with a mean photon index of Gamma = 1.7. During the INTEGRAL observations the flux at 100 keV increased by a factor of 1.5. The analysis of XMM-Newton data implies that the emission below 3 keV is decoupled from the AGN and probably due to extended emission as seen in Chandra observations. The constant iron line emission is apparently also decoupled from the direct emission of the central engine and likely to be generated in the obscuring material, e.g. in the molecular torus. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. NR 35 TC 1 Z9 1 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-863-8 J9 ESA SPEC PUBL PY 2004 VL 552 BP 535 EP 542 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR77 UT WOS:000227471700097 ER PT S AU Bloser, PF Hunter, SD AF Bloser, PF Hunter, SD BE Battrick, B TI Pixelized gas micro-well detectors for advanced gamma-ray telescopes SO PROCEEDINGS OF THE 5TH INTEGRAL WORKSHOP ON THE INTEGRAL UNIVERSE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 5th INTEGRAL Workshop on The INTEGRAL Universe CY FEB 16-20, 2004 CL Bavarian Acad Sci, Munich, GERMANY SP European Space Acgy, DLR, MPE, INTA, NASA HO Bavarian Acad Sci DE gamma-ray astronomy; Compton telescopes; pair telescopes; gas detectors; Geant4 simulations AB We describe possible applications of pixelized micro-well detectors (PMWDs) as three-dimensional charged particle trackers in advanced gamma-ray telescope concepts. A micro-well detector consists of an array of individual micro-patterned gas proportional counters opposite a planar drift electrode. When combined with pixelized thin film transistor (TFT) array readouts, large gas volumes may be imaged with very good spatial and energy resolution at reasonable cost. The third dimension is determined by timing the drift of the ionization electrons. The primary advantage of this technique is the very low scattering that the charged particles experience in a gas tracking volume, and the very accurate determination of the initial particle momenta that is thus achieved. We consider two applications of PMWDs to gamma-ray astronomy: 1) A tracker for an Advanced Compton Telescope (ACT) in which the recoil electron from the initial Compton scatter may be accurately tracked, greatly reducing the telescope's point spread function and increasing its polarization sensitivity; and 2) an Advanced Pair Telescope (APT) whose angular resolution is limited primarily by the nuclear recoil and which achieves useful polarization sensitivity near 100 MeV. We have performed Geant4 simulations of both these concepts to estimate their angular resolution and sensitivity for reasonable mission designs. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bloser, PF (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Hunter, Stanley/D-2942-2012 NR 8 TC 0 Z9 0 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-863-8 J9 ESA SP PUBL PY 2004 VL 552 BP 765 EP 768 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR77 UT WOS:000227471700140 ER PT S AU Gehrels, N AF Gehrels, N CA Swift Team BE Battrick, B TI The swift gamma-ray burst mission SO PROCEEDINGS OF THE 5TH INTEGRAL WORKSHOP ON THE INTEGRAL UNIVERSE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 5th INTEGRAL Workshop on The INTEGRAL Universe CY FEB 16-20, 2004 CL Bavarian Acad Sci, Munich, GERMANY SP European Space Acgy, DLR, MPE, INTA, NASA HO Bavarian Acad Sci ID 28 FEBRUARY 1997; AFTERGLOW; REDSHIFT AB Swift is a first-of-its-kind multiwavelength transient observatory for GRB astronomy. It has the optimum capabilities for the next breakthroughs in determining the origin of GRBs and their afterglows, as well as using bursts to probe the early Universe. Swift will also perform the first sensitive hard X-ray survey of the sky. The mission is being developed by an international collaboration and consists of three instruments, the Burst Alert Telescope (BAT), the X-ray Telescope (XRT), and the Ultraviolet and Optical Telescope (UVOT). The BAT, a wide-field gamma-ray detector, will detect > 100 GRBs per year with a sensitivity 5 times that of BATSE. The sensitive narrow-field XRT and UVOT will be autonomously slewed to the burst location in 20 to 70 seconds to determine 0.3-5.0 arcsec positions and perform optical, UV, and X-ray spectrophotometry. Strong education/public outreach and follow-up programs will help to engage the public and astronomical community. The Swift launch is planned for in 2004. C1 Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gehrels, N (reprint author), Goddard Space Flight Ctr, Mail Code 661, Greenbelt, MD 20771 USA. NR 13 TC 2 Z9 2 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-863-8 J9 ESA SP PUBL PY 2004 VL 552 BP 777 EP 780 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR77 UT WOS:000227471700143 ER PT S AU Teegarden, BJ Jean, P Weidenspointner, G Knodlseder, J Skinner, GK Von Ballmoos, P Shrader, C Sturner, S Watanabe, K AF Teegarden, BJ Jean, P Weidenspointner, G Knodlseder, J Skinner, GK Von Ballmoos, P Shrader, C Sturner, S Watanabe, K BE Battrick, B TI Characterization and prediction of the SPI background SO PROCEEDINGS OF THE 5TH INTEGRAL WORKSHOP ON THE INTEGRAL UNIVERSE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 5th INTEGRAL Workshop on The INTEGRAL Universe CY FEB 16-20, 2004 CL Bavarian Acad Sci, Munich, GERMANY SP European Space Acgy, DLR, MPE, INTA, NASA HO Bavarian Acad Sci AB The INTEGRAL Spectrometer (SPI), like most gamma-ray instruments, is background dominated, Signal-to-background ratios of a few percent are typical. The background is primarily due to interactions of cosmic rays in the instrument and spacecraft, and it characteristically varies by +/- 5% on time scales of days or longer. This variation is caused mainly by fluctuations in the interplanetary magnetic field that modulate the cosmic-ray intensity. To achieve the maximum performance from SPI it is essential to have a high quality model of the background that can predict its value to a fraction of a percent. In this paper we characterize the background and its variability, explore various models, and evaluate the accuracy of their predictions. Particular emphasis is placed on the 511-keV background as electron-positron annihilation radiation is one of the prime scientific objectives of INTEGRAL. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Teegarden, BJ (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. NR 4 TC 2 Z9 2 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-863-8 J9 ESA SP PUBL PY 2004 VL 552 BP 819 EP 822 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR77 UT WOS:000227471700153 ER PT S AU Shrader, CR AF Shrader, CR CA INTEGRAL-SPI Collaboration BE Battrick, B TI XSPEC 12: Capabilities for coded-mask spectral analysis SO PROCEEDINGS OF THE 5TH INTEGRAL WORKSHOP ON THE INTEGRAL UNIVERSE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 5th INTEGRAL Workshop on The INTEGRAL Universe CY FEB 16-20, 2004 CL Bavarian Acad Sci, Munich, GERMANY SP European Space Acgy, DLR, MPE, INTA, NASA HO Bavarian Acad Sci AB The instruments onboard INTEGRAL, which utilize the coded-mask imaging technique, pose new technical challenges to the traditional forward-folding spectroscopy. We describe some functionality that has been incorporated in to the version 12 XSPEC release to address these challenges, such as the capability to simultaneously fit multiple sources and backgrounds with distinct physical models and response matrices within a single FoV. Examples using INTEGRAL/SPI data obtained during the performance verification phase and Crab campaign are presented and discussed. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Shrader, CR (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 661, Greenbelt, MD 20771 USA. NR 5 TC 2 Z9 2 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-863-8 J9 ESA SP PUBL PY 2004 VL 552 BP 901 EP 904 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR77 UT WOS:000227471700172 ER PT S AU Goullioud, R Shen, TPJ Catanzarite, JH AF Goullioud, R Shen, TPJ Catanzarite, JH BE Warmbein, B TI Wide angle astrometric demonstration on the micro-aresecond metrology testbed for the space interferometry mission SO PROCEEDINGS OF THE 5TH INTERNATIONAL CONFERENCE ON SPACE OPTICS (ICSO 2004) SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 5th International Conference on Space Optics (ICSO 2004) CY MAR 30-JUL 02, 2004 CL Toulouse, FRANCE SP CNES, ESA, SFO, SFPT AB The Space Interferometry Mission (SIM) requires fringe measurements to the level of picometers in order to produce astrometric data at the micro-arc-second level. To be more specific, it is necessary to measure both the position of the starlight central fringe and the change in the internal optical path of the interferometer to a few hundreds of picometers. The internal path is measured with a small heterodyne metrology beam, whereas the starlight fringe position is estimated with a CCD sampling a large concentric annular beam. One major challenge for SIM is to align the metrology beam with the starlight beam to keep the consistency between these two sensors at the system level while articulating the instrument optics over the field of view, The Micro-Arcsecond Metrology testbed (MAM) developed at the Jet Propulsion Laboratory, California Institute of Technology, features an optical interferometer with a white light source, all major optical components of a stellar interferometer and heterodyne metrology sensors. The setup is installed inside a large vacuum chamber in order to mitigate the atmospheric and thermal disturbances. Wide angle astrometric observations are simulated by articulating the optics over the 15 degrees field of regard to generate multiple artificial stars. Recent data show agreement between the metrology and starlight paths to 350pm in the full wide angle field of view of SIM. This paper describes the MAM optical setup, the observation process, the current data and how the performance relates to SIM. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Goullioud, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-865-4 J9 ESA SP PUBL PY 2004 VL 554 BP 485 EP 492 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing; Optics SC Engineering; Instruments & Instrumentation; Remote Sensing; Optics GA BBA87 UT WOS:000224457000066 ER PT S AU Peters, RD Lay, OP Dubovitsky, S Burger, JP Jeganathan, M AF Peters, RD Lay, OP Dubovitsky, S Burger, JP Jeganathan, M BE Warmbein, B TI MSTAR: An absolute metrology sensor with sub-micron accuracy for space-based applications SO PROCEEDINGS OF THE 5TH INTERNATIONAL CONFERENCE ON SPACE OPTICS (ICSO 2004) SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 5th International Conference on Space Optics (ICSO 2004) CY MAR 30-JUL 02, 2004 CL Toulouse, FRANCE SP CNES, ESA, SFO, SFPT ID FREQUENCY STABILIZATION; LASER; INTERFEROMETRY; RESOLUTION; PRECISION; SYSTEM AB The MSTAR sensor (Modulation Sideband Technology for Absolute Ranging) is a new system for measuring absolute distance, capable of resolving the integer cycle ambiguity of standard interferometers, and making it possible to measure distance with sub-nanometer accuracy. The sensor uses a single laser in conjunction with fast phase modulators and low-frequency detectors. We describe the design of the system - the principle of operation, the metrology source, beam-launching optics, and signal processing and show results for target distances up to I meter. We then demonstrate how the system can be scaled to kilometer-scale distances and used for space-based applications. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Peters, RD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 17 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-865-4 J9 ESA SP PUBL PY 2004 VL 554 BP 493 EP 500 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing; Optics SC Engineering; Instruments & Instrumentation; Remote Sensing; Optics GA BBA87 UT WOS:000224457000067 ER PT S AU Halverson, PRG Alvarez-Salazar, O Azizi, A Dekens, F Nemati, B Zhao, F AF Halverson, PRG Alvarez-Salazar, O Azizi, A Dekens, F Nemati, B Zhao, F BE Warmbein, B TI Progress towards picometer accuracy laser metrology for the space interferometry mission - update SO PROCEEDINGS OF THE 5TH INTERNATIONAL CONFERENCE ON SPACE OPTICS (ICSO 2004) SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 5th International Conference on Space Optics (ICSO 2004) CY MAR 30-JUL 02, 2004 CL Toulouse, FRANCE SP CNES, ESA, SFO, SFPT ID GAUGES; KITE AB The Space Interferometry Mission, scheduled for launch in 2010, is an optical stellar interferometer with a 10 meter baseline capable of micro-arcsecond accuracy astrometry. A mission-enabling technology development program conducted at JPL, has yielded the heterodyne interferometric displacement metrology gauges required for monitoring the geometry of optical components of the stellar interferometer, and for maintaining stable starlight fringes. The gauges have <20 picometer linearity, <10 micron absolute accuracy, are stable to <200 pm over the typical SIM observation periods (similar to1 hour), have the ability to track the motion of mirrors over several meters. We discuss the technology that led to this level of performance: low-cross-talk, low thermal coefficient optics and electronics, active optical alignment, a dual wavelength laser source, and a continuously averaging, high data rate phase measurement technique. These technologies have wide applicability and are already being used outside of the SIM project, such as by the James Webb Space telescope (JWST) and Terrestrial Planet Finder (TPF) missions. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Halverson, PRG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 15 TC 2 Z9 2 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-865-4 J9 ESA SP PUBL PY 2004 VL 554 BP 515 EP 522 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing; Optics SC Engineering; Instruments & Instrumentation; Remote Sensing; Optics GA BBA87 UT WOS:000224457000070 ER PT S AU Halverson, PG Loya, FM AF Halverson, PG Loya, FM BE Warmbein, B TI Signal processing for order 10 PM accuracy displacement metrology in real-world scientific applications SO PROCEEDINGS OF THE 5TH INTERNATIONAL CONFERENCE ON SPACE OPTICS (ICSO 2004) SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 5th International Conference on Space Optics (ICSO 2004) CY MAR 30-JUL 02, 2004 CL Toulouse, FRANCE SP CNES, ESA, SFO, SFPT AB Projects such as the Space Interferometry Mission (SIM) [1] and Terrestrial Planet Finder (TPF) [2] rely heavily on sub-nanometer accuracy metrology systems to define their optical paths and geometries. The James Web Space Telescope (JWST) is using this metrology in a cryogenic dilatometer for characterizing material properties (thermal expansion, creep) of optical materials. For all these projects, a key issue has been the reliability and stability of the electronics that convert displacement metrology signals into real-time distance determinations. A particular concern is the behavior of the electronics in situations where laser heterodyne signals are weak or noisy and subject to abrupt Doppler shifts due to vibrations or the slewing of motorized optics. A second concern is the long-term (hours to days) stability of the distance measurements under conditions of drifting laser power and ambient temperature. This paper describes heterodyne displacement metrology gauge signal processing methods that achieve satisfactory robustness against low signal strength and spurious signals, and good long-term stability. We have a proven displacement-measuring approach that is useful not only to space-optical projects at JPL, but also to the wider field of distance measurements. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Halverson, PG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 12 TC 1 Z9 1 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-865-4 J9 ESA SP PUBL PY 2004 VL 554 BP 571 EP 577 PG 7 WC Engineering, Aerospace; Instruments & Instrumentation; Remote Sensing; Optics SC Engineering; Instruments & Instrumentation; Remote Sensing; Optics GA BBA87 UT WOS:000224457000078 ER PT S AU Johnston, AH Miyahira, TF AF Johnston, AH Miyahira, TF BE Sharp, R Fletcher, K TI Displacement damage characterization of laser diodes SO PROCEEDINGS OF THE 7TH EUROPEAN CONFERENCE ON RADIATION AND ITS EFFECTS ON COMPONENTS AND SYSTEMS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 7th European Conference on Radiation and Its Effects on Components and Systems CY SEP 15-19, 2003 CL Noordwijk, NETHERLANDS SP European Space Agcy ID PROTON DAMAGE; DEGRADATION; GAAS AB Displacement damage effects in laser diodes are discussed. Differences in the annealing properties of proton and neutron damage were observed which are attributed to the different microscopic structure of the damaged regions from the two types of particles. The annealing properties affect testing and characterization methods, and limit the ability to normalize damage in different environments using non-ionizing energy loss (NEEL). Key parameters for laser degradation include threshold current, slope efficiency, and the current dependence of optical power output near threshold where the laser shifts from light-emitting diode to laser operation. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Johnston, AH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 19 TC 1 Z9 1 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-846-8 J9 ESA SP PUBL PY 2004 VL 536 BP 3 EP 9 PG 7 WC Engineering, Aerospace; Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BBQ26 UT WOS:000227039100001 ER PT S AU Kniffin, SD Reed, RA Marshall, PW Howard, JW Kim, HS Schepis, JP AF Kniffin, SD Reed, RA Marshall, PW Howard, JW Kim, HS Schepis, JP BE Sharp, R Fletcher, K TI The impact of system configuration on device radiation damage testing of optical components SO PROCEEDINGS OF THE 7TH EUROPEAN CONFERENCE ON RADIATION AND ITS EFFECTS ON COMPONENTS AND SYSTEMS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 7th European Conference on Radiation and Its Effects on Components and Systems CY SEP 15-19, 2003 CL Noordwijk, NETHERLANDS SP European Space Agcy ID LIGHT-EMITTING-DIODES; INDUCED TRANSIENTS; ENERGY-DEPENDENCE; PROTON DAMAGE; OPTOCOUPLERS; DEGRADATION; UPSET AB We report on the significant impact that system configuration had on the radiation damage testing of a light emitting diode-phototransistor pair for the Hubble Space Telescope Wide Field/Planetary Camera 2. C1 NASA, Orbital Sci Corp, Dulles, VA USA. RP Kniffin, SD (reprint author), NASA, Orbital Sci Corp, Dulles, VA USA. NR 16 TC 0 Z9 0 U1 0 U2 1 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-846-8 J9 ESA SP PUBL PY 2004 VL 536 BP 17 EP 21 PG 5 WC Engineering, Aerospace; Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BBQ26 UT WOS:000227039100003 ER PT S AU Marshall, PW Wiley, PT Prusia, RN Rash, GD Kirn, H LaBel, KA AF Marshall, PW Wiley, PT Prusia, RN Rash, GD Kirn, H LaBel, KA BE Sharp, R Fletcher, K TI Proton-induced bit error studies in a 10 gigabit per second fiber optic link SO PROCEEDINGS OF THE 7TH EUROPEAN CONFERENCE ON RADIATION AND ITS EFFECTS ON COMPONENTS AND SYSTEMS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 7th European Conference on Radiation and Its Effects on Components and Systems CY SEP 15-19, 2003 CL Noordwijk, NETHERLANDS SP European Space Agcy AB We describe a stand-alone experiment with autonomous error checking and logging used to acquire proton induced bit error response of a 10 Gbps multi-mode fiber optic data link operating over a 100 meter fiber length. Comparisons with previously tested lower data rate data links indicate the primary source of bit errors arise in the link receiver's photodiode. The serial 10 Gbps results show relatively lower Bit Error Rate (BER) sensitivity to 63 MeV protons. Proton BER results of supporting high speed bipolar multiplexer and demultiplexer circuitry are also presented. C1 NASA, GSFC, Brookneal, VA 24528 USA. RP Marshall, PW (reprint author), NASA, GSFC, 7655 Hat Creek Rd, Brookneal, VA 24528 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-846-8 J9 ESA SP PUBL PY 2004 VL 536 BP 23 EP 26 PG 4 WC Engineering, Aerospace; Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BBQ26 UT WOS:000227039100004 ER PT S AU Patterson, JD Edmonds, LD AF Patterson, JD Edmonds, LD BE Sharp, R Fletcher, K TI Automating the modeling of the see cross section's angular dependence SO PROCEEDINGS OF THE 7TH EUROPEAN CONFERENCE ON RADIATION AND ITS EFFECTS ON COMPONENTS AND SYSTEMS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 7th European Conference on Radiation and Its Effects on Components and Systems CY SEP 15-19, 2003 CL Noordwijk, NETHERLANDS SP European Space Agcy ID 3-DIMENSIONAL SIMULATION; UPSET; ERRORS AB An algorithm that automates the application of the alpha law in any SEE analysis is presented. This automation is essential for the widespread acceptance of the sophisticated cross section angular dependence model. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Patterson, JD (reprint author), CALTECH, Jet Prop Lab, Mail Stop 303-220,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-846-8 J9 ESA SP PUBL PY 2004 VL 536 BP 217 EP 223 PG 7 WC Engineering, Aerospace; Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BBQ26 UT WOS:000227039100034 ER PT S AU Scheick, L Novak, F AF Scheick, L Novak, F BE Sharp, R Fletcher, K TI Hot pixel generation in active pixel sensors: Dosimetric and microdosimetric response SO PROCEEDINGS OF THE 7TH EUROPEAN CONFERENCE ON RADIATION AND ITS EFFECTS ON COMPONENTS AND SYSTEMS SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 7th European Conference on Radiation and Its Effects on Components and Systems CY SEP 15-19, 2003 CL Noordwijk, NETHERLANDS SP European Space Agcy ID ARRAYS AB The dosimetric and microdosimetric response of an active pixel sensor is analyzed. The shift in dark current before and after irradiation is the metric under study. Heavy ions are seen to damage the pixel in much the same way as proton radiation, i.e., displacement damage is the dominant mechanism. A rate of singularly highly dosed cells, i.e. hot pixels, is calculated from the distribution of dosed cells. The probability of a hot pixel is seen to exhibit behavior that is not typical of other microdose effects. The cross section of hot pixels is seen to increase with increasing NIEL. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Scheick, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 15 TC 0 Z9 0 U1 1 U2 1 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-846-8 J9 ESA SP PUBL PY 2004 VL 536 BP 471 EP 478 PG 8 WC Engineering, Aerospace; Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BBQ26 UT WOS:000227039100074 ER PT B AU Gledhill, C David, A AF Gledhill, C David, A BE Creswell, RL TI Survey of fish assemblages and habitat within two marine protected areas on the West Florida shelf SO PROCEEDINGS OF THE FIFTY-FIFTH ANNUAL GULF AND CARIBBEAN FISHERIES INSTITUTE LA English DT Proceedings Paper CT 55th Annual Meeting of the Gulf-and-Caribbean-Fishieries-Institute CY NOV 11-15, 2002 CL Xel Ha, MEXICO SP Gulf & Caribbean Fisheries Inst, CYTED CONACyT, ECOSUR, Govt Burmuda, Caribbean Fisheries Management Council, FL Fish & Wildlife Conservat Commiss, FL Sea Grant Program, Environm Def, Soc Conservat Reef Fish Aggregat, Nat Conservancy, Natl Ocean & Atmospher Adm, Natl Marine Fisheries Serv DE Gulf of Mexico; marine protected area; reef fish ID GROUPERS AB The Madison-Swanson and Steamboat Lumps MPAs were established by the Gulf of Mexico Fishery Management Council in 1999 to protect spawning aggregations of groupers. The primary goals of this project were to: i) Establish baseline estimates of fish abundance, especially for species of groupers and snappers; ii) Describe significant habitat features in the Madison-Swanson and Steamboat Lumps MPAs; and, iii) Analyze the relationship between habitat and species assemblages. The secondary objective was to locate spawning aggregations of gag (Mycteroperca microlepis), and scamp (Mycteroperca phenax). Side scan mosaics and multibeam bathymetry were used to stratify each MPA based upon benthic topography and geology. The Madison-Swanson, and Steamboat Lumps MPAs were surveyed during 5 cruises between February, 2001 and May, 2002. Gear employed during the surveys included stationary video camera arrays, (Hi-8 cameras or digital cameras), chevron fish traps, and an ROV. Spawning aggregations of gag and/or scamp were confirmed within the Madison-Swanson MPA in 2001 and 2002. Species assemblages varied with habitat. At sites along ridges and rocky outcrops, species observed included gag, scamp, red grouper (Epinephelus morio), snowy grouper (Epinephelus niveatus), speckled hind (Epinephelus drummondhayi), red snapper (Lutjanus campechanus), silk snapper (Luyanus vivanus), vermilion snapper (Rhomboplites aurorubens), red porgy (Pagruspagrus), knobbed porgy (Calamus nodosus), gray triggerfish (Balistes capriscus), and greater amberjack (Seriola dumerili). At sites on sandy substrates, species observed included honeycomb moray (Gymnothorax saxicola), bank sea bass (Centropristis ocyurus), and bandtail puffer (Sphoeroides spengleri). C1 Natl Marine Fisheries Serv, Pascagoula Lab, Pascagoula, MS 39567 USA. RP Gledhill, C (reprint author), Natl Marine Fisheries Serv, Pascagoula Lab, 3209 Freder St, Pascagoula, MS 39567 USA. NR 7 TC 1 Z9 1 U1 1 U2 8 PU GULF CARIBBEAN FISHERIES INST GCFI PI FT PIERCE PA 56OO US HIGHWAY 1 N, FT PIERCE, FL 34946 USA PY 2004 BP 614 EP 625 PG 12 WC Fisheries SC Fisheries GA BBB34 UT WOS:000224516900051 ER PT S AU Fischman, MA Le, C Rosen, PA AF Fischman, MA Le, C Rosen, PA GP IEEE TI A digital beamforming processor for the joint DoD/NASA space based radar mission SO PROCEEDINGS OF THE IEEE 2004 RADAR CONFERENCE SE Radar Conference LA English DT Proceedings Paper CT 2004 IEEE Radar Conference CY APR 26-29, 2004 CL PHILADELPHIA, PA SP IEEE Philadelphia Sect, IEEE Aerosp & Elect Syst Soc AB The Space Based Radar (SBR) program includes a joint technology demonstration between NASA and the Air Force to design a low-earth orbiting, 2x50 m L-band (1.26 GRz) radar system for both Earth science and intelligence-related observations. A key subsystem aboard SBR is the electronicatly-steerable digital beamformer (DBF) network that interfaces between 32 smaller sub-antenna panels in the array and the on-board processing electronics for Synthetic Aperture Radar (SAR) and Moving Target Indication (MTI). In this paper, we describe the development of a field-programmable gate array (FPGA) based DBF processor for handling the algorithmically simple yet computationally intensive inner-product operations for wideband, coherent beamforming across the 50 m length of the array. The core functions of the DBF-the CORDIC (Coordinate Rotation Digital Computer) phase shifters and combiners-have been designed in the Verilog hardware description language and implemented onto a high-density Xilinx Virtex II FPGA. The design takes full advantage of the massively parallel architecture of the Virtex H logic slices to achieve real-time processing at an input data rate of 25.6 Gbit/s. Tests with an antenna array simulator demonstrate that the beamformer performance metrics (0.07degrees rms phase precision per channel, -39.0 dB peak sidelobe level) will meet the system-level requirements for SAR and MTI operating modes. C1 CALTECH, Jet Prop Lab, Radar Sci & Engn Sect, Pasadena, CA 91109 USA. RP Fischman, MA (reprint author), CALTECH, Jet Prop Lab, Radar Sci & Engn Sect, 4800 Oak Grove Dr,M-S 300-241, Pasadena, CA 91109 USA. NR 7 TC 10 Z9 10 U1 1 U2 3 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1097-5764 J9 RADAR CONF PY 2004 BP 9 EP 14 DI 10.1109/NRC.2004.1316387 PG 6 WC Remote Sensing; Physics, Applied; Telecommunications SC Remote Sensing; Physics; Telecommunications GA BAE91 UT WOS:000221923200003 ER PT S AU Le, C Chan, S Cheng, F Fang, W Fischman, M Hensley, S Johnson, R Jourdan, M Marina, M Parham, B Rogez, F Rosen, P Shah, B Taft, S AF Le, C Chan, S Cheng, F Fang, W Fischman, M Hensley, S Johnson, R Jourdan, M Marina, M Parham, B Rogez, F Rosen, P Shah, B Taft, S GP IEEE TI Onboard FPGA-based SAR processing for future spaceborne systems SO PROCEEDINGS OF THE IEEE 2004 RADAR CONFERENCE SE Radar Conference LA English DT Proceedings Paper CT 2004 IEEE Radar Conference CY APR 26-29, 2004 CL PHILADELPHIA, PA SP IEEE Philadelphia Sect, IEEE Aerosp & Elect Syst Soc AB We present a real-time high-performance and fault-tolerant FPGA-based hardware architecture for the processing of synthetic aperture radar (SAR) images in future spaceborne system. In particular, we will discuss the integrated design approach, from top-level algorithm specifications and system requirements, design methodology, functional verification and performance validation, down to hardware design and implementation. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Le, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 8 TC 12 Z9 13 U1 2 U2 4 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1097-5764 J9 RADAR CONF PY 2004 BP 15 EP 20 DI 10.1109/NRC.2004.1316388 PG 6 WC Remote Sensing; Physics, Applied; Telecommunications SC Remote Sensing; Physics; Telecommunications GA BAE91 UT WOS:000221923200004 ER PT S AU McWatters, D Freedman, A Michel, T Cable, V AF McWatters, D Freedman, A Michel, T Cable, V GP IEEE TI Antenna auto-calibration and metrology approach for the AFRL/JPL space based radar SO PROCEEDINGS OF THE IEEE 2004 RADAR CONFERENCE SE Radar Conference LA English DT Proceedings Paper CT 2004 IEEE Radar Conference CY APR 26-29, 2004 CL PHILADELPHIA, PA SP IEEE Philadelphia Sect, IEEE Aerosp & Elect Syst Soc AB The Air Force Research Laboratory (AFRL) and the Jet Propulsion Laboratory (JPL) are collaborating in the technology development for a space based radar (SBR) system that would feature a large aperture lightweight antenna for a joint mission later in this decade. This antenna system is a 50m x 2m electronically steerable phased array in L-band (1260 MHz center frequency, 80 MHz bandwidth) and contains 384 x 12 Transmit/Receive modules. The radar is designed to operate in a variety of modes including Synthetic Aperture Radar (SAR) and Moving Target Indication (MTI). Stringent requirements are placed on phase center knowledge and antenna sidelobe levels during a data take, in the presence of temperature changes due to the orbital thermal environment, self heating, spacecraft platform vibrations, and mechanical deformation. We present an auto-calibration and metrology system concept to correct for phase errors and mechanical deformation during the mission. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP McWatters, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 8 TC 2 Z9 3 U1 0 U2 3 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1097-5764 J9 RADAR CONF PY 2004 BP 21 EP 26 DI 10.1109/NRC.2004.1316389 PG 6 WC Remote Sensing; Physics, Applied; Telecommunications SC Remote Sensing; Physics; Telecommunications GA BAE91 UT WOS:000221923200005 ER PT S AU Lou, Y Hensley, S Le, C Moller, D AF Lou, Y Hensley, S Le, C Moller, D GP IEEE TI On-board processor for direct distribution of change detection data products SO PROCEEDINGS OF THE IEEE 2004 RADAR CONFERENCE SE Radar Conference LA English DT Proceedings Paper CT 2004 IEEE Radar Conference CY APR 26-29, 2004 CL PHILADELPHIA, PA SP IEEE Philadelphia Sect, IEEE Aerosp & Elect Syst Soc ID RADAR INTERFEROMETRY; LANDERS EARTHQUAKE AB We are developing an on-board imaging radar data processor for repeat-pass change detection and hazards management. This is the enabling technology for NASA ESE to utilize imaging radars. This processor will enable the observation and use of surface deformation data over rapidly evolving natural hazards, both as an aid to scientific understanding and to provide timely data to agencies responsible for the management and mitigation of natural disasters. Many hazards occur over periods of hours to days, and need to be sampled quickly. The new technology has the potential to save many lives and millions of dollars by putting critical information in the hands of disaster management agencies in time to be of use. The processor architecture integrates two key technologies by combining a Field Programmable Gate Array (FPGA) front-end with a reconfigurable computing back-end. Through this approach we are able to capitalize on the strengths of both technologies for the optimization of performance while maintaining flexibility where needed within the algorithmic implementation. A searchable on-board data archive will store the reference data sets needed for change detection processing. In this paper, we will present an overview of the change detection processing algorithm and the preliminary hardware architecture. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lou, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-243, Pasadena, CA 91109 USA. NR 6 TC 6 Z9 7 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1097-5764 J9 RADAR CONF PY 2004 BP 33 EP 37 DI 10.1109/NRC.2004.1316391 PG 5 WC Remote Sensing; Physics, Applied; Telecommunications SC Remote Sensing; Physics; Telecommunications GA BAE91 UT WOS:000221923200007 ER PT S AU Chen, CW AF Chen, CW GP IEEE TI Modified polar format algorithm for processing spaceborne SAR data SO PROCEEDINGS OF THE IEEE 2004 RADAR CONFERENCE SE Radar Conference LA English DT Proceedings Paper CT 2004 IEEE Radar Conference CY APR 26-29, 2004 CL PHILADELPHIA, PA SP IEEE Philadelphia Sect, IEEE Aerosp & Elect Syst Soc AB This paper describes a modified polar format algorithm for SAR image-formation processing. The algorithm focuses raw data assuming a spherical reference surface (ground surface), and, unlike standard polar format algorithms, it assumes spherical rather than planar signal wavefronts. The algorithm, or some variant of it based on the same geometry, is therefore more suitable than the standard polar format algorithm in spaceborne applications for which there is significant curvature of the platform flight track and/or curvature of the Earth surface. The algorithm is described here in the context of spotlight-mode data acquisition. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chen, CW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 TC 2 Z9 2 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1097-5764 J9 RADAR CONF PY 2004 BP 44 EP 49 DI 10.1109/NRC.2004.1316393 PG 6 WC Remote Sensing; Physics, Applied; Telecommunications SC Remote Sensing; Physics; Telecommunications GA BAE91 UT WOS:000221923200009 ER PT S AU Chen, CW AF Chen, CW GP IEEE TI Performance assessment of along-track interferometry for detecting ground moving targets SO PROCEEDINGS OF THE IEEE 2004 RADAR CONFERENCE SE Radar Conference LA English DT Proceedings Paper CT 2004 IEEE Radar Conference CY APR 26-29, 2004 CL PHILADELPHIA, PA SP IEEE Philadelphia Sect, IEEE Aerosp & Elect Syst Soc ID STATISTICS AB Along-track interferometry (ATI) is an interferometric synthetic aperture radar technique that can be used to measure Earth-surface velocities. As such, the ATI technique holds promise for the detection of slowly moving ground targets. The models often used to characterize ATI performance were developed mainly in the context of mapping ocean currents, however, and they do not necessarily apply to the case of discrete, moving ground targets amidst clutter. In this paper, we provide expressions for more accurately modeling the behavior of an ATI system in the context of ground moving target indication. Analysis and design equations are given for topics including target defocus, signal-to-noise and signal-to-clutter ratios, interferometric correlation, interferometric phase bias, target detection, geolocation accuracy, and area coverage rate. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chen, CW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 9 TC 32 Z9 38 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1097-5764 J9 RADAR CONF PY 2004 BP 99 EP 104 DI 10.1109/NRC.2004.1316403 PG 6 WC Remote Sensing; Physics, Applied; Telecommunications SC Remote Sensing; Physics; Telecommunications GA BAE91 UT WOS:000221923200019 ER PT S AU Rosen, PA AF Rosen, PA GP IEEE TI Developments in repeat pass interferometric radar for Earth and planetary sciences SO PROCEEDINGS OF THE IEEE 2004 RADAR CONFERENCE SE Radar Conference LA English DT Proceedings Paper CT 2004 IEEE Radar Conference CY APR 26-29, 2004 CL PHILADELPHIA, PA SP IEEE Philadelphia Sect, IEEE Aerosp & Elect Syst Soc AB Repeat pass radar interferometry has developed into a wide ranging geodetic and change mapping tool from space. For large areas of the Earth, and for numerous applications that demand more persistent monitoring, the true potential of the repeat. pass technique remains largely untapped. While the research community has made enormous strides in extracting as much information as possible from existing data sets, fundamentally new observing systems are needed for breakthroughs in a number of areas. Repeat pass interferometry techniques applied on missions to the terrestrial planets, Earth's moon and the icy moons of Jupiter can reveal new insights in to the history of the surface and near subsurface. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rosen, PA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 9 TC 2 Z9 2 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1097-5764 J9 RADAR CONF PY 2004 BP 207 EP 211 DI 10.1109/NRC.2004.1316423 PG 5 WC Remote Sensing; Physics, Applied; Telecommunications SC Remote Sensing; Physics; Telecommunications GA BAE91 UT WOS:000221923200038 ER PT S AU Im, E Durden, SL Rahmat-Samii, Y Fang, HF Cable, V Lou, M Huang, J AF Im, E Durden, SL Rahmat-Samii, Y Fang, HF Cable, V Lou, M Huang, J GP IEEE TI Advanced geostationary radar for hurricane monitoring and studies SO PROCEEDINGS OF THE IEEE 2004 RADAR CONFERENCE SE Radar Conference LA English DT Proceedings Paper CT 2004 IEEE Radar Conference CY APR 26-29, 2004 CL PHILADELPHIA, PA SP IEEE Philadelphia Sect, IEEE Aerosp & Elect Syst Soc AB The current Geostationary Operational Environmental Satellites (GOES) are equipped to make cloud top measurements only. In contrast, a millimeter-wave radar allows 3-D measurements of precipitation associated with hurricanes and other convective systems. It also provide important inputs for numerical weather prediction models for improving the accuracy of weather nowcasting and forecasting. Recently, a novel instrument concept and the associated critical technologies are being developed for a 35-GHz Doppler radar for detailed monitoring of hurricanes and severe storms from a geostationary orbit. This instrument is designed to be capable of producing rainfall rate at 13-km horizontal resolution and 300-m vertical resolution, and the line-of-sight Doppler velocity at 0.3 m/s precision, of the 3-D hurricane structure once per hour throughout its life cycle. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Im, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 6 TC 2 Z9 2 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1097-5764 J9 RADAR CONF PY 2004 BP 307 EP 311 DI 10.1109/NRC.2004.1316440 PG 5 WC Remote Sensing; Physics, Applied; Telecommunications SC Remote Sensing; Physics; Telecommunications GA BAE91 UT WOS:000221923200055 ER PT S AU Wheeler, K Hensley, S Lou, YL Miller, T Hoffman, J AF Wheeler, K Hensley, S Lou, YL Miller, T Hoffman, J GP IEEE TI An L-band SAR for repeat pass deformation measurements on a UAV platform SO PROCEEDINGS OF THE IEEE 2004 RADAR CONFERENCE SE Radar Conference LA English DT Proceedings Paper CT 2004 IEEE Radar Conference CY APR 26-29, 2004 CL PHILADELPHIA, PA SP IEEE Philadelphia Sect, IEEE Aerosp & Elect Syst Soc AB We are proposing to develop a miniaturized polarimetric L-band synthetic aperture radar (SAR) for repeat-pass differential interferometric measurements of deformation for rapidly deforming surfaces of geophysical interest such as volcanoes or earthquakes that is to be flown on a unmanned aerial vehicle (UAV) or minimally piloted vehicle (MPV). With our proposed mechanical design approach for the radar electronics, the instrument can potentially be accommodated on a number of different applicable platforms. Upon surveying the capabilities and availabilities of UAVs and MPVs, the ALTAIR UAV and the Proteus aircraft appear to meet our criteria in terms of payload capabilities, flying altitude, and endurance. To support the repeat pass deformation capability it is necessary to control flight track capability of the aircraft to be within a specified 10 in tube with a goal of I m. This requires real-time GPS control of the autopilot to achieve these objectives that has not been demonstrated on these aircraft. Based on the Proteus and ALTAIR's altitude of 13.7 km (45,000 ft), we are designing a fully polarimetric L-band radar with 80 MHz bandwidth and a 16 kin range swath. The radar will have an active electronic beam steering antenna to achieve a Doppler centroid stability that is necessary for repeat-pass interferometry. This paper presents the radar configuration along with some of the trade studies for the platform and instrument. C1 Jet Prop Lab, Pasadena, CA 91109 USA. RP Wheeler, K (reprint author), Jet Prop Lab, MS 300-241,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 0 TC 2 Z9 2 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1097-5764 J9 RADAR CONF PY 2004 BP 317 EP 322 DI 10.1109/NRC.2004.1316442 PG 6 WC Remote Sensing; Physics, Applied; Telecommunications SC Remote Sensing; Physics; Telecommunications GA BAE91 UT WOS:000221923200057 ER PT S AU Okojie, RS Savrun, E Nguyen, P Nguyen, V Blaha, C AF Okojie, RS Savrun, E Nguyen, P Nguyen, V Blaha, C BE Rocha, D Sarro, PM Vellekoop, MJ TI Reliability evaluation of direct chip attached silicon carbide pressure transducers SO PROCEEDINGS OF THE IEEE SENSORS 2004, VOLS 1-3 SE IEEE Sensors LA English DT Proceedings Paper CT IEEE Sensors 2004 Conference CY OCT 24-27, 2004 CL Vienna Univ Technol, Vienna, AUSTRIA SP IEEE HO Vienna Univ Technol DE silicon carbide; high temperature; pressure sensor; package; reliability AB An accelerated stress test (AST) protocol has been developed and used to evaluate the reliability of 6H-silicon carbide (SiC) pressure transducers for operation up to 400 C for 100 hours. After several cyclic excursions to 400 C, the maximum drift of the zero pressure offset voltage at 25 C was 1.9 mV, while the maximum drift at 400 C was 2.0 mV. The full-scale sensitivity to pressure before and after the AST was 36.6 mV/V/psi at 25 C and 20.5 mV/V/psi at 400 C, with a maximum drift of 1 mV/V/psi. No systematic degradation of the zero pressure offset was observed. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Okojie, RS (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM robert.s.okojie@nasa.gov; ender.savrun@siennatech.com; charles.a.blaha@grc.nasa.gov NR 7 TC 4 Z9 4 U1 1 U2 3 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1930-0395 BN 0-7803-8692-2 J9 IEEE SENSOR PY 2004 BP 635 EP 638 DI 10.1109/ICSENS.2004.1426246 PG 4 WC Engineering, Multidisciplinary; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BCH15 UT WOS:000229268100163 ER PT S AU Grant, MS Katzberg, SJ AF Grant, MS Katzberg, SJ GP IEEE TI Combined GPS reflected signal and visual imagery for unsupervised clustering and terrain classification SO PROCEEDINGS OF THE IEEE SOUTHEASTCON 2004: ENGINEERING CONNECTS SE IEEE SoutheastCon-Proceedings LA English DT Proceedings Paper CT IEEE SoutheastCon 2004 CY MAR 26-29, 2004 CL Greensboro, NC SP IEEE, Reg 3 AB Use of the Global Positioning System (GPS) L-band (1.57542 GHz) surface-reflected signal for remote sensing is a relatively recent development. In the current study, GPS satellite reflected-signal surface reflectivity, computed along the spectral point ground track across an agricultural area, is combined with 1m x 1m orthorectified, grayscale imagery to form a 2-dimensional (2D) space where unsupervised data clustering and classification is performed Unlike intensity-only (ID) clustering and classification of the visual data, the moisture-sensitive GPS reflected signal allows water features to be readily differentiated from heavy vegetation and cultivated fields. To our knowledge, this study is the first use of the reflected GPS signal in combination with visual imagery for remotely sensed terrain data clustering and classification. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP NASA, Langley Res Ctr, MS 472, Hampton, VA 23681 USA. EM m.s.grant@larc.nasa.gov; s.j.katzberg@larc.nasa.gov NR 15 TC 2 Z9 2 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1558-058X BN 0-7803-8367-2 J9 IEEE SOUTHEASTCON PY 2004 BP 370 EP 377 PG 8 WC Computer Science, Artificial Intelligence; Computer Science, Software Engineering; Engineering, Electrical & Electronic; Imaging Science & Photographic Technology; Telecommunications SC Computer Science; Engineering; Imaging Science & Photographic Technology; Telecommunications GA BAB90 UT WOS:000221506500055 ER PT S AU Fernandez-Remolar, DC AF Fernandez-Remolar, DC CA MARTE Scientific Team BE Harris, RA Ouwehand, L TI Mars analog research and technology experiment (MARTE), a simulated Mars drilling project SO PROCEEDINGS OF THE III EUROPEAN WORKSHOP ON EXO-ASTROBIOLOGY: MARS: THE SEARCH FOR LIFE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 3rd European Workshop on Exo/Astrobiology CY NOV 18-20, 2003 CL Ctr Astrobiol, Madrid, SPAIN SP European Space Agcy, Minist Ciencia & Tecnol Spain, Minist Def Spain, Comunidad Madrid HO Ctr Astrobiol AB Searching for life in the subsurface of another planet will require drilling, sample extraction and handling, and new technologies to find and identify biomarker compounds ands search for living organisms. The Science Definition Team for the 2009 Mars Exploration Program Smart Lander mission has called for drilling as a key objective of the next Mars mission. Thus, there is a critical and immediate need for technology maduration for drilling that can be accomplished with a field mission simulation. C1 Portland State Univ, MARTE Sci Team, Ctr Astrobiol, NASA,Ames Res Ctr,Johnson Space Ctr, Portland, OR 97207 USA. RP Fernandez-Remolar, DC (reprint author), Portland State Univ, MARTE Sci Team, Ctr Astrobiol, NASA,Ames Res Ctr,Johnson Space Ctr, Portland, OR 97207 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-856-5 J9 ESA SP PUBL PY 2004 VL 545 BP 237 EP 238 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAD24 UT WOS:000221643000073 ER PT S AU Quinn, RC Grunthaner, FJ Taylor, CL Zent, AP McKay, CP Gomez-Silva, BG AF Quinn, RC Grunthaner, FJ Taylor, CL Zent, AP McKay, CP Gomez-Silva, BG BE Harris, RA Ouwehand, L TI Electrochemical studies of atacama desert soils: An analog of Martian surface chemistry SO PROCEEDINGS OF THE III EUROPEAN WORKSHOP ON EXO-ASTROBIOLOGY: MARS: THE SEARCH FOR LIFE SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 3rd European Workshop on Exo/Astrobiology CY NOV 18-20, 2003 CL Ctr Astrobiol, Madrid, SPAIN SP European Space Agcy, Minist Ciencia & Tecnol Spain, Minist Def Spain, Comunidad Madrid HO Ctr Astrobiol AB The liquid phase pH and EH kinetic profile has been measured for soil samples collected along a north-south transect in the Chilean Atacama Desert. With water addition, surface samples collected at the driest site show a shift from an acidic to a more basic pH. This trend is consistent with the pH shift (inferred from carbon dioxide uptake) seen in the Viking GEx. This kinetic response is unique to the upper most surface material collected in the driest region of the Atacama Desert and was not observed in samples taken at depth, or in samples collected from the more humid southern sites. C1 NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Quinn, RC (reprint author), NASA, Ames Res Ctr, SETI Inst, MS 239-12, Moffett Field, CA 94035 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-856-5 J9 ESA SP PUBL PY 2004 VL 545 BP 271 EP 272 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAD24 UT WOS:000221643000089 ER PT B AU Matson, DL Lebreton, JP Spilker, LJ AF Matson, DL Lebreton, JP Spilker, LJ BE Fletcher, K TI The Cassini-Huygens mission to the Saturnian system SO PROCEEDINGS OF THE INTERNATIONAL CONFERENCE TITAN: FROM DISCOVERY TO ENCOUNTER LA English DT Proceedings Paper CT International Conference on Titan - From Discovery to Encounter CY APR 13-17, 2004 CL Noordwijk, NETHERLANDS SP ESTEC ID RADIATION; VENUS AB The international Cassini-Huygens mission consists of the Cassini Saturn Orbiter spacecraft and the Huygens Titan Probe that is targeted for entry into the atmosphere of Saturn's largest moon, Titan. From launch on October 15, 1997 to arrival at Saturn in July 2004, Cassini-Huygens will travel over three billion kilometres. Once in orbit about Saturn, Huygens is released from the orbiter and enters Titan's atmosphere. The Probe descends by parachute and measures the properties of the atmosphere. If the landing is gentle, the properties of the surface will be measured too. Then the orbiter commences a four-year tour of the Saturnian system with 45 flybys of Titan and multiple encounters with the icy moons. The rings, the magnetosphere and Saturn itself are all studied as well as the interactions among them. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Matson, DL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 16 TC 0 Z9 0 U1 0 U2 2 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS BN 92-9092-997-9 PY 2004 BP I EP XVI PG 16 WC Engineering, Aerospace; Astronomy & Astrophysics; History & Philosophy Of Science SC Engineering; Astronomy & Astrophysics; History & Philosophy of Science GA BBQ27 UT WOS:000227039300020 ER PT B AU Sittler, EC Hartle, RE Vinas, AF Johnson, RE Smith, HT Mueller-Wodard, I AF Sittler, EC Hartle, RE Vinas, AF Johnson, RE Smith, HT Mueller-Wodard, I BE Fletcher, K TI Titan interaction with Saturn's magnetosphere: mass loading and ionopause location SO PROCEEDINGS OF THE INTERNATIONAL CONFERENCE TITAN: FROM DISCOVERY TO ENCOUNTER LA English DT Proceedings Paper CT International Conference on Titan - From Discovery to Encounter CY APR 13-17, 2004 CL Noordwijk, NETHERLANDS SP ESTEC ID PLANETARY EXOSPHERES; VOYAGER-1 ENCOUNTER; UPPER-ATMOSPHERE; SOLAR-WIND; MODEL; PHOTOCHEMISTRY; IONOSPHERE AB We investigate the details of Titan's interaction with Saturn's magnetosphere, which includes formation of an ionopause and its location and mass loading via ion pickup. We present some new interpretations of the Voyager 1 encounter results, not previously done by Hartle and co-workers([1]). Using arguments based on theory and observation we show that in the outer pickup region, ion pickup of H+ and H-2(+) dominates, with some mass loading effects. Only when the flow has reached the exospheric population dominated by heavy neutral species such as methane and molecular nitrogen does the flow experience major mass loading and slowing down. We do find that large ion gyroradii of the pickup ions could be important to the interaction, but not significant enough that during the Voyager 1 encounter with Titan for the plasma instrument to detect energetic beams of heavy ions in the energy spectra. The plasma instrument did measure pickup ion distributions, where the dominant ion was consistent with H-2(+), but could also be CH4+- Our calculations also include ejection of relatively energetic heavy neutrals such as atomic nitrogen from Titan's upper atmosphere due to electron, ion and photon impact. We also show finite gyroradius effects from the interaction of the ambient plasma with Titan's atmosphere, which results in an asymmetric removal of ambient plasma from Titan's ion exospheric region. The Voyager plasma data shows the removal of the keV ambient population first during the approach and then the less energetic ambient component being removed. During the outbound phase the less energetic ambient component reappeared with the keV ambient component reappearing further away. This feature is consistent with finite gyroradius effects with the energetic component being a heavy ion component like N+ and the light ion component being H+ and confirms the original analysis by Hartle and co-workers([1]) that the ambient plasma was composed of a light and heavy ion component. We comment on the position of the ionopause, its characteristics and the corresponding access of charged particles to Titan's upper atmosphere similar to that done for Triton([2]). The position of the ionopause plays a critical role with regard to the strength of the source term for Titan's nitrogen torus([3]). The addition of CH4 in our exosphere calculations indicates that Titan could also be an important source of carbon to Saturn's magnetosphere. In the future we plan to use a 2D-hybrid code with an exosphere model, to model Titan's interaction with Saturn's magnetosphere. These results can then be used to make predictions for the Cassini flybys of Titan. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sittler, EC (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. RI Smith, Howard/H-4662-2016 OI Smith, Howard/0000-0003-3537-3360 NR 31 TC 1 Z9 1 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS BN 92-9092-997-9 PY 2004 BP 377 EP 394 PG 18 WC Engineering, Aerospace; Astronomy & Astrophysics; History & Philosophy Of Science SC Engineering; Astronomy & Astrophysics; History & Philosophy of Science GA BBQ27 UT WOS:000227039300033 ER PT S AU Lowman, PD AF Lowman, PD GP American astronautical society BE Durst, SM Bohannan, CT Thomason, CG Cerney, MR Yuen, L TI LSPECS: A proposed robotic astronomy mission to the lunar south polar regions SO PROCEEDINGS OF THE INTERNATIONAL LUNAR CONFERENCE 2003/ INTERNATIONAL LUNAR EXPLORATION WORKING GROUP 5 - ILC2003/ILEWG 5 SE SCIENCE AND TECHNOLOGY SERIES LA English DT Proceedings Paper CT International Lunar Conference 2003/International Lunar Exploration Working Group 5 Conference CY NOV 16-22, 2003 CL Waikoloa, HI ID MOON; DEPOSITS AB This paper outlines a possible mission to emplace a robotic infrared/submillimeter wave interferometer array near the lunar South Pole. This region has now been investigated by the Clementine and Lunar Prospector missions, and by Earth-based radar, and its topography and thermal environment are fairly well-known. The area would be exceptionally suitable for infrared/submillimeter astronomy because of the continually low temperatures, approaching that of liquid nitrogen (77K) in some places. A submillimeter spaceborne interferometer mission, Submillimeter Probe of the Evolution of the Cosmic Structure (SPECS) has been proposed by John Mather and others, covering the 40 - 500 micron region with 3 formation flying telescopes. The present paper proposes a lunar adaptation of the SPECS concept, LSPECS. This adaptation would involve landing 4 telescopes on the area north of Shackleton crater at zero degrees longitude. This is in nearly year round darkness but is continually radar visible from Earth. The landed payload of LSPECS would include a telerobotic rover, 4 three meter submm telescopes, a solar power array to be emplaced on the continually sunlit north rim of Shackleton crater, and an S-band antenna for data relay to Earth. Passive cooling without the use of expendable cryogenics might be possible, trading long exposure time for instrument temperatures above that of liquid helium. The LSPECS would permit long-term study of an extremely wide range of cosmic and solar system phenomena in the southern celestial hemisphere. For complete sky coverage, a similar installation near the North Pole would be required. The LSPECS site would also be suitable other types of observation, such as optical interferometry or centimeter wavelength radio astronomy. The lunar South Pole is also of great interest because of its extensive ice deposits, which may represent cometary infall with pre-biotic compounds. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lowman, PD (reprint author), NASA, Goddard Space Flight Ctr, Code 921, Greenbelt, MD 20771 USA. NR 23 TC 0 Z9 0 U1 0 U2 3 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 0278-4017 BN 0-87703-513-x J9 SCI TECH PY 2004 VL 108 BP 71 EP 75 PG 5 WC Engineering, Aerospace; Geosciences, Multidisciplinary SC Engineering; Geology GA BBG51 UT WOS:000225436500009 ER PT S AU Lo, MW AF Lo, MW GP American astronautical society BE Durst, SM Bohannan, CT Thomason, CG Cerney, MR Yuen, L TI The intraplanetary superhighway and the development of the moon SO PROCEEDINGS OF THE INTERNATIONAL LUNAR CONFERENCE 2003/ INTERNATIONAL LUNAR EXPLORATION WORKING GROUP 5 - ILC2003/ILEWG 5 SE SCIENCE AND TECHNOLOGY SERIES LA English DT Proceedings Paper CT International Lunar Conference 2003/International Lunar Exploration Working Group 5 Conference CY NOV 16-22, 2003 CL Waikoloa, HI C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lo, MW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,301-140L, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 0278-4017 BN 0-87703-513-x J9 SCI TECH PY 2004 VL 108 BP 214 EP 214 PG 1 WC Engineering, Aerospace; Geosciences, Multidisciplinary SC Engineering; Geology GA BBG51 UT WOS:000225436500029 ER PT S AU Holt, AC AF Holt, AC GP American astronautical society BE Durst, SM Bohannan, CT Thomason, CG Cerney, MR Yuen, L TI ISS/lunar advanced technology testbeds and test ranges SO PROCEEDINGS OF THE INTERNATIONAL LUNAR CONFERENCE 2003/ INTERNATIONAL LUNAR EXPLORATION WORKING GROUP 5 - ILC2003/ILEWG 5 SE SCIENCE AND TECHNOLOGY SERIES LA English DT Proceedings Paper CT International Lunar Conference 2003/International Lunar Exploration Working Group 5 Conference CY NOV 16-22, 2003 CL Waikoloa, HI C1 NASA, Lyndon B Johnson Space Ctr, Res Program Off, ISS Off Space Flight, Houston, TX 77058 USA. RP Holt, AC (reprint author), NASA, Lyndon B Johnson Space Ctr, Res Program Off, ISS Off Space Flight, Code OZ4, Houston, TX 77058 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 0278-4017 BN 0-87703-513-x J9 SCI TECH PY 2004 VL 108 BP 215 EP 221 PG 7 WC Engineering, Aerospace; Geosciences, Multidisciplinary SC Engineering; Geology GA BBG51 UT WOS:000225436500030 ER PT S AU Borowski, SK AF Borowski, SK GP American astronautical society BE Durst, SM Bohannan, CT Thomason, CG Cerney, MR Yuen, L TI The use of nuclear propulsion, power and "in-situ" resources for routine lunar space transportation and commercial base development SO PROCEEDINGS OF THE INTERNATIONAL LUNAR CONFERENCE 2003/ INTERNATIONAL LUNAR EXPLORATION WORKING GROUP 5 - ILC2003/ILEWG 5 SE SCIENCE AND TECHNOLOGY SERIES LA English DT Proceedings Paper CT International Lunar Conference 2003/International Lunar Exploration Working Group 5 Conference CY NOV 16-22, 2003 CL Waikoloa, HI C1 NASA, Glenn Res Ctr, Space Transportat Project Off, Cleveland, OH 44135 USA. RP Borowski, SK (reprint author), NASA, Glenn Res Ctr, Space Transportat Project Off, MS 86-8,21000 Brookpk Rd, Cleveland, OH 44135 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 0278-4017 BN 0-87703-513-x J9 SCI TECH PY 2004 VL 108 BP 225 EP 226 PG 2 WC Engineering, Aerospace; Geosciences, Multidisciplinary SC Engineering; Geology GA BBG51 UT WOS:000225436500032 ER PT B AU Figueroa, F Schmalzel, J Morris, J Solano, W Mandayam, S Polikar, R AF Figueroa, F Schmalzel, J Morris, J Solano, W Mandayam, S Polikar, R GP IEEE TI A framework for intelligent rocket test facilities with smart sensor elements SO PROCEEDINGS OF THE ISA/IEEE SENSORS FOR INDUSTRY CONFERENCE LA English DT Proceedings Paper CT 3rd ISA/IEEE Sensors for Industry Conference CY JAN 27-29, 2004 CL New Orleans, LA SP ISA, IEEE Instrumentat & Measurement Soc AB Smart sensors are a compelling addition to large-scale data acquisition networks due to the large number of issues they successfully address. For example, smart sensors simplify and speed installation configuration due to the basic information stored in their on-board TEDS that would otherwise need to be manually input to the data acquisition system An emerging challenge is the development of smart systems, which rely on smart sensors to provide new levels of reliability. This paper reports on our on-going efforts to apply smart sensors to a rocket test facility. Key to our approach is the hierarchical organization of the intelligent rocket test facility as a system of three fundamental layers: system(s), processes, and smart sensors. C1 NASA, Stennis Space Ctr, MS USA. RP Figueroa, F (reprint author), NASA, Stennis Space Ctr, MS USA. RI Polikar, Robi/N-4742-2015 OI Polikar, Robi/0000-0002-2739-4228 NR 9 TC 1 Z9 1 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-8143-2 PY 2004 BP 91 EP 95 PG 5 WC Instruments & Instrumentation; Telecommunications SC Instruments & Instrumentation; Telecommunications GA BY73K UT WOS:000189450200017 ER PT B AU Lavelle, JP Schuet, SR Schuet, DJ AF Lavelle, JP Schuet, SR Schuet, DJ GP IEEE TI High speed 3D scanner with real-time 3D processing SO PROCEEDINGS OF THE ISA/IEEE SENSORS FOR INDUSTRY CONFERENCE LA English DT Proceedings Paper CT 3rd ISA/IEEE Sensors for Industry Conference CY JAN 27-29, 2004 CL New Orleans, LA SP ISA, IEEE Instrumentat & Measurement Soc AB A novel 3D sensing system with real-time 3D processing has been developed which is capable of scanning an object at very high speeds (greater than 500,000 3D points/second) and creating high-resolution 3D surface maps. Laser triangulation is used in conjunction with a high-resolution camera, a laser diode, and processing electronics all incorporated into a small sensor package that traverses linearly or rotates from a fixed position to scan an object. Processing is done on board the instrument and the resultant 3D data is transmitted to a PC. This results in rapid scans, with 3D images produced as the instrument is scanning. The sensing system was developed for the NASA Mars rover program and for the inspection of Shuttle Thermal Protection System (tiles), radiator, and structures. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lavelle, JP (reprint author), NASA, Ames Res Ctr, Code SFT, Moffett Field, CA 94035 USA. NR 4 TC 2 Z9 2 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-8143-2 PY 2004 BP 102 EP 108 PG 7 WC Instruments & Instrumentation; Telecommunications SC Instruments & Instrumentation; Telecommunications GA BY73K UT WOS:000189450200019 ER PT B AU Solano, WM Junell, J Schmalzel, JL Shumard, KC AF Solano, WM Junell, J Schmalzel, JL Shumard, KC GP IEEE TI Implementation of wireless and intelligent sensor technologies in the propulsion test environment SO PROCEEDINGS OF THE ISA/IEEE SENSORS FOR INDUSTRY CONFERENCE LA English DT Proceedings Paper CT 3rd ISA/IEEE Sensors for Industry Conference CY JAN 27-29, 2004 CL New Orleans, LA SP ISA, IEEE Instrumentat & Measurement Soc AB Wireless and intelligent sensors are being developed and applied to a variety of engine test applications at SSC. A Wireless Sensor Suite has been developed to provide for an easily configurable and deployable data collection capability as well as serve as an upgradeable laboratory and field platform that evolves to accommodate new technologies and smart sensor paradigms. One promising application is to use this system as a platform for experimental demonstration of facility health monitoring using arrays of intelligent networked sensors. C1 NASA, Stennis Space Ctr, MS USA. RP Solano, WM (reprint author), NASA, Stennis Space Ctr, MS USA. NR 7 TC 4 Z9 4 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-8143-2 PY 2004 BP 135 EP 138 PG 4 WC Instruments & Instrumentation; Telecommunications SC Instruments & Instrumentation; Telecommunications GA BY73K UT WOS:000189450200024 ER PT S AU Minnis, P Nguyen, L Young, DF Doelling, DR Nordeen, ML Spangenberg, DA Palikonda, R Nowicki, GD Haeffelin, M AF Minnis, P Nguyen, L Young, DF Doelling, DR Nordeen, ML Spangenberg, DA Palikonda, R Nowicki, GD Haeffelin, M BE Lacoste, H TI Comparison of cloud properties from meteosat-8 and surface observations SO Proceedings of the Second MSG RAO Workshop SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 2nd MSG RAO Workshop CY SEP 09-10, 2004 CL Salzburg, AUSTRIA SP European Space Agcy, EUMETSAT AB A set of algorithms used to derive cloud properties globally has been adapted to analyze hourly radiances taken by Meteosat-8. The initial results are evaluated using objective surface observations at several European locations. Cloud amounts appear to be underestimated due to the satellite retrievals missing some optically thin clouds. False cloud detections occur along and coastlines and for heavy aerosols. Improvement in cloud detection awaits refinements of the algorithms for the SEVIRI channels and in the clear-sky radiances used to discriminate cloudy and clear scenes. Cloud-top heights are in good agreement for liquid and optically thick ice clouds but are underestimated for optically thin ice clouds. Further enhancement of the algorithms is underway. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Minnis, P (reprint author), NASA, Langley Res Ctr, MS 420, Hampton, VA 23681 USA. NR 10 TC 1 Z9 1 U1 0 U2 0 PU EUROPEAN SPACE AGENCY PI PARIS PA 8-10 RUE MARIO NIKIS, 75738 PARIS, FRANCE SN 0379-6566 BN 92-9092-893-X J9 ESA SP PUBL PY 2004 VL 582 BP 91 EP 96 PG 6 WC Meteorology & Atmospheric Sciences; Remote Sensing SC Meteorology & Atmospheric Sciences; Remote Sensing GA BBW49 UT WOS:000228130400016 ER PT B AU Soloway, DI Haley, PJ AF Soloway, DI Haley, PJ BE Hamza, MH TI Pilots rate augmented generalized predictive control for reconfiguration SO Proceedings of the Sixth IASTED International Conference on Intelligent Systems and Control LA English DT Proceedings Paper CT 6th IASTED International Conference on Intelligent Systems and Control CY AUG 23-25, 2004 CL Honolulu, HI SP Int Assoc Sci & Technol Dev, Tech Comm Control, Tech Comm Intelligent Syst & Control DE reconfigurable control; predictive control; aircraft control; Cooper-Harper; pilot; failure AB This paper highlights a study that is part of a continuing research effort in reconfigurable flight controls at NASA Ames. Three NASA Dryden test pilots were tasked with evaluating two methodologies for reconfiguring an aircraft's control system when failures occur in the control surfaces and engine. Two neural network based controllers are being considered, specifically the Neural Generalized Predictive Controller and a Dynamic Inverse Neural Controller. Prior to the tests, the Neural Generalized Predictive Controller was enhanced with a simple augmentation to reduce zero steady-state error which unexpectedly made the neural network predictor model redundant and unnecessary for this level of reconfiguration. Instead a nominal single point linear predictor model was used with the new augmentation. This paper shows that even without a neural network the Generalized Predictive Controller performs equally well at reconfiguration as the Dynamic Inverse Neural Network controller, requires lower rates from the actuators, and avoids the validation dilemma of using a neural network. Also shown are the pilot ratings for each controller for various failure scenarios and two samples of the required control actuation during reconfiguration. Finally, the paper concludes by stepping through the Generalized Predictive Control's reconfiguration process for an elevator failure. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Soloway, DI (reprint author), NASA, Ames Res Ctr, MS 269-3, Moffett Field, CA 94035 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU ACTA PRESS PI CALGARY PA B6, STE 101, 2509 DIEPPE AVE SW, CALGARY, ALBERTA T3E 7J9, CANADA BN 0-88986-436-5 PY 2004 BP 114 EP 120 PG 7 WC Automation & Control Systems; Computer Science, Artificial Intelligence; Operations Research & Management Science SC Automation & Control Systems; Computer Science; Operations Research & Management Science GA BCC26 UT WOS:000228556100021 ER PT B AU Matessa, M AF Matessa, M BE Lovett, M Schunn, C Lebiere, C Munro, P TI Anticipatory eye movements in interleaving templates of human behaviour SO PROCEEDINGS OF THE SIXTH INTERNATIONAL CONFERENCE ON COGNITIVE MODELING LA English DT Proceedings Paper CT 6th International Conference on Cognitive Modeling CY JUL 30-AUG 01, 2004 CL Carnegie Mellon Univ, Pittsburgh, PA SP USAF, Off Sci Res, USAF Res Lab, USA Res Lab, CMU Psychol, MicroAnalysis & Design, NASA, Natl Sci Fdn, USN, Off Naval Res, Univ Pittsburgh, LRDC HO Carnegie Mellon Univ AB Performance modeling has been made easier by architectures which package psychological theory for reuse at useful levels of abstraction. CPM-GOMS uses templates of behavior to package at a task level (e.g., mouse move-click, typing) predictions of lower-level cognitive, perceptual, and motor resource use. CPM-GOMS also has a theory for interleaving resource use between templates. One example of interleaving is anticipatory eye movements. This paper describes the use of ACT-Stitch, a framework for translating CPM-GOMS templates and interleaving theory into ACT-R, to model anticipatory eye movements in skilled behavior. The anticipatory eye movements explain performance in a well-practiced perceptual/motor task, and the interleaving theory is supported with results from an eye-tracking experiment. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 22 TC 2 Z9 2 U1 1 U2 1 PU LAWRENCE ERLBAUM ASSOC PUBL PI MAHWAH PA 10 INDUSTRIAL AVE, MAHWAH, NJ 07430 USA BN 0-8058-5426-6 PY 2004 BP 184 EP 189 PG 6 WC Computer Science, Artificial Intelligence; Psychology, Experimental SC Computer Science; Psychology GA BAW01 UT WOS:000223860100031 ER PT B AU Verma, S Corker, X Jadhav, A AF Verma, S Corker, X Jadhav, A BE Lovett, M Schunn, C Lebiere, C Munro, P TI Modelling visual behavior of pilots in the human performance model - Air MIDAS SO PROCEEDINGS OF THE SIXTH INTERNATIONAL CONFERENCE ON COGNITIVE MODELING LA English DT Proceedings Paper CT 6th International Conference on Cognitive Modeling CY JUL 30-AUG 01, 2004 CL Carnegie Mellon Univ, Pittsburgh, PA SP USAF, Off Sci Res, USAF Res Lab, USA Res Lab, CMU Psychol, MicroAnalysis & Design, NASA, Natl Sci Fdn, USN, Off Naval Res, Univ Pittsburgh, LRDC HO Carnegie Mellon Univ C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 5 TC 0 Z9 0 U1 0 U2 2 PU LAWRENCE ERLBAUM ASSOC PUBL PI MAHWAH PA 10 INDUSTRIAL AVE, MAHWAH, NJ 07430 USA BN 0-8058-5426-6 PY 2004 BP 396 EP 397 PG 2 WC Computer Science, Artificial Intelligence; Psychology, Experimental SC Computer Science; Psychology GA BAW01 UT WOS:000223860100087 ER PT B AU Markus, T Green, JL Cooper, JF Fung, SF Taylor, WWL Benson, RF Gogineni, SP Ramasami, VC Reinisch, BW Song, P AF Markus, T Green, JL Cooper, JF Fung, SF Taylor, WWL Benson, RF Gogineni, SP Ramasami, VC Reinisch, BW Song, P BE Slob, EC Yarovoy, A Rhebergen, J TI Ground penetrating radar simulations for Jupiter's Icy Moons SO PROCEEDINGS OF THE TENTH INTERNATIONAL CONFERENCE ON GROUND PENETRATING RADAR, VOLS 1 AND 2 LA English DT Proceedings Paper CT 10th International Conference on Ground Penetrating Radar (GPR 2004) CY JUN 21-24, 2004 CL Delft Univ Technol, Delft, NETHERLANDS SP TU Delft, Int Res Ctr Telecommun & Radar, TU Delft, Ctr Tech Geosci, IEEE Geosci & Remote Sensing Soc, TNO-FEL, Geophys Sur Syst Inc, 3D Radar-AS, Allied Assoc, Ingegneria Sistemi-SPA, Mala Geosci, Radar Syst Inc, Roadscanners, Sensors & Software, T& A Survey HO Delft Univ Technol DE ground penetrating radar; Jupiter moons; ice; subsurface ocean ID EUROPA AB The detection of subsurface oceans underneath the icy crust of the Jovian moons is one of the primary objectives of the Jupiter Icy Moons Orbiter (JIMO) mission. A ground penetrating radar system has the potential to collect sub-surface information. In preparation for this mission we performed theoretical simulations of a GPR system to identify optimum radar characteristics. Radar frequencies are planned to be between 1 and 50 MHz. Preliminary modeling results show that for a 7 km thick icy crust the return signal of an ice-ocean interface is clearly distinguishable. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Markus, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Thorsten.Markus@nasa.gov RI Cooper, John/D-4709-2012; Markus, Thorsten/D-5365-2012; Fung, Shing/F-5647-2012 NR 13 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA PY 2004 BP 789 EP 792 PG 4 WC Physics, Applied; Imaging Science & Photographic Technology SC Physics; Imaging Science & Photographic Technology GA BBJ19 UT WOS:000225736800188 ER PT J AU Matessa, M AF Matessa, Michael BE Forbus, K Gentner, D Regier, T TI An ACT-R Modeling Framework for Interleaving Templates of Human Behavior SO PROCEEDINGS OF THE TWENTY-SIXTH ANNUAL CONFERENCE OF THE COGNITIVE SCIENCE SOCIETY LA English DT Proceedings Paper CT 26th Annual Conference of the Cognitive-Science-Society CY AUG 04-07, 2004 CL Chicago, IL SP Cognit Sci Soc AB Performance modeling has been made easier by architectures which package psychological theory for reuse at different levels. Both CPM-GOMS, which packages theory at the task level, and ACT-R, which packages theory at the lower level of rules for perceptual-motor interaction, have been shown to be useful. This paper describes ACT-Stitch, a framework for translating CPM-GOMS templates and interleaving theory into ACT-R. The research involved in producing ACT-Stitch will benefit reusable template research by showing how to implement templates and interleaving in a new architecture that processes resource information. ACT-R research will benefit from re-usable productions packaged at a higher task level and from the multi-tasking control structure used that allows ACT-R to interleave productions from different templates. The zero-parameter predictions of ACT-Stitch are empirically validated. C1 [Matessa, Michael] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM mmatessa@arc.nasa.gov NR 17 TC 1 Z9 1 U1 1 U2 1 PU LAWRENCE ERLBAUM ASSOC PUBL PI MAHWAH PA 10 INDUSTRIAL AVE, MAHWAH, NJ 07430 USA BN 978-0-8058-5464-0 PY 2004 BP 903 EP 908 PG 6 WC Computer Science, Artificial Intelligence; Language & Linguistics; Psychology; Psychology, Experimental SC Computer Science; Linguistics; Psychology GA BSN97 UT WOS:000285044800168 ER PT J AU Wu, SC Remington, RW Pashler, H AF Wu, Shu-Chieh Remington, Roger W. Pashler, Harold BE Forbus, K Gentner, D Regier, T TI Coordination of Component Mental Operations in Sequences of Discrete Responses SO PROCEEDINGS OF THE TWENTY-SIXTH ANNUAL CONFERENCE OF THE COGNITIVE SCIENCE SOCIETY LA English DT Proceedings Paper CT 26th Annual Conference of the Cognitive-Science-Society CY AUG 04-07, 2004 CL Chicago, IL SP Cognit Sci Soc ID EYE-MOVEMENTS; TASK AB In daily life we often perform sequences of actions, which with practice are accomplished by overlapping mental operations for successive actions. Is it possible to derive performance predictions for such sequences from a characterization of the mental operations for a single stimulus-response pair? We explore this by examining the joint timing of eye movements and manual responses in a typing-like task following Pashler (1994). Participants made separate choice responses to a series of five stimuli spread over a wide viewing area. Replicating Pashler's results, responses to the first stimulus (RT1) were elevated, with inter-response intervals (IRI) for subsequent items rapid and flat across items. The eyes moved toward the next letter about 800 ms before the corresponding manual response (eye-hand span). Analyses of manual responses show multiple components to the RT1 elevation. Analyses of dwell times show that the eyes move to the next stimulus before the completion of all central processing. C1 [Wu, Shu-Chieh; Remington, Roger W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM scwu@mail.arc.nasa.gov; roger.w.remington@nasa.gov; hpashler@ucsd.edu NR 12 TC 1 Z9 1 U1 0 U2 0 PU LAWRENCE ERLBAUM ASSOC PUBL PI MAHWAH PA 10 INDUSTRIAL AVE, MAHWAH, NJ 07430 USA BN 978-0-8058-5464-0 PY 2004 BP 1476 EP 1481 PG 6 WC Computer Science, Artificial Intelligence; Language & Linguistics; Psychology; Psychology, Experimental SC Computer Science; Linguistics; Psychology GA BSN97 UT WOS:000285044800265 ER PT S AU Kim, HH Wheeler, RM Sager, JC Goins, GD AF Kim, HH Wheeler, RM Sager, JC Goins, GD BE Cantliffe, DJ Stoffella, PJ Shaw, NL TI A comparison of growth and photosynthetic characteristics of lettuce grown under red and blue light-emitting diodes (LEDs) with and without supplemental green LEDs SO PROCEEDINGS OF THE VIITH INTERNATIONAL SYMPOSIUM ON PROTECTED CULTIVATION IN MILD WINTER CLIMATES: PRODUCTION, PEST MANAGEMENT AND GLOBAL COMPETITION, VOLS 1 AND 2 SE ACTA HORTICULTURAE LA English DT Proceedings Paper CT 7th International Symposium on Protected Cultivation in Mild Winter Climates - Production, Pest Management and Global Competition CY MAR 23-27, 2004 CL Kissimmee, FL DE Lactuca sativa; controlled environments; electric light source; light quality; light response curves; CO2 response curves ID CO2 FIXATION; RADIATION; PLANTS; WHEAT; PRODUCTIVITY; ENVIRONMENTS; CAROTENOIDS; EFFICIENCY; MEMBRANES; YIELD AB Plants could be an important aspect of future space missions. Lighting systems for plant growth chambers will need to be lightweight, reliable, and durable, and light-emitting diodes (LEDs) have these characteristics. Previous studies demonstrated the combination of red and blue LEDs as an effective light source for several crops. The addition of green supplemental lighting offers a psychological benefit for the crew, since most plant leaves would appear green and normal similar to a natural setting under white light. The addition of green light could offer more benefits, since green light can better penetrate the plant canopy and potentially increase plant growth by increasing photosynthesis from the lower canopy leaves. In this study, lettuce plants grown under red and blue LEDs were compared to plants given an additional 5% (6 mumol m(-2) s(-1)) of green light. Light and CO2 photosynthesis response curves were measured along with other physiological parameters, and there was no significant difference between the treatments. Future studies will examine higher levels of supplemental green light. The use of green light would be beneficial, since it did not impact plant growth, it provides useful photosynthetically active radiation once it is absorbed, and the plants would appear green and healthy to the crews on space mission. C1 NASA, Biol Sci Off, Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA. RP Kim, HH (reprint author), NASA, Biol Sci Off, Kennedy Space Ctr, YA-E4-B, Kennedy Space Ctr, FL 32899 USA. NR 36 TC 8 Z9 9 U1 2 U2 14 PU INTERNATIONAL SOCIETY HORTICULTURAL SCIENCE PI LEUVEN 1 PA PO BOX 500, 3001 LEUVEN 1, BELGIUM SN 0567-7572 BN 90-6605-259-7 J9 ACTA HORTIC PY 2004 IS 659 BP 467 EP 475 PG 9 WC Agronomy; Horticulture SC Agriculture GA BBN85 UT WOS:000226378900062 ER PT B AU Noor, AK AF Noor, A. K. BE Topping, BHV Soares, CAM TI Modeling, simulation and visualization technologies: Frontiers and beyond SO Progress in Engineering Computational Technology LA English DT Proceedings Paper CT 7th International Conference on Computational Structures Technology/4th International Conference on Engineering Computational Technology CY SEP 07-09, 2004 CL Lisbon, PORTUGAL DE modeling; simulation; visualization; virtual product development ID UNCERTAINTY AB Virtual product development systems evolved from the integration of modeling, simulation and visualization tools and facilities with other product life cycle software and management tools. As the trend of distributed collaboration, large-scale integration of computing resources, enterprise tools, facilities, and processes continues, fundamental paradigm shift will occur in modeling simulation and visualization (MSV) technologies. The present paper reviews some of the recent developments in the MSV technologies, and identifies the major components of future product development infrastructure, with particular emphasis on the role of MSV technologies. C1 Old Dominion Univ, NASA, Langley Res Ctr, Ctr Adv Engn Environm, Hampton, VA USA. RP Noor, AK (reprint author), Old Dominion Univ, NASA, Langley Res Ctr, Ctr Adv Engn Environm, Hampton, VA USA. NR 35 TC 0 Z9 0 U1 0 U2 1 PU SAXE-COBURG PUBLICATIONS PI EDINBURGH PA 10 SAXE-COBURG PLACE, EDINBURGH EH3 5BR, SCOTLAND BN 978-1-874672-22-7 PY 2004 BP 1 EP 18 PG 18 WC Computer Science, Interdisciplinary Applications SC Computer Science GA BGO98 UT WOS:000249125300001 ER PT J AU Mushotzky, R AF Mushotzky, R TI Ultra-luminous sources in nearby galaxies SO PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT LA English DT Article; Proceedings Paper CT International Workshop on Stellar-Mass, International-Mass, and Supermassive Black Holes CY OCT 28-31, 2003 CL Kyoto Int Commun House, Kyoto, JAPAN HO Kyoto Int Commun House ID X-RAY SOURCE; MASS BLACK-HOLES; OPTICAL COUNTERPART; ACCRETION DISKS; RADIO-EMISSION; CHANDRA; IC-342; POPULATION; DISCOVERY; BINARY AB I briefly review much of the X-ray and optical data on the nature of the ULXs in nearby galaxies. I present new results on radio emission, finding that the radio is usually rather luminous and extended. I review the X-ray data on timing and spectra. There is no direct evidence in the X-ray data for either geometric or relativistic beaming and in 4 objects direct evidence against beaming. I argue that the X-ray timing and spectral properties of these objects, are in general, not good analogs of AGN or galactic black holes and that the ULX may represent a new mode of accretion only rarely seen in other objects. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 48 TC 33 Z9 33 U1 3 U2 3 PU PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE PI KYOTO PA C/O KYOTO UNIV, YUKAWA HALL, KYOTO, 606-8502, JAPAN SN 0375-9687 J9 PROG THEOR PHYS SUPP JI Prog. Theor. Phys. Suppl. PY 2004 IS 155 BP 27 EP 44 PG 18 GA 874LB UT WOS:000225350800005 ER PT J AU Ebisawa, K Zycki, PT Kubota, A Mizuno, T Watarai, K AF Ebisawa, K Zycki, PT Kubota, A Mizuno, T Watarai, K TI Accretion disk spectra of the ultra-luminous X-ray sources in nearby spiral galaxies and galactic superluminal jet sources SO PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT LA English DT Article; Proceedings Paper CT International Workshop on Stellar-Mass, International-Mass, and Supermassive Black Holes CY OCT 28-31, 2003 CL Kyoto Int Commun House, Kyoto, JAPAN HO Kyoto Int Commun House ID BLACK-HOLE; GRO J1655-40; MODEL AB Ultra-luminous Compact X-ray Sources (ULXs) in nearby spiral galaxies and Galactic superluminal jet sources share the common spectral characteristic that they have unusually high disk temperatures which cannot be explained in the framework of the standard optically thick accretion disk in the Schwarzschild metric. On the other hand, the standard accretion disk around the Kerr black hole might explain the observed high disk temperature, as the inner radius of the Kerr disk gets smaller and the disk temperature can be consequently higher. However, we point out that the observable Kerr disk spectra becomes significantly harder than Schwarzschild disk spectra only when the disk is highly inclined. This is because the emission from the innermost part of the accretion disk is Doppler-boosted for an edge-on Kerr disk, while hardly seen for a, face-on disk. The Galactic superluminal jet sources are known to be highly inclined systems, thus their energy spectra may be explained with the standard Kerr disk with known black hole masses. For ULXs, on the other hand, the standard Kerr disk model seems implausible, since it is highly unlikely that their accretion disks are preferentially inclined, and, if edge-on Kerr disk model is applied, the black hole mass becomes unreasonably large (greater than or similar to 300 M-circle dot). Instead, the slim disk (advection dominated optically thick disk) model is likely to explain the observed super-Eddington luminosities, hard energy spectra, and spectral variations of ULXs. We suggest that ULXs are accreting black holes with a few tens of solar mass, which is not unexpected from the standard stellar evolution scenario, and that their X-ray emission is from the slim disk shining at super-Eddington luminosities. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. INTEGRAL Sci Data Ctr, CH-1290 Chavannes Des Bois, Switzerland. Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA. Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 6068502, Japan. RP Ebisawa, K (reprint author), Univ Space Res Assoc, 7501 Forbes Blvd 206, Searbrook, MD 20706 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE PI KYOTO PA C/O KYOTO UNIV, YUKAWA HALL, KYOTO, 606-8502, JAPAN SN 0375-9687 J9 PROG THEOR PHYS SUPP JI Prog. Theor. Phys. Suppl. PY 2004 IS 155 BP 67 EP 70 PG 4 GA 874LB UT WOS:000225350800009 ER PT J AU Uttley, P McHardy, IM AF Uttley, P McHardy, IM TI A brief review of long-term X-ray and optical variability in radio-quiet AGN SO PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT LA English DT Article; Proceedings Paper CT International Workshop on Stellar-Mass, International-Mass, and Supermassive Black Holes CY OCT 28-31, 2003 CL Kyoto Int Commun House, Kyoto, JAPAN HO Kyoto Int Commun House ID ACTIVE GALACTIC NUCLEI; SEYFERT 1 GALAXIES; BLACK-HOLE MASSES; CYGNUS X-1; ULTRAVIOLET VARIABILITY; CONTINUUM VARIABILITY; POWER SPECTRA; XMM-NEWTON; NGC 3516; EMISSION AB Long-time-scale X-ray and optical variability is a key characteristic of AGN. Here, we summarise our current understanding of the X-ray and optical continuum variability of radio-quiet AGN and the relation between the two bands. We demonstrate the strong connection between the X-ray variability properties of AGN and the variability of stellar-mass black hole candidates on much shorter time-scales, and discuss the implications of this result for the origins of the variability. The relationship between optical and X-ray variability is complex, with some AGN showing strong X-ray/optical correlations while others show no obvious correlation. We suggest a possible explanation for this variety of behaviour. C1 Univ Southampton, Sch Phys & Astron, Southampton S017 1BJ, Hants, England. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Uttley, P (reprint author), Univ Southampton, Sch Phys & Astron, Southampton S017 1BJ, Hants, England. EM pu@milkyway.gsfe.nasa.gov NR 51 TC 5 Z9 5 U1 0 U2 0 PU PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE PI KYOTO PA C/O KYOTO UNIV, YUKAWA HALL, KYOTO, 606-8502, JAPAN SN 0375-9687 J9 PROG THEOR PHYS SUPP JI Prog. Theor. Phys. Suppl. PY 2004 IS 155 BP 170 EP 177 PG 8 GA 874LB UT WOS:000225350800022 ER PT J AU Kawai, N Matsuoka, M Yoshida, A Shirasaki, Y Ricker, G Doty, J Vanderspek, R Crew, G Villasenor, J Atteia, JL Fenimore, EE Galassi, M Lamb, DQ Graziani, C Hurley, K Jernigan, JG Woosley, S Martel, F Monnelly, G Prigozhin, G Olive, JF Dezalay, JP Boer, M Pizzichini, G Cline, T Levine, A Morgan, E Tamagawa, T Butler, N Sakamoto, T Torii, K Barraud, C Donaghy, T Suzuki, M Nakagawa, Y Takahashi, D Tavenner, T Sato, R Urata, Y Manchanda, R Azzibrouck, G Braga, J Takagishi, K Yamauchi, M Hatsukade, I AF Kawai, N Matsuoka, M Yoshida, A Shirasaki, Y Ricker, G Doty, J Vanderspek, R Crew, G Villasenor, J Atteia, JL Fenimore, EE Galassi, M Lamb, DQ Graziani, C Hurley, K Jernigan, JG Woosley, S Martel, F Monnelly, G Prigozhin, G Olive, JF Dezalay, JP Boer, M Pizzichini, G Cline, T Levine, A Morgan, E Tamagawa, T Butler, N Sakamoto, T Torii, K Barraud, C Donaghy, T Suzuki, M Nakagawa, Y Takahashi, D Tavenner, T Sato, R Urata, Y Manchanda, R Azzibrouck, G Braga, J Takagishi, K Yamauchi, M Hatsukade, I TI HETE-2 observations of gamma-ray bursts and their follow-ups SO PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT LA English DT Article; Proceedings Paper CT International Workshop on Stellar-Mass, International-Mass, and Supermassive Black Holes CY OCT 28-31, 2003 CL Kyoto Int Commun House, Kyoto, JAPAN HO Kyoto Int Commun House ID EARLY OPTICAL-EMISSION; AFTERGLOW; DISCOVERY; SUPERNOVA; FLASHES AB The High Energy Transient Explorer 2 (HETE-2), launched in October 2000, is currently localizing gamma-ray bursts (GRBs) at a rate of similar to20 yr(-1) many in real time. As of September 2003, HETE-2 had localized 47 GRBs; 16 localizations had led to the detection of an X-ray, optical, or radio afterglows. The prompt position notification of HETE-2 enabled probing the nature of so-called "dark bursts" for which no optical afterglows were found despite of accurate localizations. In some cases, the optical afterglow was found to be intrinsically faint, and its flux declined rapidly. In another case, the optical emission was likely to be extinguished by the dust in the vicinity of the GRB source. The bright afterglows of GRB021004 and GRB030329 were observed in unprecedented details by telescopes around the world. Strong evidence for the association of long GRBs with the core-collapse supernovae was found. HETE-2 has localized almost as many X-ray rich GRBs as classical GRBs. The nature of the X-ray rich GRBs a-rid X-ray flashes have been studied systematically with HETE-2, and they are found to have many properties in common with the classical GRBs, suggesting that they are a single phenomenon. C1 Tokyo Inst Technol, Dept Phys, Tokyo 1528551, Japan. RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. Natl Space Dev Agcy Japan, Tsukuba, Ibaraki 3058505, Japan. Aoyama Gakuin Univ, Sagamihara, Kanagawa 2298558, Japan. Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Observ Midi Pyrenees, F-31400 Toulouse, France. Los Alamos Natl Lab, Los Alamos, NM USA. Univ Chicago, Ctr Astron & Astrophys, Chicago, IL 60637 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. Ctr Etud Spatiale Rayonnements, Toulouse, France. CNR, IASF, TESRE, I-40126 Bologna, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. Univ Sci & Tech Masuku, Franceville, Gabon. Inst Nacl Pesquisas Espaciais, BR-12201 Sao Jose Dos Campos, Brazil. Miyazaki Univ, Fac Engn, Miyazaki 8892192, Japan. RP Tokyo Inst Technol, Dept Phys, Tokyo 1528551, Japan. OI Boer, Michel/0000-0001-9157-4349 NR 45 TC 0 Z9 0 U1 0 U2 0 PU PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE PI KYOTO PA C/O KYOTO UNIV, YUKAWA HALL, KYOTO, 606-8502, JAPAN SN 0375-9687 J9 PROG THEOR PHYS SUPP JI Prog. Theor. Phys. Suppl. PY 2004 IS 155 BP 279 EP 286 PG 8 GA 874LB UT WOS:000225350800038 ER PT J AU Fiorito, R Titarchuk, L AF Fiorito, R Titarchuk, L TI Correlations of power-law spectral and QPO features in black hole candidate sources SO PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT LA English DT Article; Proceedings Paper CT International Workshop on Stellar-Mass, International-Mass, and Supermassive Black Holes CY OCT 28-31, 2003 CL Kyoto Int Commun House, Kyoto, JAPAN HO Kyoto Int Commun House ID FREQUENCY AB Recent studies have shown that strong correlations are observed between low frequency QPO's and the spectral power law index for a number of black hole candidate sources (BHC's), when these sources exhibit quasi-steady hard X-ray emission states. The dominant long standing interpretation of QPO's is that they are produced in and are the signature of the thermal accretion disk. Paradoxically, strong QPO's are present even in the cases where the thermal component is negligible. We present a model which identifies the origin of the QPO's and relates them directly to the properties of a compact coronal region which is bounded by the adjustment from Keplerian to sub-Keplerian inflow into the BH and which is primarily responsible for the observed power law spectrum. The model also predicts the relationship between high and low frequency QPO's and shows how BH's can be unique identified from observations of the soft states of NS's and BHC's. C1 Catholic Univ Amer, Washington, DC 20064 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. George Mason Univ, USN, Res Lab, Fairfax, VA 22030 USA. RP Fiorito, R (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE PI KYOTO PA C/O KYOTO UNIV, YUKAWA HALL, KYOTO, 606-8502, JAPAN SN 0375-9687 J9 PROG THEOR PHYS SUPP JI Prog. Theor. Phys. Suppl. PY 2004 IS 155 BP 325 EP 326 PG 2 WC Physics, Multidisciplinary SC Physics GA 874LB UT WOS:000225350800052 ER PT J AU Heike, K Awaki, H Hayashida, K Weaver, KA AF Heike, K Awaki, H Hayashida, K Weaver, KA TI A study of X-ray sources in the central region of NGC 1569 with Chandra SO PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT LA English DT Article; Proceedings Paper CT International Workshop on Stellar-Mass, International-Mass, and Supermassive Black Holes CY OCT 28-31, 2003 CL Kyoto Int Commun House, Kyoto, JAPAN HO Kyoto Int Commun House ID GLOBAL PARAMETERS; GALAXIES AB The dwarf starburst galaxy NGC 1569 was observed for 96.8 ks with Chandra. We detected several variable X-ray point sources in the central region of NGC 1569. Inparticular, two bright point sources, CXOU 043048.1+645050 and CXOU 043048.6+645058, exhibit a prominent variability in time. Fitting with the disk blackbody model, we find that CXOU 043048.1+645050 may be a stellar mass black hole with similar to 20Mcircle dot. From the fact that CXOU 043048.6+645058 has a short time variability and flat spectrum, we concluded that this source may be a neutron star binary. We calculated the luminosity ratio of the soft X-ray band to other energy bands, and find that NGC 1569 has a typical luminosity ratio found in starburst galaxies. C1 Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan. Osaka Univ, Dept Astrophys, Toyonaka, Osaka 5600043, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Heike, K (reprint author), Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan. EM k-heike@astro.phys.sci.ehime-u.ac.jp NR 7 TC 0 Z9 0 U1 0 U2 0 PU PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE PI KYOTO PA C/O KYOTO UNIV, YUKAWA HALL, KYOTO, 606-8502, JAPAN SN 0375-9687 J9 PROG THEOR PHYS SUPP JI Prog. Theor. Phys. Suppl. PY 2004 IS 155 BP 335 EP 336 PG 2 WC Physics, Multidisciplinary SC Physics GA 874LB UT WOS:000225350800057 ER PT J AU Ohno, I Fukazawa, Y Iyomoto, N AF Ohno, I Fukazawa, Y Iyomoto, N TI The hard X-ray observation of the Compton-thick Seyfert 2 Galaxy Mrk 1210 SO PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT LA English DT Article; Proceedings Paper CT International Workshop on Stellar-Mass, International-Mass, and Supermassive Black Holes CY OCT 28-31, 2003 CL Kyoto Int Commun House, Kyoto, JAPAN HO Kyoto Int Commun House AB We observed the Seyfert 2 galaxy Mrk 1210 with BeppoSAX and found that the X-ray spectral properties are quite different from those found in the previous observation by ASCA. We find that the reflection component describes the previously observed ASCA spectra with good precision. This indicates that the dramatic spectral variability can be attributed to a large change in the absorption column density by a factor greater than 5, rather than the variability of the nuclear emission. In this case, the torus is not homogeneous but is like a blob of size < 0.001 pc. C1 Hiroshima Univ, Sch Sci, Dept Phys Sci, Higashihiroshima 7398526, Japan. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Ohno, I (reprint author), Hiroshima Univ, Sch Sci, Dept Phys Sci, Higashihiroshima 7398526, Japan. NR 5 TC 0 Z9 0 U1 0 U2 1 PU PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE PI KYOTO PA C/O KYOTO UNIV, YUKAWA HALL, KYOTO, 606-8502, JAPAN SN 0375-9687 J9 PROG THEOR PHYS SUPP JI Prog. Theor. Phys. Suppl. PY 2004 IS 155 BP 397 EP 398 PG 2 GA 874LB UT WOS:000225350800088 ER PT J AU Sano, T Inutsuka, S Turner, NJ Stone, JM AF Sano, T Inutsuka, S Turner, NJ Stone, JM TI Angular momentum transport by MHD turbulence in accretion disks SO PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT LA English DT Article; Proceedings Paper CT International Workshop on Stellar-Mass, International-Mass, and Supermassive Black Holes CY OCT 28-31, 2003 CL Kyoto Int Commun House, Kyoto, JAPAN HO Kyoto Int Commun House ID 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; INSTABILITY AB The saturation level of the magnetorotational instability (MRI) is investigated using three-dimensional MHD simulations. The shearing box approximation is adopted and the vertical component of gravity is ignored, so that the evolution of the MRI is followed in a small local part of the disk. We focus on the dependence of the saturation level of the stress on the gas pressure, which is a key assumption in the standard alpha disk model. From our numerical experiments it is found that there is a weak power-law relation between the saturation level of the Maxwell stress and the gas pressure in the nonlinear regime; the higher the gas pressure, the larger the stress. Our numerical results are qualitatively consistent with an idea that the saturation level of the MRI is determined by a balance between the growth of the MRI and the dissipation of the field through reconnection. C1 Osaka Univ, Inst Laser Engn, Suita, Osaka 5650871, Japan. Kyoto Univ, Dept Phys, Kyoto 6068502, Japan. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Osaka Univ, Inst Laser Engn, Suita, Osaka 5650871, Japan. RI Sano, Takayoshi/E-7860-2010; OI Turner, Neal/0000-0001-8292-1943 NR 5 TC 1 Z9 1 U1 0 U2 0 PU PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE PI KYOTO PA C/O KYOTO UNIV, YUKAWA HALL, KYOTO, 606-8502, JAPAN SN 0375-9687 J9 PROG THEOR PHYS SUPP JI Prog. Theor. Phys. Suppl. PY 2004 IS 155 BP 409 EP 410 PG 2 GA 874LB UT WOS:000225350800094 ER PT S AU Berejikian, B Flagg, T Kline, P AF Berejikian, B Flagg, T Kline, P BE Nickum, MJ Mazik, PM Nickum, JG Mackinlay, DD TI Release of captively reared adult anadromous salmonids for population maintenance and recovery: Biological trade-offs and management considerations SO PROPAGATED FISH IN RESOURCE MANAGEMENT SE AMERICAN FISHERIES SOCIETY SYMPOSIUM LA English DT Proceedings Paper CT Symposium on Propagated Fish in Resource Management CY JUN 16-18, 2003 CL Boise, ID ID CHINOOK SALMON; ONCORHYNCHUS-KISUTCH; COHO SALMON; ATLANTIC SALMON; SOCKEYE-SALMON; REPRODUCTIVE-BEHAVIOR; AGONISTIC BEHAVIOR; BREEDING SUCCESS; PACIFIC SALMON; COMPETITIVE ABILITY AB Captive broodstocks have been initiated for maintenance and recovery of imperiled anadromous satmonid populations because they can provide a rapid demographic boost and reduce short-term extinction risk. As with captive propagation programs for other vertebrates, difficulties with reintroduction to the natural environment may impede success in achieving the prograds objectives. Strategies for reintroduction of anadromous salmonid captive broodstocks in the United States and Canada include release of captively reared adults (currently four programs), stocking their offspring as eyed eggs (two programs), part (six programs), or smolts (nine programs). Captive broodstock programs that release adults considered the management objectives of (i) evaluating of different reintroduction strategies, and (ii) spreading the risk of failure of any one particular strategy to be much more important than programs that do not release adults. This distinction indicates that the programs releasing adults consider the strategy to be an experimental one that may serve to offset potential risks associated with juvenile release options. However, the finding that preventing extinction was considered to be very important in adult and juvenile release programs alike indicates that programs releasing adults believe the strategy, at a minimum, will not impede that objective. We summarized the salmonid literature on (1) natural and sexual selection during reproduction, (2) homing and straying, (3) rearing effects on social behavior, (4) domestication, and (5) survival as it relates to biological trade-offs of different reintroduction strategies for captive broodstocks. The adult release strategy provides potential biological benefits that include the opportunity for natural and sexual selection to occur on the spawning grounds-selection that is relaxed during artificial spawning. Adult release and egg stocking may reduce potential for unnaturally high straying rates and may minimize domestication selection of the offspring compared to programs that artificially spawn adults and release their offspring as smolts. The potential benefits of adult and egg releases must be weighed against (and may be offset by) the greater F-1 production that could be achieved by releasing hatchery-reared smolts. A variety of reintroduction strategies will likely continue to be appropriate for captive broodstock programs. C1 NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Resource Enhancement & Utilizat Technol Div, Manchester, WA 98353 USA. RP Berejikian, B (reprint author), NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Resource Enhancement & Utilizat Technol Div, POB 130, Manchester, WA 98353 USA. NR 76 TC 12 Z9 12 U1 1 U2 8 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE, STE 110, BETHESDA, MD 20814-2199 USA SN 0892-2284 BN 1-888569-69-7 J9 AM FISH S S PY 2004 VL 44 BP 233 EP 245 PG 13 WC Fisheries SC Fisheries GA BBW47 UT WOS:000228130200020 ER PT S AU Thrower, FP Joyce, JE AF Thrower, FP Joyce, JE BE Nickum, MJ Mazik, PM Nickum, JG Mackinlay, DD TI Effects of 70 years of freshwater residency on survival, growth, early maturation, and smolting in a stock of anadromous rainbow trout from southeast Alaska SO PROPAGATED FISH IN RESOURCE MANAGEMENT SE AMERICAN FISHERIES SOCIETY SYMPOSIUM LA English DT Proceedings Paper CT Symposium on Propagated Fish in Resource Management CY JUN 16-18, 2003 CL Boise, ID ID ONCORHYNCHUS-MYKISS; GENETIC-VARIATION; STEELHEAD TROUT; SALMON; POPULATION; HATCHERY; SIZE AB Progeny of wild, freshwater sequestered (resident) rainbow trout Oncorhynchus mykiss, descendants of a stocking of steelhead (anadromous rainbow trout) in 1926, and progeny of the wild, ancestral steelhead lineage and their reciprocal crosses were compared for two brood years in a hatchery environment to determine the effects of 70 years of freshwater residency on growth, survival, early maturity and smelting proportion. Resulting smolts were tagged, released, and recovered as maturing adults to evaluate marine survival. For the 1996 brood, 75 families were maintained in separate freshwater raceways for 10 months. Approximately 100 fish from each family were tagged with passive integrated transponder tags, pooled by type, and cultured until age 2. An additional group was tagged with coded-wire tags and reared in the same manner. For the 1997 brood, 80 families were coded-wire-tagged, separated by breeding type, and cultured at different densities. Size-at-age and survival were reduced significantly in progeny of resident females when compared with progeny from anadromous females during the first 2 months after first feeding. No significant differences were observed in subsequent growth or survival through age 2. A higher proportion of smolting at age 2 and a lower proportion of early male maturity was observed in families from anadromous parents. Smolts produced by anadromous parents had four to five times higher marine survival than those from resident parents. While smolting proportions and smolt survival were lower for the progeny of freshwater resident fish, the results indicate that significant numbers of smolts and adults can still be produced by populations landlocked for up to 70 years and 20 generations. The results have substantial implications for the use of natural freshwater environments for the preservation of endangered anadromous stocks of rainbow trout, the rehabilitation of anadromous stocks, and the actual effective breeding size of anadromous rainbow trout populations. C1 Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Lab, Juneau, AK 99801 USA. RP Thrower, FP (reprint author), Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Lab, 11305 Glacier Highway, Juneau, AK 99801 USA. NR 18 TC 14 Z9 15 U1 1 U2 5 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE, STE 110, BETHESDA, MD 20814-2199 USA SN 0892-2284 BN 1-888569-69-7 J9 AM FISH S S PY 2004 VL 44 BP 485 EP 496 PG 12 WC Fisheries SC Fisheries GA BBW47 UT WOS:000228130200040 ER PT J AU Rosipal, R Trejo, LJ AF Rosipal, R Trejo, LJ TI Kernel PLS estimation of single-trial event-related potentials SO PSYCHOPHYSIOLOGY LA English DT Meeting Abstract CT 44th Annual Meeting of the Society-for-Psychophysiological-Research CY OCT 20-24, 2004 CL Santa Fe, NM SP Soc Pychophysiol Res DE nonparametric smoothing; single-trial ERPs; cognitive fatigue C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RI Rosipal, Roman/B-8060-2008 NR 0 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0048-5772 J9 PSYCHOPHYSIOLOGY JI Psychophysiology PY 2004 VL 41 SU 1 BP S94 EP S94 PG 1 WC Psychology, Biological; Neurosciences; Physiology; Psychology; Psychology, Experimental SC Psychology; Neurosciences & Neurology; Physiology GA 849RL UT WOS:000223558200362 ER PT J AU Trejo, LJ Kochavi, R Kubitz, K Montgomery, LD Rosipal, R Matthews, B AF Trejo, LJ Kochavi, R Kubitz, K Montgomery, LD Rosipal, R Matthews, B TI Measures and models for estimating and predicting cognitive fatigue SO PSYCHOPHYSIOLOGY LA English DT Meeting Abstract CT 44th Annual Meeting of the Society-for-Psychophysiological-Research CY OCT 20-24, 2004 CL Santa Fe, NM SP Soc Pychophysiol Res DE cognitive fatigue; EEG/ERP; models and measures C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Towson State Univ, Baltimore, MD 21204 USA. RI Rosipal, Roman/B-8060-2008 NR 0 TC 1 Z9 2 U1 0 U2 1 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0048-5772 J9 PSYCHOPHYSIOLOGY JI Psychophysiology PY 2004 VL 41 SU 1 BP S86 EP S86 PG 1 WC Psychology, Biological; Neurosciences; Physiology; Psychology; Psychology, Experimental SC Psychology; Neurosciences & Neurology; Physiology GA 849RL UT WOS:000223558200333 ER PT B AU Jones, FC AF Jones, FC BE Chen, P Reil, K TI An overview of astrophysical accelerators SO QUANTUM ASPECTS OF BEAM PHYSICS LA English DT Proceedings Paper CT Joint 28th ICFA Advanced Beam Dynamics and Advanced and Novel Accelerators Workshop on Quantum Aspects of Beam Physics CY JAN 07-11, 2003 CL Hiroshima, JAPAN ID COSMIC-RAYS; BLACK-HOLES; ENERGY AB There have been many acceleration mechanisms proposed to explain the presence of energetic charged particles that appear to fill the observable universe. All of these processes share an underlying similarity and they also appear to share a common upper energy limit that the charged particles are able to attain. I will discuss some of these mechanisms, several of which are presented at this conference session, and point out there similarities and argue that all of them are subject to the same scaling law that limits their maximum attainable energy (the Hillas rule). C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Jones, FC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 981-256-069-6 PY 2004 BP 373 EP 383 DI 10.1142/9789812702333_0038 PG 11 WC Astronomy & Astrophysics; Physics, Atomic, Molecular & Chemical; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA BCL63 UT WOS:000229929700038 ER PT S AU Strekalov, D Matsko, AB Maleki, L AF Strekalov, D Matsko, AB Maleki, L BE Meyers, RE Shih, Y TI Limitation on two-photon temporal correlation SO QUANTUM COMMUNICATIONS AND QUANTUM IMAGING II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Quantum Communications and Quantum Imaging II CY AUG 04-06, 2004 CL Denver, CO SP SPIE DE entanglement; biphoton; parametric down conversion; correlation function ID PODOLSKY-ROSEN CHANNELS; QUANTUM CRYPTOGRAPHY; STATE; EMISSION AB We show theoretically that two-photon correlation time for a biphoton, a pair of entangled photons generated in the process of parametric down conversion, is limited by the inverse frequency width of the single-photon spectrum, which is limited by the dispersion of the nonlinear material used for the pair generation. The dispersion is determined by the transparency window of the material, which provides the ultimate limitation for the two-photon correlation time. We discuss several experimental approaches enabling realization of such a limiting case. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Strekalov, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 26 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5489-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5551 BP 50 EP 59 DI 10.1117/12.562102 PG 10 WC Optics; Imaging Science & Photographic Technology SC Optics; Imaging Science & Photographic Technology GA BBJ22 UT WOS:000225749100006 ER PT S AU Kloepfer, JA Mielke, RE Nadeau, JL AF Kloepfer, JA Mielke, RE Nadeau, JL BE Huffaker, DL Bhattacharya, P TI CdSe quantum dot internalization by Bacillus subtilis and Escherichia coli SO QUANTUM DOTS, NANOPARTICLES, AND NANOCLUSTERS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Quantum Dots, Nanoparticles, and Nanoclusters CY JAN 26-27, 2004 CL San Jose, CA SP SPIE DE semiconductor; nanocrystal; quantum dot; CdSe; bacteria; labeling; emission lifetime; adenine ID RECOMBINANT PROTEIN; NANOCRYSTALS; LUMINESCENCE; SPECTROSCOPY; SURFACE AB Biological labeling has been demonstrated with CdSe quantum dots in a variety of animal cells, but bacteria are harder to label because of their cell walls. We discuss the challenges of using minimally coated, bare CdSe quantum dots as luminescent internal labels for bacteria. These quantum dots were solubilized with mercaptoacetic acid and conjugated to adenine. Significant evidence for the internal staining of Bacillus subtilis (Gram positive) and Escherichia coli (Gram negative) using these structures is presented via steady-state emission, epifluorescence microscopy, transmission electron microscopy, and energy dispersive spectroscopy. In particular, the E. coli adenine auxotroph, and not the wild type, took up adenine coated quantum dots, and this only occurred in adenine deficient growth media. Labeling strength was enhanced by performing the incubation under room light. This process was examined with steady-state emission spectra and time-resolved luminescence profiles obtained from time-correlated-single-photon counting. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kloepfer, JA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 24 TC 2 Z9 2 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5269-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5361 BP 133 EP 141 DI 10.1117/12.539152 PG 9 WC Materials Science, Multidisciplinary; Optics; Physics, Condensed Matter SC Materials Science; Optics; Physics GA BAM21 UT WOS:000222821000016 ER PT S AU Williams, CP AF Williams, CP BE Donkor, E Pirich, AR Brandt, HE TI Probabilistic non-unitary quantum computing SO QUANTUM INFORMATION AND COMPUTATION II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Quantum Information and Computation II CY APR 12-14, 2004 CL Orlando, FL SP SPIE DE non-unitary; quantum computing; probabilistic; non-deterministic; quantum gates; quantum circuits; NP-Complete; NP-Hard; quantum search; lattice ID COMPUTATION; GATES AB In [1] Gingrich and Williams extended the standard quantum circuit model of quantum computation to include gates that perform arbitrary linear, yet non-unitary, transformations of their input state. In this paper we use this theory to construct quantum circuits that perform desired non-unitary state transformations of the sort arising in lattice-based quantum search. Such n-qubit non-unitary gates cannot be achieved deterministically, but they can be achieved probabilistically using a single ancilla. Our approach is to use the n-qubit non-unitary gate to design an (n+1)-qubit Hamiltonian that can be seen to induce a suitable conditional dynamics such that whenever the output value of the ancilla qubit is measured and found to be \0>, then the remaining (unmeasured) n qubits will contain the desired non-unitary transform of the n-qubit input state. The scheme is necessarily probabilistic because we cannot force the measurement on the ancilla qubit to return the value we want. Fortunately, however, failed attempts are found to disturb the n-qubit input state very little. This allows us to re-use the result of successive "failed" attempts until the success condition is finally attained, and we give analytic expressions for the success probability and net fidelity in this case. By using our previous method for designing a quantum circuit for an arbitrary n-qubit gate in conjunction with our new probabilistic nonunitary procedure we are able to compute an explicit quantum circuit sufficient to implement an arbitrary linear, yet non-unitary, transformation of an input pure or mixed n-qubit state, using only a single copy of the input state. This allows us to extend the repertoire of computations that may be performed on a quantum computer, and in particular, gives the first explicit construction of the quantum circuits needed to perform some of the key operations arising in quantum lattice search. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Williams, CP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5359-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5436 BP 297 EP 306 DI 10.1117/12.542413 PG 10 WC Computer Science, Theory & Methods SC Computer Science GA BAW94 UT WOS:000223995400031 ER PT S AU Didomenico, LD Lee, H Kok, P Dowling, JP AF Didomenico, LD Lee, H Kok, P Dowling, JP BE Razeghi, M Brown, GJ TI Quantum interferometric sensors SO QUANTUM SENSING AND NANOPHOTONIC DEVICES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Quantum Sensing and Nanophotonic Devices CY JAN 25-29, 2004 CL San Jose, CA SP SPIE DE interferometry; metrology; quantum entanglement; Heisenberg limit; gravimeters; gyroscopes; atomic clocks; atom interferometers ID LIMIT; COMPUTATION; PHOTONS; STATES; NOISE; SU(2) AB Quantum entanglement has the potential to revolutionize the entire field of interferometric sensing by providing many orders of magnitude improvement in interferometer sensitivity. The quantum entangled particle interferometer approach is very general and applies to many types of interferometers. In particular, without nonlocal entanglement, a generic classical interferometer has a statistical-sampling shot-noise limited sensitivity that scales like 1/rootN, where N is the number of particles passing through the interferometer per unit time. However, if carefully prepared quantum correlations are engineered between the particles, then the interferometer sensitivity improves by a factor of rootN to scale like 1rootN, which is the limit imposed by the Heisenberg Uncertainty Principle. For optical interferometers operating at milliwatts of optical power, this quantum sensitivity boost corresponds to an eight-order-of-magnitude improvement of signal to noise. This effect can translate into a tremendous science pay-off for NASA-JPL missions. For example, one application of this new effect is to fiber optical gyroscopes for deep-space inertial guidance and tests of General Relativity (Gravity Probe B). Another application is to ground and orbiting optical interferometers for gravity wave detection, Laser Interferometer Gravity Observatory (LIGO) and the European Laser Interferometer Space Antenna (LISA), respectively. Other applications are to Satellite-to-Satellite laser Interferometry (SSI) proposed for the next generation Gravity Recovery And Climate Experiment (GRACE II). C1 CALTECH, Jet Prop Lab, Quantum Comp Technol Grp, Pasadena, CA 91109 USA. RP Didomenico, LD (reprint author), CALTECH, Jet Prop Lab, Quantum Comp Technol Grp, 4800 Oak Grove Dr,Sec 367, Pasadena, CA 91109 USA. RI Kok, Pieter/B-1658-2010 NR 25 TC 1 Z9 1 U1 1 U2 8 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5267-X J9 P SOC PHOTO-OPT INS PY 2004 VL 5359 BP 169 EP 176 DI 10.1117/12.516220 PG 8 WC Materials Science, Multidisciplinary; Optics; Physics, Condensed Matter SC Materials Science; Optics; Physics GA BAQ21 UT WOS:000223199200015 ER PT J AU Goldhagen, P Clem, JM Wilson, JW AF Goldhagen, P Clem, JM Wilson, JW TI The energy spectrum of cosmic-ray induced neutrons measured on an airplane over a wide range of altitude and latitude SO RADIATION PROTECTION DOSIMETRY LA English DT Article; Proceedings Paper CT 9th Symposium on Neutron Dosimetry CY SEP 28-OCT 03, 2003 CL Delft Univ Technol, Delft, NETHERLANDS HO Delft Univ Technol ID EXPOSURE; FLUENCE; ABOARD AB Crews of high-altitude aircraft are exposed to radiation from galactic cosmic rays (GCRs). To help determine such exposures, the Atmospheric Ionizing Radiation Project, an international collaboration of 15 laboratories, made simultaneous radiation measurements with 14 instruments on a NASA ER-2 high-altitude airplane. The primary instrument was a sensitive extended-energy multisphere neutron spectrometer. Its detector responses were calculated for energies up to 100 GeV using the radiation transport code MCNPX 2.5.d with improved nuclear models and including the effects of the airplane structure. New calculations of GCR-induced particle spectra in the atmosphere were used to correct for spectrometer counts produced by protons, pions and light nuclear ions. Neutron spectra were unfolded from the corrected measured count rates using the deconvolution code MAXED 3.1. The results for the measured cosmic-ray neutron spectrum (thermal to >10 GeV), total neutron fluence rate, and neutron dose equivalent and effective dose rates, and their dependence on altitude and geomagnetic cut-off agree well with results from recent calculations of GCR-induced neutron spectra. C1 US Dept Homeland Secur, Environm Measurements Lab, New York, NY 10014 USA. Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Goldhagen, P (reprint author), US Dept Homeland Secur, Environm Measurements Lab, New York, NY 10014 USA. EM Paul.Goldhagen@eml.doe.gov NR 23 TC 67 Z9 70 U1 0 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0144-8420 J9 RADIAT PROT DOSIM JI Radiat. Prot. Dosim. PY 2004 VL 110 IS 1-4 SI SI BP 387 EP 392 DI 10.1093/rpd/nch216 PG 6 WC Environmental Sciences; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA 856PV UT WOS:000224058000066 PM 15353679 ER PT J AU Clem, JM De Angelis, G Goldhagen, P Wilson, JW AF Clem, JM De Angelis, G Goldhagen, P Wilson, JW TI New calculations of the atmospheric cosmic radiation field - Results for neutron spectra SO RADIATION PROTECTION DOSIMETRY LA English DT Article; Proceedings Paper CT 9th Symposium on Neutron Dosimetry CY SEP 28-OCT 03, 2003 CL Delft Univ Technol, Delft, NETHERLANDS HO Delft Univ Technol ID NEAR-EARTH ORBIT; HELIUM SPECTRA; RAY PROTON; ENERGY-SPECTRUM; ENVIRONMENT; MODULATION; VALIDATION; AIRPLANE; ABOARD; MODEL AB The propagation of primary cosmic rays through the Earth's atmosphere and the energy spectra of the resulting secondary particles have been calculated using the Monte Carlo transport code FLUKA with several novel auxiliary methods. Solarmodulated primary cosmic ray spectra were determined through an analysis of simultaneous proton and helium measurements made on spacecraft or high-altitude balloon flights. Primary protons and helium ions are generated within the rigidity range of 0.5 GV-20 TV, uniform in cos(2)theta. For a given location, primaries above the effective angle-dependent geomagnetic cut-off rigidity, and re-entrant albedo protons, are transported through the atmosphere. Helium ions are initially transported using a separate transport code called HEAVY to simulate fragmentation. HEAVY interfaces with FLUKA to provide interaction starting points for each nucleon originating from a helium nucleus. Calculated cosmic ray neutron spectra and consequent dosimetric quantities for locations with a wide range of altitude (atmospheric depth) and geomagnetic cut-off are presented and compared with measurements made on a high-altitude aeroplane. Helium ion propagation using HEAVY and inclusion of re-entrant albedo protons with the incident primary spectra significantly improved the agreement of the calculated cosmic ray neutron spectra with measured spectra. These cosmic ray propagation calculations provide the basis for a new atmospheric ionising radiation (AIR) model for air-crew dosimetry, calculation of effects on microelectronics, production of cosmogenic radionuclides and other uses. C1 Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Old Dominion Univ, Norfolk, VA 23508 USA. Ist Super Sanita, I-00161 Rome, Italy. US Dept Homeland Secur, Environm Measurements Lab, New York, NY 10014 USA. RP Clem, JM (reprint author), Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. EM clem@bartol.udel.edu NR 29 TC 21 Z9 21 U1 0 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0144-8420 J9 RADIAT PROT DOSIM JI Radiat. Prot. Dosim. PY 2004 VL 110 IS 1-4 SI SI BP 423 EP 428 DI 10.1093/rpd/nch175 PG 6 WC Environmental Sciences; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA 856PV UT WOS:000224058000072 PM 15353685 ER PT B AU Mehdi, I Siegel, P AF Mehdi, I Siegel, P BE Heiter, G TI THz semiconductor-based front-end receiver technology for space applications SO RAWCON: 2004 IEEE RADIO AND WIRELESS CONFERENCE, PROCEEDINGS LA English DT Proceedings Paper CT IEEE Radio and Wireless Conference (RAWCON 2004) CY SEP 19-22, 2004 CL Atlanta, GA SP IEEE Microwave Theory & Technol Soc, IEEE Commun Soc AB Advances in the design and fabrication of very low capacitance planar Schottky diodes and millimeter-wave power amplifiers, more accurate device and circuit models for commercial 3-D electromagnetic simulators, and the availability of both MEMS and high precision metal machining, have enabled RF engineers to extend traditional waveguide-based sensor and source technologies well into the THz frequency regime. This short paper will highlight recent progress in realizing THz space-qualified receiver front-ends based on room temperature semiconductor devices. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mehdi, I (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 168-314, Pasadena, CA 91109 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-8451-2 PY 2004 BP 127 EP 130 DI 10.1109/RAWCON.2004.1389089 PG 4 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA BBB80 UT WOS:000224588200033 ER PT B AU Simons, RN Hall, DG Miranda, FA AF Simons, RN Hall, DG Miranda, FA BE Heiter, G TI Spiral chip Implantable radiator and printed loop external receptor for RF telemetry in bio-sensor systems SO RAWCON: 2004 IEEE RADIO AND WIRELESS CONFERENCE, PROCEEDINGS LA English DT Proceedings Paper CT IEEE Radio and Wireless Conference (RAWCON 2004) CY SEP 19-22, 2004 CL Atlanta, GA SP IEEE Microwave Theory & Technol Soc, IEEE Commun Soc DE biomedical RF telemetry; bio-sensor systems; bio-MEMS; capacitive pressure sensor; spiral inductor; wireless sensing; loop antenna ID INDUCTORS AB The paper describes the operation of a patented wireless RF telemetry system, consisting of a bio-MEMS implantable sensor and an external hand held unit, operating over the frequency range of few hundreds of MHz. A MEMS capacitive pressure sensor integrated with a miniature inductor/antenna together constitute the implantable sensor. Signal processing circuits collocated with a printed loop antenna together form the hand held unit, capable of inductively powering and also receiving the telemetry signals from the sensor. The paper in addition, demonstrates a technique to enhance the quality factor and inductance of the inductor in the presence of a lower ground plane and also presents the radiation characteristics of the loop antenna. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Simons, RN (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 9 TC 5 Z9 5 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-8451-2 PY 2004 BP 203 EP 206 DI 10.1109/RAWCON.2004.1389108 PG 4 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA BBB80 UT WOS:000224588200052 ER PT S AU Pisanich, G Plice, L Young, LA Lau, B Lee, P AF Pisanich, G Plice, L Young, LA Lau, B Lee, P BE Kehtarnavaz, N Laplante, PA TI Initial efforts toward mission-representative imaging surveys from aerial explorers SO REAL-TIME IMAGING VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Real-Time Imaging VIII CY JAN 20-22, 2004 CL San Jose, CA SP Soc Imaging Sci & Technol, SPIE AB Numerous researchers have proposed the use of robotic aerial explorers to perform scientific investigation of planetary bodies in our solar system. One of the essential tasks for any aerial explorer is to be able to perform scientifically valuable imaging surveys. The focus of this paper is to discuss the challenges implicit in, and recent observations related to, acquiring mission-representative imaging data from a small fixed-wing UAV, acting as a surrogate planetary aerial explorer. This question of successfully performing aerial explorer surveys is also tied to other topics of technical investigation, including the development of unique bio-inspired technologies. C1 NASA, Ames Res Ctr, QSS Grp Inc, Computat Sci Div, Moffett Field, CA 94035 USA. RP Pisanich, G (reprint author), NASA, Ames Res Ctr, QSS Grp Inc, Computat Sci Div, Moffett Field, CA 94035 USA. NR 6 TC 0 Z9 0 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5200-9 J9 P SOC PHOTO-OPT INS PY 2004 VL 5297 BP 106 EP 121 DI 10.1117/12.527338 PG 16 WC Imaging Science & Photographic Technology SC Imaging Science & Photographic Technology GA BAH96 UT WOS:000222343000012 ER PT B AU Ahmadzadeh, A Sayyar-Roudsari, B Homaifar, A AF Ahmadzadeh, A Sayyar-Roudsari, B Homaifar, A BE Butenko, S Murphey, R Pardalos, PM TI A hybrid projected gradient-evolutionary search algorithm for capacitated multi-source multi-UAVs scheduling with Time Windows SO RECENT DEVELOPMENTS IN COOPERATIVE CONTROL AND OPTIMIZATION SE COOPERATIVE SYSTEMS LA English DT Proceedings Paper CT 3rd Annual Conference on Cooperative Control and Optimization CY DEC, 2002 CL Gainesville, FL SP AF Res Lab, Univ Florida Coll Engn DE vehicle routing with time windows; mixed integer nonlinear programming; projected variable metric; penalty function; evolutionary algorithms; local search; hybrid method ID INTEGER PROGRAMMING-PROBLEMS AB The objective of this effort is to develop a hybrid evolutionary-gradient based technique to overcome the combinatorial complexity when solving large scale mixed integer nonlinear optimization problems. The basic idea relies on combining genetic algorithms (GA) and gradient projection method to exploit their complementary strengths. The effectiveness of these strategies are illustrated in the area of capacitated multi-source multi-vehicle scheduling with time windows. C1 NC A&T State Univ, Dept E&CE, NASA, ACIT Ctr, Greensboro, NC 27411 USA. RP Sayyar-Roudsari, B (reprint author), NC A&T State Univ, Dept E&CE, NASA, ACIT Ctr, Greensboro, NC 27411 USA. NR 24 TC 3 Z9 4 U1 0 U2 0 PU KLUWER ACADEMIC PUBLISHERS PI NORWELL PA 101 PHILIP DRIVE, ASSINIPPI PARK, NORWELL, MA 02061 USA BN 1-4020-7644-4 J9 COOPERAT SYST PY 2004 VL 3 BP 1 EP 21 PG 21 WC Automation & Control Systems; Operations Research & Management Science SC Automation & Control Systems; Operations Research & Management Science GA BY80N UT WOS:000189467300001 ER PT S AU Rubin, RH AF Rubin, RH BE Duc, PA Braine, J Brinks, E TI Flux ratio [Ne V] 14.3/24.3 as a test of collision strengths SO RECYCLING INTERGALACTIC AND INTERSTELLAR MATTER SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 217th Symposium of the International-Astronomical-Union on Recycling Intergalactic and Interstellar Matter held at the 25th IAU General Assembly CY AUG 06-10, 2002 CL Sydney, AUSTRALIA AB From ISO [Ne v] 14.3/24.3 mum line flux ratios, we find that 10 out of 20 planetary nebulae (PNs) have measured ratios below the low-electron density (N-e) theoretical predicted limit. Such astronomical data serve to provide important tests of atomic data, collision strengths in this case. In principle, well-calibrated measurements of the [Ne v] 14.3/24.3 flux ratio could improve upon the existing atomic data. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Rubin, RH (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-166-4 J9 IAU SYMP PY 2004 IS 217 BP 190 EP 191 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAL43 UT WOS:000222682600040 ER PT S AU Verner, E AF Verner, E BE Duc, PA Braine, J Brinks, E TI FeII emission as a probe of iron abundance at low-z quasars SO RECYCLING INTERGALACTIC AND INTERSTELLAR MATTER SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 217th Symposium of the International-Astronomical-Union on Recycling Intergalactic and Interstellar Matter held at the 25th IAU General Assembly CY AUG 06-10, 2002 CL Sydney, AUSTRALIA ID II EMISSION; QSOS; Z=3.62; RATIOS AB Whether the Fe/alpha enrichment is due to SN la explosions or massive objects is a key problem to be addressed in constructing our picture of galactic evolution in the Early Universe. Observations in the rest-frame of Mg II emission at 2800 Angstrom and the broad emission complex of Fe II spanning 2000-3000 Angstrom in high-z quasars should allow to determine the time in the Universe when increases in Fe abundance occur. This in turn provides us constraints on the stellar initial mass function and QSO formation and even the cosmological parameters. However a problem remains in developing a reliable model for this complex ion that accurately predicts the emission line spectra seen in luminous AGN at high redshift. The Fe II/Mg II emission ratios using new 830-level Fe II model are investigated with the intent to explain the observed Fe II/Mg II emission scatter. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Verner, E (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-166-4 J9 IAU SYMP PY 2004 IS 217 BP 202 EP 203 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAL43 UT WOS:000222682600046 ER PT S AU de Mello, DF Gardner, JP Dahlen, T Conselice, CJ Grogin, NA Koekemoer, AM AF de Mello, DF Gardner, JP Dahlen, T Conselice, CJ Grogin, NA Koekemoer, AM BE Duc, PA Braine, J Brinks, E TI The nature of UV-selected galaxies in the Chandra Deep Field South SO RECYCLING INTERGALACTIC AND INTERSTELLAR MATTER SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 217th Symposium of the International-Astronomical-Union on Recycling Intergalactic and Interstellar Matter held at the 25th IAU General Assembly CY AUG 06-10, 2002 CL Sydney, AUSTRALIA ID HIGH-REDSHIFT GALAXIES; STAR-FORMATION AB We report the first results of the ongoing survey using HST/WFPC2 (F300W) in parallel with ACS within the Chandra Deep Field South. A sample of 34 objects were identified in the WFPC2 images and their counterparts were found in the ACS images taken by the GOODS team; 6 of them are stars. Galaxies were classified as early-, late-types, and starbursts by template fitting which was also used to determine their photometric redshifts (z < 1). Analysis of the light concentration, asymmetry and clumpiness shows that this sample is a mixed bag, containing dwarf ellipticals, early- and late-spirals, and peculiar objects which resemble mergers in progress. This result has important implications for galaxy evolution since the intermediate redshifts are the epoch when the rise in the volume-averaged star formation rate occurs. C1 NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. RP de Mello, DF (reprint author), NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Code 681, Greenbelt, MD 20771 USA. RI Conselice, Christopher/B-4348-2013; OI Koekemoer, Anton/0000-0002-6610-2048 NR 9 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-166-4 J9 IAU SYMP PY 2004 IS 217 BP 222 EP 223 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAL43 UT WOS:000222682600056 ER PT B AU Wilson, TL Blome, HJ AF Wilson, TL Blome, HJ BE Shapiro, MM Stanev, T Wefel, JP TI The entangled Universe SO RELATIVISTIC ASTROPHYSICS AND COSMOLOGY SE SCIENCE AND CULTURE SERIES: ASTROPHYSICS LA English DT Proceedings Paper CT 13th International School of Cosmic Ray Astrophysics Course on Relativistic Astrophysics and Cosmology CY JUN 02-14, 2002 CL Erice, ITALY ID QUANTUM-FIELD-THEORY; PROBABILITY RELATIONS; PARTICLE CREATION; SEPARATED SYSTEMS; BLACK-HOLES; HORIZONS; TEMPERATURE; RADIATION; REDSHIFT; SUPERCONDUCTIVITY AB We review the importance of coherence and nonlocal entanglement in quantum cosmology. In particular, the origin of quantum temperature for the Universe itself is explored using the thermalization theorems in quantum gravity. The resulting temperatures for accelerating Friedmann-Lemaitre-Robertson-Walker models are compared with the classical Gamow temperature which follows from general relativity for the matter- and radiation-dominated eras of the Big Bang model. C1 NASA, Houston, TX 77058 USA. RP Wilson, TL (reprint author), NASA, Houston, TX 77058 USA. NR 60 TC 0 Z9 0 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 981-238-727-7 J9 SCI CULT SER ASTROPH PY 2004 VL 13 BP 23 EP 38 DI 10.1142/9789812702968_0002 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCJ55 UT WOS:000229640100002 ER PT S AU Manohara, H Dang, WL Siegel, PH Hoenk, M Husain, A Scherer, A AF Manohara, H Dang, WL Siegel, PH Hoenk, M Husain, A Scherer, A BE Tanner, DM Ramesham, R TI Field emission testing of carbon nanotubes for THz frequency vacuum micro-tube sources SO RELIABILITY, TESTING AND CHARACTERIZATION OF MEMS/MOEMS III SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT 3rd Conference on Reliability, Testing, and Characterization of MEM/MOEMS CY JAN 26-28, 2004 CL San Jose, CA SP SPIE DE nanoklystron; field emission; nanotubes; THz sources; SWNT; MWNT AB A carbon nanotube-based high current density electron field emission source is under development at Jet Propulsion Laboratory (JPL) for submillimeter-wave power generation (300 GHz to 3 THz). This source is the basis for a novel vacuum microtube component: the nanoklystron. The nanoklystron is a monolithically fabricated reflex klystron with dimensions in the micrometer range. The goal is to operate this device at much lower voltages than would be required with hot-electron sources and at much higher frequencies than have ever been demonstrated. Both single-walled (SWNTs) as well as multi-walled nanotubes (MWNTs) are being tested as potential field-emission sources. This paper presents initial results and observations of these field emission tests. SWNTs and MWNTs were fabricated using standard CVD techniques. The tube density was higher in the case of MWNT samples. As previously reported, high-density samples suffered from enhanced screening effect thus decreasing their total electron emission. The highest emission currents were measured from disordered, less dense MWNTs and were found to be similar to0.63 mA @ 3.6 V/mum (sample 1) and similar to3.55 mA @ 6.25 V/mum (sample 2). The high density vertically aligned MWNTs showed low field emission as predicted: 0.31 mA @ 4.7 V/mum. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Manohara, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 13 TC 9 Z9 9 U1 1 U2 6 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5251-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5343 BP 227 EP 234 DI 10.1117/12.531403 PG 8 WC Engineering, Electrical & Electronic; Engineering, Mechanical; Materials Science, Characterization & Testing; Optics SC Engineering; Materials Science; Optics GA BY73L UT WOS:000189450300027 ER PT B AU Morisette, JT Privette, JL Strahler, A Mayaux, P Justice, CO AF Morisette, JT Privette, JL Strahler, A Mayaux, P Justice, CO BE Lunetta, RS Lyon, JG TI Validation of global land-cover products by the committee on earth observing satellites SO REMOTE SENSING AND GIS ACCURACY ASSESSMENT LA English DT Proceedings Paper CT Symposium on Remote Sensing and GIS Accuracy Assessment CY DEC 11-13, 2001 CL Las Vegas, NV SP US EPA, Off Res & Dev ID ACCURACY ASSESSMENT; MODIS C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Morisette, JT (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 11 TC 1 Z9 1 U1 1 U2 3 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 1-56670-443-X PY 2004 BP 31 EP 40 DI 10.1201/9780203497586.ch3 PG 10 WC Remote Sensing SC Remote Sensing GA BAW11 UT WOS:000223862600003 ER PT S AU Mannucci, AJ Ao, CO Hajj, GA Iijima, BA de la Torre-Juarez, M AF Mannucci, AJ Ao, CO Hajj, GA Iijima, BA de la Torre-Juarez, M BE Bevis, M Shoji, Y Businger, S TI Towards new scientific observations from GPS occultations: Advances in retrieval methods SO REMOTE SENSING APPLICATIONS OF THE GLOBAL POSITIONING SYSTEM SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing Applications of the Global Positioning System CY NOV 08-09, 2004 CL Honolulu, HI SP SPIE DE radio occultations; weather prediction; boundary layer; tropopause; troposphere-stratosphere exchange ID RADIO OCCULTATION; WATER-VAPOR; ATMOSPHERE; CHAMP; VENUS; AIR AB Atmospheric soundings using signals received in low Earth orbit from Global Positioning System (GPS) satellite transmissions are widely recognized as important data for establishing a precise climate record of upper-air temperatures, due to their self-calibrating nature and all-weather acquisition. More recently, advances in retrieval methods using the same GPS data have opened the possibility of new scientific studies related to atmospheric processes and climate change. We will present recent innovations in extracting scientifically useful information from the phase and amplitude of received GPS transmissions, and discuss the technical challenges that need to be overcome to achieve new scientific results. Promising areas being pursued include: remote sensing of the planetary boundary layer from space, important for understanding ocean-atmosphere coupling; retrieving tropopause temperature structure at high vertical resolution, important for understanding troposphere-stratosphere exchange mechanisms and the role of convection; high accuracy and precision of upper altitude (25+ km) retrievals in the stratosphere. Using an end-to-end simulator recently developed at JPL, we will investigate in realistic detail the relationship between the atmospheric state and retrieved scientific parameters, and discuss retrieval research needed to address new scientific applications. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mannucci, AJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 25 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5622-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5661 BP 13 EP 26 DI 10.1117/12.580047 PG 14 WC Remote Sensing SC Remote Sensing GA BBP21 UT WOS:000226859600002 ER PT S AU Levine, JS Ambrosia, V Brass, JA Davis, RE Dull, CW Greenfield, PH Harrison, FW Killough, BD Kist, EH Pinto, JP Stover, G Tappan, ND Wegener, SS AF Levine, JS Ambrosia, V Brass, JA Davis, RE Dull, CW Greenfield, PH Harrison, FW Killough, BD Kist, EH Pinto, JP Stover, G Tappan, ND Wegener, SS BE Bevis, M Shoji, Y Businger, S TI Monitoring wildfires using an autonomous aerial system (AAS) SO REMOTE SENSING APPLICATIONS OF THE GLOBAL POSITIONING SYSTEM SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing Applications of the Global Positioning System CY NOV 08-09, 2004 CL Honolulu, HI SP SPIE DE wildfires; environmental effects; gaseous emissions; particulate emissions; global change; health effects; fire radiance; fire temperatures; fire propagation; remote sensing; space measurements; airplane measurements; remotely piloted aircraft; autonomous aerial observing system ID FIRE; PERIMETER; ALGORITHM; SPREAD; MODIS AB The environmental and health effects of wildfires are discussed. The monitoring of wildfires from aircraft using remote sensing techniques is reviewed. A future autonomous aerial observing system for fire monitoring is described. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Levine, JS (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 62 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5622-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5661 BP 104 EP 120 DI 10.1117/12.580312 PG 17 WC Remote Sensing SC Remote Sensing GA BBP21 UT WOS:000226859600011 ER PT S AU Sullivan, D Totah, J Wegener, S Enomoto, F Frost, C Kaneshige, J Frank, J AF Sullivan, D Totah, J Wegener, S Enomoto, F Frost, C Kaneshige, J Frank, J BE Bevis, M Shoji, Y Businger, S TI Intelligent mission management for uninhabited aerial vehicles SO REMOTE SENSING APPLICATIONS OF THE GLOBAL POSITIONING SYSTEM SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing Applications of the Global Positioning System CY NOV 08-09, 2004 CL Honolulu, HI SP SPIE DE autonomy; UAV; sensor planning service; sensor web; Intelligent Mission Management; Collaborative and Coordinated Systems; intelligent autonomous architecture; Autonomous Robust Avionics AB The National Aeronautics and Space Administration (NASA), Aeronautics Research Mission Directorate, is developing Intelligent Mission Management (IMM) technology for Uninhabited Aerial Vehicles (UAV's) under the Vehicle Systems Program's Autonomous Robust Avionics Project. The objective of the project is to develop air vehicle and associated ground element technology to enhance mission success by increasing mission return and reducing mission risk. Unanticipated science targets, uncertain conditions and changing mission requirements can all influence a flight plan and may require human intervention during the flight; however, time delays and communications bandwidth limit opportunities for operator intervention. To meet these challenges, we will develop UAV-specific technologies enabling goal-directed autonomy, i.e. the ability to redirect the flight in response to current conditions and the current goals of the flight. Our approach divides goal-directed autonomy into two components, an on-board Intelligent Agent Architecture (LAA) and a ground based Collaborative Decision Environment (CDE). These technologies cut across all aspects of a UAV system, including the payload, inner- and outer-loop onboard control, and the operator's ground station. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sullivan, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 7 TC 1 Z9 1 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5622-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5661 BP 121 EP 131 DI 10.1117/12.582446 PG 11 WC Remote Sensing SC Remote Sensing GA BBP21 UT WOS:000226859600012 ER PT S AU Hutchinson, MA Hamill, DL Harrison, FW Yetter, JA Lawrence, RW Healy, EA Wright, H AF Hutchinson, MA Hamill, DL Harrison, FW Yetter, JA Lawrence, RW Healy, EA Wright, H BE Bevis, M Shoji, Y Businger, S TI Multi-dimensional analysis of autonomous aerial observation systems (AAOS) for scientific, civil and defense applications SO REMOTE SENSING APPLICATIONS OF THE GLOBAL POSITIONING SYSTEM SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing Applications of the Global Positioning System CY NOV 08-09, 2004 CL Honolulu, HI SP SPIE DE unmanned aerial vehicles; UAV; sensorcraft; autonomous aerial observation systems; AAOS; remotely operated aircraft; ROA AB Better knowledge of the atmosphere, ocean and land are needed by a wide range of users spanning the scientific, civil and defense communities. Observations to provide this knowledge will require aerial systems with greater operational flexibility and lower life-cycle costs than are currently available. Persistent monitoring of severe storms, sampling and measurements of the Earth's carbon cycle, wildfire monitoring/management, crop assessments, ozone and polar ice changes, and natural disaster response (communications and surveillance) are but a few applications where autonomous aerial observations can effectively augment existing measurement systems. User driven capabilities include high altitude, long range, long-loiter (days/weeks), smaller deployable sensor-ships for in-situ sampling, and sensors providing data with spectral bandwidth and high temporal and three-dimensional spatial resolution. Starting with user needs and considering all elements and activities required to acquire the needed observations leads to the definition of autonomous aerial observation systems (AAOS) that can significantly complement and extend the current Earth observation capability. In this approach, UAVs are viewed as only one, albeit important, element in a mission system and overall cost and performance for the user are the critical success factors. To better understand and meet the challenges of developing such AAOSs, a systems oriented multi-dimensional analysis has been performed that illuminates the enabling and high payoff investments that best address the needs of scientific, civil, and defense users of Earth observations. The analysis further identifies technology gaps and serves to illustrate how investments in a range of mission subsystems together can enable a new class of Earth observations. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Hutchinson, MA (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 0 TC 0 Z9 0 U1 2 U2 7 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5622-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5661 BP 132 EP 141 DI 10.1117/12.582036 PG 10 WC Remote Sensing SC Remote Sensing GA BBP21 UT WOS:000226859600013 ER PT S AU Sandford, SP Harrison, FW Langford, J Johnson, JW Qualls, G Emmitt, D AF Sandford, SP Harrison, FW Langford, J Johnson, JW Qualls, G Emmitt, D BE Bevis, M Shoji, Y Businger, S TI Autonomous aerial observations to extend and complement the Earth Observing System: A science driven, systems oriented approach SO REMOTE SENSING APPLICATIONS OF THE GLOBAL POSITIONING SYSTEM SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing Applications of the Global Positioning System CY NOV 08-09, 2004 CL Honolulu, HI SP SPIE DE remote sensing; UAV; earth science; earth observing system; suborbital; autonomous aerial observation system; airborne measurements; space measurements ID TROPICS; MODIS; FIRES AB The current Earth observing capability depends primarily on spacecraft missions and ground-based networks to provide the critical on-going observations necessary for improved understanding of the Earth system. Aircraft missions play an important role in process studies but are limited to relatively short-duration flights. Suborbital observations have contributed to global environmental knowledge by providing in-depth, high-resolution observations that space-based and in-situ systems are challenged to provide; however, the limitations of aerial platforms - e.g., limited observing envelope, restrictions associated with crew safety and high cost of operations have restricted the suborbital program to a supporting role. For over a decade, it has been recognized that autonomous aerial observations could potentially be important. Advances in several technologies now enable autonomous aerial observation systems (AAOS) that can provide fundamentally new observational capability for Earth science and applications and thus lead scientists and engineers to rethink how suborbital assets can best contribute to Earth system science. Properly developed and integrated, these technologies will enable new Earth science and operational mission scenarios with long term persistence, higher-spatial and higher-temporal resolution at lower cost than space or ground based approaches. This paper presents the results of a science driven, systems oriented study of broad Earth science measurement needs. These needs identify aerial mission scenarios that complement and extend the current Earth Observing System. These aerial missions are analogous to space missions in their complexity and potential for providing significant data sets for Earth scientists. Mission classes are identified and presented based on science driven measurement needs in atmospheric, ocean and land studies. Also presented is a nominal concept of operations for an AAOS: an innovative set of suborbital assets that complements and augments current and planned space-based observing systems. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Sandford, SP (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 41 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5622-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5661 BP 142 EP 159 DI 10.1117/12.582037 PG 18 WC Remote Sensing SC Remote Sensing GA BBP21 UT WOS:000226859600014 ER PT S AU Lawrence, R Hilliard, L AF Lawrence, R Hilliard, L BE Bevis, M Shoji, Y Businger, S TI Mission concept for the remote sensing of the cryosphere using autonomous aerial observation systems SO REMOTE SENSING APPLICATIONS OF THE GLOBAL POSITIONING SYSTEM SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing Applications of the Global Positioning System CY NOV 08-09, 2004 CL Honolulu, HI SP SPIE AB Improving the understanding of the Cryosphere and its impact on global hydrology is an important element of NASA's Earth Science Enterprise (ESE). A Cold Land Processes Working Group (CLPWG) was formed by the NASA Terrestrial Hydrology Program to identify important science objectives necessary to address ESE priorities. These measurement objectives included Snow Water Equivalent (SWE), snow wetness, and freeze/thaw status of underlying soil. The spatial resolution requirement identified by the CLPWG was 100 in to 5000 in. Microwave sensors are well suited to measure these and other properties of interests to the study of the terrestrial cryosphere. It is well known that the EM properties of snow and soil at microwave frequencies are a strong function of the phase of water, i.e. ice/water. Further, both active and passive microwave sensors have demonstrated sensitivity to important properties of snowpack including, depth, density, wetness, crystal size, ice crust layer structure, and surface roughness. These sensors are also sensitive to the underlying soil state (frozen or thawed). Multiple microwave measurements including both active and passive sensors will likely be required to invert the effects of various snowpack characteristics, vegetation, and underlying soil properties to provide the desired characterization of the surface and meet the science needs required by the ESE. A major technology driver with respect to fully meeting these measurement needs is the 100 to 5000 in spatial resolution requirement. Meeting the threshold requirement of 5000 in at microwave frequencies from Low Earth Orbit is a technology challenge. The emerging capabilities of unmanned aircraft and particularly the system perspective of the Autonomous Aerial Observation Systems (AAOS) may provide high-fidelity/high-resolution measurements on regional scales or larger that could greatly improve our measurement capability. This paper explores a vehicle/sensor concept that could augment satellite measurements to enhance our understanding of the Cryosphere. The measurement performance and technology issues related to the sensor and aircraft will be assessed. Finally, specific technology needs and research necessary to enable this AAOS concept will be discussed. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Lawrence, R (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. NR 2 TC 0 Z9 0 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5622-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5661 BP 160 EP 168 DI 10.1117/12.582121 PG 9 WC Remote Sensing SC Remote Sensing GA BBP21 UT WOS:000226859600015 ER PT S AU Kuhl, CA Moses, RW Croom, MA Sandford, SP AF Kuhl, CA Moses, RW Croom, MA Sandford, SP BE Bevis, M Shoji, Y Businger, S TI Parametric study for increasing on-station duration via unconventional aircraft launch approach SO REMOTE SENSING APPLICATIONS OF THE GLOBAL POSITIONING SYSTEM SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing Applications of the Global Positioning System CY NOV 08-09, 2004 CL Honolulu, HI SP SPIE AB The need for better atmospheric predictions is causing the atmospheric science community to look for new ways to obtain longer, higher-resolution measurements over several diurnal cycles. The high resolution, in-situ measurements required to study many atmospheric phenomena can be achieved by an Autonomous Aerial Observation System (AAOS); however, meeting the long on-station time requirements with an aerial platform poses many challenges. Inspired by the half-scale drop test of the deployable Aerial Regional-scale Environmental Survey (ARES) Mars airplane, a study was conducted at the NASA Langley Research Center to examine the possibility of increasing on-station time by launching an airplane directly at the desired altitude. The ARES Mars airplane concept was used as a baseline for Earth atmospheric flight, and parametric analyses of fundamental configuration elements were performed to study their impact on achieving desired on-station time with this class of airplane. The concept involved lifting the aircraft from the ground to the target altitude by means of an air balloon, thereby unburdening the airplane of ascent requirements. The parameters varied in the study were aircraft wingspan, payload, fuel quantity, and propulsion system. The results show promising trends for further research into aircraft-payload design using this unconventional balloon-based launch approach. C1 NASA, Langley Res Ctr, Explorat Engn Branch, Hampton, VA 23665 USA. RP Kuhl, CA (reprint author), NASA, Langley Res Ctr, Explorat Engn Branch, Hampton, VA 23665 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5622-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5661 BP 169 EP 175 DI 10.1117/12.606676 PG 7 WC Remote Sensing SC Remote Sensing GA BBP21 UT WOS:000226859600016 ER PT S AU Owe, M De Jeu, R AF Owe, M De Jeu, R BE Owe, M DUrso, G Moreno, JF Calera, A TI Combining day- and nighttime SMMR observations for improved temporal resolution of surface parameter retrievals SO REMOTE SENSING FOR AGRICULTURE, ECOSYSTEMS, AND HYDROLOGY V SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing for Agriculture, Ecosystems and Hydrology V CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE DE remote sensing; microwave; soil moisture; surface temperature; SMMR ID BRIGHTNESS TEMPERATURE; SOIL-MOISTURE AB The Scanning Multichannel Microwave Radiometer (SMMR) provides ground coverage on the average of two times per week during the day and two times per week during the night. However, past problems associated with surface soil temperature estimation have resulted in both systematic and random differences between various applications utilizing both daytime and nighttime observations. This was especially true for SMMR-based soil moisture retrievals. Significant offsets were frequently observed, which prevented the daytime and nighttime soil moisture data from being combined into a single data set. This leaves one with a time series of data with very poor temporal resolution, and limits its usefulness for other applications. Improvements in surface temperature estimation have reduced the differences between day and night estimates significantly. The improved consistency between the two data sets now permits combining them into one, making the data more useful, especially for other land surface processes applications. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Owe, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5115-0 J9 P SOC PHOTO-OPT INS PY 2004 VL 5232 BP 418 EP 424 DI 10.1117/12.513907 PG 7 WC Agriculture, Multidisciplinary; Environmental Sciences; Remote Sensing; Water Resources SC Agriculture; Environmental Sciences & Ecology; Remote Sensing; Water Resources GA BY77H UT WOS:000189459600041 ER PT S AU Foster, J Sun, CJ Walker, JP Kelly, R Dong, JR Chang, A AF Foster, J Sun, CJ Walker, JP Kelly, R Dong, JR Chang, A BE Owe, M DUrso, G Gouweleeuw, BT Jochum, AM TI Mapping random and systematic errors of satellite-derived snow water equivalent observations in Eurasia SO REMOTE SENSING FOR AGRICULTURE, ECOSYSTEMS, AND HYDROLOGY VI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing for Agriculture, Ecosystems and Hydrology VI CY SEP 14-16, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, NASA, European Opt Soc ID DEPTH AB Passive microwave sensors onboard satellites can provide global snow water equivalent (SWE) observations day or night, even under cloudy conditions. However, there are both systematic (bias) and random errors associated with the passive microwave measurements. While these errors are well known, they have thus far not been adequately quantified. In this study, unbiased SWE maps, random error maps and systematic error maps of Eurasia for the 1990-1991 snow season (November-April) have been examined. Dense vegetation, especially in the taiga region., and large snow crystals 14 (>0.3 mm in radius), found in areas where the temperature/vapor gradients are greatest, (in the taiga and tundra regions) are the major source of systematic error. Assumptions about how snow crystals evolve with the progression of the season also contribute to the errors. In general, while random errors for North America and Eurasia are comparable, systematic errors are not as great for Eurasia as those observed for North America. Understanding remote sensing retrieval errors is important for correct interpretation of observations, and successful assimilation of observations into numerical models. C1 NASA, Goddard Space Flight Ctr, Lab Hydrospher Proc, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP Foster, J (reprint author), NASA, Goddard Space Flight Ctr, Lab Hydrospher Proc, Hydrol Sci Branch, Code 661, Greenbelt, MD 20771 USA. RI Sun, Chaojiao/A-9569-2011 OI Sun, Chaojiao/0000-0002-7030-0485 NR 15 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5515-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5568 BP 150 EP 158 DI 10.1117/12.564641 PG 9 WC Agriculture, Multidisciplinary; Geosciences, Multidisciplinary; Remote Sensing SC Agriculture; Geology; Remote Sensing GA BBI21 UT WOS:000225600100015 ER PT S AU Owe, M Holmes, TRH de Jeu, RAM AF Owe, M Holmes, TRH de Jeu, RAM BE Owe, M DUrso, G Gouweleeuw, BT Jochum, AM TI Spatial distributions of global soil moisture retrievals from satellite microwave observations SO REMOTE SENSING FOR AGRICULTURE, ECOSYSTEMS, AND HYDROLOGY VI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing for Agriculture, Ecosystems and Hydrology VI CY SEP 14-16, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, NASA, European Opt Soc DE remote sensing; soil moisture; microwave brightness temperature; global climate ID OPTICAL DEPTH RETRIEVAL; METHODOLOGY; CLIMATE AB A global data base of daily surface soil moisture has been compiled by applying a recently developed land parameter retrieval algorithm to a nine year historical data set of brightness temperatures from the Scanning Multichannel Microwave Radiometer (SMMR). The instrument, flew on-board the Nimbus-7 satellite, and made daily daytime and nighttime global observations of brightness temperature at five frequencies and two polarizations from 1978 to 1987. Spatial distributions of global soil moisture are examined, and they compare well with corresponding observations of global precipitation and global vegetation indices. C1 NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP Owe, M (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RI Holmes, Thomas/F-4512-2010 OI Holmes, Thomas/0000-0002-4651-0079 NR 9 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5515-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5568 BP 171 EP 178 DI 10.1117/12.565257 PG 8 WC Agriculture, Multidisciplinary; Geosciences, Multidisciplinary; Remote Sensing SC Agriculture; Geology; Remote Sensing GA BBI21 UT WOS:000225600100017 ER PT S AU Vaughan, M Rodier, S Hu, YX McGill, M Holz, R AF Vaughan, M Rodier, S Hu, YX McGill, M Holz, R BE Schafer, KP Comeron, A Carleer, MR Picard, RH Sifakis, NI TI Cloud and aerosol studies using combined CPL and MAS data SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE IX SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing of Clouds and the Atmosphere IX CY SEP 13-15, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, NASA, European Opt Soc ID INSTRUMENT DESCRIPTION; LIDAR MEASUREMENTS; MISSION; ALGORITHM; PROFILES; WATER AB Current uncertainties in the role of aerosols and clouds in the Earth's climate system limit our abilities to model the climate system and predict climate change. These limitations are due primarily to difficulties of adequately measuring aerosols and clouds on a global scale. The A-train satellites (Aqua, CALIPSO, CloudSat, PARASOL, and Aura) will provide an unprecedented opportunity to address these uncertainties. The various active and passive sensors of the A-train will use a variety of measurement techniques to provide comprehensive observations of the multi-dimensional properties of clouds and aerosols. However, to fully achieve the potential of this ensemble requires a robust data analysis framework to optimally and efficiently map these individual measurements into a comprehensive set of cloud and aerosol physical properties. In this work we introduce the Multi-Instrument Data Analysis and Synthesis (MIDAS) project, whose goal is to develop a suite of physically sound and computationally efficient algorithms that will combine active and passive remote sensing data in order to produce improved assessments of aerosol and cloud radiative and microphysical properties. These algorithms include (a) the development of an intelligent feature detection algorithm that combines inputs from both active and passive sensors, and (b) identifying recognizable multi-instrument signatures related to aerosol and cloud type derived from clusters of image pixels and the associated vertical profile information. Classification of these signatures will lead to the automated identification of aerosol and cloud types. Testing of these new algorithms is done using currently existing and readily available active and passive measurements from the Cloud Physics Lidar and the MODIS Airborne Simulator, which simulate, respectively, the CALIPSO and MODIS A-train instruments. C1 NASA, Langley Res Ctr, SAIC, Hampton, VA 23681 USA. RP Vaughan, M (reprint author), NASA, Langley Res Ctr, SAIC, Mail Stop 435, Hampton, VA 23681 USA. RI McGill, Matthew/D-8176-2012; Hu, Yongxiang/K-4426-2012 NR 30 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5518-0 J9 P SOC PHOTO-OPT INS PY 2004 VL 5571 BP 30 EP 39 DI 10.1117/12.565586 PG 10 WC Remote Sensing SC Remote Sensing GA BBN01 UT WOS:000226252700004 ER PT S AU Rault, DF AF Rault, DF BE Schafer, KP Comeron, A Carleer, MR Picard, RH Sifakis, NI TI Ozone, NO2 and aerosol retrieval from SAGE III limb scatter measurements SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE IX SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing of Clouds and the Atmosphere IX CY SEP 13-15, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, NASA, European Opt Soc DE satellite remote sensing; limb scatter; retrieval algorithms; ozone; NO2; aerosol AB The ability of SAGE III to retrieve ozone, NO2 and aerosol vertical distribution within Earth atmosphere from limb scatter measurements is being investigated. The sunlight scattered by atmospheric gases and particulates (aerosol, clouds) and the Earth's surface is measured and spectrally dispersed by SAGE III spectrometer. Ozone density vertical profiles are retrieved from 10 km (or cloud top) to 50 km at a resolution of about 1 km and a precision of less than 10% using Chappuis and Huggins ozone absorption bands. NO2 vertical density profiles are retrieved from 15 to 40 kin at a resolution of about 2 km and a precision of 20% using the NO2 absorption features in the 430-450 nm spectral range. Aerosol extinction vertical profiles (from 15 to 30 km) are retrieved using a series of non absorbing channels. Retrieved products are compared with available correlative data (ozone sondes, SAGE III in occultation, OSIRIS). C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Rault, DF (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 15 TC 4 Z9 4 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5518-0 J9 P SOC PHOTO-OPT INS PY 2004 VL 5571 BP 205 EP 216 DI 10.1117/12.564899 PG 12 WC Remote Sensing SC Remote Sensing GA BBN01 UT WOS:000226252700021 ER PT S AU Minnis, P Young, D Sun-Mack, S Heck, PW Doelling, DR Trepte, QZ AF Minnis, P Young, D Sun-Mack, S Heck, PW Doelling, DR Trepte, QZ BE Schafer, KP Comeron, A Carleer, MR Picard, RH TI CERES cloud property retrievals from imagers on TRMM, Terra, and Aqua SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing of Clouds and the Atmosphere VIII CY SEP 09-12, 2003 CL Barcelona, SPAIN SP SPIE DE radiation; clouds; remote sensing; cloud microphysics; climatology; MODIS; CERES; VIRS; Aqua; Terra ID METEOROLOGICAL SATELLITE IMAGERS; LIQUID WATER CLOUDS; RAPID CALIBRATION; REFLECTANCE; CHANNELS; ISCCP AB The micro- and macrophysical properties of clouds play a crucial role in Earth's radiation budget. The NASA Clouds and Earth's Radiant Energy System (CERES) is providing simultaneous measurements of the radiation and cloud fields on a global basis to improve the understanding and modeling of the interaction between clouds and radiation at the top of the atmosphere, at the surface, and within the atmosphere. Cloud properties derived for CERES from the Moderate Resolution Imaging Spectroradiometer (MODIS) on the Terra and Aqua satellites are compared to ensure consistency between the products to ensure the reliability of the retrievals from multiple platforms at different times of day. Comparisons of cloud fraction, height, optical depth, phase, effective particle size, and ice and liquid water paths from the two satellites show excellent consistency. Initial calibration comparisons are also very favorable. Differences between the Aqua and Terra results are generally due to diurnally dependent changes in the clouds. Additional algorithm refinement is needed over the polar regions for Aqua and at night over those same areas for Terra. The results should be extremely valuable for model validation and improvement and for improving our understanding of the relationship between clouds and the radiation budget. C1 NASA, Langley Res Ctr, Atmospher Sci, Hampton, VA 23681 USA. RP Minnis, P (reprint author), NASA, Langley Res Ctr, Atmospher Sci, MS 420, Hampton, VA 23681 USA. NR 20 TC 7 Z9 7 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5118-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5235 BP 37 EP 48 DI 10.1117/12.511210 PG 12 WC Meteorology & Atmospheric Sciences; Remote Sensing SC Meteorology & Atmospheric Sciences; Remote Sensing GA BY77K UT WOS:000189459800004 ER PT S AU Rault, DF Loughman, R Sioris, C AF Rault, DF Loughman, R Sioris, C BE Schafer, KP Comeron, A Carleer, MR Picard, RH TI Retrieval of atmospheric ozone and nitrogen dioxide vertical distribution from SAGE III limb scattering measurements SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing of Clouds and the Atmosphere VIII CY SEP 09-12, 2003 CL Barcelona, SPAIN SP SPIE DE satellite remote sensing; limb scattering; retrieval algorithms; ozone; nitrogen dioxide AB The limb scattering radiances measured by SAGE III are analyzed. After accounting for instrument issues, ozone and nitrogen dioxide vertical density profiles are retrieved from the data and compared with results from other instruments. These initial results are very promising and show the potential of SAGE III to operate in this mode. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Rault, DF (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. OI Sioris, Christopher/0000-0003-1168-8755 NR 7 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5118-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5235 BP 298 EP 309 DI 10.1117/12.509827 PG 12 WC Meteorology & Atmospheric Sciences; Remote Sensing SC Meteorology & Atmospheric Sciences; Remote Sensing GA BY77K UT WOS:000189459800027 ER PT S AU Aumann, HH Strow, L AF Aumann, HH Strow, L BE Schafer, KP Comeron, A Carleer, MR Picard, RH TI Sea surface temperature measurements with the atmospheric infrared sounder (AIRS) and aerosol SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing of Clouds and the Atmosphere VIII CY SEP 09-12, 2003 CL Barcelona, SPAIN SP SPIE AB Atmospheric Infrared Sounder (AIRS) measurements of the sea surface temperature at 2616cm-1 show an unexpected cold bias compared to the NCEP Global Real Time SST. This cold bias, which is distributed in large scale patterns which are stable on the time scale of several months, has a satellite zenith angle (sza) dependent and a sza independent component. The sza independent component is strongly temperature dependent, and is most likely related to a larger than expected gradient between the bulk and the skin temperature, possibly due to not understood regional or seasonal weather patterns. The sza dependent component of about OAK is most likely due to some form of aerosol which is not included in the radiative transfer. AIRS was launched 4 May 2002 on the EOS Aqua into polar orbit. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Aumann, HH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NR 10 TC 0 Z9 0 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5118-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5235 BP 319 EP 326 DI 10.1117/12.510838 PG 8 WC Meteorology & Atmospheric Sciences; Remote Sensing SC Meteorology & Atmospheric Sciences; Remote Sensing GA BY77K UT WOS:000189459800029 ER PT S AU Smith, WL Zhou, DK Revercomb, HE Huang, HL Antonelli, P Mango, SA AF Smith, WL Zhou, DK Revercomb, HE Huang, HL Antonelli, P Mango, SA BE Schafer, KP Comeron, A Carleer, MR Picard, RH TI Hyper-spectral atmospheric sounding SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing of Clouds and the Atmosphere VIII CY SEP 09-12, 2003 CL Barcelona, SPAIN SP SPIE AB The Geosynchronous Imaging Fourier Transform Spectrometer (GIFTS) is the first hyper-spectral remote sounding system to be orbited aboard a geosynchronous satellite. The GIFTS is designed to obtain revolutionary observations of the four dimensional atmospheric temperature, moisture, and wind structure as well as the distribution of the atmospheric trace gases, CO and O-3. Although GIFTS will not be orbited until 2006-2008, a glimpse at the its measurement capabilities has been obtained by analyzing data from the National Polar-orbiting Operational Environmental Satellite System (NPOESS) Airborne Sounder Test-bed-Interferometer (NAST-I) and Aqua satellite Atmospheric Infrared Sounder (AIRS). In this paper we review the GIFTS experiment and empirically assess measurement expectations based on meteorological profiles retrieved from the NAST aircraft and Aqua satellite AIRS spectral radiances. C1 NASA, Langley Res Ctr, AtSC, Hampton, VA 23681 USA. RP Smith, WL (reprint author), NASA, Langley Res Ctr, AtSC, Hampton, VA 23681 USA. NR 4 TC 2 Z9 2 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5118-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5235 BP 389 EP 396 DI 10.1117/12.515209 PG 8 WC Meteorology & Atmospheric Sciences; Remote Sensing SC Meteorology & Atmospheric Sciences; Remote Sensing GA BY77K UT WOS:000189459800036 ER PT S AU Tanelli, S Meagher, JP Im, E Facheris, L AF Tanelli, S Meagher, JP Im, E Facheris, L BE Schafer, KP Comeron, A Carleer, MR Picard, RH TI Dual-frequency Spaceborne Doppler Radar: analysis of performances in estimating latent heat fluxes SO REMOTE SENSING OF CLOUDS AND THE ATMOSPHERE VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Remote Sensing of Clouds and the Atmosphere VIII CY SEP 09-12, 2003 CL Barcelona, SPAIN SP SPIE DE spaceborne precipitation radar; Doppler ID VERTICAL PROFILES; CLOUD CLUSTERS; PRECIPITATION; TRMM; RELEASE AB Knowledge of the global distribution of the vertical velocity of precipitation is important for estimating latent heat fluxes, and therefore in the general study of energy transportation in the atmosphere. Such knowledge can only be acquired with the use of spaceborne Doppler precipitation radars. Recent studies have shown that the average vertical velocity can be measured to acceptable accuracy levels by appropriate selection of radar parameters. Furthermore, methods to correct for specific errors arising from Non-Uniform Beam Filling effects and pointing uncertainties have recently been developed. As detailed in the Global Precipitation Mission (GPM) preparatory studies, the use of a dual-frequency precipitation radar allows improved estimation of the main parameters of the hydrometeor size distribution (bulk quantity and one shape parameter). Such parameters, in turn, lead to improved estimates of latent heat fluxes. In this paper we address the performance of a dual-frequency Doppler Precipitation Radar (DDPR) in estimating the latent heat flux from the measured rainfall vertical velocity and DSD parameters. C1 Jet Prop Lab, Pasadena, CA 91109 USA. RP Tanelli, S (reprint author), Jet Prop Lab, 4800 Oak Grove Dr MS 300-243, Pasadena, CA 91109 USA. NR 21 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5118-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5235 BP 465 EP 476 DI 10.1117/12.508394 PG 12 WC Meteorology & Atmospheric Sciences; Remote Sensing SC Meteorology & Atmospheric Sciences; Remote Sensing GA BY77K UT WOS:000189459800044 ER PT B AU Johnston, PH Waters, KR AF Johnston, PH Waters, KR BE Thompson, DO Chimenti, DE TI Tomographic imaging of an ultrasonic field in a plane using a linear array SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 23A AND 23B SE REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION LA English DT Proceedings Paper CT 30th Annual Review of Progress in Quantitative Nondestructive Evaluation CY JUL 27-AUG 01, 2003 CL Green Bay, WI SP Iowa State Univ, Ctr Nondestruct Evaluat, QNDE Programs AB A method is presented based on tomographic reconstruction techniques for the visualization of an ultrasonic field. The tall, narrow piezoelectric elements of a one-dimensional receiving array, rotated about its central axis, provide parallel projection input data for tomographic reconstruction of the field. The technique is demonstrated using simulated ultrasonic beams and experimental measurements of an ultrasonic beam propagated through a stitched woven composite. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Johnston, PH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA BN 0-7354-0173-X J9 REV PROG Q PY 2004 VL 23 BP 694 EP 701 PN A&B PG 8 WC Acoustics; Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Materials Science, Characterization & Testing; Imaging Science & Photographic Technology SC Acoustics; Engineering; Materials Science; Imaging Science & Photographic Technology GA BY96D UT WOS:000189505300088 ER PT B AU Johnston, PH AF Johnston, PH BE Thompson, DO Chimenti, DE TI Free response of piezoelectric crystals in series and in parallel SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 23A AND 23B SE REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION LA English DT Proceedings Paper CT 30th Annual Review of Progress in Quantitative Nondestructive Evaluation CY JUL 27-AUG 01, 2003 CL Green Bay, WI SP Iowa State Univ, Ctr Nondestruct Evaluat, QNDE Programs ID TRANSDUCERS AB The free response is considered of piezoelectric crystals (lithium niobate) with various polarities (including longitudinal only, shear only, and combined longitudinal and shear), which are stacked (mechanically and electrically in series) or are parallel (electrically parallel and mechanically uncoupled). Measurements of impedance magnitude from an impedance analyzer are compared with results from PSPICE simulations using a Mason model. These PSPICE models may serve as the basis for designing physical transducers from crystal stacks. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Johnston, PH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 3 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA BN 0-7354-0173-X J9 REV PROG Q PY 2004 VL 23 BP 729 EP 736 PN A&B PG 8 WC Acoustics; Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Materials Science, Characterization & Testing; Imaging Science & Photographic Technology SC Acoustics; Engineering; Materials Science; Imaging Science & Photographic Technology GA BY96D UT WOS:000189505300092 ER PT B AU Ghoshal, A Prosser, WH Copeland, BM AF Ghoshal, A Prosser, WH Copeland, BM BE Thompson, DO Chimenti, DE TI Development of piezoelectric acoustic sensors and novel bio-inspired sensor array architecture SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 23A AND 23B SE REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION LA English DT Proceedings Paper CT 30th Annual Review of Progress in Quantitative Nondestructive Evaluation CY JUL 27-AUG 01, 2003 CL Green Bay, WI SP Iowa State Univ, Ctr Nondestruct Evaluat, QNDE Programs ID PLATES; WAVES AB This paper looks at developing novel piezoelectric acoustic sensors, which are capable of sensing high frequency acoustic emissions and impact in a composite/metallic plate. The fabrication of the piezoelectric acoustic sensors made from piezoceramic ribbons would be described in details. An attempt was made to build directionality into the sensing system itself. Continuous sensors placed at right angles on a plate are being discussed as a new approach to measure and locate the source of acoustic waves. Novel signal processing algorithms based on bio-inspired neural systems for spatial filtering of large numbers of embedded sensor arrays in laminated composite media is presented. It is expected that this present work would help in development of sensing techniques for highly efficient health monitoring of integrated aerospace vehicles and structures. C1 NASA, Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23681 USA. RP Ghoshal, A (reprint author), NASA, Langley Res Ctr, Nondestruct Evaluat Sci Branch, MS 231,3B E Taylor St,Bldg 1230B-Rm 190, Hampton, VA 23681 USA. NR 13 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA BN 0-7354-0173-X J9 REV PROG Q PY 2004 VL 23 BP 737 EP 744 PN A&B PG 8 WC Acoustics; Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Materials Science, Characterization & Testing; Imaging Science & Photographic Technology SC Acoustics; Engineering; Materials Science; Imaging Science & Photographic Technology GA BY96D UT WOS:000189505300093 ER PT B AU Roth, DJ Cosgriff, LM Martin, RE Verrilli, MJ Bhatt, RT AF Roth, DJ Cosgriff, LM Martin, RE Verrilli, MJ Bhatt, RT BE Thompson, DO Chimenti, DE TI Microstructural and defect characterization in ceramic composites using an ultrasonic guided wave scan system SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 23A AND 23B SE REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION LA English DT Proceedings Paper CT 30th Annual Review of Progress in Quantitative Nondestructive Evaluation CY JUL 27-AUG 01, 2003 CL Green Bay, WI SP Iowa State Univ, Ctr Nondestruct Evaluat, QNDE Programs AB In this study, an ultrasonic guided wave scan system was used to characterize various microstructural and flaw conditions in two types of ceramic matrix composites, SiC/SiC and C/SiC. Rather than attempting to isolate specific lamb wave modes to use for characterization (as is desired for many types of guided wave inspection problems), the guided wave scan system utilizes the total (multimode) ultrasonic response in its inspection analysis. Several time- and frequency-domain parameters are calculated from the ultrasonic guided wave signal at each scan location to form images. Microstructural and defect conditions examined include delamination, density variation, cracking, and pre/post-infiltration. Results are compared with thermographic imaging methods. Although the guided wave technique is commonly used so scanning can be eliminated, applying the technique in the scanning mode allows a more precise characterization of defect conditions. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Roth, DJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA BN 0-7354-0173-X J9 REV PROG Q PY 2004 VL 23 BP 906 EP 913 PN A&B PG 8 WC Acoustics; Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Materials Science, Characterization & Testing; Imaging Science & Photographic Technology SC Acoustics; Engineering; Materials Science; Imaging Science & Photographic Technology GA BY96D UT WOS:000189505300114 ER PT B AU Yost, WT Cramer, KE Percy, DF AF Yost, WT Cramer, KE Percy, DF BE Thompson, DO Chimenti, DE TI Characterization of effluents given off by wiring insulation SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 23A AND 23B SE REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION LA English DT Proceedings Paper CT 30th Annual Review of Progress in Quantitative Nondestructive Evaluation CY JUL 27-AUG 01, 2003 CL Green Bay, WI SP Iowa State Univ, Ctr Nondestruct Evaluat, QNDE Programs AB When an insulated wire is heated, the insulation emits a variety of effluents. This paper discusses the basis of emissions of effluents from wiring insulation. Several species are emitted at relatively low temperatures, while others are emitted when the wire reaches higher temperatures. We isolate the emissions by relative molecular weight of the effluents and measure the effluent concentration both as a function of time (temperature held constant) and by wire temperature. We find that the Law of Mass Action describes and predicts the time-dependence of the emission of a specific effluent caused by the heating. The binding energy is determined by performing an Arrhenius Plot on the temperature data. These dependencies are discussed and working equations are derived. Data collected from 20 gauge wire (MIL-W-22759/11-20) is used to illustrate and confirm the validity of the theory. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Yost, WT (reprint author), NASA, Langley Res Ctr, Mail Stop 231, Hampton, VA 23681 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA BN 0-7354-0173-X J9 REV PROG Q PY 2004 VL 23 BP 1155 EP 1161 PN A&B PG 7 WC Acoustics; Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Materials Science, Characterization & Testing; Imaging Science & Photographic Technology SC Acoustics; Engineering; Materials Science; Imaging Science & Photographic Technology GA BY96D UT WOS:000189505300147 ER PT B AU Cramer, KE Yost, WT Perey, DF AF Cramer, KE Yost, WT Perey, DF BE Thompson, DO Chimenti, DE TI Effluent based characterization of aerospace wiring SO REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION, VOLS 23A AND 23B SE REVIEW OF PROGRESS IN QUANTITATIVE NONDESTRUCTIVE EVALUATION LA English DT Proceedings Paper CT 30th Annual Review of Progress in Quantitative Nondestructive Evaluation CY JUL 27-AUG 01, 2003 CL Green Bay, WI SP Iowa State Univ, Ctr Nondestruct Evaluat, QNDE Programs AB This paper discusses a wire insulation characterization method under development, which identifies the relative molecular weight and binding energy of effluents given off during wire heating and is aimed at nondestructively assessing wire insulation degradation. An overview of how this technique can be used to monitor wire insulation emissions is presented. A series of measurements made on wire specimens (MIL-W-22759/11-20) with polytetraflouroethylene (PTFE or Teflon(R)) insulation is presented. A change of up to 55% in the emission concentration of a particular effluent was observed by repeated heating the wire specimens. Temperature measurements of the conductor and insulation were correlated to effluent emission concentrations. A basis for the changes in effluent concentration is also presented and leads to a determination of binding energies and associated time constants. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Cramer, KE (reprint author), NASA, Langley Res Ctr, 4 Langley Blvd,MS 231, Hampton, VA 23681 USA. NR 4 TC 0 Z9 0 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA BN 0-7354-0173-X J9 REV PROG Q PY 2004 VL 23 BP 1162 EP 1169 PN A&B PG 8 WC Acoustics; Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Materials Science, Characterization & Testing; Imaging Science & Photographic Technology SC Acoustics; Engineering; Materials Science; Imaging Science & Photographic Technology GA BY96D UT WOS:000189505300148 ER PT B AU Howard, A Lincoln, W Manvi, R Rodriguez, G Weisbin, CR Drummond, M AF Howard, A Lincoln, W Manvi, R Rodriguez, G Weisbin, CR Drummond, M BE Jamshidi, M Ollero, A MartinezDeDios, JR TI A methodology to determine impact of robotic technologies on space exploration missions SO Robotics: Trends, Principles and Applications, Vol 15 SE TSI PRESS SERIES LA English DT Proceedings Paper CT 10th International Symposium on Robotics and Applications held at the 6th Biannual World Automation Congress CY JUN 28-JUL 01, 2004 CL Seville, SPAIN SP ISORA, Minist Ciencia Tecnol, Univ Sevilla, Unvir Politecnicaa Madrid, Plan Andaluz Invest, World Automat Congress AB This paper presents a new method for evaluating relative strengths and impact of robotic technologies utilized for space exploration missions. The method uses a three tiered process involving mission analysis, technology performance characterization, and technology influence models. Mission analysis focuses on determining the goals of the mission and evaluating the metrics that quantify those goals. Technology performance characterization allows the method to classify the capabilities of a diverse set of robotic technologies, in a systematic fashion, whereas the technology influence models allow understanding of the relationships between technology output and mission requirements. This three-tiered process is designed to provide a general framework for understanding the relative benefits of robotic technologies. Details on the method are provided in this paper and are illustrated on a representative Mars exploration mission. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Howard, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU TSI PRESS PI ALBUQUERQUE PA PO BOX 14126, ALBUQUERQUE, NM 87191-4126 USA BN 1-889335-21-5 J9 TSI PRESS S PY 2004 VL 15 BP 229 EP 234 PG 6 WC Robotics SC Robotics GA BCO51 UT WOS:000230416700037 ER PT B AU Tunstel, E Huntsberger, T Baumgartner, E AF Tunstel, E Huntsberger, T Baumgartner, E BE Jamshidi, M Ollero, A MartinezDeDios, JR TI Earth-based rover field testing for exploration missions on Mars SO Robotics: Trends, Principles and Applications, Vol 15 SE TSI PRESS SERIES LA English DT Proceedings Paper CT 10th International Symposium on Robotics and Applications held at the 6th Biannual World Automation Congress CY JUN 28-JUL 01, 2004 CL Seville, SPAIN SP ISORA, Minist Ciencia Tecnol, Univ Sevilla, Unvir Politecnicaa Madrid, Plan Andaluz Invest, World Automat Congress DE Mars exploration; planetary rover; FIDO; MER; field test; space robotics AB The NASA Mars Exploration Rovers mission (MER) involves two robotic vehicles used to explore the geology of two surface regions on Mars in 2004. Prior to its launch, Earth-based field tests and operations campaigns were conducted in the deserts of southwestern USA to physically simulate the mission operations approach planned for MER. A prototype Mars rover called FIDO was used to conduct these field trials in complex geological settings with terrain analogous to the Martian Surface at the MER landing sites. This paper provides a high-level overview of the last major field operations test conducted in 2002 leading up to the MER mission. Objectives, approach, general results, and lessons learned are discussed. C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. RP Tunstel, E (reprint author), CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. NR 5 TC 1 Z9 1 U1 0 U2 2 PU TSI PRESS PI ALBUQUERQUE PA PO BOX 14126, ALBUQUERQUE, NM 87191-4126 USA BN 1-889335-21-5 J9 TSI PRESS S PY 2004 VL 15 BP 307 EP 312 PG 6 WC Robotics SC Robotics GA BCO51 UT WOS:000230416700049 ER PT B AU Tunstel, E AF Tunstel, E BE Jamshidi, M Ollero, A MartinezDeDios, JR TI Validation of autonomous rover functionalitv for planetary environments SO Robotics: Trends, Principles and Applications, Vol 15 SE TSI PRESS SERIES LA English DT Proceedings Paper CT 10th International Symposium on Robotics and Applications held at the 6th Biannual World Automation Congress CY JUN 28-JUL 01, 2004 CL Seville, SPAIN SP ISORA, Minist Ciencia Tecnol, Univ Sevilla, Unvir Politecnicaa Madrid, Plan Andaluz Invest, World Automat Congress DE planetary rover; software validation; functional testing; Mars AB This paper discusses autonomous rover functionality as it relates to planetary environmental issues and aspects of associated software validation. The focus is on Mars rover functionality and operational issues related to the Mars surface thermal environment, solar power usage, and terrain interactions with rover mobility systems. A liardware-centric approach to functional validation of Mars rover software is advocated. A brief example is discussed in the context of functional validation activities performed for the NASA Mars Exploration Rovers mission using a high-fidelity model of the Spirit and Opportunity rovers. C1 CALTECH, NASA, Jet Prop Lab, Robot Vehicles Grp, Pasadena, CA 91125 USA. RP Tunstel, E (reprint author), CALTECH, NASA, Jet Prop Lab, Robot Vehicles Grp, Pasadena, CA 91125 USA. NR 12 TC 0 Z9 0 U1 0 U2 0 PU TSI PRESS PI ALBUQUERQUE PA PO BOX 14126, ALBUQUERQUE, NM 87191-4126 USA BN 1-889335-21-5 J9 TSI PRESS S PY 2004 VL 15 BP 447 EP 452 PG 6 WC Robotics SC Robotics GA BCO51 UT WOS:000230416700071 ER PT B AU Behar, A Carsey, F Matthews, J Jones, J AF Behar, A Carsey, F Matthews, J Jones, J BE Jamshidi, M Ollero, A MartinezDeDios, JR TI An Antarctic deployment of the NASA/JPL Tumbleweed Polar Rover SO Robotics: Trends, Principles and Applications, Vol 15 SE TSI PRESS SERIES LA English DT Proceedings Paper CT 10th International Symposium on Robotics and Applications held at the 6th Biannual World Automation Congress CY JUN 28-JUL 01, 2004 CL Seville, SPAIN SP ISORA, Minist Ciencia Tecnol, Univ Sevilla, Unvir Politecnicaa Madrid, Plan Andaluz Invest, World Automat Congress DE mobile robotics; extreme environments AB The Tumbleweed Rover, currently under development at the Jet Propulsion Laboratory (JPL) in Pasadena, California, is a large, windblown, inflated ball, which carries an instrument payload in its interior. Such rovers offer an effective and simple means of gathering data over large spatial extents of Earth, Mars, and other solar system bodies. Tumbleweeds could prove to be a safe and economical way of deploying instruments such as a ground penetrating radar or a magnetometer in numerous hostile environments. The latest version of the rover was recently deployed in Greenland, where it completed a more than 130km autonomous traverse across ail ice sheet. Communicating via the Iridium satellite network, the rover in question successfully and reliably relayed live GPS, temperature, and pressure data to a ground station at JPL for nearly ten days. The follow-on rover is currently being readied for a traverse from the South Pole to the coast of Antarctica some 2000km away. The Antarctic test is set to take place in February of 2004 and will serve to verify Tumbleweed as an effective means of harvesting data in extreme and remote settings. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Behar, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 TC 3 Z9 3 U1 1 U2 3 PU TSI PRESS PI ALBUQUERQUE PA PO BOX 14126, ALBUQUERQUE, NM 87191-4126 USA BN 1-889335-21-5 J9 TSI PRESS S PY 2004 VL 15 BP 453 EP 460 PG 8 WC Robotics SC Robotics GA BCO51 UT WOS:000230416700072 ER PT S AU Fu, LL Menard, Y AF Fu, LL Menard, Y BE Hwang, C Shum, CK Li, JC TI Advances in large-scale ocean dynamics from a decade of satellite altimetric measurement of ocean surface topography SO SATELLITE ALTIMETRY FOR GEODESY, GEOPHYSICS AND OCEANOGRAPHY, PROCEEDINGS SE INTERNATIONAL ASSOCIATION OF GEODESY SYMPOSIA LA English DT Proceedings Paper CT International Workshop on Satellite Altimetry for Geodesy, Geophysics and Oceanography CY SEP 08-13, 2002 CL Wuhan Univ, Wuhan, PEOPLES R CHINA SP Int Assoc Geodesy Spec Study Grp, IAG Sect II HO Wuhan Univ DE satellite altimetry; ocean circulation; TOPEX/POSEIDON; El Nino; tides ID TOPEX/POSEIDON; CIRCULATION AB The past decade has seen the most intensive observations of the global ocean surface topography from satellite altimeters. The Joint U.S./France TOPEX/POSEIDON (T/P) Mission has become the longest radar mission ever flown in space, providing the most accurate measurements for the study of ocean dynamics since October, 1992. The European Space Agency's ERS-1 and -2 Mission also provided altimetric observations from 1991-2000. The combined data from T/P and ERS have higher spatial resolution and greater coverage than the individual missions. Major advances in large-scale ocean dynamics from these observations are reviewed in the paper, including the ocean general circulation and its variability, the evolution of the El Nino Southern Oscillation cycles as well as the emerging decadal variability, the response of the ocean to wind forcing, assimilation of altimeter data by ocean general circulation models and the estimation of deep ocean circulation, global sea level rise, and tidal models and mixing. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fu, LL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-323, Pasadena, CA 91109 USA. RI Symposia, IAG/K-2857-2012 NR 10 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0939-9585 BN 3-540-20211-0 J9 IAG SYMP PY 2004 VL 126 BP 33 EP 37 PG 5 WC Geosciences, Multidisciplinary; Oceanography; Remote Sensing SC Geology; Oceanography; Remote Sensing GA BY69R UT WOS:000189441200003 ER PT S AU Zuffada, C Lowe, S Chao, Y Treuhaft, R AF Zuffada, C Lowe, S Chao, Y Treuhaft, R BE Hwang, C Shum, CK Li, JC TI Oceanography with GPS SO SATELLITE ALTIMETRY FOR GEODESY, GEOPHYSICS AND OCEANOGRAPHY, PROCEEDINGS SE INTERNATIONAL ASSOCIATION OF GEODESY SYMPOSIA LA English DT Proceedings Paper CT International Workshop on Satellite Altimetry for Geodesy, Geophysics and Oceanography CY SEP 08-13, 2002 CL Wuhan Univ, Wuhan, PEOPLES R CHINA SP Int Assoc Geodesy Spec Study Grp, IAG Sect II HO Wuhan Univ DE high-resolution sea surface topography; eddy monitoring; GPS-based altimetry and scatterometry; bistatic scattering from rough surfaces ID SEA-SURFACE; SIGNALS; OCEAN; SCATTERING; ALTIMETRY; SYSTEM; MODEL AB This paper discusses a new technique for ocean remote sensing based on detecting GNSS signals, i.e. those transmitted from the Global Positioning System (GPS) or GALILEO (in the future), after they are reflected off the ocean surface, to measure sea surface topography and roughness (from which wind speeds are retrieved) at high spatial resolution and rapid temporal coverage. The topography measurement is suitable for the global monitoring of ocean eddies, which is currently precluded by the existing altimeters, due to their track separation and repeat cycle. The basic description of the technique is provided and the connection between the engineering measurement and the ocean descriptors (altimetry and winds) is outlined. A discussion of measurement accuracy and resolution is provided, and the concept of combining many independent measurements to provide an "average" over a given cell size and time interval, as opposed to repeat measurements, is outlined. To address the issue of systems needs for global coverage, an estimate of the scaling of accuracy with the number of available receivers of a hypothetical remote sensing system is given, showing that a constellation of 6 receivers with reflection antenna gain of 30 dB would be adequate for eddy resolution and monitoring. Furthermore, the latest experimental results demonstrating a measurement precision of 5 cm in a few minutes from airplane flying over rough ocean and 2 cm/sec from fixed-site over a lake are summarized, together with the basic features of a data acquisition/processing system developed for investigating the measurement phenomenology. Lastly, the requirements on the GPS receiver technology necessary to track and process reflections on board, and those of the antenna system necessary to capture all available reflections, are discussed. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zuffada, C (reprint author), CALTECH, Jet Prop Lab, MS 183-601, Pasadena, CA 91109 USA. RI Symposia, IAG/K-2857-2012 NR 21 TC 1 Z9 1 U1 1 U2 4 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0939-9585 BN 3-540-20211-0 J9 IAG SYMP PY 2004 VL 126 BP 193 EP 203 PG 11 WC Geosciences, Multidisciplinary; Oceanography; Remote Sensing SC Geology; Oceanography; Remote Sensing GA BY69R UT WOS:000189441200023 ER PT J AU Nelson, R Short, A Valenti, M AF Nelson, R Short, A Valenti, M TI Measuring biomass and carbon in Delaware using an airborne profiling LIDAR SO SCANDINAVIAN JOURNAL OF FOREST RESEARCH LA English DT Article; Proceedings Paper CT Scandlaser Workshop 2003 CY SEP 02-04, 2003 CL Umea, SWEDEN SP Nordic Forest Res Co-Operat Comm DE airborne laser profiling; forest biomass; regional forest inventory ID INVENTORY; IMAGERY AB A portable, inexpensive profiling light detection and ranging (LIDAR) system was used to inventory forests in Delaware, a small state (5205 kin 2) on the mid-Atlantic seaboard of the USA. Ground and airborne sampling procedures are described, and large-area inventory results are reported and compared to independent estimates. Systematic airborne LIDAR profiling measurements were used (1) to estimate forest merchantable Volume, biomass and above-ground carbon statewide; and (2) to estimate impervious surface and open water area. Over 1300 kin of laser profiling data acquired along parallel flight lines 4 kin apart were analysed. Four explicitly linear models were considered to predict merchantable Volume and total above-ground dry biomass. Merchantable Volume estimates were within 21%, of US Forest Service estimates at the county level and within 1% statewide. Total above-ground dry biomass estimates were within 22% of USFS estimates at the county level and within 16% statewide. LIDAR estimates of percentage impervious area surface for the three counties (Newcastle, Kent and Sussex) were 10.9, 3.4 and 2.8%, respectively, and 4.7% statewide. Comparable estimates developed using 30 in Enhanced Thematic Mapper digital data and mixture modelling were 8.8, 3.5 and 3.9%, respectively, and 4.9% statewide. Laser estimates of open water at the county and state level were comparable to 1997 Geographical Information System (GIS) estimates. Open water estimates based on laser transect data showed the three counties to have 3.0, 2.0 and 4.6% of their county area covered by water, and 3.5% of the state to be covered by open water. Comparable 1997 GIS estimates were 2.6, 2.1 and 4.8% (county), and 3.5% (state), respectively. The results of the study indicate that line intercept sampling techniques can be used in conjunction with a relatively inexpensive, portable airborne laser system to assess multiple resources regionally. C1 NASA, Goddard Space Flight Ctr, Biospher Sci Branch 923, Greenbelt, MD 20771 USA. Delaware Forest Serv, Dover, DE 19901 USA. RP Nelson, R (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch 923, Code 661, Greenbelt, MD 20771 USA. EM Ross.F.Nelson@nasa.gov RI Nelson, Ross/H-8266-2014 NR 14 TC 70 Z9 76 U1 1 U2 12 PU TAYLOR & FRANCIS AS PI OSLO PA CORT ADELERSGT 17, PO BOX 2562, SOLLI, 0202 OSLO, NORWAY SN 0282-7581 J9 SCAND J FOREST RES JI Scand. J. Forest Res. PY 2004 VL 19 IS 6 BP 500 EP 511 DI 10.1080/02827580410019508 PG 12 WC Forestry SC Forestry GA 883YA UT WOS:000226050600003 ER PT B AU Waczynski, A Beck, T Boucarut, R Cheng, E Cottingham, D Delo, G Fixsen, D Hill, RJ Johnson, S Kenny, P Landsman, W Malumuth, E Offenberg, J Polidan, E Russell, AM Schlossberg, D Sharp, E Wassell, E Wen, YT Yagelowich, J AF Waczynski, A Beck, T Boucarut, R Cheng, E Cottingham, D Delo, G Fixsen, D Hill, RJ Johnson, S Kenny, P Landsman, W Malumuth, E Offenberg, J Polidan, E Russell, AM Schlossberg, D Sharp, E Wassell, E Wen, YT Yagelowich, J BE Amico, P Beletic, JW Beletic, JE TI HgCdTe detectors for the Hubble Space Telescope wide field camera 3 IR channel SO SCIENTIFIC DETECTORS FOR ASTRONOMY: THE BEGINNING OF A NEW ERA SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Scientific Detectors for Astronomy Workshop (SDW2002) CY JUN, 2002 CL Waimea, HI DE Hubble Space Telescope (HST); Wide Field Camera 3 (WFC3); HgCdTe; infrared (IR); focal plane; multiplexer; Quantum Efficiency (QE); noise; dark AB Detector performance has been characterized for the HST WFC3 IR channel. This will be the first TEC cooled IR instrument on the Hubble Space Telescope (HST), which is made possible because of recent progress in HgCdTe technology. The original detector requirements are compared with the performance of the delivered devices. Achievements in quantum efficiency and dark current are described, as well as difficulties in meeting requirements for noise and dark stability. A special technique developed to illuminate a single pixel, which has demonstrated the excellent spatial resolution of the detectors is described. C1 NASA, Goddard Space Flight Ctr, GST, Greenbelt, MD 20771 USA. RP Waczynski, A (reprint author), NASA, Goddard Space Flight Ctr, GST, Greenbelt, MD 20771 USA. RI Polidan, Elizabeth/F-4052-2014 OI Polidan, Elizabeth/0000-0002-4940-9638 NR 0 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-1788-X J9 ASTROPHYS SPACE SC L PY 2004 VL 300 BP 175 EP 182 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAN06 UT WOS:000222918100020 ER PT B AU Waczynski, A Beck, T Boucarut, R Cheng, E Cottingham, D Delo, G Fixsen, D Hill, RJ Johnson, S Kenny, P Landsman, W Malumuth, E Offenberg, J Polidan, E Russell, AM Schlossberg, D Sharp, E Wassell, E Wen, Y Yagelowich, J AF Waczynski, A Beck, T Boucarut, R Cheng, E Cottingham, D Delo, G Fixsen, D Hill, RJ Johnson, S Kenny, P Landsman, W Malumuth, E Offenberg, J Polidan, E Russell, AM Schlossberg, D Sharp, E Wassell, E Wen, Y Yagelowich, J BE Amico, P Beletic, JW Beletic, JE TI The Hubble Space Telescope Wide Field Camera 3 instrument Charge-Coupled Device detectors SO SCIENTIFIC DETECTORS FOR ASTRONOMY: THE BEGINNING OF A NEW ERA SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Scientific Detectors for Astronomy Workshop (SDW2002) CY JUN, 2002 CL Waimea, HI DE Hubble Space Telescope (HST); Wide Field Camera 3 (WFC3); Charge Coupled Device (CCD); Charge Transfer Efficiency (CTE); Charge Transfer Inefficiency (CTI); charge injection AB The Hubble Space Telescope Wide Field Camera 3 (WFC3) is a new instrument planned for deployment during Servicing Mission 4 in 2004. One of its key scientific goals is to provide panchromatic coverage from the near UV through the near-IR. This is accomplished using two detector technologies, Marconi Applied Technologies back-thinned CCDs and Rockwell Scientific Mercury-Cadmium-Telluride (HgCdTe) IR focal planes. The Marconi CCDs have been delivered and characterized The performance of these devices is exceptionally good, and will provide a new wide-field, nearUV capability for the observatory. Several notable advances are described. C1 NASA, Goddard Space Flight Ctr, GST, Greenbelt, MD 20771 USA. RP Waczynski, A (reprint author), NASA, Goddard Space Flight Ctr, GST, Greenbelt, MD 20771 USA. RI Polidan, Elizabeth/F-4052-2014 OI Polidan, Elizabeth/0000-0002-4940-9638 NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-1788-X J9 ASTROPHYS SPACE SC L PY 2004 VL 300 BP 403 EP 406 PG 4 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAN06 UT WOS:000222918100049 ER PT S AU Burgdorf, MJ Orton, GS Encrenaz, T Davis, GR Lellouch, E Sidher, SD Swinyard, BM AF Burgdorf, MJ Orton, GS Encrenaz, T Davis, GR Lellouch, E Sidher, SD Swinyard, BM BE Lebreton, JP Agee, CB Stabekis, PD Bernhardt, P Ganguli, GI TI Far-infrared spectroscopy of the giant planets: measurements of ammonia and phosphine at Jupiter and Saturn and the continuum of Neptune SO SCIENTIFIC EXPLORATION, PLANETARY PROTECTION, ACTIVE EXPERIMENTS AND DUSTY PLASMAS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE abundances; atmospheres; infrared observations; Jovian planets; spectroscopy ID ISO-SWS OBSERVATIONS; LWS; WAVELENGTH; SPECTRUM AB We detected rotational transition features of ammonia and phosphine in the far-infrared spectra of Jupiter and Saturn and measured the far-infrared continuum of Neptune with high photometric accuracy. These observations were made with the long-wavelength spectrometer (LWS) aboard the infrared space observatory (ISO). The LWS covered the wavelength region between 43 and 197 mum (51-233 cm(-1)) with both medium and high spectral resolving power. Also 'Neptune's continuum was measured with the LWS and at shorter wavelengths with the ISO short-wavelength spectrometer (SWS). The spectra observed in the far-infrared are compared to synthetic spectra calculated from atmospheric radiative transfer models using expected values for the constituent vertical concentration profiles. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Observ Paris, LESIA, F-92195 Meudon, France. Joint Astron Ctr, Hilo, HI 96720 USA. Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. RP Burgdorf, MJ (reprint author), CALTECH, SIRTF Sci Ctr, 220-6, Pasadena, CA 91125 USA. EM burgdorf@ipac.caltech.edu NR 19 TC 8 Z9 8 U1 3 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 11 BP 2247 EP 2250 DI 10.1016/j.asr.2004.04.004 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BBN86 UT WOS:000226379100002 ER PT S AU Sears, D Allen, C Britt, D Brownlee, D Franzen, M Gefert, L Gorovan, S Pieters, C Preble, J Scheeres, D Scott, E AF Sears, D Allen, C Britt, D Brownlee, D Franzen, M Gefert, L Gorovan, S Pieters, C Preble, J Scheeres, D Scott, E BE Lebreton, JP Agee, CB Stabekis, PD Bernhardt, P Ganguli, GI TI The Hera mission: multiple near-earth asteroid sample return SO SCIENTIFIC EXPLORATION, PLANETARY PROTECTION, ACTIVE EXPERIMENTS AND DUSTY PLASMAS SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE multiple asteroid sample return; the Hera mission; near-earth asteroids AB The NEAR mission was a spectacular rehearsal for one of the most exciting and scientifically rewarding missions of the next decade, sample return from near-Earth asteroids. A unique source of information about the early solar system, the formation of the planets, and the connection between stars and our Sun, are meteorites and asteroids. Yet, studies of both are hindered by a lack of unequivocal and detailed information linking the two. Meteorites are rock samples of unknown provenance. We have no information about the geological context of their source. They are also highly non-representative sampling of primitive solar system material because the terrestrial meteorite population is dominated by the ejecta of stochastic impacts and because the atmosphere filters out all but the toughest rocks. Without sample return, asteroids are not amenable to the depth and breadth of techniques available in the laboratory, yet the NEAR images indicate that there are many processes occurring on asteroids - or that could have occurred in the past - that we must understand if the meteorite data are ever to yield a clear image of early solar system processes. Technical developments of the last few years and the discovery of large numbers of NEAs mean that sample return is now within small mission capability. A team of about 20 scientists and engineers from all relevant subject fields are now assembling a mission called Hera. This paper reviews the mission as of fall 2002. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Arkansas, Dept Chem & Biochem, Oklahoma Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Tennessee, Dept Geol Sci, Knoxville, TN 37996 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Honeybee Robot Inc, New York, NY 10012 USA. Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. SpaceWorks Inc, Carefree, AZ 85377 USA. Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA. Univ Hawaii, Inst Planetary Geophys, Dept Earth & Planetary Sci, Honolulu, HI 96822 USA. RP Sears, D (reprint author), Univ Arkansas, Dept Chem & Biochem, Oklahoma Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA. EM dsears@uark.edu NR 21 TC 12 Z9 12 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2004 VL 34 IS 11 BP 2270 EP 2275 DI 10.1016/j.asr.2003.05.059 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BBN86 UT WOS:000226379100006 ER PT S AU Sears, DWG Allen, CC Bell, MS Bogard, D Britt, D Brownlee, DE Chapman, C Clark, BC Dissley, R Franzen, MA Goldstein, J Nishiizumi, K Nyquist, L Pieters, CM Scheeres, D Scott, ERD Treiman, A AF Sears, DWG Allen, CC Bell, MS Bogard, D Britt, D Brownlee, DE Chapman, C Clark, BC Dissley, R Franzen, MA Goldstein, J Nishiizumi, K Nyquist, L Pieters, CM Scheeres, D Scott, ERD Treiman, A BE Lebreton, JP Agee, CB Stabekis, PD Bernhardt, P Ganguli, GI TI The Hera near-Earth asteroid sample return mission: science requirements of the sample collector SO SCIENTIFIC EXPLORATION, PLANETARY PROTECTION, ACTIVE EXPERIMENTS AND DUSTY PLASMAS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE sample return mission; Hera; science requirements of the sample collector; near-earth asteroids AB The Hera mission is a proposed Discovery class mission to collect three samples from each of three near-Earth asteroids. Returned samples would have information on geological context and possibly stratigraphy, would provide fresh regolith, and conceivably samples that would not naturally reach the Earth. During the development of a simple touch-and-go sample collector, questions arose concerning the nature of the samples to be collected, their maximum science return, and the simplest engineering designs. This article reports the results of a small workshop convened to discuss this topic. It is argued that the maximum science return for the Hera samples would be obtained if asteroids of different major spectral classes were visited, samples were disturbed as little as possible during collection, and samples from the very surface were obtained. Surface samples would have the utmost value in interpreting links between asteroids and meteorites, would yield maximum information in solar exposure, would avoid planetary protection concerns, and would produce material not reaching Earth as meteorites. At the same time, they would be simpler to sample than subsurface samples. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Arkansas, Dept Chem & Biochem, Oklahoma Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Tennessee, Dept Geol Sci, Knoxville, TN 37996 USA. Univ Washington, Dept Astron, Seattle, WA 98195 USA. SW Res Inst, Boulder, CO 80306 USA. Lockheed Martin Astronaut, Denver, CO 80202 USA. Ball Aerosp & Technol Corp, Boulder, CO 80306 USA. Univ Massachusetts, Coll Engn, Amherst, MA 01003 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA. Univ Hawaii Manoa, Dept Earth & Planetary Sci, Honolulu, HI 96822 USA. Univ Hawaii Manoa, Inst Planetary Geophys, Honolulu, HI 96822 USA. Lunar & Planetary Inst, Houston, TX 77058 USA. RP Sears, DWG (reprint author), Univ Arkansas, Dept Chem & Biochem, Oklahoma Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA. EM dsears@uark.edu NR 21 TC 7 Z9 8 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 11 BP 2276 EP 2280 DI 10.1016/j.asr.2003.05.058 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BBN86 UT WOS:000226379100007 ER PT S AU Gershman, R Adams, M Mattingly, R Rohatgi, N Corliss, J Dillman, R Fragola, J Minarick, J AF Gershman, R Adams, M Mattingly, R Rohatgi, N Corliss, J Dillman, R Fragola, J Minarick, J BE Lebreton, JP Agee, CB Stabekis, PD Bernhardt, P Ganguli, GI TI Planetary protection for Mars sample return SO SCIENTIFIC EXPLORATION, PLANETARY PROTECTION, ACTIVE EXPERIMENTS AND DUSTY PLASMAS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE planetary protection; Mars sample return; sample contamination avoidance AB A Mars sample return (MSR) mission must deal with two new categories of planetary protection requirements: (1) assuring a very low probability of inadvertent release of the sample in order to provide extra protection against the extremely unlikely possibility of biological hazards in the returned material and (2) keeping the samples free of round-trip Earth organisms to facilitate confirmation of safety after return to Earth. This paper describes the planetary-protection-related technical challenges awaiting an MSR mission as well as the range of capabilities being developed to meet these challenges. Containment assurance requires breaking the chain of contact with Mars: the exterior of the sample container must not be contaminated with Mars material. The sample container and its seals must be designed to survive Earth impacts corresponding to the candidate mission profiles, and the Earth entry vehicle must be designed to withstand the thermal and structural rigors of Earth atmosphere entry (all with an unprecedented degree of confidence). Sample contamination must be avoided by sterilizing the entire spacecraft, a challenge with modern avionics, or by sterilizing the sample collection and containment gear and then isolating it from other parts of the spacecraft. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Gershman, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.gershman@jpl.nasa.gov NR 0 TC 2 Z9 2 U1 3 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 11 BP 2328 EP 2337 DI 10.1016/j.asr.2003.09.062 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BBN86 UT WOS:000226379100016 ER PT S AU Davila, JM Poland, AI Harrison, RA AF Davila, JM Poland, AI Harrison, RA BE Lebreton, JP Agee, CB Stabekis, PD Bernhardt, P Ganguli, GI TI International heliophysical year: a program of global research continuing the tradition of previous international years SO SCIENTIFIC EXPLORATION, PLANETARY PROTECTION, ACTIVE EXPERIMENTS AND DUSTY PLASMAS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE international heliospherical yearn; global research; international geophysical year; international polar years AB In 1957 a program of international research, inspired by the International Polar Years of 1882-1883 and 1932-1931, was organized as the International Geophysical Year (IGY) to study global phenomena of the Earth and geospace. The IGY involved about 60,000 scientists from 66 nations, working at thousands of stations from pole to pole, in an effort to obtain simultaneous, global observations on Earth and in space. There had never been anything like it before. The 50th anniversary of the International Geophysical Year will occur in 2007. We propose to organize an international program of scientific collaboration for this time period called the International Heliophysical Year (IHY). Like its predecessors. the MY will focus on fundamental global questions of Earth science. (C) 2004 Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. RP Davila, JM (reprint author), NASA, Goddard Space Flight Ctr, Code 682, Greenbelt, MD 20771 USA. EM davila@lindsay.gsfc.nasa.gov NR 5 TC 1 Z9 1 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 11 BP 2453 EP 2458 DI 10.1016/j.asr.2004.07.008 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BBN86 UT WOS:000226379100036 ER PT S AU Benford, DJ Danchi, WC Allen, RJ Deming, D Gezari, DY Kuchner, M Leisawitz, DT Linfield, R Millan-Gabeo, R Monnier, JD Mumma, M Mundy, LG Noecker, C Rajagopal, J Rinehart, SA Seager, S Traub, WA AF Benford, DJ Danchi, WC Allen, RJ Deming, D Gezari, DY Kuchner, M Leisawitz, DT Linfield, R Millan-Gabeo, R Monnier, JD Mumma, M Mundy, LG Noecker, C Rajagopal, J Rinehart, SA Seager, S Traub, WA BE Holt, SS Deming, D TI The Fourier-Kelvin stellar interferometer: A concept for a practical interferometric mission for discovering and investigating extrasolar giant planets SO SEARCH FOR OTHER WORLDS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 14th Annual Astrophysics Conference CY OCT 13-14, 2003 CL College Pk, MD SP NASA, Goddard Space Flight Ctr, Univ Maryland AB The Fourier-Kelvin Stellar Interferometer (FKSI) is a mission concept for a nulling interferometer for the near-to-mid-infrared spectral region (3 - 8 mum). FKSI is conceived as a scientific and technological precursor to TPF. The scientific emphasis of the mission is on the evolution of protostellar systems, from just after the collapse of the precursor molecular cloud core, through the formation of the disk surrounding the protostar, the formation of planets in the disk, and eventual dispersal of the disk material. FKSI will answer key questions about extrasolar planets: What are the characteristics of the known extrasolar giant planets? What are the characteristics of the extrasolar zodiacal clouds around nearby stars? Are there giant planets around classes of stars other than those already studied? We present preliminary results of a detailed design study of the FKSI. Using a nulling interferometer configuration, the optical system consists of two 0.5 m telescopes on a 12.5 m boom feeding a Mach-zender beam combiner with a fiber wavefront error reducer to produce a 0.01% null of the central starlight. With this system, planets around nearby stars can be detected and characterized using a combination of spectral and spatial resolution. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Benford, DJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Benford, Dominic/D-4760-2012; Kuchner, Marc/E-2288-2012; mumma, michael/I-2764-2013 OI Benford, Dominic/0000-0002-9884-4206; NR 3 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0190-X J9 AIP CONF PROC PY 2004 VL 713 BP 297 EP 300 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAM87 UT WOS:000222875000051 ER PT S AU Rinehart, SA Leisawitz, DT Frey, BJ Kuchner, M Leviton, DB Lobsinger, LW Martino, AJ Mundy, LG AF Rinehart, SA Leisawitz, DT Frey, BJ Kuchner, M Leviton, DB Lobsinger, LW Martino, AJ Mundy, LG BE Holt, SS Deming, D TI Wide-field interferometric imaging: A powerful tool for the terrestrial planet finder SO SEARCH FOR OTHER WORLDS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 14th Annual Astrophysics Conference CY OCT 13-14, 2003 CL College Pk, MD SP NASA, Goddard Space Flight Ctr, Univ Maryland AB We present a discussion of the design and construction of the Wide-Field Imaging Interferometry Testbed (WIIT) at the Goddard Space Flight Center. The testbed is motivated by a need to develop techniques for wide-field interferometric imaging in the optical/IR for future space missions such as TPF. Theoretically, using multipixel detectors for spatial multiplexing/mosaicing allows this, but there are a number of practical questions which WILT will address. We present some initial data acquired with this system and demonstrate its capability to produce wide-field interferometry data. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rinehart, SA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Kuchner, Marc/E-2288-2012 NR 7 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0190-X J9 AIP CONF PROC PY 2004 VL 713 BP 305 EP 308 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAM87 UT WOS:000222875000053 ER PT S AU Nowakowski, M Bandaru, J Bell, LD Nikzad, S AF Nowakowski, M Bandaru, J Bell, LD Nikzad, S BE Norman, AG Goldman, RS Noetzel, R Stringfellow, GB TI Preparation of Ge(100) substrates for high-quality epitaxial growth of group IV materials SO SELF-ORGANIZED PROCESSES IN SEMICONDUCTOR HETEROEPITAXY SE MATERIALS RESEARCH SOCIETY SYMPOSIUM PROCEEDINGS LA English DT Proceedings Paper CT Symposium on Self-Organized Processes in Semiconductor Epitaxy held at the 2003 MRS Fall Meeting CY DEC 01-05, 2003 CL Boston, MA SP Mat Res Soc ID STABILITY; SURFACES; XPS; MBE AB We compare various wet chemical treatments, in preparing high-quality Ge (100) surfaces suitable for molecular beam epitaxy (MBE). Various surface treatments are explored such as UV-ozone treatment followed by exposure to chemical solutions such as de-ionized (DI) water, hydrofluoric acid (HF), or hydrochloric acid (HCl). Chemical treatments to remove the oxide are performed in a nitrogen environment to prevent further formation of surface oxide prior to surface analysis. Following chemical treatments, in situ reflection high-energy electron diffraction (RHEED) analysis is performed to observe the surface evolution as a function of temperature. In a separate chamber, we analyze each sample, before and after chemical treatment by x-ray photoelectron spectroscopy (XPS) to directly determine the oxide desorption following each chemical treatment. Our results of this comparative study, the effectiveness of each chemical treatment, and the stability of the passivated surface suggest that UV ozone cleaning, followed by 10% HCl is the best choice for removing most of the oxide. Furthermore, we present evidence of high quality epitaxial growth of SnxGe1-x on wafers prepared by our method. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Nowakowski, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 10 TC 0 Z9 0 U1 2 U2 3 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 USA SN 0272-9172 BN 1-55899-732-6 J9 MATER RES SOC SYMP P PY 2004 VL 794 BP 71 EP 76 PG 6 WC Materials Science, Multidisciplinary; Physics, Condensed Matter SC Materials Science; Physics GA BAH11 UT WOS:000222180100012 ER PT S AU Keller, RM Berrios, DC Carvalho, RE Hall, DR Rich, SJ Sturken, IB Swanson, KJ Wolfe, SR AF Keller, RM Berrios, DC Carvalho, RE Hall, DR Rich, SJ Sturken, IB Swanson, KJ Wolfe, SR BE McIlraith, SA Plexousakis, D VanHarmelen, F TI SemanticOrganizer: A customizable semantic repository for distributed NASA project teams SO SEMANTIC WEB - ISWC 2004, PROCEEDINGS SE LECTURE NOTES IN COMPUTER SCIENCE LA English DT Article; Proceedings Paper CT 3rd International Semantic Web Conference CY NOV 07-11, 2004 CL Hiroshima, JAPAN SP sekt, Asian Off Aerosp R&D, USA Res Off, Hitachi, Toshiba, Nokia, france telecom R&D, network inference, SEMAGIX, DERI, SWAP, AKT, NEC, Knowledge, ontopia, Gakken, UNISYS, JUSTSYSTEM, Fujitsu AB SemanticOrganizer is a collaborative knowledge management system designed to support distributed NASA projects, including multidisciplinary teams of scientists, engineers, and accident investigators. The system provides a customizable, semantically structured information repository that stores work products relevant to multiple projects of differing types. SemanticOrganizer is one of the earliest and largest semantic web applications deployed at NASA to date, and has been used in varying contexts ranging from the investigation of Space Shuttle Columbia's accident to the search for life on other planets. Although the underlying repository employs a single unified ontology, access control and ontology customization mechanisms make the repository contents appear different for each project team. This paper describes SemanticOrganizer, its customization facilities, and a sampling of its applications. The paper also summarizes some key lessons learned from building and fielding a successful semantic web application across a wide-ranging set of domains with disparate users. C1 NASA, Ames Res Ctr, Computat Sci Div, Moffett Field, CA 94035 USA. RP Keller, RM (reprint author), NASA, Ames Res Ctr, Computat Sci Div, Moffett Field, CA 94035 USA. EM rkeller@arc.nasa.gov; dberrios@arc.nasa.gov; rcarvalho@arc.nasa.gov; dhall@arc.nasa.gov; srich@arc.nasa.gov; isturken@arc.nasa.gov; kswanson@arc.nasa.gov; swolfe@arc.nasa.gov NR 16 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-23798-4 J9 LECT NOTES COMPUT SC PY 2004 VL 3298 BP 767 EP 781 PG 15 WC Computer Science, Artificial Intelligence; Computer Science, Information Systems; Computer Science, Theory & Methods SC Computer Science GA BBJ33 UT WOS:000225767000053 ER PT S AU Woodell, G Rahman, Z Jobson, DJ Hines, G AF Woodell, G Rahman, Z Jobson, DJ Hines, G BE Carapezza, EM TI Enhanced images for checked and carry-on baggage and cargo screening SO SENSORS, AND COMMAND, CONTROL, COMMUNICATIONS, AND INTELLIGENCE(C31) TECHNOLOGIES FOR HOMELAND SECURITY AND HOMELAND DEFENSE III, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors and Command, Control, Communications and Intelligence (C31) Technologies for Homeland Security and Homeland Defense III CY APR 12-16, 2004 CL Orlando, FL SP SPIE DE retinex; X-rays; image enhancement; baggage screening ID RETINEX AB The current X-ray systems used by airport security personnel for the detection of contraband, and objects such as knives and guns that can impact the security of a flight, have limited effect because of the limited display quality of the X-ray images. Since the displayed images do not possess optimal contrast and sharpness, it is possible for the security personnel to miss potentially hazardous objects. This problem is also common to other disciplines such as medical Xrays, and can be mitigated, to a large extent, by the use of state-of-the-art image processing techniques to enhance the contrast and sharpness of the displayed image. The NASA Langley Research Center's Visual Information Processing Group has developed an image enhancement technology that has direct applications to the problem of inadequate display quality. Airport security X-ray imaging systems would benefit considerably by using this novel technology, making the task of the personnel who have to interpret the X-ray images considerably easier, faster, and more reliable. This improvement would translate into more accurate screening as well as minimizing the screening time delays to airline passengers. This technology, Retinex, has been optimized for consumer applications but has been applied to medical X-rays on a very preliminary basis. The resultant technology could be incorporated into a new breed of commercial x-ray imaging systems which would be transparent to the screener yet allow them to see subtle detail much more easily, reducing the amount of time needed for screening while greatly increasing the effectiveness of contraband detection and thus improving public safety. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Woodell, G (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. NR 8 TC 1 Z9 1 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5326-9 J9 P SOC PHOTO-OPT INS PY 2004 VL 5403 BP 582 EP 589 DI 10.1117/12.530669 PN 1-2 PG 8 WC Computer Science, Interdisciplinary Applications; Engineering, Multidisciplinary; Optics; Physics, Applied; Imaging Science & Photographic Technology SC Computer Science; Engineering; Optics; Physics; Imaging Science & Photographic Technology GA BAZ63 UT WOS:000224321700062 ER PT S AU Liu, WT Tang, WQ AF Liu, WT Tang, WQ BE Meynart, R Neeck, SP Shimoda, H Lurie, JB Aten, M TI Calibration/validation of SeaWinds on ADEOS-2 SO SENSORS, SYSTEMS AND NEXT-GENERATION SATELLITES VII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems and Next-Generation Satellites VII CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE, Soc Espanola Ott, NASA, European Opt Soc AB A microwave scatterometer of the National Aeronautics and Space Administration (NASA) of the United States, SeaWinds, was launched on the second Advanced Earth Observing System (ADEOS-II) of the Japanese Space Agency (NASDA) in December 2002. A preliminary data set was released to the Ocean Vector Wind Science Team (OVWST) for calibration/validation on July 15, 2003. A comparison of this data set with ocean buoy measurements was performed and the quality of the data was found to be very similar to that from an identical scatterometer deployed on NASA QuikSCAT mission. An overview of potential unique impact of SeaWinds on ADEOS-2 is also presented. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP Liu, WT (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5117-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5234 BP 47 EP 52 DI 10.1117/12.510789 PG 6 WC Engineering, Aerospace; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Remote Sensing; Imaging Science & Photographic Technology GA BY70A UT WOS:000189442100006 ER PT S AU Neeck, SP Kakar, RK Adams, WJ Smith, EA AF Neeck, SP Kakar, RK Adams, WJ Smith, EA BE Meynart, R Neeck, SP Shimoda, H Lurie, JB Aten, M TI Formulating Global Precipitation Measurement (GPM) SO SENSORS, SYSTEMS AND NEXT-GENERATION SATELLITES VII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems and Next-Generation Satellites VII CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE, Soc Espanola Ott, NASA, European Opt Soc AB Understanding the Earth's climate and how it responds to climate perturbations relies on knowledge of how atmospheric moisture, clouds, latent heating, and the large-scale circulation vary with changing climate conditions. The physical process that links these key climate elements is precipitation. GPM will establish a benchmark for global rainfall, building upon the highly successful joint US/Japan Tropical Rainfall Measuring Mission (TRMM). GPM's global atmospheric monitoring of water and energy will be a key contributor to answering the science research strategy questions: (1) How are global precipitation, evaporation, and the cycling of water changing? (2) How are variations in local weather, precipitation, and water resources related to global climate variation? (3) How can weather forecast duration and reliability be improved by new space-based observations, data assimilation and modeling? In an era of climatic uncertainty we need to be able to detect, understand and react to early signs that rainfall patterns may be changing in concert with better-understood climate variables. The transient nature of rainfall makes the detection of subtle changes difficult. Rainfall information over similar to3 hours time scale is needed to improve weather forecast models, data assimilation models, hydrological models and flash flood forecasts. GPM will substantially improve upon the temporal and spatial coverage of TRMM and extend the measurement of rainfall globally. Global Precipitation Measurement is a global endeavor that has sparked global interest. It has received overwhelming endorsement from the World Climate Research Programme, the World Meteorological Organization, and the Committee on Earth Observation Satellites. Japan's National Space Development Agency (NASDA) plans to contribute the radar for and launch of a core satellite. The European Space Agency (ESA) is currently conducting a feasibility study for a European constellation satellite contribution to GPM. India and France have expressed their interest in participating through the Megha-Tropiques project. South Korea is proposing the contribution of a constellation satellite bus in addition to regional ground validation sites. Other nations are also expected to play major a role in GPM. GPM is now in Formulation Phase and is one of the highest priority new missions for which NASA's Earth Science Enterprise (ESE) seeks final approval. GPM launches are targeted to begin in 2009. C1 NASA Headquarters, Washington, DC 20546 USA. RP Neeck, SP (reprint author), NASA Headquarters, Washington, DC 20546 USA. NR 10 TC 0 Z9 0 U1 0 U2 4 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5117-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5234 BP 106 EP 115 DI 10.1117/12.511540 PG 10 WC Engineering, Aerospace; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Remote Sensing; Imaging Science & Photographic Technology GA BY70A UT WOS:000189442100012 ER PT S AU Stocker, EF AF Stocker, EF BE Meynart, R Neeck, SP Shimoda, H Lurie, JB Aten, M TI The GPM precipitation processing system SO SENSORS, SYSTEMS AND NEXT-GENERATION SATELLITES VII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems and Next-Generation Satellites VII CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE, Soc Espanola Ott, NASA, European Opt Soc DE architecture; ESE,GPM; ESE; measurement-based; PPS; precipitation; radar; radiometer; rolling-wave AB NASA's Earth Science Enterprise (ESE) is changing focus from single satellite missions to measurement oriented programs. An example of this paradigm shift is the Global Precipitation Measurement (GPM) project. GPM is conceptualized as a rolling-wave of measurement possibilities all focused on the key precipitation parameter. In response to this shift to measurement programs and also integral to the ESE's new strategy for processing and management of its data, a measurement based approach is also critical for data processing system that support measurement programs like GPM. This paper provides an overview of the paradigm shift from mission to measurement. It also presents a summary of the ESE's new strategy for its data systems. Building on this background the paper details the architectural, design and implementation aspects of the Precipitation Processing System (PPS). The PPS is an evolution of a single point system developed for the Tropical Rainfall Measurement Mission to a generic precipitation data system. The paper provides the context within which PPS will support the GPM program. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Stocker, EF (reprint author), NASA, Goddard Space Flight Ctr, Code 902, Greenbelt, MD 20771 USA. NR 4 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5117-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5234 BP 132 EP 143 DI 10.1117/12.521320 PG 12 WC Engineering, Aerospace; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Remote Sensing; Imaging Science & Photographic Technology GA BY70A UT WOS:000189442100015 ER PT S AU Bolton, JF AF Bolton, JF BE Meynart, R Neeck, SP Shimoda, H Lurie, JB Aten, M TI Full spectral imaging: a revisited approach to remote sensing SO SENSORS, SYSTEMS AND NEXT-GENERATION SATELLITES VII SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Sensors, Systems and Next-Generation Satellites VII CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE, Soc Espanola Ott, NASA, European Opt Soc DE remote sensing; hyperspectral imaging; data processing; data compression; information theory; calibration; characterization ID VICARIOUS CALIBRATION; INFORMATION-CONTENT; IMAGERY; COMPRESSION; SENSORS AB Current optical remote sensing instrument technology allows the acquisition and digitization of all of the reflected energy (light) across the full spectral range of interest. The current method for acquiring, transmitting, and processing this data is still based on the "multi-band" approach that has been used for the past thirty years. This approach was required due to limitations imposed by early instrument technology. This paper will present generalized concepts for acquiring, pre-processing, transmitting, and extracting information from full-spectral, remotely sensed data. The goal of the paper is to propose methods for changing from the current "bytes-per-band" approach to the "spectral curve" approach. The paper will describe how the Full Spectral Imaging (FSI) approach has the potential to greatly simplify instrument characterization and calibration and to significantly reduce data transmission and storage requirements. I will suggest how these improvements may be accomplished with no loss of remotely sensed information. C1 NASA, Goddard Space Flight Ctr, EOS Program Off, Greenbelt, MD 20771 USA. RP Bolton, JF (reprint author), NASA, Goddard Space Flight Ctr, EOS Program Off, Code 420, Greenbelt, MD 20771 USA. EM john.f.bolton@nasa.gov NR 23 TC 1 Z9 1 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5117-7 J9 PROC SPIE PY 2004 VL 5234 BP 243 EP 251 DI 10.1117/12.510485 PG 9 WC Engineering, Aerospace; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Remote Sensing; Imaging Science & Photographic Technology GA BY70A UT WOS:000189442100025 ER PT S AU Gunapala, SD Bandara, SV Liu, JK Rafol, SB Mumolo, JM AF Gunapala, SD Bandara, SV Liu, JK Rafol, SB Mumolo, JM BE Meynart, R Neeck, SP Shimoda, H Lurie, JB Aten, M TI Large format long-wavelength infrared narrow-band, multi-band, and broad-band QWIP focal plane arrays SO SENSORS, SYSTEMS AND NEXT-GENERATION SATELLITES VII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems and Next-Generation Satellites VII CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE, Soc Espanola Ott, NASA, European Opt Soc DE infrared; long-wavelength infrared; mid-wavelength infrared; narrow-band infrared; multi-band infrared; broad-band infrared; infrared imaging camera; focal plane array; quantum well infrared photodetectors ID PHOTODETECTOR; CAMERA; PERFORMANCE AB A 640x512 pixel, long-wavelength cutoff, narrow-band (Deltalambda/lambdasimilar to10%) quantum well infrared photodetector (QWIP) focal plane array (FPA), a four-band QWIP FPA in 4-16 mum spectral region, and a broad-band (Deltalambda/lambdasimilar to42%) QWIP FPA having 15.4 mum cutoff have been demonstrated. In this paper we discuss the detector designs, dark currents, quantum efficiencies, responsivities, detectivities, noise equivalent differential temperatures (NEDTs), the effect of FPA nomuniformity on performance, and the operabilities of these QWIP FPAs. In addition, we discuss the development of a very sensitive (NEDTsimilar to10.6 mK) 640x512 pixel thermal imaging camera having 9 mum cutoff. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gunapala, SD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 23 TC 2 Z9 2 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5117-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5234 BP 272 EP 286 DI 10.1117/12.504900 PG 15 WC Engineering, Aerospace; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Remote Sensing; Imaging Science & Photographic Technology GA BY70A UT WOS:000189442100028 ER PT S AU Xiong, X Chiang, K Sun, J Che, N Barnes, W AF Xiong, X Chiang, K Sun, J Che, N Barnes, W BE Meynart, R Neeck, SP Shimoda, H Lurie, JB Aten, M TI Aqua MODIS first year on-orbit calibration and performance SO SENSORS, SYSTEMS AND NEXT-GENERATION SATELLITES VII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems and Next-Generation Satellites VII CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE, Soc Espanola Ott, NASA, European Opt Soc DE Aqua; MODIS; solar diffuser; SRCA; blackbody; calibration; radiometry ID WATER AB The MODerate Resolution Imaging Spectroradiometer (MODIS) Flight Model 1 (FM1) was launched on May 4, 2002 onboard the NASA Earth Observing System (EOS) Aqua spacecraft. It has provided more than a year of global data for studies of the Earth's land, oceans, and atmosphere in support of the science community and public users. To assure the quality of the data and science products, extensive efforts have been made to collect and analyze data on the instrument's on-orbit performance using its on-board calibrators (OBCs). MODIS has 36 spectral bands: 20 reflective solar bands (RSBs) with wavelengths from 0.41 micrometer to 2.2 micrometers and 16 thermal emissive bands (TEBs) from 3.7 to 14.2 micrometers. For radiometry, the RSBs are calibrated by a solar diffuser (SD) and a solar diffuser stability monitor (SDSM) system and the TEBs by a blackbody (BB). An on-board Spectroradiometric Calibration Assembly (SRCA) is used for the instrument's spectral (RSBs only) and spatial (all 36 bands) characterization. Using the first year's calibration data sets, this paper presents Aqua MODIS on-orbit performance in three areas: radiometric, spatial, and spectral. Comparisons with the sensor's specifications and with the performance of its predecessor, Terra MODIS (launched in December 1999), are discussed. Excluding a few problems identified pre-launch, such as nonfunctional detectors in the 1.6 micrometers band and the out of specification performance for the band to band registration (BBR), the on-orbit observations and analyses show that Aqua MODIS has been performing according to its design characteristics. C1 NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. RP Xiong, X (reprint author), NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. RI Xiong, Xiaoxiong (Jack)/J-9869-2012 NR 14 TC 8 Z9 8 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5117-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5234 BP 391 EP 399 DI 10.1117/12.510580 PG 9 WC Engineering, Aerospace; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Remote Sensing; Imaging Science & Photographic Technology GA BY70A UT WOS:000189442100040 ER PT S AU Smith, GL Szewczyk, ZP Mlynczak, PE Lee, RB Wielicki, BA Priestley, KJ Harries, J DeWitt, S Clerbaux, N AF Smith, GL Szewczyk, ZP Mlynczak, PE Lee, RB Wielicki, BA Priestley, KJ Harries, J DeWitt, S Clerbaux, N BE Meynart, R Neeck, SP Shimoda, H Lurie, JB Aten, M TI Method for comparison of GERB and CERES radiances SO SENSORS, SYSTEMS AND NEXT-GENERATION SATELLITES VII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems and Next-Generation Satellites VII CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE, Soc Espanola Ott, NASA, European Opt Soc DE GERB; CERES; earth radiation budget; calibration; validation ID CALIBRATION; INSTRUMENT; MOON AB The Geostationary Earth Radiation Budget (GERB) instrument aboard the Meteosat Second Generation Satellite has 256 channels which measure total radiance and 256 channels which measure solar radiation reflected from the Earth. In order to validate the calibration of these channels, the Clouds and Earth Radiant Energy System (CERES) instrument aboard the Terra spacecraft is operated in such a way as to view Earth scenes from the same direction as the GERB, so as to measure the same total and reflected solar radiances. The method uses the capability to program the azimuth of the CERES scan plane, such that the scan plane includes the GERB. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Smith, GL (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 16 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5117-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5234 BP 423 EP 432 DI 10.1117/12.513464 PG 10 WC Engineering, Aerospace; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Remote Sensing; Imaging Science & Photographic Technology GA BY70A UT WOS:000189442100043 ER PT S AU Lee, RB Smith, GL Bush, KA Paden, J Pandey, DK Wilson, RS Priestley, KJ AF Lee, RB Smith, GL Bush, KA Paden, J Pandey, DK Wilson, RS Priestley, KJ BE Meynart, R Neeck, SP Shimoda, H Lurie, JB Aten, M TI On-orbit calibrations of the ERBE active-cavity radiometers on the Earth Radiation Budget Satellite (ERBS): 1984-2002 SO SENSORS, SYSTEMS AND NEXT-GENERATION SATELLITES VII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems and Next-Generation Satellites VII CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE, Soc Espanola Ott, NASA, European Opt Soc DE active-cavity radiometer; ERBS; ERBE; earth irradiances; total solar irradiance ID ENERGY SYSTEM CERES; INSTRUMENTS; VARIABILITY; CLOUDS AB From October 1984 until September 30, 1999, on-orbit, the Earth Radiation Budget Satellite (ERBS)/Earth Radiation Budget Experiment (ERBE) nonscanning, active cavity radiometers (ACR) were calibrated using observations of the incoming total solar irradiance, and of reference irradiances from an on-board tungsten lamp and blackbodies in order to determine drifts and shifts in the ACR responses. On October 7, 1999, the ERBE elevation drive system failed near the earth nadir viewing configuration. Thereafter, the elevation failure prevented observations of the on-board, built-in calibration systems. On July 23, August 8, and December 10, 2002, the ERBS was pitched 180 degrees to observe cold space, representative of a 3 Kelvin blackbody, in order to determine the ACR's zero-irradiance offsets. On December 4, 2002, the ERBS was pitched 180 degrees away from the earth in order to observe the sun, and to determine the ACR's gains. In this paper, the 2002, 180-degree pitch calibrations are compared with the earlier 1984-1999, calibrations which were obtained using the on-orbit, built-in calibration systems. In addition, the 2002 calibrations are compared with earlier scheduled November 21, 1984, and October 20, 1985, 180-degree pitch calibrations, as well as with deep space calibrations from unscheduled July 2, 1987, January 16, 1999, and November 16, 2000, ERBS spacecraft tumbles. The 2002 ACR offsets were found to be consistent with 1984-2000 offsets at the 1.0 Wm(-2). 1984-1999, ERBE top-of-the-atmosphere (TOA), and satellite altitude (SA) earth irradiances are presented. Analyses of the TOA ERBE earth irradiances indicate that the TOA irradiance time series exhibited a 1.7 Wm(-2) increase as a result of 1988-1992, and 1998-2002 satellite altitudinal decreases during periods of maximum solar magnetic activity. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Lee, RB (reprint author), NASA, Langley Res Ctr, MS 420, Hampton, VA 23681 USA. NR 19 TC 0 Z9 0 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5117-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5234 BP 433 EP 444 DI 10.1117/12.511181 PG 12 WC Engineering, Aerospace; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Remote Sensing; Imaging Science & Photographic Technology GA BY70A UT WOS:000189442100044 ER PT S AU Xiong, X Sun, J Xiong, S Barnes, WL AF Xiong, X Sun, J Xiong, S Barnes, WL BE Meynart, R Neeck, SP Shimoda, H Lurie, JB Aten, M TI Using the moon for MODIS on-orbit spatial characterization SO SENSORS, SYSTEMS AND NEXT-GENERATION SATELLITES VII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems and Next-Generation Satellites VII CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE, Soc Espanola Ott, NASA, European Opt Soc DE MODIS; moon; spatial characterization; BBR; terra; aqua AB The moon is a very stable reference source that has been used for the space-borne sensors' radiometric calibration and/or radiometric stability monitoring. In this paper, we present an approach that uses the sensors' on-orbit lunar observations for their spatial characterization and apply the method to the MODIS instruments that are currently operating onboard NASA EOS Terra and Aqua satellites. Both MODIS instruments perform monthly lunar observations. The spatial characterization results derived from the lunar observations using this algorithm are compared with those obtained from the MODIS Spectro-Radiometric Calibration Assembly (SRCA), which is an on-board calibrator capable of performing spatial characterizations for all MODIS spectral bands. The new approach can be applied to other remote sensing instruments. C1 NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. RP Xiong, X (reprint author), NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. RI Xiong, Xiaoxiong (Jack)/J-9869-2012 NR 15 TC 6 Z9 6 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5117-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5234 BP 480 EP 487 DI 10.1117/12.510570 PG 8 WC Engineering, Aerospace; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Remote Sensing; Imaging Science & Photographic Technology GA BY70A UT WOS:000189442100048 ER PT S AU Xiong, X Chiang, K Adimi, F Li, W Yatagai, H Barnes, W AF Xiong, X Chiang, K Adimi, F Li, W Yatagai, H Barnes, W BE Meynart, R Neeck, SP Shimoda, H Lurie, JB Aten, M TI MODIS correction algorithm for out-of-band response in the short-wave IR bands SO SENSORS, SYSTEMS AND NEXT-GENERATION SATELLITES VII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems and Next-Generation Satellites VII CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE, Soc Espanola Ott, NASA, European Opt Soc DE Terra; MODIS; SWIR; short wave infrared bands; out-of-band; calibration; correction; blackbody ID IMAGING SPECTRORADIOMETER MODIS AB The MODerate Resolution Imaging Spectroradiometer (MODIS) has 36 spectral bands with wavelengths from 0.41 to 14.2 micrometers. The 36 spectral bands, a total of 490 detectors, are distributed on four focal plane assemblies (FPAs): visible (VIS), near infrared (NIR), short- and mid-wave infrared (SMIR), and long-wave infrared (LWIR). Nearly identical copies of MODIS are currently operating onboard the NASA EOS Terra spacecraft (launched on December 18, 1999) and Aqua spacecraft (launched on May 4, 2002), providing complementing global observations for the studies of the Earth system. Pre-launch and on-orbit characterizations of both Terra and Aqua MODIS instruments have shown small but non-negligible out-of-band (OOB) response in the sensors' short-wave infrared bands (SWIR: Bands 5-7 and 26). To minimize the impact due to OOB response on the MODIS SWIR bands calibration and the Earth scene retrieval, a correction algorithm has been developed and implemented in the Level 1B (LIB) software for both Terra and Aqua MODIS. In this paper, we describe this algorithm and its applications to the MODIS calibration. We will illustrate how the correction coefficients are derived from on-orbit observations and discuss the test procedures involved before algorithm implementation in the LIB code. Actual performance of this algorithm will be evaluated and compared for both Terra and Aqua MODIS. C1 NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. RP Xiong, X (reprint author), NASA, Goddard Space Flight Ctr, Terr Phys Lab, Code 661, Greenbelt, MD 20771 USA. RI Xiong, Xiaoxiong (Jack)/J-9869-2012 NR 12 TC 12 Z9 12 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5117-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5234 BP 605 EP 613 DI 10.1117/12.510261 PG 9 WC Engineering, Aerospace; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Remote Sensing; Imaging Science & Photographic Technology GA BY70A UT WOS:000189442100061 ER PT S AU Bielski, CM AF Bielski, CM BE Meynart, R Neeck, SP Shimoda, H Lurie, JB Aten, M TI Teaching virtually: Going beyond the static web page text with virtual experiences SO SENSORS, SYSTEMS AND NEXT-GENERATION SATELLITES VII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems and Next-Generation Satellites VII CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE, Soc Espanola Ott, NASA, European Opt Soc DE distance learning; virtual classroom; optical remote sensing AB Computer based teaching has become common place as the demand for specialists continues to increase in view of continuously evolving remote sensing technologies. Moreover, content accessibility via the internet makes anytime, anywhere teaching possible while reaching a larger audience. The majority of computer based courses however, continue to use the static text model and present the student mainly with the same material found in a textbook. Student computer based learning experiences could be much more rewarding if the curriculum included more interaction and practice. It is with these goals in mind that the development of a virtual experiment and game were devised. Herschel's experiment was the first to show the existence of infrared (IR) light. Ibis virtual experiment requires the student to set up the experiment and record data in order to prove the existence of IR light. The 'Field Experiment' game requires the student to plan and execute a field collection campaign with the use of a field spectrometer. These 'beyond the book' experiences hopefully encourage and stimulate students in the subject at hand as well as provide more 'practical' experience that is not available through viewing static text and graphics. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bielski, CM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 171-B1, Pasadena, CA 91109 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5117-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5234 BP 731 EP 737 DI 10.1117/12.512080 PG 7 WC Engineering, Aerospace; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Remote Sensing; Imaging Science & Photographic Technology GA BY70A UT WOS:000189442100075 ER PT S AU Habib, S Abu Nokra, N AF Habib, S Abu Nokra, N BE Meynart, R Neeck, SP Shimoda, H Lurie, JB Aten, M TI Transferring knowledge from observations and models to decision makers - An overview and challenges SO SENSORS, SYSTEMS AND NEXT-GENERATION SATELLITES VII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems and Next-Generation Satellites VII CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE, Soc Espanola Ott, NASA, European Opt Soc AB Over the last 25 years a tremendous progress has been made in the Earth science space-based remote sensing observations, technologies and algorithms. Such advancements have improved the predictability by providing lead-time and accuracy of forecast in weather, climate, natural hazards, and natural resources. It has further reduced or bounded the overall uncertainties by partially improving our understanding of planet Earth as an integrated system that is governed by non-linear and chaotic behavior. Many countries such as the US, European Community, Japan, China and others have invested billions of dollars in developing and launching space-based assets in the low earth (LEO) and geostationary (GEO) orbits. However, the wealth of this scientific knowledge that has potential of extracting monumental socio-economic benefits from such large investments have been slow in reaching the public and decision makers. For instance, there are a number of areas such as energy forecasting, aviation safety, agricultural competitiveness, disaster management, homeland security, air quality and public health, which can directly take advantage. Nevertheless, we all live in a global economy that depends on access to the best available Earth Science information for all inhabitants of this planet. This paper surveys and examines a number such applications in terms of their architecture, maturity and economic applicability as they apply to the societal needs. A detailed analysis is also presented of various challenges and issues that pertain to a number of areas such as: (1) difficulties in making a speedy transition of data and information from observations and models to relevant Decision Support Systems (DSS) or tools, (2) data and models inter-operability issues, (3) limitations of spatial, spectral and temporal resolution, (4) communication limitations as dictated by the availability of image processing and data compression techniques. Additionally, the most critical element amongst all is the organizational and management boundaries that must be resolved at local, state, national and international levels to implement and realize free flow of such vital information. This paper also makes attempts to address this topic and discusses possible approaches to deal with this quandary. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Habib, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 4 TC 1 Z9 1 U1 0 U2 4 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5117-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5234 BP 738 EP 743 DI 10.1117/12.513892 PG 6 WC Engineering, Aerospace; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Remote Sensing; Imaging Science & Photographic Technology GA BY70A UT WOS:000189442100076 ER PT S AU Toll, D Arsenault, K Houser, P Entin, J Cosgrove, B Peters-Lidard, C Rodell, M AF Toll, D Arsenault, K Houser, P Entin, J Cosgrove, B Peters-Lidard, C Rodell, M BE Meynart, R Neeck, SP Shimoda, H Lurie, JB Aten, M TI Terrestrial water and energy systems for water resource applications SO SENSORS, SYSTEMS AND NEXT-GENERATION SATELLITES VII SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Sensors, Systems and Next-Generation Satellites VII CY SEP 08-10, 2003 CL Barcelona, SPAIN SP SPIE, Soc Espanola Ott, NASA, European Opt Soc DE water resources applications; data assimilation; weather and climate predictions ID LAND; CLIMATE; MODELS; PRECIPITATION; TRANSPIRATION AB NASA/GSFC has developed with other groups a Land Data Assimilation System (LDAS) to output water and energy budgets for the primary purpose of improving weather and climate prediction. However, LDAS water and energy cycle outputs also may be coupled with other information to help with a wide range of water resources applications. For example, LDAS results may be used for water availability and quality, agricultural management and forecasting, assessment and prediction of snowmelt runoff, and flood and drought impact and prediction. Specifically, LDAS uses various satellites and ground based observations within a land surface modeling and data assimilation framework to produce optimal output fields of terrestrial energy, water and carbon fluxes. Current land surface outputs are gridded at 1/4degrees resolution globally and 1/8degrees for North America with work in progress to convert to a I-km global grid. Integrated modeling, observations and data assimilation at various spatial and temporal scales helps LDAS to quantify terrestrial water, energy and biogeochemical processes. LDAS applications described in this paper are aimed at improving weather and seasonal forecasts. In addition, we also summarize the use of LDAS data to assist critical needs specified by the U.S. Bureau of Reclamation water resources management for selected basins in the western U.S. C1 NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP Toll, D (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. EM David.L.Toll@nasa.gov RI Rodell, Matthew/E-4946-2012; Houser, Paul/J-9515-2013; Peters-Lidard, Christa/E-1429-2012 OI Rodell, Matthew/0000-0003-0106-7437; Houser, Paul/0000-0002-2991-0441; Peters-Lidard, Christa/0000-0003-1255-2876 NR 22 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5117-7 J9 PROC SPIE PY 2004 VL 5234 BP 744 EP 753 DI 10.1117/12.514325 PG 10 WC Engineering, Aerospace; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Remote Sensing; Imaging Science & Photographic Technology GA BY70A UT WOS:000189442100077 ER PT S AU Neeck, SP Paules, GE Ramesh, JDM AF Neeck, SP Paules, GE Ramesh, JDM BE Meynart, R Neeck, SP Shimoda, H TI NASA's future Earth observation plans SO SENSORS, SYSTEMS, AND NEXT-GENERATION SATELLITES VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems, and Next-Generation Satellites VIII CY SEP 13-15, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, Natl Aeronaut & Space Adm, European Opt Soc AB NASA's Science Mission Directorate, working with its domestic and international partners, provides accurate, objective scientific data and analysis to advance our understanding of Earth system processes. Learning more about these processes will enable improved prediction capability for climate, weather, and natural hazards. Earth interactions occur on a continuum of spatial and temporal scales ranging from short-term weather to long-term climate, and from local and regional to global. Quantitatively describing these changes means precisely measuring from space scores of biological and geophysical parameters globally. New missions that SMD will launch in the coming decade will complement the first series of the Earth Observing System. These next generation systematic measurement missions are being planned to extend or enhance the record of science-quality data necessary for understanding and predicting global change. These missions include the NPOESS Preparatory Project, Ocean Surface Topography Mission, Global Precipitation Measurement, Landsat Data Continuity Mission, and an aerosol polarimetry mission called Glory. New small explorer missions will make first of a kind Earth observations. The Orbiting Carbon Observatory will measure sources and sinks of carbon to help the Nation and the world formulate effective strategies to constrain the amount of this greenhouse gas in the atmosphere. Aquarius will measure ocean surface salinity which is key to ocean circulation in the North Atlantic that produces the current era's mild climate in northern Europe. HYDROS will measure soil moisture globally. Soil moisture is critical to agriculture and to managing fresh water resources. NASA continues to design, develop and launch the Nation's civilian operational environmental satellites, in both polar and geostationary orbits, by agreement with the National Oceanic and Atmospheric Administration (NOAA). NASA plans to develop an advanced atmospheric sounder, GIFTS, for geostationary orbit to facilitate continuous measurements of weather-related phenomena, improve "nowcasting" of extreme weather events, and measure important atmospheric gases. NASA is currently developing with its partners the National Polar-orbiting Operational Environmental Satellite System (NPOESS) and the next-generation geostationary system, GOES-R. Future missions will migrate today's capabilities in low Earth orbit to higher orbits such as L1 and L2 to enable more continuous monitoring of changes in the Earth system with a smaller number of satellites. C1 NASA Headquarters, Sci Miss Directorate, Washington, DC 20546 USA. RP Neeck, SP (reprint author), NASA Headquarters, Sci Miss Directorate, Washington, DC 20546 USA. NR 11 TC 0 Z9 0 U1 0 U2 4 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5517-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5570 BP 145 EP 154 DI 10.1117/12.573033 PG 10 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BBI79 UT WOS:000225676100015 ER PT S AU Krimchansky, A Machi, D Cauffman, SA Davis, MA AF Krimchansky, A Machi, D Cauffman, SA Davis, MA BE Meynart, R Neeck, SP Shimoda, H TI Next generation geostationary operational environmental satellite (GOES-R series): A space segment overview SO SENSORS, SYSTEMS, AND NEXT-GENERATION SATELLITES VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems, and Next-Generation Satellites VIII CY SEP 13-15, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, Natl Aeronaut & Space Adm, European Opt Soc DE GOES-R; ABI; HES; GLM; SIS; SEISS AB The next-generation National Oceanic and Atmospheric Administration (NOAA) Geostationary Operational Environmental Satellite (GOES-R series) is currently being developed by NOAA in partnership with the National Aeronautics and Space Administration (NASA). The GOES-R series satellites represents a significant improvement in spatial, temporal, and spectral observations (several orders of magnitude) over the capabilities of the currently operational GOES-I/M series and GOES-N series satellite to be launched at the end of 2004. The GOES-R series will incorporate technically advanced "third-generation" instruments and spacecraft enhancements to meet evolving observational requirements of forecasting for the era 2012-2025. The GOES-R instrument complement being developed includes an Advanced Baseline Imager (ABI), a Hyperspectral Environmental Suite (HES), a GEO Lightning Mapper (GLM), a Solar Imaging Suite (SIS) and a Space Environment In-Situ Suite (SEISS). Also, candidates for a number of GOES-R Pre-Planned Product Improvements (P(3)Is) includes a Geo Microwave Sounder, a Coronagraph, a Hyperspectral Imager, and a Solar Irradiance Sensor. Currently, the GOES-R space segment architecture is being evaluated as part of a GOES-R system End-to-End Architecture Study. The GOES-R notional baseline architecture is a constellation of two satellites (A-sat and B-sat) each nominally located at 75 degrees West longitude and at 135 degrees West longitude at geostationary altitude, 0 degrees inclination. The primary mission of the A-sat is to provide imaging from the ABI. The A-sat will also contain the SIS and the GLM. The primary mission of the B-sat is to provide sounding of the hemispherical disk of the earth from the HES. The B-sat also contains the SEISS. Both satellites have mesoscale capabilities for severe weather sounding or imaging. This paper overviews the GOES-R Space Segment development including satellite constellation trade-off, improvements and differences between the current and future instrument and spacecraft capabilities, and technology infusion. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Krimchansky, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 0 TC 1 Z9 1 U1 2 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5517-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5570 BP 155 EP 164 DI 10.1117/12.565281 PG 10 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BBI79 UT WOS:000225676100016 ER PT S AU Lebair, W Kronenwetter, J Cauffman, SA Davis, MA AF Lebair, W Kronenwetter, J Cauffman, SA Davis, MA BE Meynart, R Neeck, SP Shimoda, H TI The advanced baseline imager: The next generation of geostationary imager SO SENSORS, SYSTEMS, AND NEXT-GENERATION SATELLITES VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems, and Next-Generation Satellites VIII CY SEP 13-15, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, Natl Aeronaut & Space Adm, European Opt Soc DE ABI; GOES-R; radiometer; imager; operational AB The Geostationary Operational Environmental Satellite R (GOES-R) Series is the planned next generation of operational weather satellites for the United State's National Oceanic and Atmospheric Administration (NOAA). The first launch of the GOES-R series is planned for 2012. The GOES-R Series satellites and instruments are being developed by the National Aeronautics and Space Administration (NASA). One of the key instruments on the GOES-R Series is the Advanced Baseline Imager (ABI). The ABI is a multi-channel, visible through infrared, passive imaging radiometer. The ABI will provide moderate spatial and spectral resolution at high temporal and radiometric resolution to accurately monitor rapidly changing weather. The ABI will provide sixteen spectral channels compared to five channels on the current GOES I/P Series Imager. This increase will allow more comprehensive monitoring of atmospheric conditions such as aerosol concentration, cirrus cloud location, and cloud properties. In addition, ABI will provide data products with a spatial resolution of at least half the current imager, down to 0.5 Km in the visible band. With its high temporal coverage, full disk every 5 minutes, and ability to continue operations around local midnight, ABI will provide continuous and timely monitoring of weather. This is further augmented by ABI's ability to revisit a specified 1000 Kilometer region every 30 seconds to track severe weather. This paper discusses the anticipated performance characteristics of the ABI sensor. The key data products achievable from the ABI are also discussed. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lebair, W (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5517-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5570 BP 165 EP 172 DI 10.1117/12.565581 PG 8 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BBI79 UT WOS:000225676100017 ER PT S AU Martin, G Criscione, J Cauffman, SA Davis, MA AF Martin, G Criscione, J Cauffman, SA Davis, MA BE Meynart, R Neeck, SP Shimoda, H TI Geostationary operational envirommental satellites (GOES) - R series hyperspectral environmental suite (HES) overview SO SENSORS, SYSTEMS, AND NEXT-GENERATION SATELLITES VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems, and Next-Generation Satellites VIII CY SEP 13-15, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, Natl Aeronaut & Space Adm, European Opt Soc DE GOES-R; infrared; hyperspectral; geostationary; sounding; instrument AB The Hyperspectral Environmental Suite (HES) instrument is currently under development by the NASA GOES-R Project team within the framework of the GOES Program to fulfill the future needs and requirements of the National Environmental Satellite, Data, and Information Service (NESDIS) Office. As part of the GOES-R instrument complement, HES will provide measurements of the traditional temperature and water vapor vertical profiles with higher accuracy and vertical resolution than obtained through current sounder technologies. HES will provide measurements of the properties of the shelf and coastal waters and back up imaging (at in-situ resolution) for the GOES-R Advanced Baseline Imager (ABI). The HES team is forging the future of remote environmental monitoring with the development of an operational instrument with high temporal, spatial and spectral-resolution and broad hemispheric coverage. The HES development vision includes threshold and goal requirements that encompass potential system solutions. The HES team has defined tasks for the instrument(s) that include a threshold functional complement of Disk Sounding (DS), Severe Weather/Mesoscale Sounding (SW/M), and Shelf and Coastal Waters imaging (CW) and a goal functional complement of Open Ocean (OO) imaging, and back up imaging (at in-situ resolution) for the GOES-R Advanced Baseline Imager (ABI). To achieve the best-value procurement, the GOES-R Project has base-lined a two-phase procurement approach to the HES design and development; a Formulation/study phase and an instrument Implementation phase. During Formulation, currently slated for the FY04-05 timeframe, the developing team(s) will perform Systems Requirements Analysis and evaluation, System Trade and Requirements Baseline Studies, Risk Assessment and Mitigation Strategy and complete a Preliminary Conceptual Design of the HES instrument. The results of the formulation phase will be leveraged to achieve an effective and efficient system solution during the Implementation Phase scheduled to begin FY05 for a resultant FY12 launch. The magnitude of complexity of the HES development requires an appreciation of the technologies required to achieve the functional objectives. To this end, the GOES-R project team is making available all NASA developed technologies to potential HES vendors, including, the NASA New Millennium Program's (NMP) Earth Observing-3, Geostationary Imaging Fourier Transform Spectrometer (GIFTS) instrument developed technologies, as applicable. It is anticipated that the instrument(s) meeting the HES requirements will be either a dispersive spectrometer or an interferometric spectrometer or perhaps a combination. No instrument configuration is preferred or favored by the Government. This paper outlines the HES development plan; including an overview of current requirements, existing partnerships and the GOES-R project methodologies to achieve the advanced functional objectives of the GOES Program partnership. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Martin, G (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5517-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5570 BP 173 EP 182 DI 10.1117/12.565834 PG 10 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BBI79 UT WOS:000225676100018 ER PT S AU Krimchansky, S Susskind, J Krimchansky, A Chu, D Lambeck, R Davis, M AF Krimchansky, S Susskind, J Krimchansky, A Chu, D Lambeck, R Davis, M BE Meynart, R Neeck, SP Shimoda, H TI GEO sounding using microwave instruments SO SENSORS, SYSTEMS, AND NEXT-GENERATION SATELLITES VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems, and Next-Generation Satellites VIII CY SEP 13-15, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, Natl Aeronaut & Space Adm, European Opt Soc DE geostationary microwave sounding; infrared sounding; GOES; POES; aqua; AMSU-A; ATMS; AIRS AB There are several microwave instruments in low Earth orbit (LEO) that are used for atmospheric temperature and humidity sounding by themselves and in conjunction with companion IR sounders. These instruments have achieved a certain degree of maturity and are undergoing a redesign to minimize their size, mass, and power requirements from the previous generation instruments. An example of these instruments is the AMSU-A series, now flying on POES and Aqua spacecraft, with the IR sounders HIRS3 and AIRS respectively. These older microwave instruments are going to be replaced by the ATMS instruments that will fly on NPP and NPOESS satellites with the CrIS IR sounder. A number of enabling technologies acquired from the ATMS instrument hardware design and data processing are directly applicable to performing similar microwave sounding on a geostationary platform. Because these technologies are already in place, they are readily available for the development of a geostationary orbit (GEO) microwave instrument, thereby avoiding costly technology development and minimizing the risk of not achieving the scientific requirements. In fact, the MMIC microwave components that were developed by ATMS for size and volume reduction are directly applicable to a GEO microwave sounder. The benefits of microwave sounders are well known. They penetrate non-precipitating cloud cover and allow for accurate soundings obtained with a collocated high spectral resolution IR sounder in up to 80% cloud cover. The key advantages of a microwave instrument in GEO will be its ability to provide high temporal resolution and uniform spatial resolution, and it will expand the utility of a collocated advanced IR sounder to cases in which partial cloud cover exists. A footprint in the order of 100 km by 100 km resolution with hemispherical coverage within one hour can be easily achieved for sounding channels in the 50 to 57 GHz range. A GEO microwave sounder will also allow mesoscale sampling of select regions. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Krimchansky, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 2 TC 0 Z9 0 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5517-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5570 BP 183 EP 191 DI 10.1117/12.565283 PG 9 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BBI79 UT WOS:000225676100019 ER PT S AU Neeck, SP Kakar, RK Durning, JF Smith, EA AF Neeck, SP Kakar, RK Durning, JF Smith, EA BE Meynart, R Neeck, SP Shimoda, H TI Global Precipitation Measurement (GPM) status SO SENSORS, SYSTEMS, AND NEXT-GENERATION SATELLITES VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems, and Next-Generation Satellites VIII CY SEP 13-15, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, Natl Aeronaut & Space Adm, European Opt Soc AB Global Precipitation Measurement (GPM) is a global space endeavor conceived by the US and Japan that has sparked global interest. Building upon the success of the Tropical Rainfall Measuring Mission (TRMM), it will initiate the measurement of global precipitation, a key climate factor. Its science objectives are to improve ongoing efforts to predict climate by providing near-global measurement of precipitation, its distribution, and physical processes; to improve the accuracy of weather and precipitation forecasts through more accurate measurement of rain rates and latent heating; and to provide more frequent and complete sampling of the Earth's precipitation. It has received endorsements from the World Climate Research Programme, the World Meteorological Organization, and the Committee on Earth Observation Satellites. GPM is envisioned to consist of a core spacecraft to measure precipitation structure and to provide a calibration standard for the constellation spacecraft, an international constellation of spacecraft to provide frequent precipitation measurements on a global basis, calibration/validation sites distributed globally with a broad array of precipitation-measuring instrumentation, and a global precipitation data system to produce and distribute global rain maps and climate research products. The National Aeronautics and Space Administration (NASA) plans to provide the core spacecraft, a constellation spacecraft and its launch, microwave radiometers, the precipitation processing system, the mission operations system, and an array of ground calibration and validation sites. The Japan Aerospace Exploration Agency (JAXA) plans to contribute the radar for and launch of the core spacecraft. The European Space Agency (ESA) has studied a European constellation satellite contribution. India and France have expressed their interest in participating through the Megha-Tropiques project. South Korea has proposed the contribution of regional ground validation sites. Other nations are also expected to play major a role in GPM. GPM is now in formulation phase and is one of the highest priority new Earth science missions for which NASA seeks final approval. GPM launches are targeted to begin in 2010. C1 NASA Headquarters, Washington, DC 20546 USA. RP Neeck, SP (reprint author), NASA Headquarters, Washington, DC 20546 USA. NR 9 TC 0 Z9 0 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5517-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5570 BP 192 EP 201 DI 10.1117/12.564876 PG 10 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BBI79 UT WOS:000225676100020 ER PT S AU Aumann, HH Gregorich, D Gaiser, S Chahine, MT AF Aumann, HH Gregorich, D Gaiser, S Chahine, MT BE Meynart, R Neeck, SP Shimoda, H TI Application of Atmospheric InfraRed Sounder (AIRS) data to climate research SO SENSORS, SYSTEMS, AND NEXT-GENERATION SATELLITES VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems, and Next-Generation Satellites VIII CY SEP 13-15, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, Natl Aeronaut & Space Adm, European Opt Soc DE infrared; temperature retrieval; hyper spectral; remote sensing; climate ID SPECTRAL CALIBRATION; PRELAUNCH AB The application of hyper spectral radiometric data to climate research requires very high absolute radiometric accuracy and stability. We use cloud-free tropical ocean data from the Atmospheric InfraRed Sounder (AIRS) Calibration Data Subset (ADCS) to show that the radiometric precision and stability required for climate applications has been achieved. The sea surface skin temperatures derived from the AIRS 2616cm-1 super window channel are stable relative to the RTG.SST at the better than 8 mK/year level, and the spectral calibration is stable at the 1 ppm/year level. The excellent stability and accuracy are the result of the implementation of AIRS as a grating array spectrometer, which is cooled and stabilized within 10 mK at 155 K. Analysis of daily measurements of the temperature gradient between the surface and 7 kin altitude show that the AIRS Calibration Data Subset has applications which extend its original intent for calibration support to climate research. The Atmospheric Infrared Sounder (AIRS) on the EOS Aqua satellite was launched into polar orbit in May 2002. AIRS covers the spectral region from 640 to 2700 cm-1 with 2378 independent channels and represents the first of a new generation of hyper spectral resolution sounders in support of global sounding data for weather forecasting and climate research. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91009 USA. RP Aumann, HH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91009 USA. NR 8 TC 7 Z9 7 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5517-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5570 BP 202 EP 208 DI 10.1117/12.565712 PG 7 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BBI79 UT WOS:000225676100021 ER PT S AU Xiong, X Barnes, W Chiang, K Erives, H Che, N Sun, J Isaacman, A Salomonson, V AF Xiong, X Barnes, W Chiang, K Erives, H Che, N Sun, J Isaacman, A Salomonson, V BE Meynart, R Neeck, SP Shimoda, H TI Status of aqua MODIS on-orbit calibration and characterization SO SENSORS, SYSTEMS, AND NEXT-GENERATION SATELLITES VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems, and Next-Generation Satellites VIII CY SEP 13-15, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, Natl Aeronaut & Space Adm, European Opt Soc DE aqua; Terra; MODIS; solar diffuser; SRCA; blackbody; calibration; radiometty; uncertainty ID SPATIAL CHARACTERISTICS; ASSEMBLY SRCA; WATER AB The MODIS Flight Model 1 (FM1) has been in operation for more than two years since its launch onboard the NASA's Earth Observing System (EOS) Aqua spacecraft on May 4, 2002. The MODIS has 36 spectral bands: 20 reflective solar bands (RSB) with center wavelengths from 0.41 to 2.2mum and 16 thermal emissive bands (TEB) from 3.7 to 14.5mum. It provides the science community observations (data products) of the Earth's land, oceans, and atmosphere for a board range of applications. Its primary on-orbit calibration and characterization activities are performed using a solar diffuser (SD) and a solar diffuser stability monitor (SDSM) system for the RSB and a blackbody for the TEB. Another on-board calibrator (OBC) known as the spectro-radiometric calibration assembly (SRCA) is used for the instrument's spatial (TEB and RSB) and spectral (RSB only) characterization. We present in this paper the status of Aqua MODIS calibration and characterization during its first two years of on-orbit operation. Discussions will be focused on the calibration activities executed on-orbit in order to maintain and enhance the instrument's performance and the quality of its Level 113 (LIB) data products. We also provide comparisons between Aqua MODIS and Terra MODIS (launched in December, 1999), including their similarity and difference in response trending and optics degradation. Existing data and results show that Aqua MODIS bands 8 (0.412mum) and 9 (0.443mum) have much smaller degradation than Terra MODIS bands 8 and 9. The most noticeable feature shown in the RSB trending is that the mirror side differences in Aqua MODIS are extremely small and stable (<0.1%) while the Terra MODIS RSB trending has shown significant mirror side difference and wavelength dependent degradation. The overall stability of the Aqua MODIS TEB is also better than that of the Terra MODIS during their first two years of on-orbit operation. C1 NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. RP Xiong, X (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA. RI Xiong, Xiaoxiong (Jack)/J-9869-2012 NR 19 TC 9 Z9 9 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5517-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5570 BP 317 EP 327 DI 10.1117/12.561940 PG 11 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BBI79 UT WOS:000225676100033 ER PT S AU Butler, JJ Meister, G Patt, FS Barnes, RA AF Butler, JJ Meister, G Patt, FS Barnes, RA BE Meynart, R Neeck, SP Shimoda, H TI Use of the Moon as a reference for satellite-based climate change measurements SO SENSORS, SYSTEMS, AND NEXT-GENERATION SATELLITES VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems, and Next-Generation Satellites VIII CY SEP 13-15, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, Natl Aeronaut & Space Adm, European Opt Soc DE Moon; on-orbit calibration; spacecraft ID ON-ORBIT CALIBRATION; RADIOMETRIC CALIBRATION; SPACECRAFT CALIBRATION; 350-2500 NM; IRRADIANCE; RADIANCE; TIME AB The United States Geologic Survey (USGS) has developed a lunar irradiance model for comparison with on-orbit satellite instruments. The comparisons are given as the percent difference of the satellite measurements from the model-generated lunar irradiances. For users of the USGS lunar model, details of the inner operation of the model are unknown. That operation is not examined here. Rather, we examine the outputs of the model. We treat the model-generated lunar irradiances as independent data sets, with each covering only a limited range of phase angles in the comparison with an individual satellite instrument. We correct the model irradiances to standard Sun-Moon and Moon-instrument distances and to fixed values for the phase and libration angles. These same corrections can be applied to the measurements by the comparison satellite instrument. For the model outputs examined here, the time trends in the corrected irradiances differ from zero change by less that 0.0014 % per thousand days, and the residual scatter in the results is 0.013 % (1sigma). There are no apparent oscillations in the time series. At this level, the lunar model should provide an adequate reference for instruments that measure long-term climate change. The model outputs here correspond to the bands from the Sea-viewing Wide Field-of-View Sensor (SeaWiFS) instrument and to the phase angle range for the SeaWiFS lunar measurements, which is from 5degrees to 10degrees, both before and after full phase. Similar results have been obtained for model outputs corresponding to lunar measurements from the Moderate Resolution Imaging Spectroradiometer (MODIS) instruments onboard the Terra and Aqua spacecraft. This technique is applicable to other instruments that measure at wavelengths from 400 nm to 2500 nm since, in addition to the relative spectral responses of the instrument's bands, the only requirements for the model are the time and location of the instrument's lunar measurements. C1 NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. RP Butler, JJ (reprint author), NASA, Goddard Space Flight Ctr, Terr Phys Lab, Code 924, Greenbelt, MD 20771 USA. RI Meister, Gerhard/F-7159-2012; Butler, James/D-4188-2013 NR 14 TC 3 Z9 3 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5517-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5570 BP 328 EP 341 DI 10.1117/12.565058 PG 14 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BBI79 UT WOS:000225676100034 ER PT S AU Lee, RB Wilson, RS AF Lee, RB Wilson, RS BE Meynart, R Neeck, SP Shimoda, H TI Validation of spacecraft active cavity radiometer total solar irradiance [TSI] long-term measurement trends using proxy TSI least squares analyses SO SENSORS, SYSTEMS, AND NEXT-GENERATION SATELLITES VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems, and Next-Generation Satellites VIII CY SEP 13-15, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, Natl Aeronaut & Space Adm, European Opt Soc DE total solar irradiance; active cavity; radiometry; calibration; climate; ERBE; ERBS ID MAGNETIC ACTIVITY; VARIABILITY; CALIBRATION; INSTRUMENT; CONSTANT; MODEL AB Long-term, incoming total solar irradiance (TSI) measurement trends were validated using proxy TSI values, derived from indices of solar magnetic activity. Spacecraft active cavity radiometers (ACR) are being used to measure longterm TSI variability, which may trigger global climate changes. The TSI, typically referred to as the "solar constant," was normalized to the mean earth-sun distance. Studies of spacecraft TSI data sets confirmed the existence of a 0.1 %, long-term TSI variability component within a 10-year period. The 0.1 % TSI variability component is clearly present in the spacecraft data sets from the 1984-2004 time frame. Typically, three overlapping spacecraft data sets were used to validate long-term TSI variability trends. However, during the years of 1978-1984, 1989-1991, and 1993-1996, three overlapping spacecraft data sets were not available in order to validate TSI trends. The TSI was found to vary with indices of solar magnetic activity associated with recent 10-year sunspot cycles. Proxy TSI values were derived from least squares analyses of the measured TSI variability with the solar indices of 10.7-cm solar fluxes, and with limb-darked sunspot fluxes. The resulting proxy TSI values were compared to the spacecraft ACR measurements of TSI variability to detect ACR instrument degradation, which may be interpreted as TSI variability. Analyses of ACR measurements and TSI proxies are presented primarily for the 1984-2004, Earth Radiation Budget Experiment (ERBE) ACR solar monitor data set. Differences in proxy and spacecraft measurement data sets suggest the existence of another TSI variability component with an amplitude greater than or equal to 0.5 Wm-2 (0.04%), and with a cycle of 20 years or more. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Lee, RB (reprint author), NASA, Langley Res Ctr, MS 420, Hampton, VA 23681 USA. NR 29 TC 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5517-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5570 BP 352 EP 362 DI 10.1117/12.565647 PG 11 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BBI79 UT WOS:000225676100036 ER PT S AU Dungan, J Morris, R AF Dungan, J Morris, R BE Meynart, R Neeck, SP Shimoda, H TI Specifying EO satellite campaign requests to meet science goals SO SENSORS, SYSTEMS, AND NEXT-GENERATION SATELLITES VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Sensors, Systems, and Next-Generation Satellites VIII CY SEP 13-15, 2004 CL Maspalomas, SPAIN SP SPIE, Soc Espanola Opt, Natl Aeronaut & Space Adm, European Opt Soc DE Earth Observation System; Earth science goals; remote sensing campaigns AB In the past decade, the number of Earth observation satellites has burgeoned. EO missions have been conceived to study different aspects and interacting pieces of the Earth system and scientists are designing increasingly complex, interdisciplinary campaigns to exploit multiple EO assets. In general, each EO mission has its own observation scheduling system, leading to a diverse array of specialized scheduling systems each tailored to a mission's unique requirements and characteristics. There is therefore the opportunity to allow planning and scheduling algorithms to assist a scientist requesting a set of observations, optimized over multiple sensors, to meet a science goal. This paper addresses the formal specification of a request to allow such algorithms to be exploited. The most basic parameters of a campaign request include the list of sensors required or desired in combination with the time frames or intervals and geographic regions for which the observation(s) are needed. Temporal and geographic parameters may be dependent on exogenous events, such as the occurrence of a fire, hurricane, volcanic eruption, or seasonal event. The scientist would also like to specify constraints on the needed quality of observations (e.g. cloud cover) and may have dependencies between parameters. Fulfilling preferences (e.g. new data are preferable to older data) may improve the quality of subsequent scientific analysis. The cost of the set of observations will also be an important constraint. In this paper, we propose a structure for expressing these parameters and constraints. We use a fire emissions model validation campaign as illustration. C1 NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA. RP Dungan, J (reprint author), NASA, Ames Res Ctr, Div Earth Sci, MS 242-4, Moffett Field, CA 94035 USA. OI /0000-0002-4863-1616 NR 15 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5517-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5570 BP 612 EP 618 DI 10.1117/12.570286 PG 7 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BBI79 UT WOS:000225676100062 ER PT B AU Denney, E Whittle, J AF Denney, E Whittle, J BE Arabnia, HR Reza, H TI Combining model-driven and schema-based program synthesis SO SERP'04: PROCEEDINGS OF THE INTERNATIONAL CONFERENCE ON SOFTWARE ENGINEERING RESEARCH AND PRACTICE, VOLS 1 AND 2 LA English DT Proceedings Paper CT International Conference on Software Engineering Research and Practice CY JUN 21-24, 2004 CL Las Vegas, NV SP Comp Sci Res, Educa & Applicat Press, Int Technol Inst, Korean Soc Internet Informat, World Acad Sci Informat Technol DE model-driven architecture; program synthesis; UML; Kalman filters AB We describe ongoing work which aims to extend the schema-based program synthesis paradigm with explicit models. In this context, schemas can be considered as model-to-model transformations. The combination of schemas with explicit models offers a number of advantages, namely, that building synthesis systems becomes much easier since the models can be used in verification and in adaptation of the synthesis systems. We illustrate our approach wing an example from signal processing. C1 NASA, Ames Res Ctr, QSS, Moffett Field, CA 94035 USA. RP Denney, E (reprint author), NASA, Ames Res Ctr, QSS, Moffett Field, CA 94035 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU C S R E A PRESS PI ATHENS PA 115 AVALON DR, ATHENS, GA 30606 USA BN 1-932415-30-0 PY 2004 BP 207 EP 211 PG 5 WC Computer Science, Software Engineering SC Computer Science GA BBK74 UT WOS:000225905800033 ER PT B AU Dvorak, D Bollella, G Canham, T Carson, V Champlin, V Giovannoni, B Indictor, M Meyer, K Murray, A Reinholtz, K AF Dvorak, D Bollella, G Canham, T Carson, V Champlin, V Giovannoni, B Indictor, M Meyer, K Murray, A Reinholtz, K BE Gustafsson, J Aoki, T Lee, I TI Project golden gate: Towards real-time Java in space missions SO SEVENTH IEEE INTERNATIONAL SYMPOSIUM ON OBJECT-ORIENTED REAL-TIME DISTRIBUTED COMPUTING, PROCEEDINGS LA English DT Proceedings Paper CT 7th IEEE International Symposium on Object-Oriented Real-Time Distributed Computing CY MAY 12-14, 2004 CL Vienna, AUSTRIA SP IEEE CompSoc, TC Distributed Processing, OMG, IFIP WG 10 4 AB Planetary science missions, such as those that explore Mars and Saturn, employ a variety of spacecraft such as orbiters, landers, probes, and rovers. Each of these kinds of spacecraft depend on embedded real-time control systems-systems that are increasingly being asked to do more as challenging new mission concepts are proposed For both systems engineers and software engineers the large challenges are in analysis, design and verification of complex control systems that run on relatively limited processors. Project Golden Gate-a collaboration among NASA's Jet Propulsion Laboratory, Sun Microsystems Laboratory, and Carnegie Mellon University-is exploring those challenges in the context of real-time Java applied to space mission software. This paper describes the problem domain and our experimentation with the first commercial implementation of the Real Time Specification for Java. The two main issues explored in this report are: (1) the effect of RTSJ's non-heap memory on the programming model, and (2) performance benchmarking of RTSJ/Linux relative to C++/VxWorks. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Dvorak, D (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 6 TC 9 Z9 10 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA PY 2004 BP 15 EP 22 DI 10.1109/ISORC.2004.1300324 PG 8 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BAG04 UT WOS:000222043400003 ER PT B AU Dvorak, DL Reinholtz, WK AF Dvorak, DL Reinholtz, WK BE Gustafsson, J Aoki, T Lee, I TI Separating essentials from incidentals: An execution architecture for real-time control systems SO SEVENTH IEEE INTERNATIONAL SYMPOSIUM ON OBJECT-ORIENTED REAL-TIME DISTRIBUTED COMPUTING, PROCEEDINGS LA English DT Proceedings Paper CT 7th IEEE International Symposium on Object-Oriented Real-Time Distributed Computing CY MAY 12-14, 2004 CL Vienna, AUSTRIA SP IEEE CompSoc, TC Distributed Processing, OMG, IFIP WG 10 4 AB Source code for real-time control systems often intertwines several concerns such as functionality, data flow, control flow, synchronization, timing, and architectural style. This combination of concerns makes software harder to write correctly, harder to verify, and harder to reuse. This paper proposes an execution architecture that makes such systems more analyzable, verifiable, and reusable by separating "essential code" (software specific to the physical platform, the physical environment, and mission goals) from "incidental code" (all other software, particularly architectural support software for combining together essential components). This architecture elevates two forms of processing as first-class items: individual transformations of global state, as defined in pure functions, and rules of interaction of transformations, as managed by an engine that maintains certain invariants. Importantly, the explicit specification of these two forms of processing by systems engineers reduces sources of ambiguity in requirements. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dvorak, DL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA PY 2004 BP 301 EP 304 DI 10.1109/ISORC.2004.1300392 PG 4 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BAG04 UT WOS:000222043400040 ER PT J AU Hughes, DR Ghoshal, A Rowe, E Sundaresan, MJ Schulz, MJ Feaster, JT AF Hughes, DR Ghoshal, A Rowe, E Sundaresan, MJ Schulz, MJ Feaster, JT TI Health monitoring of thick materials using piezoceramic patches, time signals, and wavelet transmittance functions SO SHOCK AND VIBRATION LA English DT Article DE health monitoring; thick materials; piezoceramic sensors; wavelet transmittance function ID CRACK; BEAMS AB A relatively overlooked factor in both global and local methods of health monitoring is the nonlinear stiffness of structures caused by the cycling of cracks and delaminations. Global methods of health monitoring use modal parameters or frequency response functions in an inverse procedure to quantify damage in structures with thick sections. Global approaches use fewer sensors that detect only significantly large damage in structures due to damage caused by transient vibration. However, local methods use Lamb wave propagation to detect small damage within a structure by an array of closely spaced sensors and actuators. Local methods also become more difficult to use on thick or non-homogeneous materials because wave propagation becomes complex. This paper develops a combined time series and wavelet analysis technique to improve damage detection in either thick, complex geometry, or non-homogeneous materials. A wavelet transmittance function (WTF) is defined as the ratio of continuous wavelet transforms from the time responses at different locations on a structure. A new damage indicator was developed based upon wavelet transmittance function. The novelty of the method lies in the fact that a near real time inference about the damage and the approximate extent of damage can be drawn without historical data. A simulated model is illustrated to highlight the potential of the new damage indicator on a thick aluminum specimen. Then, experimental signal data from two sets of different experiments conducted on thick structures with a crack and a delamination were analyzed using the wavelet transmittance function to detect the presence and extent of the damages as reflected on the WTF maps. This paper mainly deals with the development of WTF and the associated damage indicator by analyzing the simulated and experimental sets of data. C1 USN, Undersea Warfare Ctr, Div Newport, Newport, RI 02841 USA. NASA, NRC Nondestruct Evaluat Sci Branch, Langley Res Ctr, Langley, VA 23681 USA. N Carolina Agr & Tech State Univ, Dept Mech Engn, Greensboro, NC 27411 USA. Univ Cincinnati, Dept Mech Engn, Cincinnati, OH 45221 USA. RP Hughes, DR (reprint author), USN, Undersea Warfare Ctr, Div Newport, Newport, RI 02841 USA. EM hughesdr@npt.nuwc.navy.mil NR 17 TC 1 Z9 1 U1 0 U2 0 PU IOS PRESS PI AMSTERDAM PA NIEUWE HEMWEG 6B, 1013 BG AMSTERDAM, NETHERLANDS SN 1070-9622 J9 SHOCK VIB JI Shock Vib. PY 2004 VL 11 IS 1 BP 47 EP 66 PG 20 WC Acoustics; Engineering, Mechanical; Mechanics SC Acoustics; Engineering; Mechanics GA 777KB UT WOS:000189176600005 ER PT S AU Kumei, Y Morita, S Nakamura, H Katano, H Ohya, K Shimokawa, H Sams, CF Whitson, PA AF Kumei, Y Morita, S Nakamura, H Katano, H Ohya, K Shimokawa, H Sams, CF Whitson, PA BE Diederich, M TI Osteoblast responsiveness to 1 alpha,25-dihydroxyvitamin D-3 during spaceflight SO SIGNAL TRANSDUCTION PATHWAYS, CHROMATIN STRUCTURE, AND GENE EXPRESSION MECHANISMS AS THERAPEUTIC TARGETS SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Signal Transduction Pathways, Chromatin Structures and Gene Expression Mechanisms as Therapeutic Targets (Science Week 2004) CY JAN 25-31, 2004 CL Luxembourg, LUXEMBOURG SP Fdn Rech Canc & Sang, Novartis Luxembourg, Q8 Petroleum DE spaceflight; osteoblast; vitamin D receptor; osteocalcin; bone sialoprotein ID OSTEOCALCIN GENE; RECEPTOR; EXPRESSION; PROTEINS; BINDING AB Rat osteoblasts were cultured aboard a space shuttle for 4 and 5 days. Cells were treated with 1 nM 1 alpha,25-dihydroxyvitamin D-3 (VD) for the last 1 day. The conditioned media were harvested. Cells were solubilized with guanidine solution on board. We examined microgravity effects on the production/expression of osteocalcin, bone sialoprotein (BSP), and VD receptor (VD-R) in osteoblasts. Under VD treatment, the osteocalcin protein level was 243 +/- 117 and 1,718 +/- 534 pg/mu g cellular DNA in flight cultures and ground controls, respectively. Without VD treatment, the osteocalcin protein level was not different between flight cultures and ground controls. The osteocalcin mRNA level in the VD-treated flight cultures was as low as 16 % of that in ground controls. The VD-R mRNA level in the VD-treated flight cultures was also decreased to 16% of that in ground controls. Microgravity would suppress the VD-inducible production of osteocalcin but not the basal productivity. The BSP mRNA level was increased by microgravity. VDND-R binds to the vitamin D-responsive element (VDRE) on the target genes. The rat osteocalcin gene is positively regulated via "enhancer" VDRE, whereas the rat BSP gene is negatively regulated via "repressor " VDRE. Microgravity might modulate osteoblast responsiveness to VD through the suppression of VD-R. C1 Tokyo Med & Dent Univ, Grad Sch, Dept Hard Tissue Engn, Tokyo 1138549, Japan. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Kumei, Y (reprint author), Tokyo Med & Dent Univ, Grad Sch, Dept Hard Tissue Engn, Tokyo 1138549, Japan. EM kumei.bch@tmd.ac.jp NR 10 TC 6 Z9 6 U1 0 U2 1 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-573-7 J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1030 BP 121 EP 124 DI 10.1196/annals.1329.015 PG 4 WC Biochemistry & Molecular Biology; Cell Biology; Medicine, Research & Experimental; Multidisciplinary Sciences SC Biochemistry & Molecular Biology; Cell Biology; Research & Experimental Medicine; Science & Technology - Other Topics GA BBW40 UT WOS:000228128100014 PM 15659788 ER PT S AU Neudeck, PG Trunek, AJ Powell, JA AF Neudeck, PG Trunek, AJ Powell, JA BE Dudley, M Gouma, P Kimoto, T Neudeck, PG Saddow, SE TI Atomic force microscope observation of growth and defects on as-grown (111) 3C-SiC mesa surfaces SO SILICON CARBIDE 2004-MATERIALS, PROCESSING AND DEVICES SE MATERIALS RESEARCH SOCIETY SYMPOSIUM PROCEEDINGS LA English DT Proceedings Paper CT Symposium on Silicon Carbide-Materials, Processing and Devices held at the 2004 MRS Spring Meeting CY APR 14-15, 2004 CL San Francisco, CA SP Mat Res Soc AB This paper presents experimental atomic force microscope (AFM) observations of the surface morphology of as-grown (111) silicon-face 3C-SiC mesa heterofilms. Wide variations in 3C surface step structure are observed as a function of film growth conditions and film defect content. The vast majority of as-grown 3C-SiC surfaces consisted of trains of single bilayer height (0.25 nm) steps. Macrostep formation (i.e., step-bunching) was rarely observed, and then only on mesa heterofilms with extended crystal defects. As supersaturation is lowered by decreasing precursor concentration, terrace nucleation on the top (111) surface becomes suppressed, sometimes enabling the formation of thin 3C-SiC film surfaces completely free of steps. For thicker films, propagation of steps inward from mesa edges is sometimes observed, suggesting that enlarging 3C mesa sidewall facets begin to play an increasingly important role in film growth. The AFM observation of stacking faults (SF's) and 0.25 nm Burgers vector screw component growth spirals on the as-grown surface of defective 3C films is reported. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Neudeck, PG (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,M-S 77-1, Cleveland, OH 44135 USA. NR 10 TC 4 Z9 4 U1 0 U2 0 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 USA SN 0272-9172 BN 1-55899-765-2 J9 MATER RES SOC SYMP P PY 2004 VL 815 BP 59 EP 64 PG 6 WC Engineering, Electrical & Electronic; Materials Science, Ceramics; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA BBA64 UT WOS:000224426400008 ER PT S AU Okojie, RS Zhang, M AF Okojie, RS Zhang, M BE Dudley, M Gouma, P Kimoto, T Neudeck, PG Saddow, SE TI Thermoplastic deformation and residual stress topography of 4H-SiC wafers SO SILICON CARBIDE 2004-MATERIALS, PROCESSING AND DEVICES SE MATERIALS RESEARCH SOCIETY SYMPOSIUM PROCEEDINGS LA English DT Proceedings Paper CT Symposium on Silicon Carbide-Materials, Processing and Devices held at the 2004 MRS Spring Meeting CY APR 14-15, 2004 CL San Francisco, CA SP Mat Res Soc ID SIC BULK GROWTH AB We have measured thermoplastic deformation in as-received, single-side polished, 4H-SiC wafers and also residual stresses in homoepitaxially grown epilayers on wafers by radius curvature measurements. The wafers studied had n-type resistivities of 0.010-0.011 Omega-cm and p-type resistivities of 4.42, 4.72, 9.57 Omega-cm. In a first therinal excursion to 900 degreesC in vacuum, the bow height of the bare substrates in all cases decreased with temperature. Upon cooling down, however, the bow heights remained largely unchanged from their values at 900 T. A second cyclic excursion to 900 degreesC did not yield any significant change in the curvature, thus indicating that the substrates had thermoplastically deformed in the first heating cycle. Epilayers having nitrogen doping between 5 x 10(17) and 2 x 10(19) cm(-3) grown on the n- and p-type substrates resulted in compressive stresses ranging between 190 and 400 MPa in the epilayers. Transmission electron microscopy (TEM) examination of the n-type epilayer (with doping levels of 5 x 10(17) cm(-3) and 5 x 10(18) cm(-3)) on the n-type substrate, revealed bands of stacking faults (SFs) confined within the epilayers after the bicrystals were further annealed at 1150degreesC in nitrogen for thirty minutes. These doping levels are approximately one and two orders of magnitude below the reported threshold value of 3 x 10(19) cm(-3) previously suggested for the onset generation of SFs in annealed n-type 4H-SiC epilayers. The calculated residual stresses in all the epilayers were above the critical stress for the motion of dislocations above 1000 degreesC in 4H-SiC. Thus the SFs that form by glide of pre-existing partial dislocations may actually be stress induced and occur across a much wider range of doping levels. Therefore, it is possible that a significant mechanism for formation of the stacking faults and 3C bands observed in thermally treated 4H-SiC wafer is stress relief via the generation and motion of new and pre-existing partial dislocations on the basal planes of 4H-SiC. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Okojie, RS (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,M-S 77-1, Cleveland, OH 44135 USA. NR 17 TC 4 Z9 4 U1 0 U2 1 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 USA SN 0272-9172 BN 1-55899-765-2 J9 MATER RES SOC SYMP P PY 2004 VL 815 BP 133 EP 138 PG 6 WC Engineering, Electrical & Electronic; Materials Science, Ceramics; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA BBA64 UT WOS:000224426400018 ER PT S AU Hunter, GW Neudeck, PG Xu, J Lukco, D Trunek, A Artale, M Lampard, P Androjna, D Makel, D Ward, B Liu, CC AF Hunter, GW Neudeck, PG Xu, J Lukco, D Trunek, A Artale, M Lampard, P Androjna, D Makel, D Ward, B Liu, CC BE Dudley, M Gouma, P Kimoto, T Neudeck, PG Saddow, SE TI Development of SiC-based gas sensors for aerospace applications SO SILICON CARBIDE 2004-MATERIALS, PROCESSING AND DEVICES SE MATERIALS RESEARCH SOCIETY SYMPOSIUM PROCEEDINGS LA English DT Proceedings Paper CT Symposium on Silicon Carbide-Materials, Processing and Devices held at the 2004 MRS Spring Meeting CY APR 14-15, 2004 CL San Francisco, CA SP Mat Res Soc ID SILICON-CARBIDE; SURFACES; GROWTH AB Silicon carbide (SiC) based gas sensors have the ability to meet the needs of a range of aerospace applications including leak detection, environmental control, emission monitoring, and fire detection. While each of these applications require that the sensor and associated packaging be tailored for that individual application, they all require sensitive detection, The sensing approach taken to meet these needs is the use of SiC as a semiconductor in a Schottky diode configuration due to the demonstrated high sensitivity of Schottky diode-based sensors. However, Schottky diode structures require good control of the interface between the gas sensitive metal and SiC in order to meet required levels of sensitivity and stability. Two examples of effort to better control the SiC gas sensitive Schottky diode interface will be discussed. First, the use of chrome carbide as a barrier layer between the metal and SiC is discussed. Second, we report the first use of atomically flat SiC to provide an improved SiC semiconductor surface for gas sensor deposition. An example of the demonstration of a SiC gas sensor in an aerospace applications is given. It is concluded that, while significant progress has been made, the development of SiC gas sensor systems is still at a relatively early level of maturity for a number of applications. C1 NASA, Glenn Res Ctr, Div Instrumentat & Controls, Cleveland, OH 44135 USA. RP Hunter, GW (reprint author), NASA, Glenn Res Ctr, Div Instrumentat & Controls, 21000 Brookpk Rd,M-S 77-1, Cleveland, OH 44135 USA. NR 16 TC 10 Z9 10 U1 0 U2 0 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 USA SN 0272-9172 BN 1-55899-765-2 J9 MATER RES SOC SYMP P PY 2004 VL 815 BP 287 EP 298 PG 12 WC Engineering, Electrical & Electronic; Materials Science, Ceramics; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA BBA64 UT WOS:000224426400040 ER PT S AU Huang, XR Dudley, M Cho, W Okojie, RS Neudeck, PG AF Huang, XR Dudley, M Cho, W Okojie, RS Neudeck, PG BE Madar, R Camassel, J TI Characterization of SiC epitaxial structures using high-resolution X-ray diffraction techniques SO SILICON CARBIDE AND RELATED MATERIALS 2003, PRTS 1 AND 2 SE MATERIALS SCIENCE FORUM LA English DT Article; Proceedings Paper CT 10th International Conferece on Silicon Carbide and Related Materials 2003 (ICSCRM 2003) CY OCT 05-10, 2003 CL Lyon, FRANCE DE SiC epitaxial structure; characterization; high-resolution X-ray diffraction; reciprocal space mapping ID MESAS; GROWTH AB For devices based SiC epitaxial technology to function satisfactorily, the lattice parameters, perfection, thickness and roughness of the epilayers must be accurately controlled. Xray diffraction is one of the most powerful and widely used techniques for this aim. In this papaper, we introduce a series of advanced X-ray diffraction/scattering techniques, including double-axis diffraction, multiple-order reflections, triple-axis diffraction and reciprocal space mapping, for characterization of SiC epitaxial structures. These techniques are capable of extracting very detailed structural information of SiC homo- and hetero-epitaxial systems, such as accurate lattice parameters, lattice mismatch and misorientation, polytype identifications, dopant concentration, layer thickness, and lattice perfection. The application of these techniques to measurements of small lattice mismatch or misorientation in 3C/4H and 3C/6H SiC heterostructures and in highly doped hornoepitaxial 4H SiC epilayers are demonstrated. C1 SUNY Stony Brook, Dept Mat Sci & Engn, Stony Brook, NY 11794 USA. NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Huang, XR (reprint author), SUNY Stony Brook, Dept Mat Sci & Engn, Stony Brook, NY 11794 USA. NR 11 TC 9 Z9 9 U1 1 U2 4 PU TRANS TECH PUBLICATIONS LTD PI ZURICH-UETIKON PA BRANDRAIN 6, CH-8707 ZURICH-UETIKON, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2004 VL 457-460 BP 157 EP 162 PN 1&2 PG 6 WC Materials Science, Multidisciplinary SC Materials Science GA BAM18 UT WOS:000222802200035 ER PT S AU Neudeck, PG Powell, JA Trunek, AJ Spry, DJ AF Neudeck, PG Powell, JA Trunek, AJ Spry, DJ BE Madar, R Camassel, J TI Step free surface heteroepitaxy of 3C-SiC layers on patterned 4H/6H-SiC mesas and cantilevers SO SILICON CARBIDE AND RELATED MATERIALS 2003, PRTS 1 AND 2 SE MATERIALS SCIENCE FORUM LA English DT Article; Proceedings Paper CT 10th International Conferece on Silicon Carbide and Related Materials 2003 (ICSCRM 2003) CY OCT 05-10, 2003 CL Lyon, FRANCE DE 3C-SiC; step-free surface; heteroepitaxy; epitaxial growth; CVD; etch pits; dislocations; screw dislocations; web growth; cantilevers; mesas; on-axis epitaxy; KOH ID X-RAY TOPOGRAPHY; POLYTYPE IDENTIFICATION; GROWTH AB The off-axis approach to SiC epitaxial growth has not prevented many substrate crystal defects from propagating into SiC epilayers, and does not permit the realization of SiC heteropolytype devices. This paper reviews recent advancements in SiC epitaxial growth that begin to overcome the above shortcomings for arrays of device-sized mesas patterned into on-axis 4H/6H-SiC wafers. These on-axis mesa growth techniques have produced 4H/6H-SiC homoepilayers and 3C-SiC heteroepilayers with substantially lower dislocation densities. The results should enable improved homojunction and heterojunction silicon carbide prototype devices. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NASA Glenn, Sest Inc, Cleveland, OH 44135 USA. NASA Glenn, OAI, Cleveland, OH 44135 USA. RP Neudeck, PG (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk RD,MS 77-1, Cleveland, OH 44135 USA. NR 25 TC 7 Z9 8 U1 0 U2 0 PU TRANS TECH PUBLICATIONS LTD PI ZURICH-UETIKON PA BRANDRAIN 6, CH-8707 ZURICH-UETIKON, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2004 VL 457-460 BP 169 EP 174 PN 1&2 PG 6 WC Materials Science, Multidisciplinary SC Materials Science GA BAM18 UT WOS:000222802200037 ER PT S AU Trunek, AJ Neudeck, PG Powell, JA Spry, DJ AF Trunek, AJ Neudeck, PG Powell, JA Spry, DJ BE Madar, R Camassel, J TI Comparative growth behavior of 3C-SiC mesa heterofilms with and without extended defects SO SILICON CARBIDE AND RELATED MATERIALS 2003, PRTS 1 AND 2 SE MATERIALS SCIENCE FORUM LA English DT Article; Proceedings Paper CT 10th International Conferece on Silicon Carbide and Related Materials 2003 (ICSCRM 2003) CY OCT 05-10, 2003 CL Lyon, FRANCE DE 3C-SiC; epitaxial growth; CVD; heteroepitaxy; AFM; stacking faults; nucleation AB 3C-SiC was grown by step-free surface heteroepitaxy on 4H/6H-SiC on-axis wafers patterned with mesa structures. Under proper growth conditions, 3C-SiC films without stacking faults (SF's) or double positioning boundaries (DPB's) were achieved on many of the mesas. The growth rate of the 3C-SiC films with extended defects such as SF's and DPB's was considerably enhanced over SF/DPB-free 3C-SiC films. The experimental data, including atomic force microscope (AFM) studies of as-grown surfaces, indicate that defects act as preferred sites for nucleation of new 3C bilayers on the (111) growth surface. Larger growth rate discrepancies between mesas with and without SF defects are observed at higher 3C growth temperatures. C1 NASA Glenn, QAI, Cleveland, OH 44135 USA. NASA Glenn, Sest Inc, Cleveland, OH 44135 USA. RP Trunek, AJ (reprint author), NASA Glenn, QAI, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. NR 12 TC 4 Z9 4 U1 0 U2 0 PU TRANS TECH PUBLICATIONS LTD PI ZURICH-UETIKON PA BRANDRAIN 6, CH-8707 ZURICH-UETIKON, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2004 VL 457-460 BP 261 EP 264 PN 1&2 PG 4 WC Materials Science, Multidisciplinary SC Materials Science GA BAM18 UT WOS:000222802200059 ER PT S AU Okojie, RS AF Okojie, RS BE Madar, R Camassel, J TI Inelastic stress relaxation in single crystal SiC substrates SO SILICON CARBIDE AND RELATED MATERIALS 2003, PRTS 1 AND 2 SE MATERIALS SCIENCE FORUM LA English DT Article; Proceedings Paper CT 10th International Conferece on Silicon Carbide and Related Materials 2003 (ICSCRM 2003) CY OCT 05-10, 2003 CL Lyon, FRANCE DE 4H-SiC; 6H-SiC; thermal stress; annealing; thermoplasticity ID DEFORMATION; GROWTH AB Optical methods were used to measure thermal deformations in commercial 4H- and 6H-SiC wafers. In general, during thermal excursions to 500 degreesC, the radii of curvature of the wafers increased (i.e., the wafers became less bowed). Upon cooling to room temperature, nearly all the wafers retained the high temperature radius of curvature values, a characteristic of thermoplastic deformation. Further cyclic excursions to 500 degreesC did not yield any significant changes in the radii of curvature, thus signifying the irreversibility of the thermal deformation. The magnitude of the relieved stress following thermal deformation at 500 degreesC was estimated to be up to 2.14 MPa. Also observed was a significant difference in the thermoplastic deformation between the off- and on-axis wafers of both polytypes, with the former having more deformation (DeltaR > 3 m) than the latter (DeltaR < 2 m). An on-axis n-type 6H-SiC that was subjected to thermal cycling to 900 degreesC in vacuum also exhibited thermoplastic deformation, with an activation energy of 3.14 +/- 0.8 eV and a relieved stress magnitude of 5.67 MPa. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Okojie, RS (reprint author), NASA, Glenn Res Ctr, M-S 77-1,21000 Brookpk Rd, Cleveland, OH 44135 USA. NR 12 TC 5 Z9 5 U1 0 U2 0 PU TRANS TECH PUBLICATIONS LTD PI ZURICH-UETIKON PA BRANDRAIN 6, CH-8707 ZURICH-UETIKON, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2004 VL 457-460 BP 375 EP 378 PN 1&2 PG 4 WC Materials Science, Multidisciplinary SC Materials Science GA BAM18 UT WOS:000222802200087 ER PT S AU Okojie, RS Zhang, M Pirouz, P AF Okojie, RS Zhang, M Pirouz, P BE Madar, R Camassel, J TI Residual stresses and stacking faults in n-type 4H-SiC epilayers SO SILICON CARBIDE AND RELATED MATERIALS 2003, PRTS 1 AND 2 SE MATERIALS SCIENCE FORUM LA English DT Article; Proceedings Paper CT 10th International Conferece on Silicon Carbide and Related Materials 2003 (ICSCRM 2003) CY OCT 05-10, 2003 CL Lyon, FRANCE DE in-situ optical measurement; TEM; stress; stacking faults; 4H-SiC AB Residual stresses were measured in n-type 4H-SiC epilayers having nitrogen-doping levels of 5 x 10(17), 5 x 10(18), and 2 x 10(19) cm(-3) and grown homoepitaxially on n-type 4H-SiC substrates having doping levels between 1.82 and 2.10 x 10(19) cm(-3) (rho = 0.010-0.01 Omega-cm). Radius of curvature measurement of the epilayer/substrate bicrystals indicates the existence of compressive stresses of magnitudes between 250 and 400 Mpa. Transmission electron microscopy (TEM) examination of the epilayer/substrate bicrystals, after they were annealed at 1150degreesC in nitrogen for thirty minutes, revealed bands of stacking faults (SFs) confined within the epilayers that have doping levels of 5 x 10(17) cm(-3) and 5 x 10(18) cm(-3). The SFs, some as wide as 80 nm, give rise to a 3C-SiC like stacking sequence. The lowest doping level is approximately two orders of magnitude below the threshold value of 3 x 10(19) cm(-3) previously proposed for the onset of SF generation in thermally annealed epilayers. The residual stress in all the epilayers was above the critical stress for dislocation formation above 1000degreesC in 4H-SiC, thus the partial dislocations giving rise to SI's may be stress induced and can occur across a much wider range of doping levels than previously believed. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA. RP Okojie, RS (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,M-S 77-1, Cleveland, OH 44135 USA. NR 10 TC 7 Z9 7 U1 0 U2 3 PU TRANS TECH PUBLICATIONS LTD PI ZURICH-UETIKON PA BRANDRAIN 6, CH-8707 ZURICH-UETIKON, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2004 VL 457-460 BP 529 EP 532 PN 1&2 PG 4 WC Materials Science, Multidisciplinary SC Materials Science GA BAM18 UT WOS:000222802200124 ER PT S AU Spry, DJ Trunek, AJ Neudeck, PG AF Spry, DJ Trunek, AJ Neudeck, PG BE Madar, R Camassel, J TI High breakdown field P-type 3C-SiC Schottky diodes grown on step-free 4H-SiC mesas SO SILICON CARBIDE AND RELATED MATERIALS 2003, PRTS 1 AND 2 SE MATERIALS SCIENCE FORUM LA English DT Article; Proceedings Paper CT 10th International Conferece on Silicon Carbide and Related Materials 2003 (ICSCRM 2003) CY OCT 05-10, 2003 CL Lyon, FRANCE DE 3C-SiC; 4H-SiC; Schottky diode; breakdown electric field; step-free surface ID FREE SURFACE HETEROEPITAXY; ELECTRICAL-PROPERTIES; SUBSTRATE AB Step-free surface heteroepitaxy of 3C-SiC films with improved dislocation density on patterned 4H/6H-SiC substrate mesas has recently been reported. This paper details initial investigations of the performance of electrical devices implemented in stacking-fault-free 3C-SiC. Small-area p-type Schottky diodes with 50 nm Ti / 150 nm Ni contacts were fabricated on N-A = 1-5 x 10(17) cm(-3) unintentionally boron-doped 3C-SiC mesa films. Capacitance-voltage (CV) and current-voltage (IV) properties of the devices were measured at 24 degreesC, 200 degreesC, and 300 degreesC. CV measured doping profiles (verified also by secondary ion mass spectroscopy for two of the diodes) were essentially temperature independent. The IV characteristics show excellent rectification properties with low reverse leakage and relatively sharp reverse breakdown. Room temperature breakdown voltages (where current sharply increased to exceed 0.1 A/cm(2)) from 96 V down to 53 V were observed, corresponding to peak electric fields near 2 MV/cm for N-A near 1 x 10(17) cm(-3) to above 3 MV/cm for N-A near 5 x 10(17) cm(-3). These measured 3C-SiC electric fields are comparable to reported <11 (2) over bar0> and <03 (3) over bar8> 4H-SiC breakdown fields. C1 NASA, OAI, Cleveland, OH 44135 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Spry, DJ (reprint author), NASA, OAI, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. NR 15 TC 5 Z9 5 U1 0 U2 0 PU TRANS TECH PUBLICATIONS LTD PI ZURICH-UETIKON PA BRANDRAIN 6, CH-8707 ZURICH-UETIKON, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2004 VL 457-460 BP 1061 EP 1064 PN 1&2 PG 4 WC Materials Science, Multidisciplinary SC Materials Science GA BAM18 UT WOS:000222802200252 ER PT S AU Brillson, LJ Tumakha, S Okojie, RS Zhang, M Pirouz, P AF Brillson, LJ Tumakha, S Okojie, RS Zhang, M Pirouz, P BE Madar, R Camassel, J TI SiC studied via LEEN and cathodoluminescence spectroscopy SO SILICON CARBIDE AND RELATED MATERIALS 2003, PTS 1 AND 2 SE Materials Science Forum LA English DT Article; Proceedings Paper CT 10th International Conferece on Silicon Carbide and Related Materials 2003 (ICSCRM 2003) CY OCT 05-10, 2003 CL Lyon, FRANCE DE luminescence spectroscopy; nanoscale; metal-SiC interface; defect; polytype; stacking fault ID STACKING-FAULTS; SILICON-CARBIDE; TRANSFORMATION; CONTACTS; 4H; LUMINESCENCE; OXIDATION AB We have used low energy electron-excited nanoscale (LEEN) luminescence spectroscopy, a low energy variant of cathodoluminescence spectroscopy, to measure localized states at 4H- and 6H SiC surfaces and interfaces. Both discrete and continuum states appear across the band gap that depend sensitively on surface chemical treatment, thermal processing, or metallization. These localized states form not only as a result of interface chemical bonding but also due to the formation of new local structures/polytypes. Luminescence measurements reveal a striking polytype change of 4H- to 3C-SiC in quantum-scale transformation bands activated by high temperature thermal annealing and high n-type doping. Deep level correlations with Schottky barriers highlight the importance of interface chemical as well as structural interactions. C1 Ohio State Univ, Dreese Lab 205, Columbus, OH 43210 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA. RP Ohio State Univ, Dreese Lab 205, Columbus, OH 43210 USA. NR 18 TC 3 Z9 3 U1 0 U2 0 PU TRANS TECH PUBLICATIONS LTD PI DURNTEN-ZURICH PA KREUZSTRASSE 10, 8635 DURNTEN-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2004 VL 457-460 BP 543 EP 548 PN 1&2 PG 6 WC Materials Science, Multidisciplinary SC Materials Science GA BAM18 UT WOS:000222802200127 ER PT J AU Oyung, RL Mallis, MM AF Oyung, RL Mallis, MM TI Cockpit light exposure in flight crew spanning 30 days of night flight activity SO SLEEP LA English DT Meeting Abstract CT 18th Annual Meeting of the Associated-Professional-Sleep-Societies CY JUN 05-10, 2004 CL Philadelphia, PA SP Associated Profess Sleep Soc C1 San Jose State Univ, Moffett Field, CA USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER ACADEMY SLEEP MEDICINE PI WESTCHESTER PA ONE WESTBROOK CORPORATE CENTER STE 920, WESTCHESTER, IL 60154 USA SN 0161-8105 J9 SLEEP JI Sleep PY 2004 VL 27 SU S MA 177 BP 80 EP 81 PG 2 WC Clinical Neurology; Neurosciences SC Neurosciences & Neurology GA 844OX UT WOS:000223169400179 ER PT J AU Mallis, MM Neri, DF Colletti, LM Oyung, RL Raduta, DD Van Dongen, H Dinges, DF AF Mallis, MM Neri, DF Colletti, LM Oyung, RL Raduta, DD Van Dongen, H Dinges, DF TI Feasibility of an automated drowsiness monitoring device on the flightdeck SO SLEEP LA English DT Meeting Abstract CT 18th Annual Meeting of the Associated-Professional-Sleep-Societies CY JUN 05-10, 2004 CL Philadelphia, PA SP Associated Profess Sleep Soc C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Off Naval Res, Arlington, VA USA. QSS Grp Inc, Moffett Field, CA USA. San Jose State Univ, Moffett Field, CA USA. Univ Penn, Sch Med, Philadelphia, PA 19104 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER ACADEMY SLEEP MEDICINE PI WESTCHESTER PA ONE WESTBROOK CORPORATE CENTER STE 920, WESTCHESTER, IL 60154 USA SN 0161-8105 J9 SLEEP JI Sleep PY 2004 VL 27 SU S MA 367 BP 167 EP 168 PG 2 WC Clinical Neurology; Neurosciences SC Neurosciences & Neurology GA 844OX UT WOS:000223169400369 ER PT J AU Mallis, MM Rosekind, MR Chapman, PM Colletti, LM Neri, DF AF Mallis, MM Rosekind, MR Chapman, PM Colletti, LM Neri, DF TI Evaluation of the NASA Education and Training Module on alertness management: Knowledge gained and organizational impact SO SLEEP LA English DT Meeting Abstract CT 18th Annual Meeting of the Associated-Professional-Sleep-Societies CY JUN 05-10, 2004 CL Philadelphia, PA SP Associated Profess Sleep Soc C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Alertness Solut, Cupertino, CA USA. San Jose State Univ, Moffett Field, CA USA. QSS Grp Inc, Moffett Field, CA USA. Off Naval Res, Arlington, VA 22217 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER ACADEMY SLEEP MEDICINE PI WESTCHESTER PA ONE WESTBROOK CORPORATE CENTER STE 920, WESTCHESTER, IL 60154 USA SN 0161-8105 J9 SLEEP JI Sleep PY 2004 VL 27 SU S MA 842 BP 376 EP 376 PG 1 WC Clinical Neurology; Neurosciences SC Neurosciences & Neurology GA 844OX UT WOS:000223169400844 ER PT S AU Sherrit, S Bao, XQ Bar-Cohen, Y Chang, ZS AF Sherrit, S Bao, XQ Bar-Cohen, Y Chang, ZS BE Lagoudas, DC TI Resonance analysis of high temperature piezoelectric materials for actuation and sensing SO SMART STRUCTURES AND MATERIALS 2004: ACTIVE MATERIALS: BEHAVIOR AND MECHANICS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2004 Conference CY MAR 15-18, 2004 CL San Diego, CA SP SPIE, Amer Inst Aeronaut & Astronaut, Amer Soc Mech Engineers, Soc Expt Mech, Boeing Co, Journal Intelligent Mat Syst & Struct, Rhombus Consultants Grp, CSA Engn Inc, ISIS Canada DE High Temperature Piezoelectric; curie temperature; piezoelectric response; mechanical Q; bulk acoustic waves devices ID REAL AB The current NASA Decadal mission planning effort has identified Venus as a significant scientific target for a surface in-situ sampling mission. The Venus environment represents several extremes including high temperature (460degreesC), high pressure (similar to9 MPa.), and potentially corrosive (condensed sulfuric acid droplets that adhere to surfaces during entry) environments. This technology challenge requires new actuator and sensor designs that can withstand these extreme conditions. In addition a variety of industrial applications could benefit from an extended operating temperature range of actuators and sensors. Piezoelectric materials can potentially operate over a wide temperature range reaching as low as -270degreesC to as high as +650degreesC. Single crystals, like LiNbO3, have a Curie temperature that is higher than +1000degreesC. In order to investigate the feasibility of producing actuators/sensors that can operate under these conditions we have initiated a study of the properties of a variety of piezoelectric materials in the temperature range 25degreesC to 500degreesC. These piezoelectric materials were chosen because they are solid state and can be designed as actuators to provide high torque, stroke, and speed. However the feasibility of this critical actuation capability has never been demonstrated under the extreme conditions mentioned above. We will present the results of our measurements on a variety of piezoelectric materials that can be operated at temperatures above 460degreesC. The data for small signal resonance analysis (ring, radial and thickness extensional modes) of disk and ring samples made of BST-PT and BMT-PT (TRS Technologies Inc.) and Bismuth Titanate BT (Ferroperm Piezoceramics A/S, Sinoceramics) as a function of the temperature will be presented. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP Sherrit, S (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. NR 4 TC 12 Z9 12 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5304-8 J9 P SOC PHOTO-OPT INS PY 2004 VL 5387 BP 411 EP 420 DI 10.1117/12.540102 PG 10 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering; Physics, Applied SC Materials Science; Metallurgy & Metallurgical Engineering; Physics GA BAS07 UT WOS:000223342000043 ER PT S AU Bar-Cohen, Y AF Bar-Cohen, Y BE BarCohen, Y TI EAP as artifical muscles - Progress and challenges SO SMART STRUCTURES AND MATERIALS 2004: ELECTROACTIVE POLYMER ACTUATORS AND DEVICES (EAPAD) SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2004 Conference CY MAR 15-18, 2004 CL San Diego, CA SP SPIE, Amer Inst Aeronaut & Astronaut, Amer Soc Mech Engineers, Soc Expt Mech, Boeing Co, Journal Intelligent Mat Syst & Struct, Rhombus Consultants Grp, CSA Engn Inc, ISIS Canada DE EAP; artificial muscles; armwrestling; actuators; biomimetics ID ELECTROSTRICTION; POLYMER AB During the last decade and a half new polymers have emerged that respond to electrical stimulation with a significant shape or size change. This capability of electroactive polymer (EAP) materials is attracting the attention of engineers and scientists from many different disciplines. Practitioners in biomimetics are particularly excited about these materials since the artificial muscle aspect of EAPs can be applied to mimic the movements of animals and insects. In the foreseeable future, robotic mechanisms actuated by EAP will enable engineers to create devices previously imaginable only in science fiction. Last year, significant accomplishments were reported including the emergence of the first commercial product and the possibility that an arm can be made with EAP actuators having the potential of winning a wrestling match with a human. As such major accomplishments continue to be reported it is interesting to review the progress and provide a prospective regarding the development since the first EAPAD conference in 1999. This manuscript covers the progress in the field of EAP and the challenges that are being addressed. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bar-Cohen, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 82-105, Pasadena, CA 91109 USA. NR 20 TC 11 Z9 11 U1 2 U2 19 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5302-1 J9 P SOC PHOTO-OPT INS PY 2004 VL 5385 BP 10 EP 16 DI 10.1117/12.538698 PG 7 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Polymer Science SC Engineering; Instruments & Instrumentation; Polymer Science GA BAS49 UT WOS:000223368700002 ER PT S AU Bao, XQ Bar-Cohen, Y Chang, ZS Sherrit, S AF Bao, XQ Bar-Cohen, Y Chang, ZS Sherrit, S BE BarCohen, Y TI Characterization of bending EAP beam actuators SO SMART STRUCTURES AND MATERIALS 2004: ELECTROACTIVE POLYMER ACTUATORS AND DEVICES (EAPAD) SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2004 Conference CY MAR 15-18, 2004 CL San Diego, CA SP SPIE, Amer Inst Aeronaut & Astronaut, Amer Soc Mech Engineers, Soc Expt Mech, Boeing Co, Journal Intelligent Mat Syst & Struct, Rhombus Consultants Grp, CSA Engn Inc, ISIS Canada DE electroactive polymer; EAP evaluation; bending actuator; nonlinear; large deformation ID IPMC AB Electroactive polymers (EAP) are attractive actuation materials because of their large deformation, flexibility, and low density. The large deformation, especially in the bending mode, poses a challenge to the material and actuator characterization due to the geometric nonlinearity that is developed during the characterization. A CCD camera system was constructed to record the curved shapes of bending during the activation of EAP films and image-processing software was developed to digitize the bending curve s. A computer program was written to solve the inverse problem of cantilever EAP beams with a tip position limiter. Using the program and acquired curve images with and without a tip position limiter as well as the corresponding tip force, the performance of the beam under different applied voltages and tip force loads was determined. The experimental setup, and the principles of the computer program are described and discussed in this paper. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bao, XQ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 9 TC 4 Z9 4 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5302-1 J9 P SOC PHOTO-OPT INS PY 2004 VL 5385 BP 388 EP 394 DI 10.1117/12.539083 PG 7 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Polymer Science SC Engineering; Instruments & Instrumentation; Polymer Science GA BAS49 UT WOS:000223368700044 ER PT S AU Su, J Xu, TB Zhang, SJ Shrout, TR Zhang, QM AF Su, J Xu, TB Zhang, SJ Shrout, TR Zhang, QM BE BarCohen, Y TI A hybrid actuation system demonstrating significantly enhanced electromechanical performance SO SMART STRUCTURES AND MATERIALS 2004: ELECTROACTIVE POLYMER ACTUATORS AND DEVICES (EAPAD) SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2004 Conference CY MAR 15-18, 2004 CL San Diego, CA SP SPIE, Amer Inst Aeronaut & Astronaut, Amer Soc Mech Engineers, Soc Expt Mech, Boeing Co, Journal Intelligent Mat Syst & Struct, Rhombus Consultants Grp, CSA Engn Inc, ISIS Canada DE hybrid; actuation system; electroactive polymer; electrostrictive; electroactive ceramics; single crystal ID POLY(VINYLIDENE FLUORIDE-TRIFLUOROETHYLENE) COPOLYMER; SINGLE-CRYSTALS; ELECTROSTRICTION AB A hybrid actuation system (HYBAS) utilizing advantages of a combination of electromechanical responses of an electroative polymer (EAP), an electrostrictive copolymer, and an electroactive ceramic single crystal, PZN-PT single crystal, has been developed. The system employs the contribution of the actuation elements cooperatively and exhibits a significantly enhanced electromechanical performance compared to the performances of the device made of each constituting material, the electroactive polymer or the ceramic single crystal, individually. The theoretical modeling of the performances of the HYBAS is in good agreement with experimental observation. The consistence between the theoretical modeling and experimental test make the design concept an effective route for the development of high performance actuating devices for many applications. The theoretical modeling, fabrication of the HYBAS and the initial experimental results will be presented and discussed. C1 NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Su, J (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA. NR 19 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5302-1 J9 P SOC PHOTO-OPT INS PY 2004 VL 5385 BP 461 EP 467 DI 10.1117/12.539817 PG 7 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Polymer Science SC Engineering; Instruments & Instrumentation; Polymer Science GA BAS49 UT WOS:000223368700053 ER PT S AU Bar-Cohen, Y Sherrit, S Chang, Z Wessel, L Bao, X Doran, PT Fritsen, CH Kenig, F McKay, CP Murray, A Peterson, T AF Bar-Cohen, Y Sherrit, S Chang, Z Wessel, L Bao, X Doran, PT Fritsen, CH Kenig, F McKay, CP Murray, A Peterson, T BE Anderson, EH TI Subsurface ice and brine sampling using an ultrasonic/sonic gopher for life detection and characterization in the McMurdo Dry valleys SO SMART STRUCTURES AND MATERIALS 2004: INDUSTRIAL AND COMMERCIAL APPLICATIONS OF SMART STRUCTURES TECHNOLOGIES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2004 Conference CY MAR 15-18, 2004 CL San Diego, CA SP SPIE, Amer Inst Aeronaut & Astronaut, Amer Soc Mech Engineers, Soc Expt Mech, Boeing Co, Journal Intelligent Mat Syst & Struct, Rhombus Consultants Grp, CSA Engn Inc, ISIS Canada DE USDC; life detection; ultrasonic/sonic gopher; planetary sampling; ice drilling ID MARS AB There is growing evidence for ice and fluids near the surface of Mars with potential discharge of brines, which may preserve a record of past life on the planet. Proven techniques to sample Mars subsurface will be critical for future NASA astrobiology missions that will search for such records. The required technology studies are underway in the McMurdo Dry valleys, Antarctica, which is serving as a Mars analog. The ice layer on Lake Vida in the dry valleys is estimated to be 20-meter thick where below 16-m depth there is a mix of ice and brine, which has never been sampled directly due to logistical constraints. A novel light weight, low power ultrasonic/sonic driller/corer (USDC) mechanism was developed that overcomes the need for high axial loads required by drilling via conventional techniques. The USDC was modified to produce an Ultrasonic/Sonic Gopher that is being developed to core down to the 20-m depth for in situ analysis and sample collection. Coring ice at -20degreesC as in Lake Vida suggests that it is a greater challenge and current efforts are focused on the problems of ice core cutting, ice chip handling and potential ice melt (and refreezing) during drilling. An analytical model and a prototype are being developed with an effort to optimize the design while addressing the thermal issues, drilling rate, power, mass and the electromechanical behavior. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bar-Cohen, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Kenig, Fabien/0000-0003-4868-5232 NR 9 TC 1 Z9 1 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5305-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5388 BP 53 EP 61 DI 10.1117/12.539280 PG 9 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BAV19 UT WOS:000223715000006 ER PT S AU Chang, ZS Sherrit, S Bao, XQ Bar-Cohen, Y AF Chang, ZS Sherrit, S Bao, XQ Bar-Cohen, Y BE Anderson, EH TI Design and analysis of ultrasonic horn for USDC (ultrasonic/sonic driller/corer) SO SMART STRUCTURES AND MATERIALS 2004: INDUSTRIAL AND COMMERCIAL APPLICATIONS OF SMART STRUCTURES TECHNOLOGIES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2004 Conference CY MAR 15-18, 2004 CL San Diego, CA SP SPIE, Amer Inst Aeronaut & Astronaut, Amer Soc Mech Engineers, Soc Expt Mech, Boeing Co, Journal Intelligent Mat Syst & Struct, Rhombus Consultants Grp, CSA Engn Inc, ISIS Canada DE ultrasonic/sonic driller/corer (USDC); ultrasonic horn; planetary exploration AB In-situ sampling and analysis is one of the major objectives of future NASA exploration missions. Existing drilling techniques are limited by the need for large axial forces, holding torques, and high power consumption. Lightweight robots and rovers have difficulties accommodating these requirements. These requirements are becoming increasingly tougher to meet as the need for drilling techniques is expanding to reach deeper into the subsurface. To address these key challenges to the NASA objective of planetary in-situ rock sampling and analysis, a drilling technology called ultrasonic/sonic driller/corer (USDC) was developed. The USDC uses a novel driving mechanism, transferring ultrasonic vibration to sonic frequency impacts with the aid of a free-flying mass block (free-mass). The free mass then drives the drill bit. The actuator consists of a stack of piezoelectric disks with a horn that amplifies the induced vibration amplitudes. To meet the need for deep driller the USDC was modified to form the Ultrasonic/Sonic Gopher. Drilling to the depth of several meters in ice or hard rocks requires the optimization of the amplification of the vibration displacement and velocity that are generated by the piezoelectric materials. For this purpose, various horn designs were examined analytically. Conventional and new designs of the horn were analyzed using finite element modeling and the results allow for the determination of the control parameters that can enhance the tip displacement and velocity. The results of the modeling are described and discussed in this paper. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chang, ZS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 4 TC 6 Z9 6 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5305-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5388 BP 320 EP 326 DI 10.1117/12.540000 PG 7 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA BAV19 UT WOS:000223715000031 ER PT S AU Turner, TL Patel, HD AF Turner, TL Patel, HD BE Smith, RC TI Analysis of SMA hybrid composite structures using commercial codes SO SMART STRUCTURES AND MATERIALS 2004: MODELING, SIGNAL PROCESSING, AND CONTROL SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2004 Conference CY MAR 15-18, 2004 CL San Diego, CA SP SPIE, Amer Inst Aeronaut & Astronaut, Amer Soc Mech Engineers, Soc Expt Mech, Boeing Co, Journal Intelligent Mat Syst & Struct, Rhombus Consultants Grp, CSA Engn Inc, ISIS Canada DE shape memory alloys; Nitinol; commercial codes; MSC.Nastran; ABAQUS; finite element analysis; postbuckling control; vibration control; shape control; deflection control ID SHAPE-MEMORY ALLOY; MULTIVARIANT MICROMECHANICAL MODEL; NITINOL-REINFORCED PLATES; THERMOELASTIC MODEL AB A thermomechanical model for shape memory alloy (SMA) actuators and SMA hybrid composite (SMAHC) structures has been recently implemented in the commercial finite element codes MSC.Nastran and ABAQUS. The model may be easily implemented in any code that has the capability for analysis of laminated composite structures with temperature dependent material properties. The model is also relatively easy to use and requires input of only fundamental engineering properties. A brief description of the model is presented, followed by discussion of implementation and usage in the commercial codes. Results are presented from static and dynamic analysis of SMAHC beams of two types; a beam clamped at each end and a cantilevered beam. Nonlinear static (post-buckling) and random response analyses are demonstrated for the first specimen. Static deflection (shape) control is demonstrated for the cantilevered beam. Approaches for modeling SMAHC material systems with embedded SMA in ribbon and small round wire product forms are demonstrated and compared. The results from the commercial codes are compared to those from a research code as validation of the commercial implementations; excellent correlation is achieved in all cases. C1 NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Turner, TL (reprint author), NASA Langley Res Ctr, Mail Stop 463, Hampton, VA 23681 USA. NR 15 TC 10 Z9 10 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5300-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5383 BP 82 EP 93 DI 10.1117/12.540002 PG 12 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA BAT29 UT WOS:000223423300009 ER PT S AU King, GC Choi, SH Chu, SH Kim, JW Park, Y Lillehei, P Watt, GD Davis, R Harb, JN AF King, GC Choi, SH Chu, SH Kim, JW Park, Y Lillehei, P Watt, GD Davis, R Harb, JN BE Varadan, VK TI Development of a bio-nanobattery for distributed power storage systems SO SMART STRUCTURES AND MATERIALS 2004: SMART ELECTRONICS, MEMS, BIOMEMS AND NANOTECHNOLOGY SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2004 Conference CY MAR 15-18, 2004 CL San Diego, CA SP SPIE, Amer Inst Aeronaut & Astronaut, Amer Soc Mech Engineers, Soc Expt Mech, Boeing Co, Journal Intelligent Mat Syst & Struct, Rhombus Consultants Grp, CSA Engn Inc, ISIS Canada DE ferritin; bio-nanobattery; battery; power; storage; cell; electronic ID FERRITIN; FABRICATION AB Currently available power storage systems, such as those used to supply-power to microelectronic devices, typically consist of a single centralized canister and a series of wires to supply electrical power to where it is needed in a circuit. As the size of electrical circuits and components become smaller, there exists a need for a distributed power. system to reduce Joule heating, wiring, and to allow autonomous operation of the various functions performed by the circuit. Our research is being conducted to develop a bio-nanobattery using ferritins reconstituted with both an iron core (Fe-ferritin) and a cobalt core (Co-ferritin). Both Co-ferritin and Fe-ferritin were synthesized and characterized as candidates for the bio-nanobattery. The reducing capability was determined as well as the half-cell electrical potentials, indicating an electrical output of nearly 0.5-V for the battery cell. Ferritins having other metallic cores are also being investigated, in order to increase the overall electrical output. Two dimensional ferritin arrays were also produced on various substrates, demonstrating the necessary building blocks for the bio-nanobattery. The bio-nanobattery will play a key role in moving to a distributed power storage system for electronic applications. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Choi, SH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. RI Kim, Jae-Woo/A-8314-2008 NR 9 TC 0 Z9 0 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5306-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5389 BP 461 EP 467 DI 10.1117/12.539778 PG 7 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Materials Science, Multidisciplinary SC Engineering; Instruments & Instrumentation; Materials Science GA BAV21 UT WOS:000223715800049 ER PT S AU Engberg, RC Ooi, TK AF Engberg, RC Ooi, TK BE Udd, E Inaudi, D TI Methods and piezoelectric imbedded sensors for damage detection in composite plates under ambient and cryogenic conditions SO SMART STRUCTURES AND MATERIALS 2004: SMART SENSOR TECHNOLOGY AND MEASUREMENT SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2004 Conference CY MAR 15-18, 2004 CL San Diego, CA SP SPIE, Amer Inst Aeronaut & Astronaut, Amer Soc Mech Engineers, Soc Expt Mech, Boeing Co, Journal Intelligent Mat Syst & Struct, Rhombus Consultants Grp, CSA Engn Inc, ISIS Canada DE structural health monitoring; impedance; piezoelectric sensors; cementitious composites; unidirectional epoxy matrix composites; NDE AB New methods for structural health monitoring are being assessed, especially in high-performance, extreme environment, safety-critical applications. One such application is for composite cryogenic fuel tanks. The work presented here attempts to characterize and investigate the feasibility of using imbedded piezoelectric sensors to detect cracks and delaminations under cryogenic and ambient conditions. A variety of damage detection methods and different sensors are employed in the different composite plate samples to aid in determining an optimal algorithm, sensor placement strategy, and type of imbedded sensor to use. Variations of frequency, impedance measurements, and pulse echoing techniques of the sensors are employed and compared. Statistical and analytic techniques are then used to determine which method is most desirable for a specific type of damage. These results are furthermore compared with previous work using externally mounted sensors. Results and optimized methods from this work can then be incorporated into a larger composite structure to validate and assess its structural health. This could prove to be important in the development and qualification of any 2nd generation reusable launch vehicle using composites as a structural element. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Engberg, RC (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NR 4 TC 1 Z9 1 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5301-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5384 BP 80 EP 88 DI 10.1117/12.539276 PG 9 WC Instruments & Instrumentation; Materials Science, Multidisciplinary; Optics; Physics, Applied SC Instruments & Instrumentation; Materials Science; Optics; Physics GA BAT33 UT WOS:000223423700010 ER PT S AU Turner, TL Buehrle, RD Cano, RJ Fleming, GA AF Turner, TL Buehrle, RD Cano, RJ Fleming, GA BE Flatau, AB TI Design, fabrication, and testing of SMA enabled adaptive chevrons for jet noise reduction SO SMART STRUCTURES AND MATERIALS 2004: SMART STRUCTURES AND INTEGRATED SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2004 Conference CY MAR 15-18, 2004 CL San Diego, CA SP SPIE, Amer Inst Aeronaut & Astronaut, Amer Soc Mech Engineers, Soc Expt Mech, Boeing Co, Journal Intelligent Mat Syst & Struct, Rhombus Consultants Grp, CSA Engn Inc, ISIS Canada DE shape memory alloys; Nitinol; embedded actuators; jet engine chevrons; adaptive chevrons; shape control; deflection control.; jet noise control AB This study presents the status and results from an effort to design, fabricate, and test an adaptive jet engine chevron concept based upon embedding shape memory alloy (SMA) actuators in a composite laminate, termed a SMA hybrid composite (SMAHC). The approach for fabricating the adaptive SMAHC chevrons involves embedding prestrained Nitinol actuators on one side of the mid-plane of the composite laminate such that thermal excitation generates a thermal moment and deflects the structure. A glass-epoxy pre-preg/Nitinol ribbon material system and a vacuum hot press consolidation approach are employed. A versatile test system for control and measurement of the chevron deflection performance is described. Projection moire interferometry (PMI) is used for global deformation measurement and infrared (IR) thermography is used for 2-D temperature measurement and feedback control. A recently commercialized constitutive model for SMA and SMAHC materials is used in the finite element code ABAQUS to perform nonlinear static analysis of the chevron prototypes. Excellent agreement is achieved between the predicted and measured chevron deflection performance, thereby validating the design tool. Although the performance results presented in this paper fall short of the requirement, the concept is proven and an approach for achieving the performance objectives is evident. C1 NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Turner, TL (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA. NR 10 TC 8 Z9 8 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5307-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5390 BP 297 EP 308 DI 10.1117/12.540013 PG 12 WC Engineering, Electrical & Electronic; Engineering, Mechanical SC Engineering GA BAV92 UT WOS:000223848600031 ER PT S AU Richards, WL Lee, DG Piazza, A Stewart, A Carman, GP AF Richards, WL Lee, DG Piazza, A Stewart, A Carman, GP BE Flatau, AB TI Characterization of embedded fiber optic sensors in advanced composite materials for structural health monitoring SO SMART STRUCTURES AND MATERIALS 2004: SMART STRUCTURES AND INTEGRATED SYSTEMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2004 Conference CY MAR 15-18, 2004 CL San Diego, CA SP SPIE, Amer Inst Aeronaut & Astronaut, Amer Soc Mech Engineers, Soc Expt Mech, Boeing Co, Journal Intelligent Mat Syst & Struct, Rhombus Consultants Grp, CSA Engn Inc, ISIS Canada DE embedded EFPI; Fiber Optic Smart Structures (FOSS); composites; Structural Health Monitoring (SHM) system AB This paper presents comprehensive studies on sensor performance of an embedded Extrinsic Fabry Perot Interferometer (EFPI) fiber optic strain sensor in an aerospace grade composite system to support fiber optic smart structures (FOSS) development for Structural Health Monitoring (SHM) System. A major portion of this study is focused on establishing the accuracy of the embedded EFPI sensors in a graphite epoxy composite material system at different stress levels under quasi-static loading conditions. The NASA Dryden calibrated EFPI's were used for accurate measurements. Two collocated surface-mounted strain gages and a calibrated surface-mounted EFPI sensor are used to validate the calibrated embedded EFPI sensor. Experimental results suggest that once calibrated, the embedded and surface-mounted EFPI sensors provide robust, reliable and accurate measurement for values up to similar to5,400 muis an element of higher than sensor's durability limit similar to3,000 muepsilon at 10(6) cycles. This validation provides evidence that the sensing information emanating from FOSS can be used to monitor accurate health information. C1 NASA, Dryden Flight Res Ctr, Aerostruct Branch, Edwards AFB, CA 93523 USA. RP Richards, WL (reprint author), NASA, Dryden Flight Res Ctr, Aerostruct Branch, MS 4820-1C, Edwards AFB, CA 93523 USA. NR 18 TC 3 Z9 5 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5307-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5390 BP 505 EP 512 DI 10.1117/12.540151 PG 8 WC Engineering, Electrical & Electronic; Engineering, Mechanical SC Engineering GA BAV92 UT WOS:000223848600051 ER PT B AU Hussain, M Ahmadzadeh, A Sayyar-Roudsari, B Kimiaghalam, B Homaifar, A Walls, J AF Hussain, M Ahmadzadeh, A Sayyar-Roudsari, B Kimiaghalam, B Homaifar, A Walls, J BE Jamshidi, M Reuter, M Andina, D Jamshidi, JS TI A novel algorithm for mixed integer nonlinear optimization problems SO SOFT COMPUTING WITH INDUSTRIAL APPLICATIONS, VOL 17 SE TSI PRESS SERIES LA English DT Proceedings Paper CT 5th International Symposium on Soft Computing for Industry held at the 6th Biannual World Automation Congress CY JUN 28-JUL 01, 2004 CL Seville, SPAIN SP World Automat Congress, ISSCI, Minist Cienc Tecnol, Univ Sevilla, Univ Politecn Madrid, Plan Andaluz Invest DE mixed integer nonlinear programming; projected gradient method; projected variable metric methods; penalty function ID PROGRAMMING-PROBLEMS AB The main objective of this research is to develop a computationally efficient hybrid algorithm for the constrained mixed integer, nonlinear optimization problems (MINLPs). The developed algorithm provides a general framework for solving a large class of problems formulated as MINLPs. Although the utility of the algorithms is tested on sample graph-partitioning problems, the application is not limited to any particular field of application. For instance the coordinated decision and control problem for multiple unmanned aerial vehicles (UAVs) can be cast as a MINLP and hence efficiently solved by the proposed technique. C1 NC A&T Univ, NASA, ACIT Ctr, Greensboro, NC 27411 USA. RP NC A&T Univ, NASA, ACIT Ctr, Greensboro, NC 27411 USA. EM muddie27@yahoo.com; farhad_ahmadzadeh@yahoo.com; bijan@pav.com; bahram@ncat.edu; homaifar@ncat.edu; walls_jamie@yahoo.com NR 14 TC 0 Z9 0 U1 0 U2 0 PU TSI PRESS PI ALBUQUERQUE PA PO BOX 14126, ALBUQUERQUE, NM 87191-4126 USA BN 1-889335-23-1 J9 TSI PRESS S PY 2004 VL 17 BP 543 EP 548 PG 6 WC Computer Science, Artificial Intelligence; Engineering, Industrial SC Computer Science; Engineering GA BCO59 UT WOS:000230424800084 ER PT B AU Snowden, SL AF Snowden, SL BE Lieu, R Mittaz, J TI The ISM from the soft X-ray background perspective SO SOFT X-RAY EMISSION FROM CLUSTERS OF GALAXIES AND RELATED PHENOMENA SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Meeting on Soft X-Ray Emissions from Clusters of Galaxies and Related Phenomena CY DEC 11-13, 2002 CL Univ Alabama Huntsville, Huntsville, AL HO Univ Alabama Huntsville ID LOCAL BUBBLE; COMPONENTS; EMISSION; MAPS AB In the past few years progress in understanding the local and Galactic ISM in terms of the diffuse X-ray background has been as much about what hasn't been seen as it has been about detections. High resolution spectra of the local SXRB have been observed, but are inconsistent with current thermal emission models. An excess over the extrapolation of the high-energy (most clearly visible at E > 1.5 keV) extragalactic power law down to (4)/(3) keV has been observed but only at the level consistent with cosmological models, implying the absence of at least a bright hot Galactic halo. A very recent FUSE result indicates that O VI emission from the Local Hot Bubble is insignificant, if it exists at all. a result which is also inconsistent with current thermal emission models. A (very) short review of the Galactic SXRB and ISM is presented. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Snowden, SL (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. RI Snowden, Steven/D-5292-2012 NR 20 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-2563-7 J9 ASTROPHYS SPACE SC L PY 2004 VL 309 BP 103 EP 110 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBI15 UT WOS:000225598000012 ER PT S AU Gilliam, DP AF Gilliam, DP BE Futatsugi, K Mizoguchi, F Yonezaki, N TI Managing Information Technology Security Risk SO SOFTWARE SECURITY - THEORIES AND SYSTEMS SE LECTURE NOTES IN COMPUTER SCIENCE LA English DT Article; Proceedings Paper CT 2nd International Symposium on Software Security CY NOV 04-06, 2003 CL Tokyo Inst Technol, Tokyo, JAPAN SP Japnese Minist Educ, Sci & Culture, Natl Sci Fdn, Japanese Soc Promot Sci HO Tokyo Inst Technol AB Information Technology (IT) Security Risk Management is a critical task for the organization to protect against the loss of confidentiality, integrity, and availability of IT resources and data. Due to system complexity and sophistication of attacks, it is increasingly difficult to manage IT security risk. This paper describes a two-pronged approach for managing IT security risk: 1) an institutional approach, that addresses automating the process of providing and maintaining security for IT systems and the data they contain; and 2) a project life cycle approach that addresses providing semi-automated means for integrating security into the project life cycle. It also describes the use of a security template with a risk reduction/mitigation tool, the Defect Detection and Prevention (DDP) tool developed at the Jet Propulsion Laboratory (JPL). C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gilliam, DP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 144-210, Pasadena, CA 91109 USA. EM david.p.gillliam@jpl.nasa.gov RI Caposaldo, Marica/I-8659-2014 NR 30 TC 2 Z9 2 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-23635-X J9 LECT NOTES COMPUT SC PY 2004 VL 3233 BP 296 EP 317 PG 22 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BBE02 UT WOS:000225088600016 ER PT B AU Brosius, JW AF Brosius, JW BE Gary, DE Keller, CU TI Coronal diagnostics with coordinated radio and EUV/soft X-ray observations SO SOLAR AND SPACE WEATHER RADIOPHYSICS: CURRENT STATUS AND FUTURE DEVELOPMENTS SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Conference on Solar and Space Weather Radiophysics held at the 200th American-Astronomical-Society Meeting CY JUN, 2002 CL Albuquerque, NM SP Amer Astron Soc DE active regions; corona; elemental abundances; line emission; magnetic fields; polarization; radio radiation; sunspots; ultraviolet radiation; X-ray radiation ID SOLAR ACTIVE-REGION; STRUCTURES OBSERVING CAMPAIGN; HIGH-SPATIAL-RESOLUTION; OPTICALLY THIN PLASMAS; TO-LIMB VARIATION; MAGNETIC-FIELDS; EXTREME-ULTRAVIOLET; EMISSION-LINES; ATOMIC DATABASE; MICROWAVE POLARIZATION AB A brief review is provided of what has been learned about the solar corona from existing coordinated radio and EUV (or soft X-ray) observations. Topics include: introduction to radio thermal bremsstrahlung and thermal gyroemission; two-dimensional coronal magnetography measurements; measurements of coronal elemental abundances; measurements of physical properties of quasi-transverse (QT) layers in the coronal magnetic field; and three-dimensional coronal magnetography measurements (the primary subject of this Chapter). Results from these studies are used to help focus on coronal diagnostics that can be performed with similar coordinated observations involving FASR, as well as to recommend FASR instrument requirements. C1 Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Brosius, JW (reprint author), Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Code 682, Greenbelt, MD 20771 USA. NR 56 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-2813-X J9 ASTROPHYS SPACE SC L PY 2004 VL 314 BP 265 EP 286 PG 22 WC Astronomy & Astrophysics; Engineering, Electrical & Electronic; Instruments & Instrumentation SC Astronomy & Astrophysics; Engineering; Instruments & Instrumentation GA BBO84 UT WOS:000226770500013 ER PT S AU Gopalswamy, N AF Gopalswamy, N BE Gary, DE Keller, CU TI Interplanetary radio bursts SO SOLAR AND SPACE WEATHER RADIOPHYSICS: CURRENT STATUS AND FUTURE DEVELOPMENTS SE Astrophysics and Space Science Library LA English DT Proceedings Paper CT Conference on Solar and Space Weather Radiophysics held at the 200th American-Astronomical-Society Meeting CY JUN, 2002 CL Albuquerque, NM SP Amer Astron Soc ID CORONAL MASS EJECTIONS; ENERGETIC PARTICLE EVENTS; SOLAR-WIND SPEED; II BURSTS; MAGNETIC CLOUD; ALFVEN WAVES; SHOCK-WAVE; 1 AU; EMISSION; STORMS AB Nonthermal radio bursts in the interplanetary medium indicate the far-reaching effect of solar eruptions that inject energetic particles, plasmas and shock waves into the inner heliosphere. More than half a century of ground-based observations and subsequent space-based observations exist on this phenomena. In this paper, I summarize the understanding we have gained on the type III and type II radio bursts, which are indicative of electron beams and shocks, respectively. Observations in the new radio window (1 - 14 MHz) from Wind/WAVES have not only confirmed previous results, but also led to a number of new discoveries. Availability of simultaneous white light (SOHO) and radio (Wind) observations from the same spatial domain in the near-Sun IP medium is largely responsible for these discoveries on the IP propagation of CMEs, so this paper discusses radio bursts in the context of white light observations. After exploring the origin of normal, complex and storm type III bursts, I discuss the type II bursts and their relation to coronal mass ejections. Finally I discuss some of the recent developments on IP radio emission. C1 GSFC, NASA, Extraterr Phys Lab, Greenbelt, MD USA. RP Gopalswamy, N (reprint author), GSFC, NASA, Extraterr Phys Lab, Greenbelt, MD USA. RI Gopalswamy, Nat/D-3659-2012 NR 87 TC 15 Z9 15 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0067-0057 BN 1-4020-2813-X J9 ASTROPHYS SPACE SC L PY 2004 VL 314 BP 305 EP 333 PG 29 WC Astronomy & Astrophysics; Engineering, Electrical & Electronic; Instruments & Instrumentation SC Astronomy & Astrophysics; Engineering; Instruments & Instrumentation GA BBO84 UT WOS:000226770500015 ER PT B AU Choudhary, DP Balasubramaniam, KS Suematsu, Y AF Choudhary, DP Balasubramaniam, KS Suematsu, Y BE Sakurai, T Sekii, T TI Asymmetric Stokes-V profiles at the penumbral boundary of a sunspot SO Solar-B Mission and the Forefront of Solar Physics, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 5th Solar-B Science Meeting CY NOV 12-14, 2003 CL Int House Japan, Tokyo, JAPAN HO Int House Japan ID SOLAR MAGNETIC ELEMENTS; VELOCITY-FIELDS; FLUX; LINES AB We present the spectropolarimetric measurements of a sunspot situated near central meridian disk passage. The sunspot was of positive polarity with several opposite polarity magnetic elements at and beyond the penumbral boundary. The Ha images of the sunspot show bright emission regions near the penumbral boundary towards the sun-center, which was of opposite polarity to the main spot. Doppler velocities determined by measuring the center-of-gravity (COG) of the Stokes-I profile, in general, agree with Evershed flow. In addition, it shows strong flows in the penumbra. The velocities derived from zero-crossing wavelengths of Stokes-V profiles show strong downflows at the penumbral boundary. Double-lobed Stokes-V profiles are observed at locations where penumbral fibrils terminate coinciding with H alpha plages. Double lobed profiles have an unshifted component similar to the Stokes-V profiles of the sunspot penumbra and a shifted component with a velocity of about 5 kms(-1). The amplitude of the second component increases along the penumbral fibril as a function of the distance from the center of the sunspot. In this paper we present the preliminary results and propose to observe with the Solar-B Solar Optical Telescope (SOT) for understanding the nature of emerging flux near the sunspots. C1 NASA, George C Marshall Space Flight Ctr, Solar Phys Div, Huntsville, AL 35805 USA. RP Choudhary, DP (reprint author), NASA, George C Marshall Space Flight Ctr, Solar Phys Div, SD 50, Huntsville, AL 35805 USA. NR 16 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-187-7 J9 ASTR SOC P PY 2004 VL 325 BP 137 EP 142 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCY30 UT WOS:000231851500016 ER PT B AU Moore, RL Falconer, DA Porter, JG Hathaway, DI Yamauchi, Y Rabin, DM AF Moore, RL Falconer, DA Porter, JG Hathaway, DI Yamauchi, Y Rabin, DM BE Sakurai, T Sekii, T TI Coronal heating, spicules, and Solar-B SO Solar-B Mission and the Forefront of Solar Physics, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 5th Solar-B Science Meeting CY NOV 12-14, 2003 CL Int House Japan, Tokyo, JAPAN HO Int House Japan ID MAGNETIC-STRUCTURE; TRANSITION REGION; HOLES; NETWORK; FLUX AB We summarize certain observations of coronal luminosity, network magnetic flux, spicules, and macrospicules. These observations together imply that in quiet regions that are not influenced by active regions the coronal heating comes from magnetic activity in the edges of the network flux, possibly from explosions of sheared core fields around granule-sized inclusions of opposite-polarity flux. This scenario can be tested by Solar-B. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Moore, RL (reprint author), NASA, George C Marshall Space Flight Ctr, SD50, Huntsville, AL 35812 USA. NR 19 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-187-7 J9 ASTR SOC P PY 2004 VL 325 BP 283 EP 288 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCY30 UT WOS:000231851500035 ER PT B AU Yamauchi, Y Moore, RL Suess, ST Wang, HM Sakurai, T AF Yamauchi, Y Moore, RL Suess, ST Wang, HM Sakurai, T BE Sakurai, T Sekii, T TI Macrospicules, coronal heating, and Solar-B SO Solar-B Mission and the Forefront of Solar Physics, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 5th Solar-B Science Meeting CY NOV 12-14, 2003 CL Int House Japan, Tokyo, JAPAN HO Int House Japan ID X-RAY JETS; MAGNETIC-FLUX; H-ALPHA AB We investigated the magnetic structures of macrospicules in polar coronal holes using Ha images taken at Big Bear Solar Observatory. We found a total of 35 macrospicules. Half of the events were in the form of an erupting loop while the rest were in the form of a single-column spiked jet. These erupting loop and spiked-jet macrospicules are considered to support models in which the coronal heating and solar wind acceleration in coronal holes are driven by explosive reconnection events seated in the network. We believe that the vector magnetograph on the forthcoming Solar-B mission will provide critical clues to the mechanisms of coronal heating and solar wind acceleration by detecting magnetic activities at the base of macrospicules in the network and spicules rooted in the edges of the network flux clumps. These results are also presented in Astrophysical Journal (Yamauchi et al. 2004). C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Yamauchi, Y (reprint author), NASA, George C Marshall Space Flight Ctr, Mail Code SD50, Huntsville, AL 35812 USA. NR 19 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-187-7 J9 ASTR SOC P PY 2004 VL 325 BP 301 EP 306 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCY30 UT WOS:000231851500038 ER PT B AU Sterling, AC AF Sterling, AC BE Sakurai, T Sekii, T TI Tether-cutting energetics of a solar quiet region prominence eruption SO Solar-B Mission and the Forefront of Solar Physics, Proceedings SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 5th Solar-B Science Meeting CY NOV 12-14, 2003 CL Int House Japan, Tokyo, JAPAN HO Int House Japan ID RECONNECTION; FILAMENT; FLARES; MASS AB We study the morphology and energetics of a slowly-evolving quiet region solar prominence eruption occurring on 1999 February 8-9 in the solar north polar crown region, using Fe xv EUV 284 angstrom data from the EUV Imaging Telescope (EIT) on SOHO and soft X-ray data from the soft X-ray telescope (SXT) on Yohkoh. After rising at approximately I km s(-1) for about six hours, the prominence accelerates to a velocity of approximately 10 km s(-1) leaving behind EUV and soft X-ray loop arcades of a weak flare in its source region. These flare brightenings are consistent with "tether-cutting" reconnection occurring beneath the rising prominence, but they only become apparent about two hours after the prominence's acceleration. Nonetheless, via energetic arguments we show that tether cutting could have been occurring nearer the time of the start of the fast rise, but not yet discernible in SXT images. Therefore we are unable to assess whether tether cutting was responsible for the the prominence's acceleration from these data alone. C1 NASA, George C Marshall Space Flight Ctr, Space Sci Div SD50, Huntsville, AL 35812 USA. RP Sterling, AC (reprint author), NASA, George C Marshall Space Flight Ctr, Space Sci Div SD50, Huntsville, AL 35812 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-187-7 J9 ASTR SOC P PY 2004 VL 325 BP 395 EP 399 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BCY30 UT WOS:000231851500054 ER PT J AU Aschwanden, MJ Metcalf, TR Krucker, S Sato, J Conway, AJ Hurford, GJ Schmahl, EJ AF Aschwanden, MJ Metcalf, TR Krucker, S Sato, J Conway, AJ Hurford, GJ Schmahl, EJ TI On the photometric accuracy of RHESSI imaging and spectrosocopy SO SOLAR PHYSICS LA English DT Article ID HARD X-RAY; 20 FEBRUARY 2002; SOLAR-FLARE; CHROMOSPHERIC HEIGHT; DENSITY-MEASUREMENTS; RECONSTRUCTION; SPECTRA; TELESCOPE; IMAGES AB We compare the photometric accuracy of spectra and images in flares observed with the Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) spacecraft. We test the accuracy of the photometry by comparing the photon fluxes obtained in different energy ranges from the spectral-fitting software SPEX with those fluxes contained in the images reconstructed with the Clean, MEM, MEM-Vis, Pixon, and Forward-fit algorithms. We quantify also the background fluxes, the fidelity of source geometries, and spatial spectra reconstructed with the five image reconstruction algorithms. We investigate the effects of grid selection, pixel size, field of view, and time intervals on the quality of image reconstruction. The detailed parameters and statistics are provided in an accompanying CD-ROM and web page. We find that Forward-fit, Pixon, and Clean have a robust convergence behavior and a photometric accuracy in the order of a few percent, while MEM does not converge optimally for large degrees of freedom ( for large field of view and/or small pixel sizes), and MEM-Vis suffers in the case of time-variable sources. This comparative study documents the current status of the RHESSI spectral and imaging software, one year after launch. C1 Lockheed Martin, Ctr Adv Technol, Solar & Astrophys Lab, Dept L9 41, Palo Alto, CA 94304 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. NASA, Goddard Space Flight Ctr, Solar & Astrophys Lab, Greenbelt, MD 20770 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Aschwanden, MJ (reprint author), Lockheed Martin, Ctr Adv Technol, Solar & Astrophys Lab, Dept L9 41, Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA. EM aschwanden@lmsal.com NR 14 TC 18 Z9 18 U1 0 U2 1 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JAN PY 2004 VL 219 IS 1 BP 149 EP 157 DI 10.1023/B:SOLA.0000021801.83038.aa PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 806SQ UT WOS:000220454000010 ER PT J AU Kuzmin, RO Zabalueva, EV Mitrofanov, IG Litvak, ML Boynton, WV Saunders, RS AF Kuzmin, RO Zabalueva, EV Mitrofanov, IG Litvak, ML Boynton, WV Saunders, RS TI Regions of potential existence of free water (ice) in the near-surface Martian ground: Results from the Mars Odyssey high-energy neutron detector (HEND) SO SOLAR SYSTEM RESEARCH LA English DT Article ID VOLATILES; BEHAVIOR; HYDROGEN AB We report results of the analysis of the data on global mapping of neutron fluxes from the Martian surface, which have been obtained during the first ten months of measurements carried out by the Russian high-energy neutron detector HEND mounted aboard the American Mars Odyssey orbiter. This analysis allowed us to separate regions where free water (in ice form) prevailed in the surface layer (with a thickness of up to 2 in) of the Martian ground from regions where physically and chemically bound ground water was most likely to be the dominant form of water. The global mapping of regions with increased ice content in the ground-surface layer revealed a direct correlation with regions of polygonal terrains morphologically similar to terrestrial polygonal forms of permafrost origin. The potential content of bound water forms in the ground of circumpolar areas of the planet is also estimated. C1 VI Vernadskii Inst Geochem & Analyt Chem, Russian Acad Sci, Moscow 117975, Russia. Russian Acad Sci, Space Res Inst, Moscow 117810, Russia. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kuzmin, RO (reprint author), VI Vernadskii Inst Geochem & Analyt Chem, Russian Acad Sci, Ul Kosygina 19, Moscow 117975, Russia. NR 35 TC 14 Z9 14 U1 0 U2 2 PU MAIK NAUKA/INTERPERIODICA PI NEW YORK PA C/O KLUWER ACADEMIC-PLENUM PUBLISHERS, 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 0038-0946 J9 SOLAR SYST RES+ JI Solar Syst. Res. PD JAN-FEB PY 2004 VL 38 IS 1 BP 1 EP 11 DI 10.1023/B:SOLS.0000015150.61420.5b PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779BU UT WOS:000189276400001 ER PT S AU DeLand, MT Floyd, LE Rottman, GJ Pap, JM AF DeLand, MT Floyd, LE Rottman, GJ Pap, JM BE Pap, JM Kuhn, J Labitzke, K Shea, MA TI Status of UARS solar UV irradiance data SO SOLAR VARIABILITY AND CLIMATE CHANGE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE solar UV irradiance; UARS solar UV irradiance data; SUSIM and SOLSTICE instruments ID BACKSCATTERED ULTRAVIOLET; COMPARISON EXPERIMENT-1; SUSIM UARS; VARIABILITY; VALIDATION; CYCLE-22; MONITOR; INDEX AB Accurate measurement of solar ultraviolet (UV) irradiance variations is important for understanding both solar processes and energetic input to the Earth's atmosphere. Satellite instruments are capable of providing such data, but must correct for significant spectral and temporal response changes during the observing lifetime of the instrument. The Upper Atmospheric Research Satellite (UARS) carries two instruments dedicated to monitoring long-term solar UV irradiance: the Solar Ultraviolet Spectral Irradiance Monitor (SUSIM) and the Solar Stellar Intercomparison Experiment (SOLSTICE). Both instruments include comprehensive on-board calibration systems designed to characterize and remove response changes from the irradiance data. This paper presents the status of the SUSIM and SOLSTICE data sets. We find that both instruments produce meaningful direct estimates of solar cycle UV irradiance variations in the wavelength range 120-250 nm. Between 250 and 300 nm, the reduced magnitude of solar variability becomes comparable to the long-term calibration uncertainty. Longward of 300 nm, solar cycle irradiance variations cannot be detected. The SUSIM and SOLSTICE irradiance data sets represent the first fully calibrated solar UV irradiance data sets to cover a complete solar cycle. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Sci Syst & Applicat Inc, Lanham, MD 20706 USA. Interferometr Inc, Chantilly, VA USA. Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. NASA, Goddard Space Flight Ctr, GEST, UMBC, Greenbelt, MD 20771 USA. RP DeLand, MT (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd,Suite 400, Lanham, MD 20706 USA. EM matt_deland@sesda.com NR 27 TC 9 Z9 9 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 2 BP 243 EP 250 DI 10.1016/j.asr.2003.03.043 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAS51 UT WOS:000223368900003 ER PT S AU Thuillier, G Floyd, L Woods, TN Cebula, R Hilsenrath, E Herse, M Labs, D AF Thuillier, G Floyd, L Woods, TN Cebula, R Hilsenrath, E Herse, M Labs, D BE Pap, JM Kuhn, J Labitzke, K Shea, MA TI Solar irradiance reference spectra for two solar active levels SO SOLAR VARIABILITY AND CLIMATE CHANGE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE solar irradiance reference spectra; two solar activity levels ID MONITOR-SUSIM-EXPERIMENT; ATLAS-I MISSION; SOLSPEC SPECTROMETER; NM; UARS; RADIATION; BOARD; FLUX; MU AB Two new composite solar irradiance reference spectra extending from 0.1 to 2400 nm are constructed using recent space measurements for two distinct time periods during solar cycle 22. For wavelengths above Lyman alpha, data were gathered from the instruments placed aboard three space platforms, the ATmospheric Laboratory for Applications and Science (ATLAS), the Upper Atmosphere Research Satellite (UARS) and the EUropean Retrieval Carrier (EURECA). Below Lyman a, data from an instrument flown on rockets are used. The two spectra obtained at the time of ATLAS I and 3 missions cover about half of the total solar cycle amplitude as gauged by the Mg II and F10.7 solar indices. The accuracy of the spectra varies from 40% in the X-ray to about 3% in the UV-visible, and near IR ranges. A comparison between the total solar irradiance obtained through integration of the reference spectra and their observed values at the time of the ATLAS missions shows agreements of the order of 1%. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 CNRS, Serv Aeron, F-91370 Verrieres Le Buisson, France. Interferometr Inc, Chantilly, VA USA. Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO USA. Sci Syst & Applicat, Lanham, MD USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Thuillier, G (reprint author), CNRS, Serv Aeron, F-91370 Verrieres Le Buisson, France. EM gerard.thuillier@aerov.jussieu.fr NR 29 TC 47 Z9 49 U1 1 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 2 BP 256 EP 261 DI 10.1016/j.asr.2002.12.004 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAS51 UT WOS:000223368900005 ER PT S AU Gyori, L Baranyi, T Turmon, M Pap, JM AF Gyori, L Baranyi, T Turmon, M Pap, JM BE Pap, JM Kuhn, J Labitzke, K Shea, MA TI Study of differences between sunspot area data determined from ground-based and space-borne observations SO SOLAR VARIABILITY AND CLIMATE CHANGE SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE sunspots; solar irradiance; sunspot area measurements; solarphysics ID SOLAR IRRADIANCE VARIATIONS; ACTIVE REGIONS AB The determination of the area of sunspots is important from several points of view, e.g, in study of the evolution of sunspots and their effect on solar irradiance. Automated sunspot area measurements are now replacing time-consuming and subjective hand-made measurements. Also, terrestrial solar observations have been supplemented by observations from space. The resolution of the ground observations is limited by the seeing, while space-borne observations are limited by the size of the CCD array. The use of different data sources, as well as of different region identification algorithms, causes discrepancies in reported sunspot areas. An important task is to determine to what extent these differences can be attributed to different analysis methods and to what extent to different data. It is also important to establish the required spatial resolution of space-based images. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Heliophys Observ, Gyula Observing Stn, H-5701 Gyula, Hungary. Heliophys Observ, H-4010 Debrecen, Hungary. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Greenbelt, MD USA. RP Gyori, L (reprint author), Heliophys Observ, Gyula Observing Stn, POB 93, H-5701 Gyula, Hungary. EM ls@bekesnet.hu NR 11 TC 5 Z9 5 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2004 VL 34 IS 2 BP 269 EP 273 DI 10.1016/j.asr.2004.02.009 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAS51 UT WOS:000223368900008 ER PT S AU Ruzmaikin, A Lawrence, JK Cadavid, AC AF Ruzmaikin, A Lawrence, JK Cadavid, AC BE Pap, JM Kuhn, J Labitzke, K Shea, MA TI A simple model of solar variability influence on climate SO SOLAR VARIABILITY AND CLIMATE CHANGE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE solar variability; global climate; solar UV; cold and warm winters ID ARCTIC OSCILLATION; STRATOSPHERE; CIRCULATION; PROPAGATION; MECHANISM; OZONE; CYCLE; SUN AB We present a simple dynamic model of solar variability influence on climate, which is truncated from the stratospheric wavezonal flow interaction dynamics over a beta-plane. The model consists of three ordinary differential equations controlled by two parameters: the initial amplitude of planetary waves and the vertical gradient of the zonal wind. The changes associated with the solar UV variability, as well as with seasonal variations, are introduced as periodic modulations of the zonal wind gradient. Influence of the Quasi-Biennial Oscillation is included as a periodic change of the width of the latitudinal extent of the beta-plane. The major climate response to these changes is seen through modulation of the number of cold and warm winters. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. RP Ruzmaikin, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-506, Pasadena, CA 91109 USA. EM aruzmaik@pop.jpl.nasa.gov NR 25 TC 3 Z9 3 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 2 BP 349 EP 354 DI 10.1016/j.asr.2003.02.048 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAS51 UT WOS:000223368900021 ER PT S AU Reames, DV AF Reames, DV BE Pap, JM Kuhn, J Labitzke, K Shea, MA TI Solar energetic particle variations SO SOLAR VARIABILITY AND CLIMATE CHANGE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE solar energetic particles; solar particle events; particle acceleration; coronal mass ejections ID CORONAL MASS EJECTIONS; COSMIC-RAY EVENTS; PROTON EVENTS; ANGULAR-DISTRIBUTIONS; TEMPORAL EVOLUTION; SHOCK ACCELERATION; FLARES; INTENSITIES; TRANSPORT; SPECTRA AB In the largest solar energetic-particle (SEP) events, acceleration occurs at shock waves driven out from the Sun by coronal mass ejections (CMEs). In fact, the highest proton intensities directly measured near Earth at energies up to similar to1 GeV occur at the time of passage of shocks, which arrive about a day after the CMEs leave the Sun. CME-driven shocks expanding across magnetic fields can fill over half of the heliosphere with SEPs. Proton-generated Alfven waves trap particles near the shock for efficient acceleration but also throttle the intensities at Earth to the "streaming limit" early in the events. At high energies, particles begin to leak from the shock and the spectrum rolls downward to form an energy-spectral "knee" that can vary in energy from similar to1 MeV to similar to1 GeV in different events. All of these factors affect the radiation dose as a function of depth and latitude in the Earth's atmosphere and the risk to astronauts and equipment in space. SEP ionization of the polar atmosphere produces nitrates that precipitate to become trapped in the polar ice. Observations of nitrate deposits in ice cores reveal individual large SEP events and extend back similar to400 years. Unlike sunspots, SEP events follow the similar to80-100 year Gleissberg cycle rather faithfully and are now at a minimum in that cycle. The largest SEP event in the last 400 years appears to be related to the flare observed by Carrington in 1859, but the probability of SEP events with such large fluences falls off sharply because of the streaming limit. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Reames, DV (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM reames@milkyway.gsfc.nasa.gov NR 35 TC 25 Z9 25 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 2 BP 381 EP 390 DI 10.1016/j.asr.2003.02.046 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAS51 UT WOS:000223368900027 ER PT S AU Gopalswamy, N Nunes, S Yashiro, S Howard, RA AF Gopalswamy, N Nunes, S Yashiro, S Howard, RA BE Pap, JM Kuhn, J Labitzke, K Shea, MA TI Variability of solar eruptions during cycle 23 SO SOLAR VARIABILITY AND CLIMATE CHANGE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE solar activity; coronal mass ejections; solar cycles; solar radio bursts ID CORONAL MASS EJECTIONS; WIND SPACECRAFT; WAVES; BURSTS; ORIGIN; EARTH; RADIO AB We report on the solar cycle variation of the rate of coronal mass ejections (CMEs), their mean and median speeds, and the rate of type II radio bursts. We found that both CME rate and speed (mean and median) increased from solar minimum to maximum by factors of 10 and 2, respectively. The CME rate during solar maximum is nearly twice the rates quoted previously. Large spikes in the speed variation were due to active regions that were highly active. The poor correlation between metric and DH type II bursts is confirmed, and the difference is attributed to the different Alfven speeds in the respective source regions. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Catholic Univ Amer, Washington, DC 20064 USA. USN, Res Lab, Washington, DC 20375 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Bldg 26,Room G-1,Mailcode 682-3, Greenbelt, MD 20771 USA. EM gopals@fugee.gsfe.nasa.gov RI Gopalswamy, Nat/D-3659-2012 NR 16 TC 20 Z9 20 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 2 BP 391 EP 396 DI 10.1016/j.asr.2003.10.054 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAS51 UT WOS:000223368900028 ER PT S AU Roelof, EC Andrews, GB Liewer, PC Moses, D AF Roelof, EC Andrews, GB Liewer, PC Moses, D BE Pap, JM Kuhn, J Labitzke, K Shea, MA TI Telemachus: a mission for a polar view of solar activity SO SOLAR VARIABILITY AND CLIMATE CHANGE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE Telemachus; solar physics; solar polar flows; helioseismology; solar wind; heliospheric magnetic field; solar energetic particles AB Telemachus is a polar solar-heliospheric mission described in the current NASA Sun-Earth Connections Roadmap (2003-2028). To continue the quest begun by Ulysses, Telemachus will be injected into a 0.2 AU x 2.5 AU solar polar orbit after gravitational encounters with Venus, Earth (twice) and Jupiter, followed by a maneuver at first perihelion. With an orbital period of 1.5 years, it will pass over the solar poles at a radial distance of 0.37 AU. The behavior of solar polar flows (heretofore unobservable) will provide critical boundary conditions on the transport of solar magnetic fields. Manifestations of the global flows and fields are the solar dynamo, formation of active regions, emission of the solar wind and the heliospheric magnetic field, launching of coronal mass ejections, eruption of solar flares, acceleration of solar energetic particles, and ultimately the dynamics of the entire heliosphere. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. NASA, Jet Prop Lab, Pasadena, CA 91109 USA. USN, Res Lab, Washington, DC 20375 USA. RP Roelof, EC (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM edmond.roelof@jhuapl.edu NR 3 TC 2 Z9 2 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 2 BP 467 EP 471 DI 10.1016/j.asr.2004.01.014 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAS51 UT WOS:000223368900040 ER PT S AU Hovis, F Rhoades, M Burnham, R Force, J Schum, T Gentry, B Chen, H Li, S Hair, J Cook, A Hostetler, C AF Hovis, F Rhoades, M Burnham, R Force, J Schum, T Gentry, B Chen, H Li, S Hair, J Cook, A Hostetler, C BE Scheps, R Hoffman, HJ TI Single frequency lasers for remote sensing SO SOLID STATE LASERS XIII: TECHNOLOGY AND DEVICES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Solid State Lasers XIII CY JAN 27-29, 2004 CL San Jose, CA SP SPIE DE solid-state lasers; lidar; single-frequency lasers; diode-pumped lasers ID ND-YAG LASER; SPECTRAL-RESOLUTION LIDAR; OPERATION AB We have designed and built two versions of a space-qualifiable, single-frequency Nd:YAG laser. Our approach to frequency stabilization of the seeded oscillator is a variation of the "ramp and fire" technique. In this design, the length of the pulsed laser cavity is periodically varied until a resonance with the seed laser is optically detected. At that point the pulsed laser is fired, ensuring that it is in resonance with the seed laser. For one of the lasers the resulting single frequency pulses are amplified and frequency tripled. This system operates at 50 Hz and provides over 50 mJ/pulse of single-frequency 355 nm output. It has been integrated into the GLOW (Goddard Lidar Observatory for Winds) mobile Doppler lidar system for field testing. The second laser is a 200 Hz oscillator only system that is frequency doubled for use in the High Spectral Resolution Lidar (HSRL) system being built at NASA Langley Research Center. It provides 4 mJ of single-frequency 532 nm output that has a spectral purity of >10,000. In this paper we describe the design details, environmental testing, and integration of these lasers into their respective lidar systems. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hovis, F (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 14 TC 12 Z9 12 U1 0 U2 8 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5240-8 J9 P SOC PHOTO-OPT INS PY 2004 VL 5332 BP 263 EP 270 DI 10.1117/12.538772 PG 8 WC Materials Science, Multidisciplinary; Materials Science, Characterization & Testing; Optics; Physics, Applied SC Materials Science; Optics; Physics GA BAQ78 UT WOS:000223223800030 ER PT B AU Grugel, RN Anilkumar, AV Lee, CP AF Grugel, RN Anilkumar, AV Lee, CP BE Rappaz, M Beckermann, C Trivedi, R TI Direct observation of pore formation and bubble mobility during controlled melting and re-solidification in microgravity SO SOLIDIFICATION PROCESSES AND MICROSTRUCTURES: A SYMPOSIUM IN HONOR OF WILFRIED KURZ LA English DT Proceedings Paper CT Symposium on Solidification Processes and Microstructures in Honor of Wilfried Kurz held at the TMS Annual Meeting CY MAR 14-18, 2004 CL Charlotte, NC SP Minerals , Met & Mat Soc, Solidificat Comm, Mat Proc & Mfg Div DE solidification; porosity; GASAR; microgravity; and succinonitrile ID GASAR PROCESS AB Detailed studies on the controlled melting and subsequent re-solidification of succinonitrile were conducted in the microgravity environment aboard the International Space Station (ISS) using the PFMI apparatus (Pore Formation and Mobility Investigation) located in the ISS' glovebox facility (GBX). Samples were initially prepared on ground by filling glass tubes, I cm ID and approximately 30 cm in length, with pure succinonitrile (SCN) under 450 millibar of nitrogen. During Space processing, experimental parameters like temperature gradient and translation speed, for melting and solidification, were remotely monitored and controlled from the ground Telescience Center (TSC) at the Marshall Space Flight Center. Real time visualization during controlled melting revealed bubbles of different sizes initiating at the solid/liquid interface, and traveling up the temperature gradient ahead of them. Subsequent controlled re-solidification of the SCN revealed the details of porosity formation and evolution. A preliminary analysis of the melt back and re-solidification and its implications to future microgravity materials processing is presented and discussed. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Grugel, RN (reprint author), NASA, George C Marshall Space Flight Ctr, SD46, Huntsville, AL 35812 USA. NR 5 TC 1 Z9 1 U1 1 U2 2 PU MINERALS, METALS & MATERIALS SOC PI WARRENDALE PA 184 THORN HILL RD, WARRENDALE, PA 15086-7514 USA BN 0-87339-572-7 PY 2004 BP 111 EP 116 PG 6 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA BY80J UT WOS:000189466900013 ER PT J AU Fisher, T Galyardt, D AF Fisher, T Galyardt, D TI Getting the rover to Mars in working order SO SOUND AND VIBRATION LA English DT Editorial Material C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. LDS Dactron, Fremont, CA USA. RP Fisher, T (reprint author), CALTECH, Jet Propuls Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ACOUSTICAL PUBL INC PI BAY VILLAGE PA 27101 E OVIATT RD, PO BOX 40416, BAY VILLAGE, OH 44140 USA SN 1541-0161 J9 SOUND VIB JI Sound Vib. PD JAN PY 2004 VL 38 IS 1 BP 6 EP + PG 2 WC Acoustics; Engineering, Mechanical; Mechanics SC Acoustics; Engineering; Mechanics GA 767PQ UT WOS:000188460000002 ER PT S AU Thompson, SL AF Thompson, SL BE Bainum, PM Furong, L Nakajima, T TI KUTESat sensing of radiation energies, fluxes and exposure geometry in the space environment using a RADFET array SO SPACE ACTIVITIES AND COOPERATION CONTRIBUTING TO ALL PACIFIC BASIN COUNTRIES SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT 10th International Space Conference of Pacific Basin Societies CY DEC 10-12, 2003 CL Tokyo, JAPAN SP Amer Astronaut Soc, Chinese Soc Astronaut, Japanese Rocket Soc AB The Kansas Universities Technology Evaluation Satellite (KUTESat) program will design, test, and build a small pico-class satellite. KUTESat will employ multiple Radiation Field Effect Transistors (RADFET) dosimeters placed throughout the structure, measuring the ionizing radiation in and around the satellite. The critical objective of the KUTESat payload subsystem is to demonstrate how an array of multiple RADFET sensors not only supplies a total dose measurement in real time but also retains a permanent record of the ionizing radiation exposure effects after it has been electronically interrogated to determine the total ionizing radiation exposure. The RADFET can be designed and configured to monitor ionizing radiation for a broad range of applications, such as performing radiation dose measurements without applied electrical power or remote sensing in locations with limited access. The radiation dose measurements will offer a convenient method for continuously monitoring the total radiation dose. The RADFETs will be utilized in an array of four dosimeters strategically placed at the four corners of the satellite to be used to measure the space environment, including the radiation energies, fluxes, and exposure geometry. The use of RADFET dosimeters in an array will be advantageous, adding to the overall scientific benefits with increased observation ability and decreased size and cost constraints. They also are beneficial for measuring radiation seen by individual satellite instruments. The use of these small RADFET dosimeters have many advantages such as size, cost, power requirements, and simple operation, and, most importantly, better data acquisition. Also discussed will be drawbacks to using an array of RADFETs in measuring the space environment. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Thompson, SL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-87703-510-5 J9 ADV ASTRONAUT SCI PY 2004 VL 117 BP 99 EP 106 PG 8 WC Engineering, Aerospace SC Engineering GA BBD58 UT WOS:000225038800014 ER PT S AU Wilson, K Troy, A Srinivasan, M Platt, B Vilnrotter, V Wright, M Garkanian, V Heinmati, H AF Wilson, K Troy, A Srinivasan, M Platt, B Vilnrotter, V Wright, M Garkanian, V Heinmati, H BE Bainum, PM Furong, L Nakajima, T TI Daytime adaptive optics for deep space communications SO SPACE ACTIVITIES AND COOPERATION CONTRIBUTING TO ALL PACIFIC BASIN COUNTRIES SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT 10th International Space Conference of Pacific Basin Societies CY DEC 10-12, 2003 CL Tokyo, JAPAN SP Amer Astronaut Soc, Chinese Soc Astronaut, Japanese Rocket Soc AB The deep space optical communications subsystem offers a higher bandwidth communications link in smaller size, lower mass, and lower power consumption subsystem than does RF. To demonstrate the benefit of this technology to deep space communications NASA plans to launch an optical telecommunications package on the 2009 Mars Telecommunications Orbiter spacecraft. Current performance goals are 30-Mbps from opposition, and 1-Mbps near conjunction (similar to3 degrees Sun-Earth-Probe angle). Yet, near conjunction the background noise from the day sky will degrade the performance of the optical link. Spectral and spatial filtering and higher modulation formats can mitigate the effects of background sky. Narrowband spectral filters can result in loss of link margin, and higher modulation formats require higher transmitted peak powers. In contrast, spatial filtering at the receiver has the potential of being lossless while providing the required sky background rejection. Adaptive optics techniques can correct wave front aberrations caused by atmospheric turbulence and enable near-diffraction-limited performance of the receiving telescope. Such performance facilitates spatial filtering, and allows the receiver field-of-view and hence the noise from the sky background to be reduced. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Wilson, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-87703-510-5 J9 ADV ASTRONAUT SCI PY 2004 VL 117 BP 481 EP 492 PG 12 WC Engineering, Aerospace SC Engineering GA BBD58 UT WOS:000225038800048 ER PT S AU Vilnrotter, V Lau, CW Srinivasan, M Mukai, R Andrews, K AF Vilnrotter, V Lau, CW Srinivasan, M Mukai, R Andrews, K BE Bainum, PM Furong, L Nakajima, T TI Optical array receiver for deep-space communication through atmospheric turbulence SO SPACE ACTIVITIES AND COOPERATION CONTRIBUTING TO ALL PACIFIC BASIN COUNTRIES SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT 10th International Space Conference of Pacific Basin Societies CY DEC 10-12, 2003 CL Tokyo, JAPAN SP Amer Astronaut Soc, Chinese Soc Astronaut, Japanese Rocket Soc AB The theoretical foundations of an optical array receiver consisting of small telescopes are developed and analyzed. It is shown that optical array receivers can be designed to perform as well as a single-aperture receiver on the ground, while enjoying significant advantages in terms of operational reliability, ease of future expansion to achieve greater capacity, and further advantages in terms of cost and implementation due to the highly parallel architecture inherent in the array design. Optical array receivers for deep-space communications applications are analyzed using the accepted modal techniques for background radiation; however, the signal fields are represented using a novel aperture-plane expansion that takes into account the characteristics of atmospheric turbulence. it is shown that for ground-based reception the number of array elements can be increased without suffering any performance degradation, as long as the telescope diameters exceed the coherence-length of the atmosphere. Maximum likelihood detection of turbulence-degraded signal fields, using an array of telescopes, each equipped with its own focal-plane detector array to mitigate turbulence effects, is developed for the case of pulse-position modulated signals observed in the presence of background radiation. The performance of optical array receivers is compared to single-aperture receivers with diameters ranging from 4 to 8 meters, both in the presence of turbulence and in a turbulence-free environment such as space: it is shown that without atmospheric turbulence to break up the signal, single-aperture receivers outperform receiver arrays whenever significant background radiation is present. However, for ground-based reception of deep-space signals, the number of array elements can be as great as several thousand without incurring any performance degradation relative to a large single-aperture receiver. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vilnrotter, V (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-87703-510-5 J9 ADV ASTRONAUT SCI PY 2004 VL 117 BP 493 EP 510 PG 18 WC Engineering, Aerospace SC Engineering GA BBD58 UT WOS:000225038800049 ER PT S AU Lee, MC Israelsson, UE AF Lee, MC Israelsson, UE BE Bainum, PM Furong, L Nakajima, T TI Fundamental physics research aboard the International Space Station SO SPACE ACTIVITIES AND COOPERATION CONTRIBUTING TO ALL PACIFIC BASIN COUNTRIES SE ADVANCES IN THE ASTRONAUTICAL SCIENCES LA English DT Proceedings Paper CT 10th International Space Conference of Pacific Basin Societies CY DEC 10-12, 2003 CL Tokyo, JAPAN SP Amer Astronaut Soc, Chinese Soc Astronaut, Japanese Rocket Soc AB NASA's research plans aboard the International Space Station (ISS) are discussed. Experiments in low temperature physics and atomic physics are planned to commence in early 2008. Experiments in gravitational physics are planned to begin also in 2008. A low temperature microgravity physics facility is under development for the low temperature and gravitation experiments. The facility provides a 2 K environment for two instruments and an experimental lifetime of 4.5 months. Each instrument will be capable of accomplishing a primary investigation and one or more guest investigations. Experiments on the first flight will study non-equilibrium phenomena near the superfluid 4He transition. The first couple of atomic physics experiments will take advantage of the free-fall environment to operate laser cooled atomic fountain clocks with 10 to 100 times better performance than any Earth based clock. These clocks will be used for experimental studies in General and Special Relativity. Flight definition experiment studies are underway by investigators studying Bose Einstein Condensates and use of atom interferometers as potential future flight candidates. C1 NASA, Washington, DC 20546 USA. RP Lee, MC (reprint author), NASA, Mail Code UG, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 0-87703-510-5 J9 ADV ASTRONAUT SCI PY 2004 VL 117 BP 807 EP 808 PG 2 WC Engineering, Aerospace SC Engineering GA BBD58 UT WOS:000225038800077 ER PT S AU Stansbery, EG Foster, JL AF Stansbery, EG Foster, JL BE Flury, W Klinkrad, H TI Monitoring the low earth orbit debris environment over an 11-year solar cycle SO SPACE DEBRIS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space debris; low earth orbit debris; 11-year solar cycle; monitoring AB Orbital debris is a concern for all space faring nations. Prior to 1990, there were no statistically significant measurements of the debris environment for debris sizes below 10 cm diameter. Late in that year, NASA/Johnson Space Center began using the Haystack long range imaging radar to statistically sample the low earth orbit (LEO) debris environment for debris sizes as small as 0.5 cm diameter. These measurements have continued since that date. Models of the LEO debris environment predict a change in the debris flux due to solar activity. High solar activity heats the earth's atmosphere causing it to expand creating an increased atmospheric drag which causes debris to reenter the earth's atmosphere at a higher rate thereby depleting the population at low altitudes. This paper will summarize the Haystack measurements over a complete 11-year solar cycle. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. GB Tech, Houston, TX 77058 USA. RP Stansbery, EG (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Rd 1, Houston, TX 77058 USA. EM eugene.g.stansbery@nasa.gov NR 4 TC 0 Z9 0 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 5 SI 2004 BP 878 EP 883 DI 10.1016/j.asr.2003.02.021 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAU50 UT WOS:000223619400003 ER PT S AU Africano, JL Stansbery, EG Kervin, PW AF Africano, JL Stansbery, EG Kervin, PW BE Flury, W Klinkrad, H TI The optical orbital debris measurement program at NASA and AMOS SO SPACE DEBRIS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space debris; optical observations; AMOS AB The National Aeronautics and Space Administration (NASA) has been making optical observations of the Low Earth Orbit (LEO) and the Geosynchronous Earth Orbit (GEO) orbital debris environment. NASA operates two telescopes located near Cloudcroft, NM that obtain these observations. The 3.0 m Liquid Mirror Telescope (LMT) is used for LEO observations and the 0.32 m Charged Coupled Device (CCD) Debris Telescope (CDT) is used for GEO observations. The optical observations are being used to help characterize the debris environment in LEO and GEO and to assist in the modeling projections generated by NASA. NASA is also collaborating with the Air Force Maui Optical and Supercomputing Site (AMOS), which is located at the 10,000 foot summit of Haleakala on the island of Maui. There are three main observational programs at AMOS. There is an imaging program utilizing the 3.67 m telescope adaptive optics system to image objects that have had anomalous events or breakups. There is a spectroscopic program utilizing spectrographs on the 3.67 and 1.6 m telescopes to determine surface materials. There is also a program utilizing instrumentation on the 3.67 m telescope to determine the albedo of objects based upon simultaneous visible and thermal IR photometry. AMOS is also obtaining statistical observations of the GEO debris environment supporting NASA and the Inter-Agency Space Debris Coordination Committee (IADC) activities using the Near-Earth Asteroid Tracking (NEAT) camera on the 1.2 m telescope, In addition, a renovated Baker-Nunn telescope is available for observations. Results from these observation programs will be presented, as well as future plans. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Boeing Co, Colorado Springs, CO 80910 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. AFRL, Directed Energy Directorate, Detachment 15, Kihei, HI 96753 USA. RP Africano, JL (reprint author), Boeing Co, 1250 Acad Pk Loop,Suite 110, Colorado Springs, CO 80910 USA. EM john.l.africano@boeing.com NR 13 TC 10 Z9 15 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 5 SI 2004 BP 892 EP 900 DI 10.1016/j.asr.2003.02.022 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAU50 UT WOS:000223619400005 ER PT S AU Johnson, NL AF Johnson, NL BE Flury, W Klinkrad, H TI Environmentally-induced debris sources SO SPACE DEBRIS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space debris; environmentally-induced debris sources AB Resident spacecraft and rocket bodies are known to spontaneously produce large fragments (>10 cm), usually released at low velocities in small numbers and normally exhibiting large area-to-mass ratios. Potential causes of these anomalous events, which are not related to the more dramatic satellite breakups, include material degradation due to environmental stresses and impact by small natural or man-made particles. An examination of known and previously undocumented anomalous events was undertaken to gain better insight into the frequency of such events and the resultant consequences to the overall orbital debris environment. Some space vehicle types, e.g., US Transit spacecraft and former Soviet Vostok orbital stages, demonstrate a propensity for debris generation, while other satellite designs appear less vulnerable. Some satellites are known to produce numerous debris over a period of many years, and the debris exhibit wide-ranging characteristics. It is concluded that such debris currently account for a small portion of the large orbital debris population, but the number of smaller debris cannot yet be estimated. Better identification and analysis of anomalous events might indicate the degree to which small particle impacts are responsible and whether the frequency of anomalous events in given orbital regimes can be used to monitor changes in the small particle population. Modifications to some satellite designs might mitigate anomalous event debris generation. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Lyndon B Johnson Space Ctr, Orbital Debris Program Off, Houston, TX 77058 USA. RP Johnson, NL (reprint author), NASA, Lyndon B Johnson Space Ctr, Orbital Debris Program Off, Mail Code SX, Houston, TX 77058 USA. EM nicholas.l.johnson1@jsc.nasa.gov NR 1 TC 1 Z9 2 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 5 SI 2004 BP 993 EP 999 DI 10.1016/j.asr.2003.02.029 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAU50 UT WOS:000223619400020 ER PT S AU Lambour, R Rajan, N Morgan, T Kupiec, I Stansbery, E AF Lambour, R Rajan, N Morgan, T Kupiec, I Stansbery, E BE Flury, W Klinkrad, H TI Assessment of orbital debris size estimation from radar cross-section measurements SO SPACE DEBRIS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space debris; assessment of orbital debris size estimation; radar cross-section measurements; space surveillance network AB MIT Lincoln Laboratory has conducted a measurement program for man-made orbital debris since 1991 in response to NASA's need to characterize the orbital debris population and facilitate manned spaceflight activities. The primary sensors used in that effort are the Haystack and Haystack auxiliary (HAX) radars located at the Lincoln space surveillance complex (LSSC) in Westford, Massachusetts. This paper will describe the results from a new effort conducted at LSSC, the objective of which is to assess the variability in NASA's current procedure for determination of size from radar data. RCS data have been acquired on 39 NASA-selected resident space objects (RSO). Results are also compared to the size estimates from the FPS-85 radar, an asset of the Space Surveillance Network. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 MIT, Lincoln Lab, Lexington, MA 02420 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Lambour, R (reprint author), MIT, Lincoln Lab, 244 Wood St, Lexington, MA 02420 USA. EM lambour@ll.mit.edu NR 5 TC 6 Z9 13 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 5 SI 2004 BP 1013 EP 1020 DI 10.1016/j.asr.2003.02.043 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAU50 UT WOS:000223619400023 ER PT S AU Jorgensen, K Africano, J Hamada, K Stansbery, E Sydney, P Kervin, P AF Jorgensen, K Africano, J Hamada, K Stansbery, E Sydney, P Kervin, P BE Flury, W Klinkrad, H TI Physical properties of orbital debris from spectroscopic observations SO SPACE DEBRIS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space debris; spectroscopic observations; low-earth orbit; geosynchronous orbit AB Currently, certain physical properties, such as material type and albedo, of orbital debris are assumed when used to determine the size of the objects. A study to ascertain whether or not the assumed values are valid has begun using reflectance spectroscopy as a means of determining the material type of the object. What appears to some as a squiggly line is actually the reflectance of sunlight from the object. By comparing the location, depth, and width of the absorption features on the squiggly lines, the material type of the debris object is identified. Once the material type is known, the albedo of the object can be determined. This paper discusses the results from observations of large rocket bodies and satellites in both lower and geosynchronous Earth orbits (LEO and GEO, respectively) taken at the air force maui optical and supercomputing (AMOS) site located in Maui, Hawaii. Using the 1.6-m telescope and a spectral range of 0.3-0.9 mum, differences between rocket bodies of different types and launch dates, as well as satellites of different types and launch dates are determined. Variations seen in the squiggle lines are due to colors of paint, space weathering, and for the satellites, orientation and size of the solar panels. Future direction of the project will be discussed as well as plans for future observations. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Boeing Co, Colorado Springs, CO 80910 USA. AFRL, Directed Energy Directorate, Detachment 15, Kihei, HI 96753 USA. RP Jorgensen, K (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 Nasa Rd 1,Mail Code SX, Houston, TX 77058 USA. EM kira.jorgensen1@jsc.nasa.gov NR 6 TC 5 Z9 7 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 5 SI 2004 BP 1021 EP 1025 DI 10.1016/j.asr.2003.02.031 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAU50 UT WOS:000223619400024 ER PT S AU Mrozinski, RB Mendeck, GF Cutri-Kohart, RM AF Mrozinski, RB Mendeck, GF Cutri-Kohart, RM BE Flury, W Klinkrad, H TI Overview of entry risk predictions SO SPACE DEBRIS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space debris; entry risk predictions; satellite disposal AB This paper discusses many aspects of "casualty expectation", defined as the expected number of people suffering death or injury due to a spacecraft entry event, normally used when planning the end-of-life disposal of satellites. United States guidelines state a disposal via atmospheric entry should be controlled rather than uncontrolled whenever casualty expectation estimates exceed a specified limit. Since this guideline can have serious impacts on the cost, lifetime, and even the mission and functionality of a satellite, it is critical that casualty expectation (E-c) be estimated well, and decision-makers understand all assumptions and limitations inherent in the result. This paper begins with an overview of relevant United States guidelines. The equation the space industry typically uses to estimate E-c is presented, along with its sensitivity to typical assumptions, models, and initial condition uncertainties. An alternate quantity is introduced, called "probability of casualty", or P-c Two examples are given of both E-c and P-c estimations. Because E-c and P-c are dependent on variables with significant uncertainty, confidence in the estimates themselves can be challenged. Fortunately, a precise value is rarely needed. Results typically are well above or well below guideline limits to the extent that even if all variable values were certain, the resulting recommended course of action would not change. E-c and P-c are then ideal to use in relative analyses using a standard tool to assess compliance with guidelines. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Mrozinski, RB (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code DM4,2101 NASA Rd 1, Houston, TX 77058 USA. EM richard.b.mrozinski@nasa.gov NR 8 TC 1 Z9 1 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 5 SI 2004 BP 1044 EP 1048 DI 10.1016/j.asr.2003.02.038 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAU50 UT WOS:000223619400027 ER PT S AU Rochelle, WC Marichalar, JJ Johnson, NL AF Rochelle, WC Marichalar, JJ Johnson, NL BE Flury, W Klinkrad, H TI Analysis of reentry survivability of UARS spacecraft SO SPACE DEBRIS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE reentry; UARS; orbital debris AB An analysis of reentry survivability of the NASA Goddard space flight center (GSFC) upper atmosphere research satellite (UARS) was performed by Lockheed Martin space operations (LMSO), Houston, TX. The objective of this study was to use the NASA Lyndon B. Johnson space center (JSC)/LMSO object reentry survival analysis tool (ORSAT) to investigate reentry, breakup, demise, and impact of approximately 160 specific components of the UARS. This paper contains descriptions of the UARS spacecraft as modeled by ORSAT, method of approach (including assumptions), and results obtained. The analysis showed that about 150 component types, including the parent body, will demise, and 12 types (26 counting multiple components) will survive. The components that survive produce a debris casualty area of 22 m(2), a surviving mass of 532 kg, a casualty risk of 1:2800, and a debris footprint length of nearly 800 km. The 22 m(2) debris casualty area reflects the results of a parametric assessment; otherwise the casualty area would have been larger. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Lockheed Martin Space Operat, Houston, TX 77058 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Rochelle, WC (reprint author), Lockheed Martin Space Operat, 2400 NASA Rd 1,Mail Code C87, Houston, TX 77058 USA. EM bill.rochelle@lmco.com NR 10 TC 8 Z9 8 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 5 SI 2004 BP 1049 EP 1054 DI 10.1016/j.asr.2003.01.011 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAU50 UT WOS:000223619400028 ER PT S AU Christiansen, EL Hyde, JL Bernhard, RP AF Christiansen, EL Hyde, JL Bernhard, RP BE Flury, W Klinkrad, H TI Space shuttle debris and meteoroid impacts SO SPACE DEBRIS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space debris; space shuttle; meteor impact; debris impacts ID ORBITAL DEBRIS AB This paper describes observations and analyses of meteoroid and debris impact damage to the Space Shuttle Orbiter over the past decade. Since 1992, NASA Space Shuttle Orbiter post-flight inspection procedures have been altered to allow systematic identification and sampling of meteoroid/debris impacts in selected areas of the vehicle. These areas include the crew module windows and radiator panels that line the interior of the payload bay doors. In addition, other significant impact damage is identified and sampled on other critical surfaces or exposed structures such as wing leading-edge panels, external thermal-protection materials, radiator interconnect lines, and Ku-band antenna components. Samples of the impact damage are obtained and subjected to scanning electron microscope energy dispersive X-ray analysis to determine elemental composition of impactor materials recovered from the impact site. Based on these results, the source of the impact damage is categorized as meteoroid or debris, and debris particle types are identified. Historical trends indicate a large variability in debris impact rates from mission-to-mission with higher impact rates than average occurring more regularly since 1998. Predictions of post-flight damage are compared to observed damage using BUMPER code and as-flown attitude timelines. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA Johnson Space Ctr, Houston, TX 77058 USA. Lockheed Martin Space Operat, Houston, TX 77058 USA. RP Christiansen, EL (reprint author), NASA Johnson Space Ctr, Mail Code SX2, Houston, TX 77058 USA. EM eric.l.christiansen@nasa.gov NR 15 TC 9 Z9 11 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 5 SI 2004 BP 1097 EP 1103 DI 10.1016/j.asr.2003.12.008 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAU50 UT WOS:000223619400035 ER PT S AU Evans, S Lewis, H Williamsen, J Evans, H Bohl, W AF Evans, S Lewis, H Williamsen, J Evans, H Bohl, W BE Flury, W Klinkrad, H TI Bounding the risk of crew loss following orbital debris penetration of the International Space Station at assembly stages 1J and 1E SO SPACE DEBRIS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space debris; International Space Station; assembly stages 1J and 1E; manned spacecraft crew survivability code AB Orbital debris impacts on the International Space Station occur frequently. To date, none of the impacting particles has been large enough to penetrate manned pressurized volumes. We used the Manned Spacecraft Crew Survivability code to evaluate the risk to crew of penetrations of pressurized modules at two assembly stages: after Flight 1J, when the pressurized elements of Kibo, the Japanese Experiment Module, are present, and after Flight 1E, when the European Columbus Module is present. Our code is a Monte-Carlo simulation of impacts on the Station that considers several potential event types that could lead to crew loss. Among the statistics tabulated by the program is the probability of death of one or more crew members in the event of a penetration, expressed as the risk factor, R. This risk factor is dependent on details of crew operations during both ordinary circumstances and decompression emergencies, as well as on details of internal module configurations. We conducted trade studies considering these procedure and configuration details to determine the bounds on R at the 1J and 1E stages in the assembly sequence. Here we compare the R-factor bounds, and procedures could that reduce R at these stages. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Denver, Res Inst, Denver, CO 80208 USA. RP Evans, S (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM Steven.W.Evans@nasa.gov NR 9 TC 1 Z9 1 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 5 SI 2004 BP 1104 EP 1108 DI 10.1016/j.asr.2003.01.014 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAU50 UT WOS:000223619400036 PM 15739282 ER PT S AU Seitzer, P Smith, R Africano, J Jorgensen, K Stansbery, E Monet, D AF Seitzer, P Smith, R Africano, J Jorgensen, K Stansbery, E Monet, D BE Flury, W Klinkrad, H TI MODEST observations of space debris at geosynchronous orbit SO SPACE DEBRIS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space debris; geosynchronous orbit; MODEST observation AB Results will be presented from a new NASA optical survey of objects at geosynchronous orbit (GEO). The goal is to determine the total population of debris objects at GEO to as small a limiting size as possible. This survey uses the University of Michigan's 0.6/0.9 m Schmidt telescope Michigan Orbital Debris Survey Telescope (MODEST). Located at Cerro Tololo Inter-American Observatory in Chile, the system is equipped with a scanning CCD with a field of view of 1.3degrees x 1.3degrees, and can detect objects smaller than 10 cm diameter at GEO, Each night the telescope scans a strip of sky 110degrees long x 1.3degrees high, Up to eight independent detections are made of each candidate GEO object in a 5 min time span, yielding measurements of brightness, position, and angular motion. Since February 2001, an extensive series of observations of the GEO regime has been carried out with this system, revealing a considerable population of objects smaller than 1 m in diameter. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. CALTECH, Pasadena, CA 91125 USA. Boeing Co, Maui, HI 96753 USA. NASA, JSC, Houston, TX 77058 USA. US Naval Observ, Flagstaff Stn, Flagstaff, AZ 86002 USA. RP Seitzer, P (reprint author), Univ Michigan, Dept Astron, 818 Dennison Bldg, Ann Arbor, MI 48109 USA. EM pseitzer@umich.edu NR 3 TC 9 Z9 14 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 5 SI 2004 BP 1139 EP 1142 DI 10.1016/j.asr.2003.12.009 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAU50 UT WOS:000223619400042 ER PT S AU Opiela, JN Liou, JC Stansbery, EG AF Opiela, JN Liou, JC Stansbery, EG BE Flury, W Klinkrad, H TI A proposed in situ debris measurement in GEO SO SPACE DEBRIS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space debris; geosynchronous orbit; polyvinylidene fluoride material ID ORBITING ARGOS SPACECRAFT; SPADUS INSTRUMENT ABOARD; COSMIC DUST; PARTICLES; CLOUD AB In situ measurements are required to characterize the particle environment below the threshold of remote sensors. Ground-based geosynchronous Earth orbit (GEO) optical measurements in general have been limited to objects greater than about 15 cm. It is highly unlikely that any ground-based telescope can detect GEO debris smaller than 1 cm. Firsthand knowledge of the untrackable debris population is critical to GEO environment definition, if we are to control that environment. The current, general debris mitigation and protection measures may be applied to GEO satellites, but characterizing the GEO debris environment (flux, size distribution, orbit distribution, sources) will also allow measures tailored specifically for that environment. Two specific issues need to be addressed for any effective in situ measurements in GEO: detector type and potential contamination from interplanetary and interstellar dust. In this paper, we will discuss why the polyvinylidene fluoride (PVDF) material makes an ideal GEO debris detector. We will also show that impacts from debris, interplanetary dust, and interstellar dust are very different in many ways (size, impact speed, flux, etc.). Debris impacts can be easily distinguished from other impacts. Published by Elsevier Ltd on behalf of COSPAR. C1 Lockheed Martin Space Operat, Houston, TX 77058 USA. NASA Johnson Space Ctr, Houston, TX 77058 USA. RP Opiela, JN (reprint author), Lockheed Martin Space Operat, 2400 NASA Rd 1, Houston, TX 77058 USA. EM john.n.opiela@jsc.nasa.gov NR 14 TC 0 Z9 1 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 5 SI 2004 BP 1150 EP 1154 DI 10.1016/j.asr.2003.02.034 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAU50 UT WOS:000223619400044 ER PT S AU Matney, MJ Stansbery, E Africano, J Jarvis, K Jorgensen, K Thumm, T AF Matney, MJ Stansbery, E Africano, J Jarvis, K Jorgensen, K Thumm, T BE Flury, W Klinkrad, H TI Extracting GEO orbit populations from optical surveys SO SPACE DEBRIS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space debris; geosynchronous orbit; optical surveys AB A number of optical instruments are involved in making systematic surveys of the geosynchronous Earth orbit (GEO) region. Because of the limited field of view of an optical instrument, it is impossible at any one time to observe objects in all orbit planes in the region. Therefore, the orbit distributions seen are biased relative to the true populations of orbits in space. Because the observations represent a statistical sample of the population, statistical variations must be accounted for. The full procedure to remove the biases is extremely difficult with the limited orbit data measured because objects in GEO can have a wide spectrum of possible orbits. The measurements themselves are often insufficient to distinguish whether the object is in an elliptical or circular orbit. However, by limiting the range of possible orbit types it is possible to simplify the problem and obtain reasonable orbit distribution estimates. These distributions can in turn be used to identify interesting groupings of objects that may be part of an unrecognized breakup event. This paper describes the methods used to remove observational biases, and presents estimates of orbit distributions of uncatalogued objects at GEO visible to the instruments. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Lockheed Martin Sp Operat, Houston, TX 77058 USA. NASA Johnson Space Ctr, Houston, TX 77058 USA. Boeing Corp, Colorado Springs, CO 80910 USA. RP Matney, MJ (reprint author), Lockheed Martin Sp Operat, 2400 NASA Rd 1,Mail Code C104, Houston, TX 77058 USA. EM mark.matney-1@nasa.gov NR 6 TC 6 Z9 9 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 5 SI 2004 BP 1160 EP 1165 DI 10.1016/j.asr.2003.11.014 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAU50 UT WOS:000223619400046 ER PT S AU Johnson, NL AF Johnson, NL BE Bendisch, J TI Revisions to NASA policy directive and safety standard for orbital debris mitigation SO SPACE DEBRIS AND SPACE TRAFFIC MANAGEMENT SYMPOSIUM 2003 SE SCIENCE AND TECHNOLOGY SERIES LA English DT Proceedings Paper CT Symposium on Space Debris and Space Traffic Management CY SEP 29-OCT 03, 2003 CL Bremen, GERMANY SP Int Acad Astronaut AB NASA Policy Directive (NPD) 8710.3, NASA Policy for Limiting Orbital Debris Generation, was revised as NPD 8710.3A in January 2003, reflecting the growing importance of orbital debris mitigation and a need to identify and to expand the responsibilities of various organizations within NASA. The agency has acquired considerable experience in assessing orbital debris potential for a large number of human space flight and robotic satellite missions, and this experience indicated that more explicit guidance to NASA enterprises and centers was necessary to ensure that orbital debris mitigation issues were handled in an efficient and comprehensive manner. Work is now underway to revise the 1995 NASA Safety Standard (NSS) 1740.14, Guidelines and Assessment Procedures for Limiting Orbital Debris, to update the document and to correct deficiencies and areas of ambiguity. Although the technical elements will remain largely unchanged, some guidelines will be improved, and the document will be more consistent with the U.S. Government Orbital Debris Mitigation Standard Practices and other national and international guidelines. An important lesson in the management of orbital debris learned by NASA during the past eight years is that an effective orbital debris mitigation program requires a detailed, formal process which is supported by all agency organizations. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Johnson, NL (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 7 TC 1 Z9 1 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 0278-4017 BN 0-87703-517-2 J9 SCI TECH PY 2004 VL 109 BP 493 EP 501 PG 9 WC Engineering, Aerospace; Geosciences, Multidisciplinary SC Engineering; Geology GA BBP89 UT WOS:000226974800034 ER PT S AU Johnson, NL AF Johnson, NL BE Bendisch, J TI Space traffic management concepts and practices SO SPACE DEBRIS AND SPACE TRAFFIC MANAGEMENT SYMPOSIUM 2003 SE SCIENCE AND TECHNOLOGY SERIES LA English DT Proceedings Paper CT Symposium on Space Debris and Space Traffic Management CY SEP 29-OCT 03, 2003 CL Bremen, GERMANY SP Int Acad Astronaut AB Concepts of space traffic management have been discussed for many years with little progress to date due both to the complexity of the issue and to a perceived lack of urgency. Although a renewed interest in the subject has arisen in some corners of the aerospace community, the challenges of space traffic management remain unchanged. Perhaps the greatest challenge is reaching a consensus on the definition of space traffic management and its objectives. In the simplest terms, space traffic management should promote physical and electromagnetic non-interference among the multitude of operational space systems. However, contrary to popular belief, air and ground traffic control concepts and techniques offer few analogies applicable to the space environment. The value of a space traffic management system must weigh the historical and legally entrenched concept of the freedom of operation in near-Earth orbit against the potential benefits of a new regulatory regime. Most space-faring nations do not yet exert control over the selection of orbital parameters for new space systems within their own countries, much less in an international context. The prospects for such intrusive space traffic management in the foreseeable future are not bright. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Johnson, NL (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 13 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 0278-4017 BN 0-87703-517-2 J9 SCI TECH PY 2004 VL 109 BP 505 EP 514 PG 10 WC Engineering, Aerospace; Geosciences, Multidisciplinary SC Engineering; Geology GA BBP89 UT WOS:000226974800035 ER PT S AU Hublitz, I Henninger, DL Drake, BG Eckart, P AF Hublitz, I Henninger, DL Drake, BG Eckart, P BE Henninger, DL Drysdale, AE Kondyurin, AV TI Engineering concepts for inflatable Mars surface greenhouses SO SPACE LIFE SCIENCES: LIFE SUPPORT SYSTEMS AND BIOLOGICAL SYSTEMS UNDER INFLUENCE OF PHYSICAL FACTORS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE Mars surface greenhouse; life support systems; bioregenerative life support systems; space life science AB A major challenge of designing a bioregenerative life support system for Mars is the reduction of the mass, volume, power, thermal and crew-time requirements. Structural mass of the greenhouse could be saved by operating the greenhouse at low atmospheric pressure. This paper investigates the feasibility of this concept. The method of equivalent system mass is used to compare greenhouses operated at high atmospheric pressure to greenhouses operated at low pressure for three different lighting methods: natural, artificial and hybrid lighting. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Florida, Dept Agr & Biol Engn, Gainesville, FL 32611 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. McKinsey & Co Inc, D-80538 Munich, Germany. RP Hublitz, I (reprint author), Univ Florida, Dept Agr & Biol Engn, POB 110570, Gainesville, FL 32611 USA. EM inka@ufl.edu RI Kondyurin, Alexey/B-9580-2011 OI Kondyurin, Alexey/0000-0002-8837-9734 NR 12 TC 7 Z9 9 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 7 BP 1546 EP 1551 DI 10.1016/j.asr.2004.06.002 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BBH90 UT WOS:000225592800011 PM 15846884 ER PT S AU Berkovich, YA Chetirkin, PV Wheeler, RM Sager, JC AF Berkovich, YA Chetirkin, PV Wheeler, RM Sager, JC BE Henninger, DL Drysdale, AE Kondyurin, AV TI Evaluating and optimizing horticultural regimes in space plant growth facilities SO SPACE LIFE SCIENCES: LIFE SUPPORT SYSTEMS AND BIOLOGICAL SYSTEMS UNDER INFLUENCE OF PHYSICAL FACTORS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE optimization criterion; space plant growth facilities; horticultural regimes ID YIELD AB In designing innovative space plant growth facilities (SPGF) for long duration space flight, various limitations must be addressed including onboard resources: volume, energy consumption, heat transfer and crew labor expenditure. The required accuracy in evaluating onboard resources by using the equivalent mass methodology and applying it to the design of such facilities is not precise. This is due to the uncertainty of the structure and not completely understanding the properties of all associated hardware, including the technology in these systems. We present a simple criteria of optimization for horticultural regimes in SPGF: Q(max) = max [M (.) (EBI)(2)/(V (.) E (.) T)], where M is the crop harvest in terms of total dry biomass in the plant growth system; EBI is the edible biomass index (harvest index), V is volume occupied by the crop; E is the crop light energy supply during growth; T is the crop growth duration. The criterion reflects directly on the consumption of onboard resources for crop production. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Dynamac Corp, Kennedy Space Ctr, FL 32899 USA. Moscow Biomed Problems Inst, Moscow 123007, Russia. NASA, Kennedy Space Ctr, FL 32899 USA. RP Chetirkin, PV (reprint author), Dynamac Corp, DYN-3, Kennedy Space Ctr, FL 32899 USA. EM peter.chetirkin-1@ksc.nasa.gov RI Kondyurin, Alexey/B-9580-2011 OI Kondyurin, Alexey/0000-0002-8837-9734 NR 25 TC 6 Z9 7 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 7 BP 1612 EP 1618 DI 10.1016/j.asr.2003.08.080 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BBH90 UT WOS:000225592800022 PM 15880901 ER PT S AU Wilson, JW Clowdsley, MS Cucinotta, FA Tripathi, RK Nealy, JE De Angelis, G AF Wilson, JW Clowdsley, MS Cucinotta, FA Tripathi, RK Nealy, JE De Angelis, G BE Cucinotta, F Reitz, G TI Deep space environments for human exploration SO SPACE LIFE SCIENCES: RADIATION RISK ASSESSMENT AND RADIATION MEASUREMENT IN LOW EARTH ORBIT SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE galactic cosmic rays; solar cosmic rays; albedo particles; trapped radiations ID INTERPLANETARY SPACE; COSMIC-RAYS; EXPOSURES AB Mission scenarios outside the Earth's protective magnetic shield are being studied. Included are high usage assets in the near-Earth environment for casual trips, for research, and for commercial/operational platforms, in which career exposures will be multimission determined over the astronaut's lifetime. The operational platforms will serve as launching points for deep space exploration missions, characterized by a single long-duration mission during the astronaut's career. The exploration beyond these operational platforms will include missions to planets, asteroids, and planetary satellites. The interplanetary environment is evaluated using convective diffusion theory. Local environments for each celestial body are modeled by using results from the most recent targeted spacecraft, and integrated into the design environments. Design scenarios are then evaluated for these missions. The underlying assumptions in arriving at the model environments and their impact on mission exposures within various shield materials will be discussed. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. NASA, NRC, Langley Res Ctr, Hampton, VA 23681 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Old Dominion Univ, Norfolk, VA 23508 USA. RP Wilson, JW (reprint author), NASA, Langley Res Ctr, 4 S Wright St,MS 188B, Hampton, VA 23681 USA. EM john.w.wilson@nasa.gov NR 20 TC 22 Z9 22 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 6 BP 1281 EP 1287 DI 10.1016/j.asr.2003.10.052 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BBH88 UT WOS:000225592600002 PM 15880915 ER PT S AU Mashnik, SG Gudima, KK Moskalenko, IV Prael, RE Sierk, AJ AF Mashnik, SG Gudima, KK Moskalenko, IV Prael, RE Sierk, AJ BE Cucinotta, F Reitz, G TI CEM2K and LAQGSM codes as event generators for space-radiation-shielding and cosmic-ray-propagation applications SO SPACE LIFE SCIENCES: RADIATION RISK ASSESSMENT AND RADIATION MEASUREMENT IN LOW EARTH ORBIT SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space radiation shielding; cosmic rays; CEM2k and LAQGSM codes; astrophysics ID CROSS-SECTIONS; NUCLEAR-REACTIONS; GEV PROTONS; MODEL; FRAGMENTATION; COLLISIONS; HYDROGEN; GALAXY; YIELDS AB The CEM2k and LAQGSM codes have been recently developed at Los Alamos National Laboratory to simulate nuclear reactions for a number of applications. We have benchmarked our codes against most available data measured at incident particle energies from 10 MeV to 800 GeV and have compared our results with predictions of other current models used by the nuclear community. Here, we present a brief description of our codes and show some illustrative results that testify that CEM2k and LAQGSM can be used as reliable event generators for space-radiation-shielding, cosmic-ray (CR) propagation, and other astro-physical applications. Finally, we show an example of combining of our calculated cross-sections with experimental data from our LANL T-16 compilation to produce evaluated files. Such evaluated files were successfully used in the model of particle propagation in the Galaxy GALPROP to better constrain the size of the CR halo. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Moldavian Acad Sci, Inst Appl Phys, MD-2028 Kishinev, Moldova. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA. RP Los Alamos Natl Lab, Mailstop B283, Los Alamos, NM 87545 USA. EM mashnik@lanl.gov RI Moskalenko, Igor/A-1301-2007 OI Moskalenko, Igor/0000-0001-6141-458X NR 46 TC 26 Z9 26 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2004 VL 34 IS 6 BP 1288 EP 1296 DI 10.1016/j.asr.2003.08.057 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BBH88 UT WOS:000225592600003 PM 15880916 ER PT S AU Tweed, J Wilson, JW Tripathi, RK AF Tweed, J Wilson, JW Tripathi, RK BE Cucinotta, F Reitz, G TI An improved Green's function for ion beam transport SO SPACE LIFE SCIENCES: RADIATION RISK ASSESSMENT AND RADIATION MEASUREMENT IN LOW EARTH ORBIT SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE radiation risk; Boltzman transport equation; ion beam transport; an improved Green's function AB Ion beam transport theory allows testing of material transmission properties in the laboratory environment generated by particle accelerators. This is a necessary step in materials development and evaluation for space use. The approximations used in solving the Boltzmann transport equation for the space setting are often not sufficient for laboratory work and those issues are the main emphasis of the present work. In consequence, an analytic solution of the linear Boltzmann equation is pursued in the form of a Green's function allowing flexibility in application to a broad range of boundary value problems. It has been established that simple solutions can be found for high charge and energy (HZE) ions by ignoring nuclear energy downshifts and dispersion. Such solutions were found to be supported by experimental evidence with HZE ion beams when multiple scattering was added. Lacking from the prior solutions were range and energy straggling and energy downshift with dispersion associated with nuclear events. Recently, we have found global solutions including these effects providing a broader class of HZE ion solutions. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Old Dominion Univ, Dept Math & Stat, Norfolk, VA 23529 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Tweed, J (reprint author), Old Dominion Univ, Dept Math & Stat, Hampton Blvd, Norfolk, VA 23529 USA. EM jtweed@odu.edu NR 9 TC 7 Z9 7 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 6 BP 1311 EP 1318 DI 10.1016/j.asr.2003.11.021 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BBH88 UT WOS:000225592600006 PM 15880918 ER PT S AU Wilson, JW Tripathi, RK Qualls, GD Cucinotta, FA Prael, RE Norbury, JW Heinbockel, JH Tweed, J AF Wilson, JW Tripathi, RK Qualls, GD Cucinotta, FA Prael, RE Norbury, JW Heinbockel, JH Tweed, J BE Cucinotta, F Reitz, G TI A space radiation transport method development SO SPACE LIFE SCIENCES: RADIATION RISK ASSESSMENT AND RADIATION MEASUREMENT IN LOW EARTH ORBIT SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE radiation constraints; space radiation transport; spacecrafting shield design; HZETRN ID SHUTTLE; FRAGMENTATION; PROPAGATION; ISSUES; DEPTH; WATER; NE-20; MODEL; IONS AB Improved spacecraft shield design requires early entry of radiation constraints into the design process to maximize performance and minimize costs. As a result, we have been investigating high-speed computational procedures to allow shield analysis from the preliminary design concepts to the final design. In particular, we will discuss the progress towards a full three-dimensional and computationally efficient deterministic code for which the current HZETRN evaluates the lowest-order asymptotic term. HZETRN is the first deterministic solution to the Boltzmann equation allowing field mapping within the International Space Station (ISS) in tens of minutes using standard finite element method (FEM) geometry common to engineering design practice enabling development of integrated multidisciplinary design optimization methods. A single ray trace in ISS FEM geometry requires 14 ms and severely limits application of Monte Carlo methods to such engineering models. A potential means of improving the Monte Carlo efficiency in coupling to spacecraft geometry is given in terms of re-configurable computing and could be utilized in the final design as verification of the deterministic method optimized design. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Los Alamos Natl Lab, US DOE, Los Alamos, NM 87545 USA. Univ Wisconsin, Milwaukee, WI 53201 USA. Old Dominion Univ, Norfolk, VA 23508 USA. RP Wilson, JW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM john.w.wilson@nasa.gov NR 52 TC 7 Z9 9 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 6 BP 1319 EP 1327 DI 10.1016/j.asr.2003.10.048 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BBH88 UT WOS:000225592600007 PM 15880919 ER PT S AU De Angelis, G Clowdsley, MS Singleterry, RC Wilson, JW AF De Angelis, G Clowdsley, MS Singleterry, RC Wilson, JW BE Cucinotta, F Reitz, G TI A new Mars radiation environment model with visualization SO SPACE LIFE SCIENCES: RADIATION RISK ASSESSMENT AND RADIATION MEASUREMENT IN LOW EARTH ORBIT SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE manned space missions; Mars; planetary environments; radiation analysis; radiation environments ID GENERAL-CIRCULATION MODEL; SOUTH POLAR-CAP; ATMOSPHERIC DYNAMICS; NORTHERN-HEMISPHERE; COSMIC-RAYS; SURFACE; CONSTRAINTS; TOPOGRAPHY; PATHFINDER; ROCKS AB A new model for the radiation environment to be found on the planet Mars due to Galactic Cosmic Rays (OCR) has been developed at the NASA Langley Research Center. Solar modulated primary particles rescaled for Mars conditions are transported through the Martian atmosphere, with temporal properties modeled with variable timescales, down to the surface, with altitude and backscattering patterns taken into account. The Martian atmosphere has been modeled by using the Mars Global Reference Atmospheric Model - version 2001 (Mars-GRAM 2001). The altitude to compute the atmospheric thickness profile has been determined by using a model for the topography based on the data provided by the Mars Orbiter Laser Altimeter (MOLA) instrument on board the Mars Global Surveyor (MGS) spacecraft. The Mars surface composition has been modeled based on averages over the measurements obtained from orbiting spacecraft and at various landing sites, taking into account the possible volatile inventory (e.g., CO2 ice, H2O ice) along with its time variation throughout the Martian year. Particle transport has been performed with the HZETRN heavy ion code. The Mars Radiation Environment Model has been made available worldwide through the Space Ionizing Radiation Effects and Shielding Tools (SIREST) website, a project of NASA Langley Research Center. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Old Dominion Univ, Norfolk, VA 23508 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP De Angelis, G (reprint author), Old Dominion Univ, Norfolk, VA 23508 USA. EM g.deangelis@larc.nasa.gov NR 48 TC 16 Z9 16 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 6 BP 1328 EP 1332 DI 10.1016/j.asr.2003.09.059 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BBH88 UT WOS:000225592600008 PM 15880920 ER PT S AU Shavers, MR Zapp, N Barber, RE Wilson, JW Qualls, G Toupes, L Ramsey, S Vinci, V Smith, G Cucinotta, FA AF Shavers, MR Zapp, N Barber, RE Wilson, JW Qualls, G Toupes, L Ramsey, S Vinci, V Smith, G Cucinotta, FA BE Cucinotta, F Reitz, G TI Implementation of ALARA radiation protection on the ISS through polyethylene shielding augmentation of the Service Module Crew Quarters SO SPACE LIFE SCIENCES: RADIATION RISK ASSESSMENT AND RADIATION MEASUREMENT IN LOW EARTH ORBIT SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE ALARA; space radiation protection; space radiation shielding; polyethylene shielding; international space station; cosmic radiation exposure AB With 5-7 month long duration missions at 51.6degrees inclination in Low Earth Orbit, the ionizing radiation levels to which International Space Station (ISS) crewmembers are exposed will be the highest planned occupational exposures in the world. Even with the expectation that regulatory dose limits will not be exceeded during a single tour of duty aboard the ISS, the "as low as reasonably achievable" (ALARA) precept requires that radiological risks be minimized when possible through a dose optimization process. Judicious placement of efficient shielding materials in locations where crewmembers sleep, rest, or work is an important means for implementing ALARA for spaceflight. Polyethylene (C H) is a relatively inexpensive, stable, and, with a low atomic number, an effective shielding material that has been certified for use aboard the ISS. Several designs for placement of slabs or walls of polyethylene have been evaluated for radiation exposure reduction in the Crew Quarters (CQ) of the Zvezda (Star) Service Module. Optimization of shield designs relies on accurate characterization of the expected primary and secondary particle environment and modeling of the predicted radiobiological responses of critical organs and tissues. Results of the studies shown herein indicate that 20% or more reduction in equivalent dose to the CQ occupant is achievable. These results suggest that shielding design and risk analysis are necessary measures for reducing long-term radiological risks to ISS inhabitants and for meeting legal ALARA requirements. Verification of shield concepts requires results from specific designs to be compared with onboard dosimetry. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Wyle Labs, Radiat Biophys Grp, Houston, TX 77058 USA. Lockheed Martin, Houston, TX 77058 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Johnson Engn, Houston, TX 77058 USA. RP Shavers, MR (reprint author), Loma Linda Univ, Radiol Program, 11175 Campus St,CSP A-1010, Loma Linda, CA 92354 USA. EM mshavers@emsjsc.nasa.gov NR 8 TC 19 Z9 20 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 6 BP 1333 EP 1337 DI 10.1016/j.asr.2003.10.051 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BBH88 UT WOS:000225592600009 PM 15880921 ER PT S AU Desai, N Wu, H George, K Gonda, SR Cucinotta, FA AF Desai, N Wu, H George, K Gonda, SR Cucinotta, FA BE Cucinotta, F Reitz, G TI Simultaneous measurement of multiple radiation-induced protein expression profiles using the Luminex(TM) system SO SPACE LIFE SCIENCES: RADIATION RISK ASSESSMENT AND RADIATION MEASUREMENT IN LOW EARTH ORBIT SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE radiation risk; LUMINEXTM system; radiation exposure; space radiation ID DOUBLE-STRAND BREAKS; IONIZING-RADIATION; DNA-DAMAGE; BLOOD-LYMPHOCYTES; MEIOTIC CELLS; P53; RESPONSES; EXPOSURE; QUANTIFICATION; IDENTIFICATION AB Space flight results in the exposure of astronauts to a mixed field of radiation composed of energetic particles of varying energies, and biological indicators of space radiation exposure provides a better understanding of the associated long-term health risks. Current methods of biodosimetry have employed the use of cytogenetic analysis for biodosimetry, and more recently the advent of technological progression has led to advanced research in the use of genomic and proteomic expression profiling to simultaneously assess biomarkers of radiation exposure. We describe here the technical advantages of the Luminex(TM) 100 system relative to traditional methods and its potential as a tool to simultaneously profile multiple proteins induced by ionizing radiation. The development of such a bioassay would provide more relevant post-translational dynamics of stress response and will impart important implications in the. advancement of space and other radiation contact monitoring. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Lyndon B Johnson Space Ctr, Radiat Hlth Program, Houston, TX 77058 USA. Wyle Labs, Houston, TX 77058 USA. NASA, Lyndon B Johnson Space Ctr, Biotechnol Program, Houston, TX 77058 USA. RP Wu, H (reprint author), NASA, Lyndon B Johnson Space Ctr, Radiat Hlth Program, Mail Code SK21, Houston, TX 77058 USA. EM hwu@ems.isc.nasa.gov NR 38 TC 11 Z9 13 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 6 BP 1362 EP 1367 DI 10.1016/j.asr.2004.011 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BBH88 UT WOS:000225592600014 PM 15881190 ER PT S AU Cucinotta, FA Schimmerling, W Wilson, JW Peterson, LE Saganti, PB Dicello, JF AF Cucinotta, FA Schimmerling, W Wilson, JW Peterson, LE Saganti, PB Dicello, JF BE Cucinotta, F Reitz, G TI Uncertainties in estimates of the risks of late effects from space radiation SO SPACE LIFE SCIENCES: RADIATION RISK ASSESSMENT AND RADIATION MEASUREMENT IN LOW EARTH ORBIT SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE radiation risk; risk projections; human space exploration; Mars exploration; galactic cosmic radiation ID EXPOSURE; RAYS AB Methods used to project risks in low-Earth orbit are of questionable merit for exploration missions because of the limited radiobiology data and knowledge of galactic cosmic ray (GCR) heavy ions, which causes estimates of the risk of late effects to be highly uncertain. Risk projections involve a product of many biological and physical factors, each of which has a differential range of uncertainty due to lack of data and knowledge. Using the linear-additivity model for radiation risks, we use Monte-Carlo sampling from subjective uncertainty distributions in each factor to obtain an estimate of the overall uncertainty in risk projections. The resulting methodology is applied to several human space exploration mission scenarios including a deep space outpost and Mars missions of duration of 360, 660, and 1000 days. The major results are the quantification of the uncertainties in current risk estimates, the identification of factors that dominate risk projection uncertainties, and the development of a method to quantify candidate approaches to reduce uncertainties or mitigate risks. The large uncertainties in GCR risk projections lead to probability distributions of risk that mask any potential risk reduction using the "optimization" of shielding materials or configurations. In contrast, the design of shielding optimization approaches for solar particle events and trapped protons can be made at this time and promising technologies can be shown to have merit using our approach. The methods used also make it possible to express risk management objectives in terms of quantitative metrics, e.g., the number of days in space without exceeding a given risk level within well-defined confidence limits. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NASA, Headquarters, Washington, DC 20546 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Baylor Coll Med, Dept Med, Houston, TX 77030 USA. Johns Hopkins Med Sch, Baltimore, MD 21287 USA. RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Rd 1, Houston, TX 77058 USA. OI Peterson, Leif/0000-0002-1187-0883 NR 18 TC 30 Z9 31 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 6 BP 1383 EP 1389 DI 10.1016/j.asr.2003.10.053 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BBH88 UT WOS:000225592600018 PM 15881779 ER PT S AU De Angelis, G Clowdsley, MS Nealy, JE Tripathi, RK Wilson, JW AF De Angelis, G Clowdsley, MS Nealy, JE Tripathi, RK Wilson, JW BE Cucinotta, F Reitz, G TI Radiation analysis for manned missions to the Jupiter system SO SPACE LIFE SCIENCES: RADIATION RISK ASSESSMENT AND RADIATION MEASUREMENT IN LOW EARTH ORBIT SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE Jupiter; manned space missions; planetary environments; radiation analysis; radiation environments ID GALILEAN SATELLITES; CALLISTO; DISTRIBUTIONS; GEOLOGY; SURFACE AB An analysis for manned missions targeted to the Jovian system has been performed in the framework of the NASA RASC (Revolutionary Aerospace Systems Concepts) program on Human Exploration beyond Mars. The missions were targeted to the Jupiter satellite Callisto. The mission analysis has been divided into three main phases, namely the interplanetary cruise, the Jupiter orbital insertion, and the surface landing and exploration phases. The interplanetary phase is based on departure from the Earth-Moon L1 point. Interplanetary trajectories based on the use of different propulsion systems have been considered, with resulting overall cruise phase duration varying between two and five years. The Jupiter-approach and the orbital insertion trajectories are considered in detail, with the spacecraft crossing the Jupiter radiation belts and staying around the landing target. In the surface exploration phase the stay on the Callisto surface is considered. The satellite surface composition has been modeled based on the most recent results from the GALILEO spacecraft. In the transport computations the surface backscattering has been duly taken into account. Particle transport has been performed with the HZETRN heavy ion code for hadrons and with an in-house developed transport code for electrons and bremsstrahlung photons. The obtained doses have been compared to dose exposure limits. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Old Dominion Univ, Norfolk, VA 23508 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP De Angelis, G (reprint author), Old Dominion Univ, Norfolk, VA 23508 USA. EM g.deangelis@larc.nasa.gov NR 37 TC 8 Z9 8 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 6 BP 1395 EP 1403 DI 10.1016/j.asr.2003.09.061 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BBH88 UT WOS:000225592600020 PM 15881781 ER PT S AU O'Sullivan, D Zhou, D Semones, E Heinrich, W Flood, E AF O'Sullivan, D Zhou, D Semones, E Heinrich, W Flood, E BE Cucinotta, F Reitz, G TI Dose equivalent, absorbed dose and charge spectrum investigation in low Earth orbit SO SPACE LIFE SCIENCES: RADIATION RISK ASSESSMENT AND RADIATION MEASUREMENT IN LOW EARTH ORBIT SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space radiation; radiation dose ID COSMIC-RAYS AB Particle intensity, dose equivalent and absorbed dose have been measured on board the space shuttle Endeavour during STS-108 in December 2001 by Dublin Institute for Advanced Studies (DIAS). The dose estimates are based on very accurate measurements of recoils produced in CR-39 by cosmic ray primary and secondary protons and heavier nuclei and by secondary neutrons. The corresponding LET spectra were used to determine dose equivalent and absorbed dose values. Estimates of the total flux of Z greater than or equal to 2 nuclei have been undertaken and a preliminary charge spectrum was measured. Some comparisons are made with preliminary data obtained on STS-105 (ISS Expedition) and other missions using CR-39 detectors. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Dublin Inst Adv Studies, Astrophys Sect, Dublin 2, Ireland. Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Siegen, Dept Phys, D-57068 Siegen, Germany. RP O'Sullivan, D (reprint author), Dublin Inst Adv Studies, Astrophys Sect, 5 Merr Sq, Dublin 2, Ireland. EM dos@cp.dias.ie NR 9 TC 20 Z9 20 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 6 BP 1420 EP 1423 DI 10.1016/j.asr.2003.05.048 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BBH88 UT WOS:000225592600023 PM 15881785 ER PT S AU Fung, SF AF Fung, SF BE Cucinotta, F Reitz, G TI Survey of current situation in radiation belt modeling SO SPACE LIFE SCIENCES: RADIATION RISK ASSESSMENT AND RADIATION MEASUREMENT IN LOW EARTH ORBIT SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE radiation belt models; energetic particles; magnetospheric configuration; dynamics ID TRAPPED-PARTICLES; SOLAR-WIND; ELECTRON; DIFFUSION; STORM; MAGNETOSPHERE; SIMULATIONS; ALTITUDES; SALAMMBO; INNER AB The study of Earth's radiation belts is one of the oldest subjects in space physics. Despite the tremendous progress made in the last four decades, we still lack a complete understanding of the radiation belts in terms of their configurations, dynamics, and detailed physical accounts of their sources and sinks. The static nature of early empirical trapped radiation models, for examples, the NASA AP-8 and AE-8 models, renders those models inappropriate for predicting short-term radiation belt behaviors associated with geomagnetic storms and substorms. Due to incomplete data coverage, these models are also inaccurate at low altitudes (e.g., < 1000 km) where many robotic and human space flights occur. The availability of radiation data from modern space missions and advancement in physical modeling and data management techniques have now allowed the development of new empirical and physical radiation belt models. In this paper, we will review the status of modern radiation belt modeling. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Goddard Space Flight Ctr, Space Phys Data Facil, Greenbelt, MD 20771 USA. RP Fung, SF (reprint author), NASA, Goddard Space Flight Ctr, Space Phys Data Facil, Greenbelt, MD 20771 USA. EM shing.fung@gsfc.nasa.gov RI Fung, Shing/F-5647-2012 NR 53 TC 7 Z9 7 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 6 BP 1441 EP 1450 DI 10.1016/S0273-1177(03)00078-4 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BBH88 UT WOS:000225592600027 PM 15881789 ER PT S AU Abyzov, SS Hoover, RB Imura, S Mitskevich, IN Naganuma, T Poglazova, MN Ivanov, MV AF Abyzov, SS Hoover, RB Imura, S Mitskevich, IN Naganuma, T Poglazova, MN Ivanov, MV BE Horneck, G LevasseurRegourd, AC Rabin, BM Slenzka, KB TI Use of different methods for discovery of ice-entrapped microorganisms in ancient layers of the Antarctic glacier SO SPACE LIFE SCIENCES: SEARCH FOR SIGNATURES OF LIFE, AND SPACE FLIGHT ENVIRONMENTAL EFFECTS ON THE NERVOUS SYSTEM SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE ice-entrapped microorganisms; Lake Vostok; Antarctic glacier; methods for microorganism discovery; astrobiology ID LAKE VOSTOK; SHEET AB Investigations throughout the thickness of the ice sheet above Lake Vostok show the presence of microorganisms belonging to different well-known taxonomic groups, even in the very ancient horizons near close to floor of the glacier. Different methods were used to search for microorganisms that are rarely found in the deep ancient layers of an ice sheet. Primary investigations tried the usual methods of sowing samples onto different nutrient media, and the result was that only a few microorganisms grew on the media used. Further investigations of the very ancient layers of the ice sheet by radioisotopic, luminescence, and scanning electron microscopy methods at different modifications, revealed the quantity and morphological diversity of the cells of microorganisms that were distributed on the different horizons. Microbiological investigations in the very ancient strata of the Antarctic ice cover, nearest to the bedrock, support the effectiveness of using a combination of different methods to search for signs of life in ancient icy formations, which might play a role in the long-term preservation and transportation of microbial life throughout the Universe. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Russian Acad Sci, Inst Microbiol, Moscow 11731260, Letya, Russia. NASA, NSSTC, Dept Space Sci, Huntsville, AL 35805 USA. Natl Inst Polar Res, Itabashi Ku, Tokyo 1738515, Japan. Hiroshima Univ, Biol Oceanog Lab, Higashihiroshima 7398528, Japan. RP Abyzov, SS (reprint author), Russian Acad Sci, Inst Microbiol, Oktyabrya 7A, Moscow 11731260, Letya, Russia. EM abyzov@inmi.host.ru; rich-ard.hoover@nasa.gov; imura@nipr.ac.jp; takn@hiroshima-u.ac.jp NR 22 TC 14 Z9 15 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 33 IS 8 BP 1222 EP 1230 DI 10.1016/j.asr.2003.08.033 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BAF41 UT WOS:000222000200002 ER PT S AU Cockell, CS AF Cockell, CS BE Horneck, G LevasseurRegourd, AC Rabin, BM Slenzka, KB TI Impact-shocked rocks - insights into Archean and extraterrestrial microbial habitats (and sites for prebiotic chemistry?) SO SPACE LIFE SCIENCES: SEARCH FOR SIGNATURES OF LIFE, AND SPACE FLIGHT ENVIRONMENTAL EFFECTS ON THE NERVOUS SYSTEM SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE astrobiology; Archean extraterrestrial microbial habitats; prebiotic chemistry ID DEVON ISLAND; CANADA; MARS; CRATER AB Impact-shocked gneiss shocked to greater than 10 GPa in the Haughton impact structure in the Canadian High Arctic has an approximately 25-times greater pore surface area than unshocked rocks. These pore spaces provide microhabitats for a diversity of heterotrophic microorganisms and in the near-surface environment of the rocks, where light levels are sufficient, cyanobacteria. Shocked rocks provide a moisture retaining, UV protected microenvironment. During the Archean, when impact fluxes were more than two orders of magnitude higher than today, the shocked-rock habitat was one of the most common terrestrial habitats and might have provided a UV-shielded refugium for primitive life. These potential habitats are in high abundance on Mars where impact crater habitats could have existed over geologic time periods of billions of years, suggesting that impact-shocked rocks are important sites to search for biomolecules in extraterrestrial life detection strategies. In addition to being favourable sites for life, during the prebiotic period of planetary history impact-shocked rocks might have acted as a site for the concentration of reactants for prebiotic syntheses. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. British Antarctic Survey, Cambridge CB3 0ET, England. RP Cockell, CS (reprint author), NASA, Ames Res Ctr, SETI Inst, M-S 245-3, Moffett Field, CA 94035 USA. EM csco@bas.ac.uk NR 27 TC 9 Z9 10 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 33 IS 8 BP 1231 EP 1235 DI 10.1016/j.asr.2003.06.027 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BAF41 UT WOS:000222000200003 PM 15803603 ER PT S AU Mancinelli, RL Fahlen, TF Landheim, R Klovstad, MR AF Mancinelli, RL Fahlen, TF Landheim, R Klovstad, MR BE Horneck, G LevasseurRegourd, AC Rabin, BM Slenzka, KB TI Brines and evaporites: analogs for Martian life SO SPACE LIFE SCIENCES: SEARCH FOR SIGNATURES OF LIFE, AND SPACE FLIGHT ENVIRONMENTAL EFFECTS ON THE NERVOUS SYSTEM SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE astrobiology; brines and evaporites; analogs for Martian life; halophiles; osmophiles ID METABOLIC-ACTIVITY; WATER-STRESS; MARS; BACTERIA; EVOLUTION AB Data from recent Mars missions suggest that Mars almost certainly had abundant liquid water on its surface at some time in the past. As a result, Mars has emerged as a key solar system target that could have harbored some form of life in the past, and which could perhaps still possess remnants of life in brine-containing permafrost. As Mars lost its atmosphere it became cold and dry. Any remaining water on the surface may have formed saline brine pockets within the permafrost. These brine pockets may either be an "oasis" for an extant Martian biota, or the last refuge of an extinct Martian biota. Eventually, these brine pockets would have dried to form evaporites. Evaporites are deposits that result from the evaporation of saline water, which on earth represent primarily halite (NaCl), gypsum, (CaSO(4)2H(2)O), and anhydrite (CaSO4). Evaporites that contain bacterial and algal assemblages exist on earth today and are well known in the fossil record. The most likely organism type to survive in a brine or evaporite on earth is a halophile. The objective of this study was to determine the potential of microbes to survive in frozen evaporites. Washed mid-log phase and stationary phase cultures of Haloarcula-G (a species isolated by us during a previous study) and Halobacterium salinarum were either suspended in brine (25% NaCl solution), dried, and then exposed to -20 or -80 degreesC. For comparison, cultures of Deinococcus radiodurans, Escherichia coli, and Pseudomonas fluorescens were treated similarly, except they were resuspended in 0.5% NaCl solution. Also, to mimic a brine pocket samples of washed mid-log phase cells of each organism were placed in an aqueous solution of 25% NaCl, or in their respective nutrient medium containing 25% NaCl. Periodically, samples of the cells were removed and tested for survival. Data from these experiments suggest that halophiles survive better than non-halophiles under low temperature conditions. These observations would suggest that halophiles might survive in evaporites contained in permafrost. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Mancinelli, RL (reprint author), NASA, Ames Res Ctr, SETI Inst, Mail Stop 239-12, Moffett Field, CA 94035 USA. EM rmancinelli@mail.arc.nasa.gov RI Mancinelli, Rocco/L-8971-2016 NR 22 TC 59 Z9 62 U1 1 U2 33 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 33 IS 8 BP 1244 EP 1246 DI 10.1016/j.asr.2003.08.034 PG 3 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BAF41 UT WOS:000222000200005 ER PT S AU Schelble, RT Westall, F Allen, CC AF Schelble, RT Westall, F Allen, CC BE Horneck, G LevasseurRegourd, AC Rabin, BM Slenzka, KB TI similar to 1.8 Ga iron-mineralized microblota from the Gunflint Iron Formation, Ontcario, Canada: implications for Mars SO SPACE LIFE SCIENCES: SEARCH FOR SIGNATURES OF LIFE, AND SPACE FLIGHT ENVIRONMENTAL EFFECTS ON THE NERVOUS SYSTEM SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE astrobiology; iron-mineralized microbiota; Mars ID BACTERIA; ONTARIO; MICROORGANISMS; CHERT AB A similar to1.8 Ga banded-iron stromatolite from the Mink Mountain locality (PPRG 336) of the Gunflint Iron Formation, Ontario, Canada was investigated as an analogue to Martian hematite deposits which have the potential to contain fossilized Martian life. The stromatolitic sample was primarily composed of quartz (SiO2) with fractional amounts of hematite (Fe2O3), greenalite ((Fe,Mg)(3)Si2O5(OH)(2)), and minor amounts of stilpnomelane (K(Fe2+,Mg,Fe3+, Al)(8)(Si,Al)(12)(O,OH)(27) . 2H(2)O). Iron-bearing minerals were present within thin, discontinuous bands aligned roughly parallel. Octahedral pseudomorphs of hematite after magnetite occurred as localized elongate clusters, as well as on the outer rims of detrital oncolitic structures. Microcrystalline greenalite was present as a clay occurring in layers subparallel to the stromatolitic layering. Greenalite was observed in both the silica- and iron-rich layers, as well as within oncolitic structures. Irregular aggregates of radiating stilpnomelane needles extended into the silica matrix. Optical microscopy (OM) and scanning electron microscopy (SEM) revealed 5-10 mum diameter iron-mineralized or siliceous, concentrically laminated, ooid-like structures in localized patches. OM, SEM, and energy dispersive X-ray analyses (EDX) were used to characterize microfossils mineralized by iron-oxides in the stromatolite. The microfossils consisted of coccoidal and filamentous forms. The coccoids (similar to0.5 to 2 mum diameter) were present both in chains and individually throughout the silica- and iron-rich bands, while the filamentous remnants (similar to1-3 mum diameter, and up to 200 mum length) were localized and patchy in the sample. While the Gunflint Iron Formation does not provide us with a perfect analogue to the Martian hematite site, it does establish the potential for finding iron-mineralized microorganisms within Martian sediments. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ So Calif, Dept Earth Sci, Los Angeles, CA 90089 USA. CNRS, Ctr Biophys Mol, F-45071 Orleans 2, France. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Schelble, RT (reprint author), Univ So Calif, Dept Earth Sci, Los Angeles, CA 90089 USA. EM rachels@usc.edu NR 21 TC 14 Z9 14 U1 1 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 33 IS 8 BP 1268 EP 1273 DI 10.1016/j.asr.2003.10.036 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BAF41 UT WOS:000222000200009 ER PT S AU Lupisella, ML AF Lupisella, ML BE Horneck, G LevasseurRegourd, AC Rabin, BM Slenzka, KB TI Using artificial life to assess the typicality of terrestrial life SO SPACE LIFE SCIENCES: SEARCH FOR SIGNATURES OF LIFE, AND SPACE FLIGHT ENVIRONMENTAL EFFECTS ON THE NERVOUS SYSTEM SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE astrobiology; artificial life; terrestrial life AB The extent to which extraterrestrial life questions can be confidently addressed rests in large measure on the extent to which terrestrial life is representative of life in general since we will have to draw from terrestrial life knowledge. This paper outlines a long-term research program that could inform the extent to which terrestrial life is representative of life more generally, which might then help inform our level of confidence in applying terrestrial life knowledge to extraterrestrial life issues. The approach involves appealing to the relatively new field of Artificial Life to: (1) use minimal characterizations of life in (2) a large number of open-ended Artificial Life computer experiments to generate "life possibility spaces" (3) the results of which can be examined for their plausibility within the context of relevant constraining knowledge, so that (4) the remaining results can be examined for variability relative to terrestrial life, where low variability might suggest that terrestrial life is typical of life in general, and high variability could be interpreted to suggest that terrestrial life might be atypical. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Lupisella, ML (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt Rd, Greenbelt, MD 20771 USA. EM mark.l.lupisella@nasa.gov NR 22 TC 3 Z9 3 U1 1 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 33 IS 8 BP 1318 EP 1324 DI 10.1016/j.asr.2003.03.030 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BAF41 UT WOS:000222000200017 ER PT S AU Sannita, WG Acquaviva, M Ball, SL Belli, F Bisti, S Bidoli, V Carozzo, S Casolino, M Cucinotta, F De Pascale, MP Di Fino, L Di Marco, S Maccarone, R Martello, C Miller, J Narici, L Peachey, NS Picozza, P Rinaldi, A Ruggieri, D Saturno, M Schardt, D Vazquez, M AF Sannita, WG Acquaviva, M Ball, SL Belli, F Bisti, S Bidoli, V Carozzo, S Casolino, M Cucinotta, F De Pascale, MP Di Fino, L Di Marco, S Maccarone, R Martello, C Miller, J Narici, L Peachey, NS Picozza, P Rinaldi, A Ruggieri, D Saturno, M Schardt, D Vazquez, M BE Horneck, G LevasseurRegourd, AC Rabin, BM Slenzka, KB TI Effects of heavy ions on visual function and electrophysiology of rodents: the ALTEA-MICE project SO SPACE LIFE SCIENCES: SEARCH FOR SIGNATURES OF LIFE, AND SPACE FLIGHT ENVIRONMENTAL EFFECTS ON THE NERVOUS SYSTEM SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE the ALTEA-MICE project; visual impairment; heavy ions ID LIGHT-FLASHES; NITROGEN NUCLEI; RAY; ASTRONAUTS; RADIATION; SPACE; EYE; RETINA; MUONS AB ALTEA-MICE will supplement the ALTEA project on astronauts and provide information on the functional visual impairment possibly induced by heavy ions during prolonged operations in microgravity. Goals of ALTEA-MICE are: (1) to investigate the effects of heavy ions on the visual system of normal and mutant mice with retinal defects; (2) to define reliable experimental conditions for space research; and (3) to develop animal models to study the physiological consequences of space travels on humans. Remotely controlled mouse setup, applied electrophysiological recording methods, remote particle monitoring, and experimental procedures were developed and tested. The project has proved feasible under laboratory-controlled conditions comparable in important aspects to those of astronauts' exposure to particle in space. Experiments are performed at the Brookhaven National Laboratories (BNL] (Upton, NY, USA) and the Gesellschaft fur Schwerionenforschung mbH [GSI]/Biophysik (Darmstadt, ERG) to identify possible electrophysiological changes and/or activation of protective mechanisms in response to pulsed radiation. Offline data analyses are in progress and observations are still anecdotal. Electrophysiological changes after pulsed radiation are within the limits of spontaneous variability under anesthesia, with only indirect evidence of possible retinal/cortical responses. Immunostaining showed changes (e.g increased expression of FGF2 protein in the outer nuclear layer) suggesting a retinal stress reaction to high-energy particles of potential relevance in space. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Ist Nazl Fis Nucl Roma 2, Rome, Italy. Univ Genoa, Dept Motor Sci, Genoa, Italy. SUNY Stony Brook, Dept Psychiat, Stony Brook, NY 11794 USA. Cleveland Clin Fdn, Cole Eye Inst, Cleveland, OH 44195 USA. Cleveland VAMC, Cleveland, OH USA. Univ Roma Tor Vergata, Dept Phys, Rome, Italy. Univ Aquila, Inst Physiol, I-67100 Laquila, Italy. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. GSI Darmstadt, D-6100 Darmstadt, Germany. Brookhaven Natl Lab, Upton, NY 11973 USA. RP Sannita, WG (reprint author), Ist Nazl Fis Nucl Roma 2, Rome, Italy. EM 29537@unige.it RI Peachey, Neal/G-5533-2010; Di Marco, Stefano/C-6386-2009; Schardt, Dieter/M-1517-2014; OI Di Marco, Stefano/0000-0003-4847-6270; Schardt, Dieter/0000-0001-7851-5993; Ball, Sherry/0000-0002-2362-9499; MACCARONE, Rita/0000-0003-0648-3771; casolino, marco/0000-0001-6067-5104; Picozza, Piergiorgio/0000-0002-7986-3321; CAROZZO, Simone/0000-0003-4536-9832 NR 24 TC 7 Z9 8 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 33 IS 8 BP 1347 EP 1351 DI 10.1016/j.asr.2003.11.007 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Meteorology & Atmospheric Sciences GA BAF41 UT WOS:000222000200022 PM 15803626 ER PT S AU Charnley, SB AF Charnley, SB BE Bernstein, MP Kress, M NavarroGonzalez, R TI Acetaldehyde in star-forming regions SO SPACE LIFE SCIENCES: STEPS TOWARD ORIGIN(S) OF LIFE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TEXAS SP Comm Space Res DE ISM : abundances; ISM : clouds; ISM : molecules; stars : information ID DENSE INTERSTELLAR CLOUDS; INTER-STELLAR CLOUDS; MOLECULAR CLOUDS; GALACTIC-CENTER; ETHYLENE-OXIDE; ABUNDANCES; CHEMISTRY; COMETS; CO; HYDROCARBONS AB Observations of acetaldehyde (CH3CHO) in a survey of nine star-forming regions are presented. Emission is clearly detected from both the A and E symmetry states in the 4(04)-3(03) and 5(05)-4(04) transitions. Both the range of the measured CH3CHO column densities (similar to 4 x 10(12) -10(14) cm(-2)), and the derived fractional abundances, are in good agreement with other studies. The origin of interstellar CH3CHO and its structural isomers is discussed in the light of this work and previous observations. It is concluded that specific grain-surface chemistries are responsible for the production of the C2H4O compounds and other related organic molecules. Possible observational tests to distinguish between different Surface pathways are Suggested. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Charnley, SB (reprint author), NASA, Ames Res Ctr, Div Space Sci, MS 245-3, Moffett Field, CA 94035 USA. EM charnley@dusty.arc.nasa.gov RI Charnley, Steven/C-9538-2012 NR 43 TC 30 Z9 30 U1 1 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 33 IS 1 BP 23 EP 30 DI 10.1016/j.asr.2003.08.005 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Biochemistry & Molecular Biology; Biology; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Geology; Meteorology & Atmospheric Sciences GA BY96E UT WOS:000189505400003 ER PT S AU Kuan, YJ Charnley, SB Huang, HC Kisiel, Z Ehrenfreund, P Tseng, WL Yan, CH AF Kuan, YJ Charnley, SB Huang, HC Kisiel, Z Ehrenfreund, P Tseng, WL Yan, CH BE Bernstein, MP Kress, M NavarroGonzalez, R TI Searches for interstellar molecules of potential preblotic importance SO SPACE LIFE SCIENCES: STEPS TOWARD ORIGIN(S) OF LIFE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TEXAS SP Comm Space Res DE astrobiology; ISM : abundances; ISM : individual (Orion kleinmann-low Sagittarius B2(N-LMH), W51 el/e2); ISM : molecules; line : identification; radio lines : ISM ID LINE SURVEY; ORGANIC-MOLECULES; AMINO-ACIDS; SAGITTARIUS B2; GAS-PHASE; ORION-KL; GLYCINE; GHZ; ABUNDANCES; CONFORMER AB Interstellar chemistry leads to the formation of many prebiologically important molecules and is therefore of the fundamental interest to Astrobiology. Many organics can be produced in the gas phase where they can be detected. Molecules formed by reactions on the surfaces of dust grains are also best detected by millimeter-wave observations of sources in which the products of grain-surface chemistry have been deposited into the gas phase. In this article, we present a summary of the status of several searches for potential prebiotic molecules - aziridine, 2H-azirine, pyrimidine and glycine - in the hot molecular cores Sgr B2(N-LMH), W51 e1/e2 and Orion KL. Detections of these organic molecules would strengthen the thesis that interstellar organic matter, delivered in cometary impacts, could have played an important role in the prebiotic chemistry of the early Earth. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 116, Taiwan. Acad Sinica, Inst Astron & Astrophys, Tokyo 106, Japan. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94305 USA. Polish Acad Sci, Inst Phys, PL-02668 Warsaw, Poland. Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Kuan, YJ (reprint author), Natl Taiwan Normal Univ, Dept Earth Sci, 88 Ting Chou Rd,Sec 4, Taipei 116, Taiwan. EM kuan@sgrb2.geos.ntnu.edu.tw RI Charnley, Steven/C-9538-2012; Kisiel, Zbigniew/K-8798-2016 OI Kisiel, Zbigniew/0000-0002-2570-3154 NR 46 TC 33 Z9 33 U1 2 U2 16 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 33 IS 1 BP 31 EP 39 DI 10.1016/j.asr.2003.04.004 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Biochemistry & Molecular Biology; Biology; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Geology; Meteorology & Atmospheric Sciences GA BY96E UT WOS:000189505400004 ER PT S AU Bernstein, MP Bauschlicher, CW Sandford, SA AF Bernstein, MP Bauschlicher, CW Sandford, SA BE Bernstein, MP Kress, M NavarroGonzalez, R TI The infrared spectrum of matrix isolated aminoacetonitrile, a precursor to the amino acid glycine SO SPACE LIFE SCIENCES: STEPS TOWARD ORIGIN(S) OF LIFE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TEXAS SP Comm Space Res DE amino acid; glycine; meteorite; IR spectroscopy; nitrile ID ICE ANALOGS AB We present infrared (IR) spectral data from matrix isolation experiments and density functional theory calculations on the pre-biologically interesting molecule aminoacetonitrile, a precursor to glycine. We find that this nitrile has an unusually weak nitrile (CdropN) stretch in the infrared, in contrast to expectations based on measurements and models of other nitriles under astrophysical conditions. The absence of an observable nitrile absorption feature in the infrared will make the search for this molecule by IR considerably more difficult, if not impossible. This is also of relevance to assessing the formation routes of the amino acid glycine, since aminoacetonitrile is the putative precursor to glycine via the Strecker synthesis, the mechanism postulated to have produced the amino acid glycine in meteorites. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. SETI Inst, Mountain View, CA 94043 USA. RP Bernstein, MP (reprint author), NASA, Ames Res Ctr, Mail Stop 245-6, Moffett Field, CA 94035 USA. EM mbernstein@mail.arc.nasa.gov; mbernstein@mail.arc.nasa.gov NR 15 TC 21 Z9 21 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 33 IS 1 BP 40 EP 43 DI 10.1016/j.asr.2003.07.002 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Biochemistry & Molecular Biology; Biology; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Geology; Meteorology & Atmospheric Sciences GA BY96E UT WOS:000189505400005 ER PT S AU Flynn, GJ Keller, LP Jacobsen, C Wirick, S AF Flynn, GJ Keller, LP Jacobsen, C Wirick, S BE Bernstein, MP Kress, M NavarroGonzalez, R TI An assessment of the amount and types of organic matter contributed to the Earth by interplanetary dust SO SPACE LIFE SCIENCES: STEPS TOWARD ORIGIN(S) OF LIFE SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE interplanetary dust; organic matter; carbonyl; aliphatic hydrocarbons; murchison meteorite ID COSMIC DUST; PARTICLES; IDENTIFICATION; SPECTROSCOPY; ASTEROIDS; COMETS AB A continuous, planet-wide rain of about 30,000 tons/year of interplanetary dust accretes onto the Earth. The mass-frcquency distribution of this dust is sharply peaked at about 400 pin, but the larger particles are most severely heated during atmospheric deceleration, with many of them vaporizing as meteors. Modeling of the peak temperature distribution experienced during atmospheric entry indicates that particles near 10 mum in size contribute the bulk of the mass that is not heated above 600 degreesC, which is believed to be the mean pyrolysis temperature of extraterrestrial organic matter. We have used infrared spectroscopy and X-ray absorption near-edge structure spectroscopy to characterize the types and abundance of organic matter in similar to10 mum interplanetary dust particles collected from the Earth's stratosphere. These particles contain high abundance, from a few to over 90 vol% of carbon, including percent-levels of both carbonyl (C=O) and aliphatic hydrocarbons (C-H(3) and C-H(2)). We estimate that, in the current era interplanetary dust contributes similar to15 tons/year of unpyrolized organic matter to the surface of the Earth. During the first 0.6 billion years of Earth's history, this contribution is likely to have been much greater. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77051 USA. SUNY Stony Brook, Dept Phys, Stony Brook, NY 11794 USA. RP Flynn, GJ (reprint author), SUNY Coll Plattsburgh, Dept Phys, 101 Broad St, Plattsburgh, NY 12901 USA. EM George.flynn@plattsburgh.edu RI Jacobsen, Chris/E-2827-2015 OI Jacobsen, Chris/0000-0001-8562-0353 NR 24 TC 43 Z9 44 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2004 VL 33 IS 1 BP 57 EP 66 DI 10.1016/j.asr.2003.09.036 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Biochemistry & Molecular Biology; Biology; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Geology; Meteorology & Atmospheric Sciences GA BY96E UT WOS:000189505400008 ER PT S AU Dworkin, JP Gillette, JS Bernstein, MP Sandford, SA Allamandola, LJ Elsila, JE McGlothlin, DR Zare, RN AF Dworkin, JP Gillette, JS Bernstein, MP Sandford, SA Allamandola, LJ Elsila, JE McGlothlin, DR Zare, RN BE Bernstein, MP Kress, M NavarroGonzalez, R TI An evolutionary connection between interstellar ices and IDPs? Clues from mass spectroscopy measurements of laboratory simulations SO SPACE LIFE SCIENCES: STEPS TOWARD ORIGIN(S) OF LIFE SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res ID ANALOGS; IRRADIATION; PHOTOLYSIS; METEORITES; MOLECULES; METHANOL; CLOUDS AB We present mass spectra of the residual organic matter that results from the ultraviolet photolysis of realistic interstellar ice analogs in the laboratory. The mass spectra show that this residue is a complex mixture of high molecular weight organic molecules, reminiscent of those reported for interplanetary dust particles (IDPs) - asteroidal and cometary dust. This represents a further characterization of the material for which we have already reported amphiphilic properties (Dworkin et al., 2001). If we assume that the compounds observed are conjugated hydrocarbons, the mass spectra of the organics are consistent with organic Compounds of up to 22 carbon atoms. Heating in air at low-pressure up to 1470 K as a simulation of atmospheric entry increases the molecular masses detected by muL(2)MS, resulting in a spectrum similar to those of the IDPs Florianus, and Aurelian. The results presented here are consistent with the notion that some of the large organic molecules delivered to the Earth on IDPs could have had their origin in low-temperature ice chemistry. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Stanford Univ, Dept Chem, Stanford, CA 94305 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. SETI Inst, Mountain View, CA 94043 USA. RP Dworkin, JP (reprint author), NASA, Goddard Space Flight Ctr, Code 691-0, Greenbelt, MD 20771 USA. EM jason.p.dworkin@nasa.gov RI Zare, Richard/A-8410-2009; Elsila, Jamie/C-9952-2012; Dworkin, Jason/C-9417-2012 OI Dworkin, Jason/0000-0002-3961-8997 NR 18 TC 13 Z9 13 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2004 VL 33 IS 1 BP 67 EP 71 DI 10.1016/j.asr.2003.08.004 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Biochemistry & Molecular Biology; Biology; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Geology; Meteorology & Atmospheric Sciences GA BY96E UT WOS:000189505400009 ER PT S AU Glavin, DP Matrajt, G Bada, JL AF Glavin, DP Matrajt, G Bada, JL BE Bernstein, MP Kress, M NavarroGonzalez, R TI Re-examination of amino acids in Antarctic micrometeorites SO SPACE LIFE SCIENCES: STEPS TOWARD ORIGIN(S) OF LIFE SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE amino acids; micrometeorites; prebiotic organic inventory ID CARBONACEOUS CHONDRITES; ATMOSPHERIC ENTRY; EXTRATERRESTRIAL DELIVERY; ACCRETION RATE; COSMIC DUST; PARENT BODY; COLLECTION; HYDROLYSIS; MURCHISON; METEORITE AB The delivery of amino acids by micrometeorites to the early Earth during the period of heavy bombardment (4.5-3.5 Ga) could have been a significant source of the Earth's prebiotic organic inventory. Antarctic micrometeorites (AMMs) in the 100-200 mum size range represent the dominant mass fraction of extraterrestrial material accreted by the Earth today. However, one problem is that these 'large' micrometeorite grains can be heated to very high temperatures (1000 to 1500 degreesC) during atmospheric deceleration, causing the amino acids to decompose. In this study, we have analyzed the acid-hydrolyzed, hot water extracts from 455 AMMs for the presence of amino acids using high performance liquid chromatography. For comparison, a 5 mg sample of the CM meteorite Murchison was also investigated. In the Murchison sample we found high levels (similar to3-4 parts-per-million, ppm) of alpha-aminoisobutyric acid (AIB) and isovaline, two non-protein amino acids that are extremely rare on Earth and are characteristic of amino acids of apparent extraterrestrial origin. In contrast, we were unable to detect any AIB above the 0.1 ppm level in the AMM samples studied. Only in one AMM sample from a previous study has AIB been detected (similar to300 ppm). To date, more than 600 AMMs have been analyzed for extraterrestrial amino acids. Although our results indicate that less than 5% of all AMMs contain detectable levels of AIB, we cannot rule out the possibility that AIB can be delivered to the Earth intact by a small percentage of AMMs that escaped extensive heating during atmospheric entry. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. CNRS, CSNSM, F-91405 Orsay, France. Univ Paris 11, IAS, F-91405 Orsay, France. RP Glavin, DP (reprint author), NASA, Goddard Space Flight Ctr, Code 915, Greenbelt, MD 20771 USA. EM dglavin@comcast.net RI Glavin, Daniel/D-6194-2012 OI Glavin, Daniel/0000-0001-7779-7765 NR 35 TC 26 Z9 26 U1 0 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2004 VL 33 IS 1 BP 106 EP 113 DI 10.1016/j.asr.2003.02.011 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Biochemistry & Molecular Biology; Biology; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Geology; Meteorology & Atmospheric Sciences GA BY96E UT WOS:000189505400016 ER PT S AU DeVore, E Oliver, C Wilmoth, K Vozzo, L AF DeVore, E Oliver, C Wilmoth, K Vozzo, L BE Lopez, RE Morrow, CA Machado, ME Fellous, JL TI Science Education in Partnership: The 2002 Australian-American Fulbright Symposium SO SPACE SCIENCE EDUCATION AND PROMOTING NORTH-SOUTH PARTNERSHIP IN SPACE RESEARCH SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE Fulbright Symposium; science education; American and Australian science education; bioastronomy; astrobiology AB The Australian American Fulbright 2002 Symposium: Science Education in Partnership was held in parallel-in partnership-with the scientific meeting of the IAU 213 Bioastronomy 2002 Symposium: Life Among the Stars. In practice, the two meetings modeled partnership between educators and scientists, both professional events interacting while maintaining individual goals. Leading scientists attending the IAU meeting participated in the Fulbright with presentations based upon their work and their experiences. Educators and scientists interacted on how their work impacts science education and strategies for building direct connections between scientists and classrooms. Educators attending the Fulbright Symposium attended a number of scientific presentations in IAU meeting as well. A major issue in science education is teaching science in a way that is relevant to the student. Partnerships between scientists and teachers can provide real-life scientific research experience in the laboratory and the field for teachers and students. These partnerships enhance the quality of both teaching and learning, and engage students directly in projects and curricula that lead to a better understanding of the nature and practice of science. Scientists are often engaged in the development of new curricula as a part of the education and public outreach programs affiliated with research programs. Participants explored the similarities and differences between the approach to this endeavor in Australia and the US. Partnerships between all the professionals involved-scientists, teachers, and writers-creates an opportunity for innovative, cutting-edge research to reach the classroom. The excitement of seeking new knowledge, exploring the unknown, can motivate students to pursue science studies in high school and beyond at the university. Oral papers, posters and workshops presented the results of partnerships between scientists and educators in Australian and the USA as well as opportunities for future partnerships. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 SETI Inst, Mountain View, CA 95148 USA. Macquarie Univ, Australian Ctr Astrobiol, Dept Earth & Planetary Sci, Sydney, NSW 2109, Australia. NASA, Ames Res Ctr, Astrobiol Inst, Moffett Field, CA 94035 USA. Univ Western Sydney, Sch Educ & Early Childhood Studies, Penrith, NSW, Australia. RP DeVore, E (reprint author), SETI Inst, 2035 Landings Dr, Mountain View, CA 95148 USA. EM edevore@seti.org NR 0 TC 1 Z9 1 U1 3 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 10 BP 2116 EP 2120 DI 10.1016/j.asr.2003.09.066 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Education, Scientific Disciplines; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Education & Educational Research; Geology; Meteorology & Atmospheric Sciences GA BBN84 UT WOS:000226378300002 ER PT S AU Rosendhal, J Sakimoto, P Pertzborn, R Cooper, L AF Rosendhal, J Sakimoto, P Pertzborn, R Cooper, L BE Lopez, RE Morrow, CA Machado, ME Fellous, JL TI The NASA Office of Space Science Education and Public Outreach Program SO SPACE SCIENCE EDUCATION AND PROMOTING NORTH-SOUTH PARTNERSHIP IN SPACE RESEARCH SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE Space Science education; NASA; outreach program; astronomy education AB Over the past six years, NASA's Office of Space Science has implemented what may well be the largest single program in astronomy and space science education ever undertaken. The program goals include the public sharing of the excitement of space science discoveries. enhancement of the quality of science. mathematics and technology education, particularly at the precollege level. and supporting the creation of our 21st century scientific and technical workforce. This paper provides an overview of the program origins, policies and philosophies, and describes the development and growth of the program. Program accomplishments and the challenges that remain are discussed along with potential opportunities for international collaboration. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Off Space Sci, NASA Headquarters, Washington, DC 20546 USA. RP Cooper, L (reprint author), NASA, Off Space Sci, NASA Headquarters, Code S, Washington, DC 20546 USA. EM Larry.P.Cooper@nasa.gov NR 17 TC 3 Z9 3 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 10 BP 2127 EP 2135 DI 10.1016/j.asr.2003.03.069 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Education, Scientific Disciplines; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Education & Educational Research; Geology; Meteorology & Atmospheric Sciences GA BBN84 UT WOS:000226378300004 ER PT S AU Marshall, J Taylor, W Pine, B Green, J AF Marshall, J Taylor, W Pine, B Green, J BE Lopez, RE Morrow, CA Machado, ME Fellous, JL TI Authentic science experiences for high school students: the INSPIRE example SO SPACE SCIENCE EDUCATION AND PROMOTING NORTH-SOUTH PARTNERSHIP IN SPACE RESEARCH SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE NASA INSPIRE program; VLF radio receivers; high school students; space science investigations for students AB The National Science Education Standards call for students to participate in authentic scientific investigation [National Science Education Standards, National Academies Press, Washington, DC, 1996]. Opportunities are rare. however. for students to experience the full spectrum of space science investigation: developing and assembling equipment, planning observations. obtaining and recording data in coordination with other observers, analyzing data and, finally, publishing results. The interactive NASA Space Physics Ionospheric Radio Experiment (INSPIRE) is one outgoing program that provides high school students withjust such opportunities. INSPIRE participants assemble and test very low frequency (VLF) radio receivers. use them to record natural and artificial atmospheric radio signals as part of a coordinated campaign, analyze the resulting data, and publish their results in The INSPIRE Journal and elsewhere. The investigations students carry out as part of INSPIRE are not the canned experiments usually found in high school laboratories. Rather. INSPIRE seeks to answer authentic questions about the propagation of radio waves in the ionosphere and magnetosphere. For example, INSPIRE participants provided around stations for a virtual antenna experiment on a 1992 Shuttle mission. This article presents the history of the program, an example of student observations. and reports of how INSPIRE has affected students' views of science and of themselves as scientists. Published by Elsevier Ltd on behalf of COSPAR. C1 Univ Texas, Dept Curriculum & Instruct, Austin, TX 78712 USA. Raytheon ITSS, GSFCI, Greenbelt, MD 20771 USA. Chaffey High Sch, Ontario, CA 91762 USA. Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Marshall, J (reprint author), Univ Texas, Dept Curriculum & Instruct, Austin, TX 78712 USA. EM marshall@mail.utexas.edu NR 20 TC 0 Z9 0 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 10 BP 2145 EP 2152 DI 10.1016/j.asr.2003.03.071 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Education, Scientific Disciplines; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Education & Educational Research; Geology; Meteorology & Atmospheric Sciences GA BBN84 UT WOS:000226378300006 ER PT S AU Piacentini, RD Luccini, E Micheletti, MI Quel, E Wolfram, EA Pazmino, AF Fochesatto, J Crino, E Cede, A Blumthaler, M Herman, J Godin-Beekmann, S Megie, G AF Piacentini, RD Luccini, E Micheletti, MI Quel, E Wolfram, EA Pazmino, AF Fochesatto, J Crino, E Cede, A Blumthaler, M Herman, J Godin-Beekmann, S Megie, G BE Lopez, RE Morrow, CA Machado, ME Fellous, JL TI Satellite and ground measurements of solar erythemal UV radiation and ozone in Argentina SO SPACE SCIENCE EDUCATION AND PROMOTING NORTH-SOUTH PARTNERSHIP IN SPACE RESEARCH SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE solar erythermal UV radiation; ozone; satellite and ground measurements; Argentina; TOMS measurements ID SURFACES; ALBEDO AB Solar erythemal UV radiation incident on Argentina from tropical to high latitude regions has been measured with ground-based instruments as well as with the TOMS instrument on board of the NASA Earth-Probe satellite. These data permit validation of the UV index, a measure of solar risk to UV exposure, forecasted daily by CONAE (Argentina National Commission on Space Activities) and the Argentine National Weather Service. Model calculations of this index are also presented. In addition. we analyzed the UV effects from the Antarctic ozone hole passing over the continental part of the country using TOMS data corrected by a factor derived from the intercomparison of TOMS satellite data with those determined with Southern Hemisphere ground-based spectroradiometers. In this way, we obtained a rather comprehensive description of the amount of erythemal UV radiation and consequently of the UV index for the entire country, as well as the ozone total column and profile (the latter one at Buenos Aires). The results presented in this work were determined through collaboration between the following institutions: GSFC/NASA in USA. Institute Pierre Simon Laplace in France, University of Innsbruck in Austria and CEILAP. IFIR. CONAE. SMN. Universities of Rosario and San Luis in Argentina. The need to use erythemal irradiance and ozone results in Argentina. one of the most exposed regions of the Southern Hemisphere to study the effects of ozone depletion and consequently UV detrimental effects. has. been partially covered in the framework of this North-South collaboration. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Nacl Rosario, Inst Fis Rosario, CONICET, RA-2000 Rosario, Santa Fe, Argentina. Univ Nacl Rosario, Fac Ciencias Exactas Ingn & Agrimensura, RA-2000 Rosario, Santa Fe, Argentina. Univ Nacl Rosario, Fac Ciencias Bioquim & Farmaceut, RA-2000 Rosario, Santa Fe, Argentina. CEILAP, CITEFA, CONICET, Buenos Aires, DF, Argentina. IPSL, Serv Aeron, Paris, France. Univ Nacl San Luis, San Luis Obispo, Argentina. Univ Innsbruck, Inst Med Phys, A-6020 Innsbruck, Austria. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Piacentini, RD (reprint author), Univ Nacl Rosario, Inst Fis Rosario, CONICET, 27 Febrero 210Bis, RA-2000 Rosario, Santa Fe, Argentina. EM ruben@ifir.edu.ar OI Herman, Jay/0000-0002-9146-1632 NR 23 TC 5 Z9 5 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2004 VL 34 IS 10 BP 2221 EP 2226 DI 10.1016/j.asr.2003.07.058 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Education, Scientific Disciplines; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Education & Educational Research; Geology; Meteorology & Atmospheric Sciences GA BBN84 UT WOS:000226378300020 ER PT S AU Fochesatto, J Ristori, P Flamant, P Machado, ME Singh, U Quel, E AF Fochesatto, J Ristori, P Flamant, P Machado, ME Singh, U Quel, E BE Lopez, RE Morrow, CA Machado, ME Fellous, JL TI Backscatter LIDAR signal simulation applied to spacecraft LIDAR instrument design SO SPACE SCIENCE EDUCATION AND PROMOTING NORTH-SOUTH PARTNERSHIP IN SPACE RESEARCH SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE space LIDAR; aerosols; LIDAR simulation AB in the framework of the scientific cooperation between the CEILAP laboratory (Argentina) and IPSL Institut Pierre Simon Laplace (France), devoted to the development of LIDAR techniques for Atmospheric sciences. a new area of scientific research. involving LIDARs, is starting in Argentine space technology. This new research area is under consideration at CEILAP in a joint effort with CONAE, the Argentine space agency, responsible for the development of future space missions. The LIDAR technique is necessary to improve our knowledge of meteorological, dynamic, and radiative processes in the South American region. for the whole troposphere and the lower stratosphere. To study this future mission, a simple model for the prediction of back-scatter LIDAR signal from a spacecraft platform has been used to determine dimensions and detection characteristics of the space borne LIDAR instrument. The backscatter signal was retrieved from a modeled atmosphere considering its molecular density profile and taking into account different aerosols and clouds conditions. Signal-to-noise consideration. within the interval of possible dimension of the instrument parameters, allows us to constrain the telescope receiving area and to derive maximum range achievable. integration time and the final spatial and temporal resolutions of backscatter profiles. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Consejo Nacl Invest Cient & Tecn, CEILAP, CITEFA, RA-1033 Buenos Aires, DF, Argentina. Ecole Polytech, LMD, IPSL, F-91128 Palaiseau, France. CONAE, RA-1063 Buenos Aires, DF, Argentina. NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Quel, E (reprint author), Consejo Nacl Invest Cient & Tecn, CEILAP, CITEFA, San Juan B Salle 4397,B1603 ALO,Villa Martelli, RA-1033 Buenos Aires, DF, Argentina. EM quel@citefa.gov.ar; quel@citefa.gov.ar NR 14 TC 4 Z9 4 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 10 BP 2227 EP 2231 DI 10.1016/j.asr.2003.07.062 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Education, Scientific Disciplines; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Education & Educational Research; Geology; Meteorology & Atmospheric Sciences GA BBN84 UT WOS:000226378300021 ER PT S AU Otero, LA Fochesatto, GJ Ristori, PR Flamant, PH Piacentini, RD Holben, B Quel, EJ AF Otero, LA Fochesatto, GJ Ristori, PR Flamant, PH Piacentini, RD Holben, B Quel, EJ BE Lopez, RE Morrow, CA Machado, ME Fellous, JL TI Simple method to derive aerosol microphysical properties from AERONET multiwavelength direct solar measurements SO SPACE SCIENCE EDUCATION AND PROMOTING NORTH-SOUTH PARTNERSHIP IN SPACE RESEARCH SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE derive aerosol microphysical properties; aeronet multiwavelength solar measurements; aerosol optical properties; aerosol robotic network ID OPTICAL-PROPERTIES; INVERSION; RETRIEVAL AB We present a simple method to retrieve aerosol optical properties from direct solar measurements obtained using sun-photometer measurements from AERONET (Aerosol Robotic Network). This monitoring program is a federation of ground-based remote sensing aerosol network conducted by NASA. The goal of this network is to assess the aerosol optical properties and to validate their retrievals with satellite information. Data from this collaboration provide globally distributed observations of spectral aerosol optical thickness, precipitation water, and aerosol volume size distribution (derived from the inversion products) in geographically diverse aerosol regimes. In this work, we present a simple method to deduce the aerosol microphysical properties in the submicrometer radius range, which were derived from the aerosol optical thickness measurements using Mie kernel functions with a proposed synthetic radius spectrum. Results and comparison of this inversion procedure with other standard inversion products are shown for Buenos Aires (CEILAP) and Cordoba (CETT) sites of AERONET network. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Consejo Nacl Invest Cient & Tecn, CEILAP, CITEFA, RA-1033 Buenos Aires, DF, Argentina. Ecole Polytech Fed Lausanne, Lab Pollut Air & Sol, Lausanne, Switzerland. Ecole Polytech, LMD, IPSL, F-91128 Palaiseau, France. Univ Nacl Rosario, CONICET, Inst Fis Rosario, RA-2000 Rosario, Santa Fe, Argentina. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Otero, LA (reprint author), Consejo Nacl Invest Cient & Tecn, CEILAP, CITEFA, San Juan,B Salle 4397,B1603 ALO Villa Martelli, RA-1033 Buenos Aires, DF, Argentina. EM otero@citefa.gov.ar OI FOCHESATTO, Gilberto J/0000-0003-0813-6765 NR 12 TC 3 Z9 3 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 10 BP 2232 EP 2235 DI 10.1016/j.asr.2003.07.059 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Education, Scientific Disciplines; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Education & Educational Research; Geology; Meteorology & Atmospheric Sciences GA BBN84 UT WOS:000226378300022 ER PT J AU Kliore, AJ Anderson, JD Armstrong, JW Asmar, SW Hamilton, CL Rappaport, NJ Wahlquist, HD Ambrosini, R Flasar, FM French, RG Iess, L Marouf, EA Nagy, AF AF Kliore, AJ Anderson, JD Armstrong, JW Asmar, SW Hamilton, CL Rappaport, NJ Wahlquist, HD Ambrosini, R Flasar, FM French, RG Iess, L Marouf, EA Nagy, AF TI Cassini radio science SO SPACE SCIENCE REVIEWS LA English DT Review DE atmospheres; Cassini; gravitational fields; gravitational waves; general relativity; ionospheres; occultations; planetary rings; radio science; Saturn; Titan ID PARTICLE-SIZE DISTRIBUTIONS; TITANS UPPER-ATMOSPHERE; SATURNS RINGS; OCCULTATION MEASUREMENTS; URANIAN RINGS; PLANETARY RINGS; DENSITY WAVES; VOYAGER OBSERVATIONS; DOPPLER MEASUREMENTS; COALESCING BINARIES AB Cassini radio science investigations will be conducted both during the cruise ( gravitational wave and conjunction experiments) and the Saturnian tour of the mission ( atmospheric and ionospheric occultations, ring occultations, determinations of masses and gravity fields). New technologies in the construction of the instrument, which consists of a portion on-board the spacecraft and another portion on the ground, including the use of the Ka-band signal in addition to that of the S- and X-bands, open opportunities for important discoveries in each of the above scientific areas, due to increased accuracy, resolution, sensitivity, and dynamic range. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CNR, Ist Radioastron, I-40129 Bologna, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Wellesley Coll, Wellesley, MA 02481 USA. Univ Roma La Sapienza, I-00184 Rome, Italy. San Jose State Univ, San Jose, CA 95192 USA. Univ Michigan, Ann Arbor, MI 48109 USA. RP Kliore, AJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM akliore@jpl.nasa.gov RI IESS, Luciano/F-4902-2011; Flasar, F Michael/C-8509-2012 OI IESS, Luciano/0000-0002-6230-5825; NR 277 TC 49 Z9 49 U1 1 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD JAN PY 2004 VL 115 IS 1-4 BP 1 EP 70 DI 10.1007/s11214-004-1436-y PG 70 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905EE UT WOS:000227549900001 ER PT J AU Elachi, C Allison, MD Borgarelli, L Encrenaz, P Im, E Janssen, MA Johnson, WTK Kirk, RL Lorenz, RD Lunine, JI Muhleman, DO Ostro, SJ Picardi, G Posa, F Rapley, CG Roth, LE Seu, R Soderblom, LA Vetrella, S Wall, SD Wood, CA Zebker, HA AF Elachi, C Allison, MD Borgarelli, L Encrenaz, P Im, E Janssen, MA Johnson, WTK Kirk, RL Lorenz, RD Lunine, JI Muhleman, DO Ostro, SJ Picardi, G Posa, F Rapley, CG Roth, LE Seu, R Soderblom, LA Vetrella, S Wall, SD Wood, CA Zebker, HA TI Radar: The Cassini Titan RADAR Mapper SO SPACE SCIENCE REVIEWS LA English DT Review ID DIELECTRIC-CONSTANT; SURFACE; MAGELLAN; VENUS; ATMOSPHERE; METHANE; OCEAN; TROPOSPHERE; OCCULTATION; TOPOGRAPHY AB The Cassini RADAR instrument is a multimode 13.8 GHz multiple-beam sensor that can operate as a synthetic-aperture radar (SAR) imager, altimeter, scatterometer, and radiometer. The principal objective of the RADAR is to map the surface of Titan. This will be done in the imaging, scatterometer, and radiometer modes. The RADAR altimeter data will provide information on relative elevations in selected areas. Surfaces of the Saturn's icy satellites will be explored utilizing the RADAR radiometer and scatterometer modes. Saturn's atmosphere and rings will be probed in the radiometer mode only. The instrument is a joint development by JPL/NASA and ASI. The RADAR design features significant autonomy and data compression capabilities. It is expected that the instrument will detect surfaces with backscatter coefficient as low as -40 dB. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Alenia Aerosp, I-00131 Rome, Italy. Observ Paris, F-92195 Meudon, France. US Geol Survey, Flagstaff, AZ 86001 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Univ Roma La Sapienza, I-00184 Rome, Italy. Politecn Bari, Dip Interateneo Fis, I-70126 Bari, Italy. British Antarctic Survey, Cambridge CB3 0ET, England. Fac Ingn, I-80125 Naples, Italy. Univ N Dakota, Grand Forks, ND 58202 USA. Stanford Univ, Stanford, CA 94305 USA. RP Wall, SD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM stephen.d.wall@jpl.nasa.gov RI Lorenz, Ralph/B-8759-2016 OI Lorenz, Ralph/0000-0001-8528-4644 NR 54 TC 92 Z9 94 U1 0 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD JAN PY 2004 VL 115 IS 1-4 BP 71 EP 110 DI 10.1007/s11214-004-1438-9 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905EE UT WOS:000227549900002 ER PT J AU Flasar, FM Kunde, VG Abbas, MM Achterberg, RK Ade, P Barucci, A Bezard, B Bjoraker, GL Brasunas, JC Calcutt, S Carlson, R Esarsky, CJC Conrath, BJ Coradini, A Courtin, R Coustenis, A Edberg, S Edgington, S Ferrari, C Fouchet, T Gautier, D Gierasch, PJ Grossman, K Irwin, P Jennings, DE Lellouch, E Mamoutkine, AA Marten, A Meyer, JP Nixon, CA Orton, GS Owen, TC Pearl, JC Prange, R Raulin, F Read, PL Romani, PN Samuelson, RE Segura, ME Showalter, MR Simon-Miller, AA Smith, MD Spencer, JR Spilker, LJ Taylor, FW AF Flasar, FM Kunde, VG Abbas, MM Achterberg, RK Ade, P Barucci, A Bezard, B Bjoraker, GL Brasunas, JC Calcutt, S Carlson, R Esarsky, CJC Conrath, BJ Coradini, A Courtin, R Coustenis, A Edberg, S Edgington, S Ferrari, C Fouchet, T Gautier, D Gierasch, PJ Grossman, K Irwin, P Jennings, DE Lellouch, E Mamoutkine, AA Marten, A Meyer, JP Nixon, CA Orton, GS Owen, TC Pearl, JC Prange, R Raulin, F Read, PL Romani, PN Samuelson, RE Segura, ME Showalter, MR Simon-Miller, AA Smith, MD Spencer, JR Spilker, LJ Taylor, FW TI Exploring the Saturn system in the thermal infrared: The Composite Infrared Spectrometer SO SPACE SCIENCE REVIEWS LA English DT Review DE infrared spectroscopy; Saturn; Titan; Saturn's rings; Saturn's moons; atmospheric temperatures; atmospheric composition; atmospheric dynamics; Cassini ID VOYAGER-1 RADIO-OCCULTATION; HUBBLE-SPACE-TELESCOPE; SUBMILLIMETER HETERODYNE OBSERVATIONS; EXTREME-ULTRAVIOLET OBSERVATIONS; FOURIER-TRANSFORM SPECTROMETERS; 1990 EQUATORIAL DISTURBANCE; LARGE-SCALE INSTABILITIES; ABSOLUTE BAND INTENSITY; PROBE MASS-SPECTROMETER; PARA-HYDROGEN FRACTION AB The Composite Infrared Spectrometer (CIRS) is a remote-sensing Fourier Transform Spectrometer (FTS) on the Cassini orbiter that measures thermal radiation over two decades in wavenumber, from 10 to 1400 cm(-1) (1 mm to 7 mu m), with a spectral resolution that can be set from 0.5 to 15.5 cm(-1). The far infrared portion of the spectrum (10-600 cm(-1)) is measured with a polarizing interferometer having thermopile detectors with a common 4-mrad field of view (FOV). The middle infrared portion is measured with a traditional Michelson interferometer having two focal planes (600-1100 cm(-1), 1100-1400 cm(-1)). Each focal plane is composed of a 1 x 10 array of HgCdTe detectors, each detector having a 0.3-mrad FOV. CIRS observations will provide three-dimensional maps of temperature, gas composition, and aerosols/condensates of the atmospheres of Titan and Saturn with good vertical and horizontal resolution, from deep in their tropospheres to high in their mesospheres. CIRS's ability to observe atmospheres in the limb-viewing mode ( in addition to nadir) offers the opportunity to provide accurate and highly resolved vertical profiles of these atmospheric variables. The ability to observe with high-spectral resolution should facilitate the identification of new constituents. CIRS will also map the thermal and compositional properties of the surfaces of Saturn's icy satellites. It will similarly map Saturn's rings, characterizing their dynamical and spatial structure and constraining theories of their formation and evolution. The combination of broad spectral range, programmable spectral resolution, the small detector fields of view, and an orbiting spacecraft platform will allow CIRS to observe the Saturnian system in the thermal infrared at a level of detail not previously achieved. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, College Pk, MD 20742 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. Cardiff Univ, Cardiff CF24 3YB, S Glam, Wales. Observ Paris, F-92195 Meudon, France. Univ Oxford, Oxford OX1 3PU, England. European So Observ, D-85748 Garching, Germany. Cornell Univ, Ithaca, NY 14853 USA. Ist Astrofis Spaziale, I-00133 Rome, Italy. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CEA, Serv Astrophys, F-91191 Gif Sur Yvette, France. Univ Gesamthsch Wuppertal, D-5600 Wuppertal, Germany. Univ Hawaii, Honolulu, HI 96822 USA. Univ Paris & 12, F-94010 Creteil, France. QSS Grp Inc, Lanham, MD 20706 USA. Stanford Univ, Stanford, CA 94305 USA. SW Res Inst, Boulder, CO 80302 USA. RP Flasar, FM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM f.m.flasar@nasa.gov RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; Smith, Michael/C-8875-2012; Romani, Paul/D-2729-2012; Bjoraker, Gordon/D-5032-2012; Jennings, Donald/D-7978-2012; brasunas, john/I-2798-2013; Simon, Amy/C-8020-2012; Ferrari, Cecile/P-9735-2016; Fouchet, Thierry/C-6374-2017; OI Nixon, Conor/0000-0001-9540-9121; Simon, Amy/0000-0003-4641-6186; Ferrari, Cecile/0000-0001-5962-7439; Fouchet, Thierry/0000-0001-9040-8285; Calcutt, Simon/0000-0002-0102-3170; Irwin, Patrick/0000-0002-6772-384X NR 369 TC 181 Z9 181 U1 2 U2 20 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD JAN PY 2004 VL 115 IS 1-4 BP 169 EP 297 DI 10.1007/s11214-004-1454-9 PG 129 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905EE UT WOS:000227549900004 ER PT J AU Esposito, LW Barth, CA Colwell, JE Lawrence, GM McClintock, WE Stewart, AIF Keller, HU Korth, A Lauche, H Festou, MC Lane, AL Hansen, CJ Maki, JN West, RA Jahn, H Reulke, R Warlich, K Shemansky, DE Yung, YL AF Esposito, LW Barth, CA Colwell, JE Lawrence, GM McClintock, WE Stewart, AIF Keller, HU Korth, A Lauche, H Festou, MC Lane, AL Hansen, CJ Maki, JN West, RA Jahn, H Reulke, R Warlich, K Shemansky, DE Yung, YL TI The Cassini Ultraviolet Imaging Spectrograph investigation SO SPACE SCIENCE REVIEWS LA English DT Review DE Cassini; rings; Saturn; spectroscopy on Titan and on Saturn ID OUTER SOLAR-SYSTEM; VOYAGER INFRARED OBSERVATIONS; LYMAN-ALPHA EMISSION; TITANS ATMOSPHERE; D/H RATIO; MONODEUTERATED METHANE; VERTICAL-DISTRIBUTION; STELLAR OCCULTATION; PLANETARY RINGS; CARBON-MONOXIDE AB The Cassini Ultraviolet Imaging Spectrograph (UVIS) is part of the remote sensing payload of the Cassini orbiter spacecraft. UVIS has two spectrographic channels that provide images and spectra covering the ranges from 56 to 118 nm and 110 to 190 nm. A third optical path with a solar blind CsI photocathode is used for high signal-to-noise-ratio stellar occultations by rings and atmospheres. A separate Hydrogen Deuterium Absorption Cell measures the relative abundance of deuterium and hydrogen from their Lyman-alpha emission. The UVIS science objectives include investigation of the chemistry, aerosols, clouds, and energy balance of the Titan and Saturn atmospheres; neutrals in the Saturn magnetosphere; the deuterium-to-hydrogen (D/H) ratio for Titan and Saturn; icy satellite surface properties; and the structure and evolution of Saturn's rings. C1 Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. Max Planck Inst Aeron, D-37191 Katlenburg Lindau, Germany. Observ Midi Pyrenees, F-31400 Toulouse, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Deutsch Zentrum Luft & Raumfahrt, Inst Weltraumsensor & Planetenerkundung, D-12489 Berlin, Germany. Univ So Calif, Dept Aerosp Engn, Los Angeles, CA 90089 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Esposito, LW (reprint author), Univ Colorado, Atmospher & Space Phys Lab, 1234 Innovat Dr, Boulder, CO 80303 USA. EM larry.esposito@lasp.colorado.edu NR 165 TC 106 Z9 106 U1 0 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD JAN PY 2004 VL 115 IS 1-4 BP 299 EP 361 DI 10.1007/s11214-004-1455-8 PG 63 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905EE UT WOS:000227549900005 ER PT J AU Porco, CC West, RA Squyres, S McEwen, A Thomas, P Murray, CD Delgenio, A Ingersoll, AP Johnson, TV Neukum, G Veverka, J Dones, L Brahic, A Burns, JA Haemmerle, V Knowles, B Dawson, D Roatsch, T Beurle, K Owen, W AF Porco, CC West, RA Squyres, S McEwen, A Thomas, P Murray, CD Delgenio, A Ingersoll, AP Johnson, TV Neukum, G Veverka, J Dones, L Brahic, A Burns, JA Haemmerle, V Knowles, B Dawson, D Roatsch, T Beurle, K Owen, W TI Cassini Imaging Science: Instrument characteristics and anticipated scientific investigations at Saturn SO SPACE SCIENCE REVIEWS LA English DT Review DE Cassini; Saturn; imaging; rings; moons ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; DENSE PLANETARY RINGS; CONTROL POINT NETWORK; GREAT RED SPOT; GALILEAN SATELLITES; ICY SATELLITES; JUPITERS ATMOSPHERE; VOYAGER PHOTOMETRY; INTERNAL STRUCTURE; RADIO OCCULTATION AB The Cassini Imaging Science Subsystem (ISS) is the highest-resolution two-dimensional imaging device on the Cassini Orbiter and has been designed for investigations of the bodies and phenomena found within the Saturnian planetary system. It consists of two framing cameras: a narrow angle, reflecting telescope with a 2-m focal length and a square field of view (FOV) 0.35 degrees. across, and a wide-angle refractor with a 0.2-m focal length and a FOV 3.5 degrees. across. At the heart of each camera is a charged coupled device (CCD) detector consisting of a 1024 square array of pixels, each 12 mu on a side. The data system allows many options for data collection, including choices for on-chip summing, rapid imaging and data compression. Each camera is outfitted with a large number of spectral filters which, taken together, span the electromagnetic spectrum from 200 to 1100 nm. These were chosen to address a multitude of Saturn-system scientific objectives: sounding the three-dimensional cloud structure and meteorology of the Saturn and Titan atmospheres, capturing lightning on both bodies, imaging the surfaces of Saturn's many icy satellites, determining the structure of its enormous ring system, searching for previously undiscovered Saturnian moons ( within and exterior to the rings), peering through the hazy Titan atmosphere to its yet-unexplored surface, and in general searching for temporal variability throughout the system on a variety of time scales. The ISS is also the optical navigation instrument for the Cassini mission. We describe here the capabilities and characteristics of the Cassini ISS, determined from both ground calibration data and in-flight data taken during cruise, and the Saturn-system investigations that will be conducted with it. At the time of writing, Cassini is approaching Saturn and the images returned to Earth thus far are both breathtaking and promising. C1 Inst Space Sci, CICLOPS, Boulder, CO USA. Jet Propuls Lab, Pasadena, CA USA. Cornell Univ, Ithaca, NY USA. Univ Arizona, Tucson, AZ USA. Univ London Queen Mary Coll, London E1 4NS, England. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. CALTECH, Pasadena, CA 91125 USA. Free Univ Berlin, D-1000 Berlin, Germany. SW Res Inst, Boulder, CO USA. Univ Paris 07, Paris, France. DLR, Berlin, Germany. RP Porco, CC (reprint author), Inst Space Sci, CICLOPS, Boulder, CO USA. EM carolyn@ciclops.org RI Del Genio, Anthony/D-4663-2012 OI Del Genio, Anthony/0000-0001-7450-1359 NR 300 TC 188 Z9 189 U1 5 U2 31 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD JAN PY 2004 VL 115 IS 1-4 BP 363 EP 497 DI 10.1007/s11214-004-1456-7 PG 135 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 905EE UT WOS:000227549900006 ER PT J AU Young, DT Berthelier, JJ Blanc, M Burch, JL Coates, AJ Goldstein, R Grande, M Hill, TW Johnson, RE Kelha, V McComas, DJ Sittler, EC Svenes, KR Szego, K Tanskanen, P Ahola, K Anderson, D Bakshi, S Baragiola, RA Barraclough, L Black, RK Bolton, S Booker, T Bowman, R Casey, P Crary, FJ Delapp, D Dirks, G Eaker, N Funsten, H Furman, JD Gosling, JT Hannula, H Holmlund, C Huomo, H Illiano, JM Jensen, P Johnson, MA Linder, DR Luntama, T Maurice, S McCabe, KP Mursula, K Narheim, BT Nordholt, JE Preece, A Rudzki, J Ruitberg, A Smith, K Szalai, S Thomsen, MF Viherkanto, K Vilppola, J Vollmer, T Wahl, TE Wuest, M Ylikorpi, T Zinsmeyer, C AF Young, DT Berthelier, JJ Blanc, M Burch, JL Coates, AJ Goldstein, R Grande, M Hill, TW Johnson, RE Kelha, V McComas, DJ Sittler, EC Svenes, KR Szego, K Tanskanen, P Ahola, K Anderson, D Bakshi, S Baragiola, RA Barraclough, L Black, RK Bolton, S Booker, T Bowman, R Casey, P Crary, FJ Delapp, D Dirks, G Eaker, N Funsten, H Furman, JD Gosling, JT Hannula, H Holmlund, C Huomo, H Illiano, JM Jensen, P Johnson, MA Linder, DR Luntama, T Maurice, S McCabe, KP Mursula, K Narheim, BT Nordholt, JE Preece, A Rudzki, J Ruitberg, A Smith, K Szalai, S Thomsen, MF Viherkanto, K Vilppola, J Vollmer, T Wahl, TE Wuest, M Ylikorpi, T Zinsmeyer, C TI Cassini Plasma Spectrometer investigation SO SPACE SCIENCE REVIEWS LA English DT Review DE Saturn; Titan; magnetosphere; space plasma; ion composition ID ION MASS-SPECTROMETER; ULTRATHIN CARBON FOILS; SATURNS E-RING; TITANS IONOSPHERE; SOLAR-WIND; PICKUP IONS; WATER ICE; ELECTROSTATIC ANALYZERS; NEUTRAL GAS; MHD MODEL AB The Cassini Plasma Spectrometer (CAPS) will make comprehensive three-dimensional mass-resolved measurements of the full variety of plasma phenomena found in Saturn's magnetosphere. Our fundamental scientific goals are to understand the nature of saturnian plasmas primarily their sources of ionization, and the means by which they are accelerated, transported, and lost. In so doing the CAPS investigation will contribute to understanding Saturn's magnetosphere and its complex interactions with Titan, the icy satellites and rings, Saturn's ionosphere and aurora, and the solar wind. Our design approach meets these goals by emphasizing two complementary types of measurements: high-time resolution velocity distributions of electrons and all major ion species; and lower-time resolution, high-mass resolution spectra of all ion species. The CAPS instrument is made up of three sensors: the Electron Spectrometer (ELS), the Ion Beam Spectrometer (IBS), and the Ion Mass Spectrometer (IMS). The ELS measures the velocity distribution of electrons from 0.6 eV to 28,250 keV, a range that permits coverage of thermal electrons found at Titan and near the ring plane as well as more energetic trapped electrons and auroral particles. The IBS measures ion velocity distributions with very high angular and energy resolution from 1 eV to 49,800 keV. It is specially designed to measure sharply defined ion beams expected in the solar wind at 9.5 AU, highly directional rammed ion fluxes encountered in Titan's ionosphere, and anticipated field-aligned auroral fluxes. The IMS is designed to measure the composition of hot, diffuse magnetospheric plasmas and low-concentration ion species 1 eV to 50,280 eV with an atomic resolution M/DeltaM similar to70 and, for certain molecules., (such as N(2)(+) and CO(+)) effective resolution as high as similar to2500. The three sensors are mounted on a motor-driven actuator that rotates the entire instrument over approximately one-half of the sky every 3 min. C1 SW Res Inst, San Antonio, TX 78228 USA. Los Alamos Natl Lab, Los Alamos, NM USA. CNRS, Ctr Etud Environm Terr & Planetaires, St Maur, France. Observ Midi Pyrenees, F-31400 Toulouse, France. UCL, Mullard Space Sci Lab, Surrey, England. Jet Prop Lab, Pasadena, CA USA. Rutherford Appleton Lab, Didcot, Oxon, England. Rice Univ, Houston, TX 77251 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Virginia, Charlottesville, VA USA. VTT Informat Technol, Espoo, Finland. Norwegian Def Res Estab, N-2007 Kjeller, Norway. KFKI Res Inst Particle & Nucl Phys, Budapest, Hungary. Univ Oulu, Oulu, Finland. Nokia Electr Ltd, Helsinki, Finland. TEKES Technol Dev Ctr, Helsinki, Finland. RP Young, DT (reprint author), SW Res Inst, San Antonio, TX 78228 USA. RI Coates, Andrew/C-2396-2008; Mursula, Kalevi/L-8952-2014; Funsten, Herbert/A-5702-2015; Grande, Manuel/C-2242-2013 OI Coates, Andrew/0000-0002-6185-3125; Mursula, Kalevi/0000-0003-4892-5056; Funsten, Herbert/0000-0002-6817-1039; Grande, Manuel/0000-0002-2233-2618 NR 129 TC 305 Z9 305 U1 3 U2 24 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PY 2004 VL 114 IS 1-4 BP 1 EP 112 DI 10.1007/s11214-004-1406-4 PG 112 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904BY UT WOS:000227472300002 ER PT J AU Waite, JH Lewis, S Kasprzak, WT Anicich, VG Block, BP Cravens, TE Fletcher, GG Ip, WH Luhmann, JG McNutt, RL Niemann, HB Parejko, JK Richards, JE Thorpe, RL Walter, EM Yelle, RV AF Waite, JH Lewis, S Kasprzak, WT Anicich, VG Block, BP Cravens, TE Fletcher, GG Ip, WH Luhmann, JG McNutt, RL Niemann, HB Parejko, JK Richards, JE Thorpe, RL Walter, EM Yelle, RV TI The Cassini ion and neutral mass spectrometer (INMS) investigation SO SPACE SCIENCE REVIEWS LA English DT Review DE Cassini; Titan; Saturn; Huygens; Mass Spectrometry ID TITANS UPPER-ATMOSPHERE; SUBMILLIMETER HETERODYNE OBSERVATIONS; EXTREME-ULTRAVIOLET OBSERVATIONS; VOYAGER INFRARED OBSERVATIONS; SATURNS MAGNETOSPHERE; PLASMA OBSERVATIONS; RADIO-OCCULTATION; VERTICAL PROFILE; RING ATMOSPHERE; CARBON-MONOXIDE AB The Cassini Ion and Neutral Mass Spectrometer (INMS) investigation will determine the mass composition and number densities of neutral species and low-energy ions in key regions of the Saturn system. The primary focus of the INMS investigation is on the composition and structure of Titan's upper atmosphere and its interaction with Saturn's magnetospheric plasma. Of particular interest is the high-altitude region, between 900 and 1000 km, where the methane and nitrogen photochemistry is initiated that leads to the creation of complex hydrocarbons and nitriles that may eventually precipitate onto the moon's surface to form hydrocarbon-nitrile lakes or oceans. The investigation is also focused on the neutral and plasma environments of Saturn's ring system and icy moons and on the identification of positive ions and neutral species in Saturn's inner magnetosphere. Measurement of material sputtered from the satellites and the rings by magnetospheric charged particle and micrometeorite bombardment is expected to provide information about the formation of the giant neutral cloud of water molecules and water products that surrounds Saturn out to a distance of similar to12 planetary radii and about the genesis and evolution of the rings. The INMS instrument consists of a closed ion source and an open ion source, various focusing lenses, an electrostatic quadrupole switching lens, a radio frequency quadrupole mass analyzer, two secondary electron multiplier detectors, and the associated supporting electronics and power supply systems. The INMS will be operated in three different modes: a closed source neutral mode, for the measurement of non-reactive neutrals such as N-2 and CH4; an open source neutral mode, for reactive neutrals such as atomic nitrogen; and an open source ion mode, for positive ions with energies less than 100 eV. Instrument sensitivity is greatest in the first mode, because the ram pressure of the inflowing gas can be used to enhance the density of the sampled non-reactive neutrals in the closed source antechamber. In this mode, neutral species with concentrations on the order of greater than or equal to10(4) cm(-3) will be detected (compared with greater than or equal to10(5) cm(-3) in the open source neutral mode). For ions the detection threshold is on the order of 10(-2) cm(-3) at Titan relative velocity (6 km sec(-1)). The INMS instrument has a mass range of 1-99 Daltons and a mass resolution M/DeltaM of 100 at 10% of the mass peak height, which will allow detection of heavier hydrocarbon species and of possible cyclic hydrocarbons such as C6H6. The INMS instrument was built by a team of engineers and scientists working at NASA's Goddard Space Flight Center (Planetary Atmospheres Laboratory) and the University of Michigan (Space Physics Research Laboratory). INNIS development and fabrication were directed by Dr. Hasso B. Niemann (Goddard Space Flight Center). The instrument is operated by a Science Team, which is also responsible for data analysis and distribution. The INMS Science Team is led by Dr. J. Hunter Waite, Jr. (University of Michigan). C1 Univ Michigan, Ann Arbor, MI 48109 USA. SW Res Inst, San Antonio, TX USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NASA, Jet Prop Lab, Pasadena, CA USA. Univ Kansas, Lawrence, KS 66045 USA. Natl Cent Univ, Chungli 32054, Taiwan. Univ Calif Berkeley, Berkeley, CA 94720 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. Univ Arizona, Flagstaff, AZ USA. RP Univ Michigan, Ann Arbor, MI 48109 USA. EM hunterw@umich.edu RI McNutt, Ralph/E-8006-2010 OI McNutt, Ralph/0000-0002-4722-9166 NR 141 TC 96 Z9 96 U1 2 U2 21 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PY 2004 VL 114 IS 1-4 BP 113 EP 231 DI 10.1007/s11214-004-1408-2 PG 119 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904BY UT WOS:000227472300003 ER PT J AU Dougherty, MK Kellock, S Southwood, DJ Balogh, A Smith, EJ Tsurutani, BT Gerlach, B Glassmeier, KH Gleim, F Russell, CT Erdos, G Neubauer, EM Cowley, SWH AF Dougherty, MK Kellock, S Southwood, DJ Balogh, A Smith, EJ Tsurutani, BT Gerlach, B Glassmeier, KH Gleim, F Russell, CT Erdos, G Neubauer, EM Cowley, SWH TI The Cassini magnetic field investigation SO SPACE SCIENCE REVIEWS LA English DT Review DE Cassini; magnetometer; saturn ID ZONAL HARMONIC MODEL; ION-CYCLOTRON WAVES; SATURNS MAGNETOSPHERE; JOVIAN MAGNETOSPHERE; GALILEO MAGNETOMETER; DISPERSION ANALYSIS; ALIGNED CURRENTS; SOLAR-WIND; ULYSSES; JUPITER AB The dual technique magnetometer system onboard the Cassini orbiter is described. This instrument consists of vector helium and fluxgate magnetometers with the capability to operate the helium device in a scalar mode. This special mode is used near the planet in order to determine with very high accuracy the interior field of the planet. The orbital mission will lead to a detailed understanding of the Satum/Titan system including measurements of the planetary magnetosphere, and the interactions of Saturn with the solar wind, of Titan with its environments, and of the icy satellites within the magnetosphere. C1 Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Tech Univ Carolo Wilhelmina Braunschweig, D-38106 Braunschweig, Germany. Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. KFKI Res Inst Particle & Nucl Phys, H-1525 Budapest, Hungary. Univ Cologne, Inst Geophys & Meterol, D-50923 Cologne, Germany. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Dougherty, MK (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Prince Consort Rd, London SW7 2BZ, England. EM m.dougherty@imperial.ac.uk OI Russell, Christopher/0000-0003-1639-8298 NR 69 TC 280 Z9 280 U1 1 U2 25 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PY 2004 VL 114 IS 1-4 BP 331 EP 383 DI 10.1007/s11214-004-1432-2 PG 53 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904BY UT WOS:000227472300005 ER PT J AU Narvaez, P AF Narvaez, P TI The magnetostatic cleanliness program for the Cassini spacecraft SO SPACE SCIENCE REVIEWS LA English DT Review DE spacecraft magnetic cleanliness; spacecraft magnetic tests AB The Cassini spacecraft, launched in October 1997 and expected to reach Saturn in 2004, carries two magnetometer experiments on a 10-m boom, one at the mid-section of the boom and the other situated at the end of the boom. In order to gather valid scientific magnetic field data and avoid electromagnetic interference, the spacecraft had to comply with stringent magnetostatic cleanliness requirements. This paper describes the results of the Cassini magnetics cleanliness program that achieved the goal of minimizing the magnetic field interference with Cassini's DC magnetic field science instruments. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Narvaez, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM pablo.narvaez@jpl.nasa.gov NR 2 TC 6 Z9 8 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PY 2004 VL 114 IS 1-4 BP 385 EP 394 DI 10.1007/s11214-004-1433-1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904BY UT WOS:000227472300006 ER PT J AU Gurnett, DA Kurth, WS Kirchner, DL Hospodarsky, GB Averkamp, TF Zarka, P Lecacheux, A Manning, R Roux, A Canu, P Cornilleau-Wehrlin, N Galopeau, P Meyer, A Bostrom, R Gustafsson, G Wahlund, JE Ahlen, L Rucker, HO Ladreiter, HP Macher, W Woolliscroft, LJC Alleyne, H Kaiser, ML Desch, MD Farrell, WM Harvey, CC Louarn, P Kellogg, PJ Goetz, K Pedersen, A AF Gurnett, DA Kurth, WS Kirchner, DL Hospodarsky, GB Averkamp, TF Zarka, P Lecacheux, A Manning, R Roux, A Canu, P Cornilleau-Wehrlin, N Galopeau, P Meyer, A Bostrom, R Gustafsson, G Wahlund, JE Ahlen, L Rucker, HO Ladreiter, HP Macher, W Woolliscroft, LJC Alleyne, H Kaiser, ML Desch, MD Farrell, WM Harvey, CC Louarn, P Kellogg, PJ Goetz, K Pedersen, A TI The Cassini radio and plasma wave investigation SO SPACE SCIENCE REVIEWS LA English DT Review ID SATURNIAN KILOMETRIC RADIATION; HIGH-FREQUENCY LIMIT; ELECTROSTATIC DISCHARGES; MAGNETIC-FIELD; RING PLANE; ASTRONOMY OBSERVATIONS; LIGHTNING ACTIVITY; PARTICLE IMPACTS; ROTATION PERIOD; GRAIN IMPACTS AB The Cassini radio and plasma wave investigation is designed to study radio emissions, plasma waves, thermal plasma, and dust in the vicinity of Saturn. Three nearly orthogonal electric field antennas are used to detect electric fields over a frequency range from 1 Hz to 16 MHz, and three orthogonal search coil magnetic antennas are used to detect magnetic fields over a frequency range from 1 Hz to 12 kHz. A Langmuir probe is used to measure the electron density and temperature. Signals from the electric and magnetic antennas are processed by five receiver systems: a high frequency receiver that covers the frequency range from 3.5 kHz to 16 MHz, a medium frequency receiver that covers the frequency range from 24 Hz to 12 kHz, a low frequency receiver that covers the frequency range from 1 Hz to 26 Hz, a five-channel waveform receiver that covers the frequency range from 1 Hz to 2.5 kHz in two bands, 1 Hz to 26 Hz and 3 Hz to 2.5 kHz, and a wideband receiver that has two frequency bands, 60 Hz to 10.5 kHz and 800 Hz to 75 kHz. In addition, a sounder transmitter can be used to stimulate plasma resonances over a frequency range from 3.6 kHz to 115.2 kHz. Fluxes of micron-sized dust particles can be counted and approximate masses of the dust particles can be determined using the same techniques as Voyager. Compared to Voyagers 1 and 2, which are the only spacecraft that have made radio and plasma wave measurements in the vicinity of Saturn, the Cassini radio and plasma wave instrument has several new capabilities. These include (1) greatly improved sensitivity and dynamic range, (2) the ability to perform direction-finding measurements of remotely generated radio emissions and wave normal measurements of plasma waves, (3) both active and passive measurements of plasma resonances in order to give precise measurements of the local electron density, and (4) Langmuir probe measurements of the local electron density and temperature. With these new capabilities, it will be possible to perform a broad range of studies of radio emissions, wave-particle interactions, thermal plasmas and dust in the vicinity of Saturn. C1 Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. Observ Paris, Meudon, France. CETP UVSQ, Velizy Villacoublay, France. Swedish Inst Space Phys, Uppsala, Sweden. Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. Univ Sheffield, Dept Automat Control & Syst Engn, Sheffield, S Yorkshire, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. CNRS, CESR, Toulouse, France. Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA. Univ Oslo, Dept Phys, Oslo, Norway. RP Gurnett, DA (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. EM donald-gurnett@uiowa.edu RI Farrell, William/I-4865-2013; OI Hospodarsky, George/0000-0001-9200-9878; Kurth, William/0000-0002-5471-6202 NR 116 TC 259 Z9 259 U1 3 U2 17 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PY 2004 VL 114 IS 1-4 BP 395 EP 463 DI 10.1007/s11214-004-1434-0 PG 69 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904BY UT WOS:000227472300007 ER PT J AU Srama, R Ahrens, TJ Altobelli, N Auer, S Bradley, JG Burton, M Dikarev, VV Economou, T Fechtig, H Gorlich, M Grande, M Graps, A Grun, E Havnes, O Helfert, S Horanyi, M Igenbergs, E Jessberger, EK Johnson, TV Kempf, S Krivov, AV Kruger, H Mocker-Ahlreep, A Moragas-Klostermeyer, G Lamy, P Landgraf, M Linkert, D Linkert, G Lura, F McDonnell, JAM Mohlmann, D Morfill, GE Muller, M Roy, M Schafer, G Schlotzhauer, G Schwehm, GH Spahn, F Stubig, M Svestka, J Tschernjawski, V Tuzzolino, AJ Wasch, R Zook, HA AF Srama, R Ahrens, TJ Altobelli, N Auer, S Bradley, JG Burton, M Dikarev, VV Economou, T Fechtig, H Gorlich, M Grande, M Graps, A Grun, E Havnes, O Helfert, S Horanyi, M Igenbergs, E Jessberger, EK Johnson, TV Kempf, S Krivov, AV Kruger, H Mocker-Ahlreep, A Moragas-Klostermeyer, G Lamy, P Landgraf, M Linkert, D Linkert, G Lura, F McDonnell, JAM Mohlmann, D Morfill, GE Muller, M Roy, M Schafer, G Schlotzhauer, G Schwehm, GH Spahn, F Stubig, M Svestka, J Tschernjawski, V Tuzzolino, AJ Wasch, R Zook, HA TI The Cassini Cosmic Dust Analyzer SO SPACE SCIENCE REVIEWS LA English DT Review DE CDA; Cassini; dust sensor; E-ring; interplanetary dust ID SOLAR-SYSTEM DUST; SATURNS E-RING; JOVIAN MAGNETOSPHERE; INTERSTELLAR GRAINS; GOSSAMER RING; SPACE PROBES; HALLEY DUST; HEOS 2; PARTICLES; INTERPLANETARY AB The Cassini-Huygens Cosmic Dust Analyzer (CDA) is intended to provide direct observations of dust grains with masses between 10(-19) and 10(-9) kg in interplanetary space and in the jovian and saturnian systems, to investigate their physical, chemical and dynamical properties as functions of the distances to the Sun, to Jupiter and to Saturn and its satellites and rings, to study their interaction with the saturnian rings, satellites and magnetosphere. Chemical composition of interplanetary meteoroids will be compared with asteroidal and cometary dust, as well as with Saturn dust, ejecta from rings and satellites. Ring and satellites phenomena which might be effects of meteoroid impacts will be compared with the interplanetary dust environment. Electrical charges of particulate matter in the magnetosphere and its consequences will be studied, e.g. the effects of the ambient plasma and the magnetic held on the trajectories of dust particles as well as fragmentation of particles due to electrostatic disruption. The investigation will be performed with an instrument that measures the mass, composition, electric charge, speed, and flight direction of individual dust particles. It is a highly reliable and versatile instrument with a mass sensitivity 106 times higher than that of the Pioneer 10 and I I dust detectors which measured dust in the saturnian system. The Cosmic Dust Analyzer has significant inheritance from former space instrumentation developed for the VEGA, Giotto, Galileo, and Ulysses missions. It will reliably measure impacts from as low as I impact per month up to 104 impacts per second. The instrument weighs 17 kg and consumes 12 W, the integrated time-of-flight mass spectrometer has a mass resolution of up to 50. The nominal data transmission rate is 524 bits/s and varies between 50 and 4192 bps. C1 Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. Jet Prop Lab, Pasadena, CA 91103 USA. CALTECH, Seismol Lab, Pasadena, CA 91125 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. Univ Tromso, Auroral Observ, N-9000 Tromso, Norway. Tech Univ Munich, Fachgebiet Raumfahrttech, D-85748 Garching, Germany. Univ Munster, D-48149 Munster, Germany. Astron Spatiale Lab, F-13376 Marseille 12, France. DLR Berlin, D-12489 Berlin, Germany. Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. Max Planck Inst Phys & Astron, D-85740 Garching, Germany. European Space Agcy, ESTEC, Planetary & Space Sci Div, NL-2200 AG Noordwijk, Netherlands. Prague Observ, Prague 11846 1, Czech Republic. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Atmospher & Space Phys Lab, Boulder, CO 80303 USA. Univ Potsdam, AG Nonlinear Dynam, D-14469 Potsdam, Germany. Univ Mannheim, Lehrstuhl Prakt Informat, D-68131 Mannheim, Germany. Univ Hawaii, HIGP, Honolulu, HI 96822 USA. St Petersburg State Univ, Astron Inst, St Petersburg, Russia. ESA, ESOC, D-64293 Darmstadt, Germany. RP Srama, R (reprint author), Max Planck Inst Kernphys, Postf 103980, D-69029 Heidelberg, Germany. EM ralf.srama@mpi-hd.mpg.de RI Grande, Manuel/C-2242-2013; OI Grande, Manuel/0000-0002-2233-2618; KEMPF, SASCHA/0000-0001-5236-3004; Horanyi, Mihaly/0000-0002-5920-9226 NR 105 TC 123 Z9 123 U1 5 U2 25 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PY 2004 VL 114 IS 1-4 BP 465 EP 518 DI 10.1007/s11214-004-1435-z PG 54 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 904BY UT WOS:000227472300008 ER PT J AU Saunders, RS Arvidson, RE Badhwar, GD Boynton, WV Christensen, PR Cucinotta, FA Feldman, WC Gibbs, RG Kloss, C Landano, MR Mase, RA McSmith, GW Meyer, MA Mitrofanov, IG Pace, GD Plaut, JJ Sidney, WP Spencer, DA Thompson, TW Zeitlin, CJ AF Saunders, RS Arvidson, RE Badhwar, GD Boynton, WV Christensen, PR Cucinotta, FA Feldman, WC Gibbs, RG Kloss, C Landano, MR Mase, RA McSmith, GW Meyer, MA Mitrofanov, IG Pace, GD Plaut, JJ Sidney, WP Spencer, DA Thompson, TW Zeitlin, CJ TI 2001 Mars Odyssey mission summary SO SPACE SCIENCE REVIEWS LA English DT Review ID DEPOSITS; HYDROGEN AB The 2001 Mars Odyssey spacecraft, now in orbit at Mars, will observe the Martian surface at infrared and visible wavelengths to determine surface mineralogy and morphology, acquire global gamma ray and neutron observations for a full Martian year, and study the Mars radiation environment from orbit. The science objectives of this mission are to: ( 1) globally map the elemental composition of the surface, ( 2) determine the abundance of hydrogen in the shallow subsurface, ( 3) acquire high spatial and spectral resolution images of the surface mineralogy, ( 4) provide information on the morphology of the surface, and ( 5) characterize the Martian near-space radiation environment as related to radiation-induced risk to human explorers. To accomplish these objectives, the 2001 Mars Odyssey science payload includes a Gamma Ray Spectrometer (GRS), a multi-spectral Thermal Emission Imaging System (THEMIS), and a radiation detector, the Martian Radiation Environment Experiment (MARIE). THEMIS and MARIE are mounted on the spacecraft with THEMIS pointed at nadir. GRS is a suite of three instruments: a Gamma Subsystem (GSS), a Neutron Spectrometer (NS) and a High-Energy Neutron Detector (HEND). The HEND and NS instruments are mounted on the spacecraft body while the GSS is on a 6-m boom. Some science data were collected during the cruise and aerobraking phases of the mission before the prime mission started. THEMIS acquired infrared and visible images of the Earth-Moon system and of the southern hemisphere of Mars. MARIE monitored the radiation environment during cruise. The GRS collected calibration data during cruise and aerobraking. Early GRS observations in Mars orbit indicated a hydrogen-rich layer in the upper meter of the subsurface in the Southern Hemisphere. Also, atmospheric densities, scale heights, temperatures, and pressures were observed by spacecraft accelerometers during aerobraking as the spacecraft skimmed the upper portions of the Martian atmosphere. This provided the first in-situ evidence of winter polar warming in the Mars upper atmosphere. The prime mission for 2001 Mars Odyssey began in February 2002 and will continue until August 2004. During this prime mission, the 2001 Mars Odyssey spacecraft will also provide radio relays for the National Aeronautics and Space Administration ( NASA) and European landers in early 2004. Science data from 2001 Mars Odyssey instruments will be provided to the science community via NASA's Planetary Data System (PDS). The first PDS release of Odyssey data was in October 2002; subsequent releases occur every 3 months. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. NASA Headquarters, Washington, DC 20546 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Russian Aviat & Space Agcy, Inst Space Res, Lab Space Gamma Ray Spect, Moscow, Russia. Lockheed Martin Astronaut, Denver, CO 80201 USA. Baylor Coll Med, Natl Space Biomed Res Inst, Houston, TX 77030 USA. RP Plaut, JJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM plaut@jpl.nasa.gov NR 26 TC 35 Z9 35 U1 3 U2 21 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PY 2004 VL 110 IS 1-2 BP 1 EP 36 DI 10.1023/B:SPAC.0000021006.84299.18 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 806AI UT WOS:000220406400002 ER PT J AU Boynton, WV Feldman, WC Mitrofanov, IG Evans, LG Reedy, RC Squyres, SW Starr, R Trombka, JI D'Uston, C Arnold, JR Englert, PAJ Metzger, AE Wanke, H Bruckner, J Drake, DM Shinohara, C Fellows, C Hamara, DK Harshman, K Kerry, K Turner, C Ward, M Barthe, H Fuller, KR Storms, SA Thornton, GW Longmire, JL Litvak, ML Ton'chev, AK AF Boynton, WV Feldman, WC Mitrofanov, IG Evans, LG Reedy, RC Squyres, SW Starr, R Trombka, JI D'Uston, C Arnold, JR Englert, PAJ Metzger, AE Wanke, H Bruckner, J Drake, DM Shinohara, C Fellows, C Hamara, DK Harshman, K Kerry, K Turner, C Ward, M Barthe, H Fuller, KR Storms, SA Thornton, GW Longmire, JL Litvak, ML Ton'chev, AK TI The Mars Odyssey Gamma-Ray Spectrometer instrument suite SO SPACE SCIENCE REVIEWS LA English DT Review ID LUNAR NEUTRON-FLUX; CHEMICAL-COMPOSITION; ELEMENTAL COMPOSITION; GERMANIUM DETECTORS; PLANETARY SURFACES; RADIATION-DAMAGE; LANDING SITE; 433 EROS; SPECTROSCOPY; SUBSURFACE AB The Mars Odyssey Gamma-Ray Spectrometer is a suite of three different instruments, a gamma subsystem (GS), a neutron spectrometer, and a high-energy neutron detector, working together to collect data that will permit the mapping of elemental concentrations on the surface of Mars. The instruments are complimentary in that the neutron instruments have greater sensitivity to low amounts of hydrogen, but their signals saturate as the hydrogen content gets high. The hydrogen signal in the GS, on the other hand, does not saturate at high hydrogen contents and is sensitive to small differences in hydrogen content even when hydrogen is very abundant. The hydrogen signal in the neutron instruments and the GS have a different dependence on depth, and thus by combining both data sets we can infer not only the amount of hydrogen, but constrain its distribution with depth. In addition to hydrogen, the GS determines the abundances of several other elements. The instruments, the basis of the technique, and the data processing requirements are described as are some expected applications of the data to scientific problems. C1 Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Space Res Inst, Moscow, Russia. Comp Sci Corp, Sci Programs, Lanham, MD 20706 USA. Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Ctr Etud Spatiale Rayonnements, Toulouse, France. Univ Calif San Diego, Dept Chem, La Jolla, CA 92093 USA. Univ Hawaii Manoa, Honolulu, HI 96822 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Max Planck Inst Chem, D-55128 Mainz, Germany. Techsource, Santa Fe, NM 87505 USA. RP Boynton, WV (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM WBoynton@GAMMA1.lpl.arizona.edu OI Reedy, Robert/0000-0002-2189-1303 NR 77 TC 134 Z9 135 U1 5 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PY 2004 VL 110 IS 1-2 BP 37 EP 83 DI 10.1023/B:SPAC.0000021007.76126.15 PG 47 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 806AI UT WOS:000220406400003 ER PT J AU Christensen, PR Jakosky, B Kieffer, HH Malin, MC McSween, HY Nealson, K Mehall, GL Silverman, SH Ferry, S Caplinger, M Ravine, M AF Christensen, PR Jakosky, B Kieffer, HH Malin, MC McSween, HY Nealson, K Mehall, GL Silverman, SH Ferry, S Caplinger, M Ravine, M TI The Thermal Emission Imaging System (THEMIS) for the Mars 2001 Odyssey Mission SO SPACE SCIENCE REVIEWS LA English DT Review ID PARTICULATE PLANETARY SURFACES; POLAR LAYERED DEPOSITS; INFRARED-EMISSION; REFLECTANCE SPECTRA; MARTIAN SURFACE; MU-M; MARS PATHFINDER; SNC METEORITES; PARTICLE-SIZE; ICE CLOUDS AB The Thermal Emission Imaging System (THEMIS) on 2001 Mars Odyssey will investigate the surface mineralogy and physical properties of Mars using multi-spectral thermal-infrared images in nine wavelengths centered from 6.8 to 14.9 mum, and visible/near-infrared images in five bands centered from 0.42 to 0.86 mum. THEMIS will map the entire planet in both day and night multi-spectral infrared images at 100-m per pixel resolution, 60% of the planet in one-band visible images at 18-m per pixel, and several percent of the planet in 5-band visible color. Most geologic materials, including carbonates, silicates, sulfates, phosphates, and hydroxides have strong fundamental vibrational absorption bands in the thermal-infrared spectral region that provide diagnostic information on mineral composition. The ability to identify a wide range of minerals allows key aqueous minerals, such as carbonates and hydrothermal silica, to be placed into their proper geologic context. The specific objectives of this investigation are to: ( 1) determine the mineralogy and petrology of localized deposits associated with hydrothermal or sub-aqueous environments, and to identify future landing sites likely to represent these environments; ( 2) search for thermal anomalies associated with active sub-surface hydrothermal systems; ( 3) study small-scale geologic processes and landing site characteristics using morphologic and thermophysical properties; and ( 4) investigate polar cap processes at all seasons. THEMIS follows the Mars Global Surveyor Thermal Emission Spectrometer (TES) and Mars Orbiter Camera (MOC) experiments, providing substantially higher spatial resolution IR multi-spectral images to complement TES hyperspectral (143-band) global mapping, and regional visible imaging at scales intermediate between the Viking and MOC cameras. The THEMIS uses an uncooled microbolometer detector array for the IR focal plane. The optics consists of all-reflective, three-mirror anastigmat telescope with a 12-cm effective aperture and a speed of f/1.6. The IR and visible cameras share the optics and housing, but have independent power and data interfaces to the spacecraft. The IR focal plane has 320 cross-track pixels and 240 down-track pixels covered by 10 similar to 1-mum-bandwidth strip filters in nine different wavelengths. The visible camera has a 1024 x 1024 pixel array with 5 filters. The instrument weighs 11.2 kg, is 29 cm by 37 cm by 55 cm in size, and consumes an orbital average power of 14 W. C1 Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Malin Space Sci Syst, San Diego, CA 92121 USA. Univ Tennessee, Dept Geol Sci, Knoxville, TN 37996 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91006 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Raytheon Co, Santa Barbara Remote Sensing, Goleta, CA USA. RP Christensen, PR (reprint author), Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. EM phil.christensen@asu.edu NR 134 TC 415 Z9 416 U1 7 U2 51 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PY 2004 VL 110 IS 1-2 BP 85 EP 130 DI 10.1023/B:SPAC.0000021008.16305.94 PG 46 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 806AI UT WOS:000220406400004 ER PT J AU Badhwar, GD AF Badhwar, GD TI Martian Radiation Environment Experiment (MARIE) SO SPACE SCIENCE REVIEWS LA English DT Review ID EXPOSURE; ODYSSEY AB Measurements of radiation levels at Mars including the contributions of protons, neutrons, and heavy ions, are pre-requisites for human exploration. The MARIE experiment on the Mars-01 Odyssey spacecraft consists of a spectrometer to make such measurements in Mars orbit. MARIE is measuring the galactic cosmic ray energy spectra during the maximum of the 24(th) solar cycle, and studying the dynamics of solar particle events and their radial dependence in orbit of Mars. The MARIE spectrometer is designed to measure the energy spectrum from 15 to 500 MeV/n, and when combined other space based instruments, such as the Advanced Composition Explorer ( ACE), would provide accurate GCR spectra. Similarly, observations of solar energetic particles can be combined with observations at different points in the inner heliosphere from, for example, the Solar Heliospheric Observatory (SOHO), to gain information on the propagation and radial dependence in the Earth-Mars space. Measurements can be compared with the best available radiation environment and transport models in order to improve these models for subsequent use, and to provide key inputs for the engineering of spacecraft to better protect the human crews exploring Mars. C1 NASA, Lyndon B Johnson Space Ctr, Earth & Solar Syst Explorat Div, Houston, TX 77058 USA. RP Badhwar, GD (reprint author), NASA, Lyndon B Johnson Space Ctr, Earth & Solar Syst Explorat Div, Houston, TX 77058 USA. EM FrancisA.Cuccinotta1@jsc.nasa.gov NR 13 TC 11 Z9 11 U1 0 U2 2 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PY 2004 VL 110 IS 1-2 BP 131 EP 142 DI 10.1023/B:SPAC.0000021009.68228.a8 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 806AI UT WOS:000220406400005 ER PT J AU Saganti, PB Cucinotta, FA Wilson, JW Simonsen, LC Zeitlin, C AF Saganti, PB Cucinotta, FA Wilson, JW Simonsen, LC Zeitlin, C TI Radiation climate map for analyzing risks to astronauts on the Mars surface from galactic cosmic rays SO SPACE SCIENCE REVIEWS LA English DT Review ID SPACE RADIATION; EXPLORATION; EXPOSURE; MODEL AB The potential risks for late effects including cancer, cataracts, and neurological disorders due to exposures to the galactic cosmic rays (GCR) is a large concern for the human exploration of Mars. Physical models are needed to project the radiation exposures to be received by astronauts in transit to Mars and on the Mars surface, including the understanding of the modification of the GCR by the Martian atmosphere and identifying shielding optimization approaches. The Mars Global Surveyor (MGS) mission has been collecting Martian surface topographical data with the Mars Orbiter Laser Altimeter (MOLA). Here we present calculations of radiation climate maps of the surface of Mars using the MOLA data, the radiation transport model HZETRN ( high charge and high energy transport), and the quantum multiple scattering fragmentation model, QMSFRG. Organ doses and the average number of particle hits per cell nucleus from GCR components ( protons, heavy ions, and neutrons) are evaluated as a function of the altitude on the Martian surface. Approaches to improve the accuracy of the radiation climate map, presented here using data from the 2001 Mars Odyssey mission, are discussed. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. Lockheed Martin, Space Operat, Houston, TX 77058 USA. RP Saganti, PB (reprint author), A&M Univ, NASA, Ctr Appl Radiat Res, Prairie View, TX 77446 USA. EM premkumeur.saqanti1@jsc.nasa.gov NR 22 TC 34 Z9 34 U1 1 U2 3 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PY 2004 VL 110 IS 1-2 BP 143 EP 156 DI 10.1023/B:SPAC.0000021010.20082.1a PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 806AI UT WOS:000220406400006 ER PT J AU Mann, I Kimura, H Biesecker, DA Tsurutani, BT Grun, E Mckibben, RB Liou, JC Macqueen, RM Mukai, T Guhathakurta, M Lamy, P AF Mann, I Kimura, H Biesecker, DA Tsurutani, BT Grun, E Mckibben, RB Liou, JC Macqueen, RM Mukai, T Guhathakurta, M Lamy, P TI Dust near the Sun SO SPACE SCIENCE REVIEWS LA English DT Review ID SOLAR F-CORONA; ORBITING ARGOS SPACECRAFT; SPADUS INSTRUMENT ABOARD; INTERPLANETARY DUST; CIRCUMSOLAR DUST; SUNGRAZING COMETS; INFRARED OBSERVATIONS; THERMAL RADIATION; INTERSTELLAR DUST; MASS-DISTRIBUTION AB We review the current knowledge and understanding of dust in the inner solar system. The major sources of the dust population in the inner solar system are comets and asteroids, but the relative contributions of these sources are not quantified. The production processes inward from 1 AU are: Poynting-Robertson deceleration of particles outside of 1 AU, fragmentation into dust due to particle-particle collisions, and direct dust production from comets. The loss processes are: dust collisional fragmentation, sublimation, radiation pressure acceleration, sputtering, and rotational bursting. These loss processes as well as dust surface processes release dust compounds in the ambient interplanetary medium. Between 1 and 0.1 AU the dust number densities and fluxes can be described by inward extrapolation of 1 AU measurements, assuming radial dependences that describe particles in close to circular orbits. Observations have confirmed the general accuracy of these assumptions for regions within 30degrees latitude of the ecliptic plane. The dust densities are considerably lower above the solar poles but Lorentz forces can lift particles of sizes < 5 mu m to high latitudes and produce a random distribution of small grains that varies with the solar magnetic field. Also long-period comets are a source of out-of-ecliptic particles. Under present conditions no prominent dust ring exists near the Sun. We discuss the recent observations of sungrazing comets. Future in-situ experiments should measure the complex dynamics of small dust particles, identify the contribution of cometary dust to the inner-solar-system dust cloud, and determine dust interactions in the ambient interplanetary medium. The combination of in-situ dust measurements with particle and field measurements is recommended. C1 Univ Munster, Inst Planetol, D-4400 Munster, Germany. NOAA, Space Environm Ctr, Boulder, CO USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. Lockheed Martin Space Operat, Houston, TX USA. Rhodes Coll, Memphis, TN 38112 USA. Kobe Univ, Grad Sch Sci & Technol, Kobe, Hyogo 657, Japan. NASA Headquarters, Washington, DC USA. Astrophys Lab, Marseille, France. RP Mann, I (reprint author), Univ Munster, Inst Planetol, D-4400 Munster, Germany. EM imann@uni-muenster.de NR 112 TC 71 Z9 71 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PY 2004 VL 110 IS 3-4 BP 269 EP 305 DI 10.1023/B:SPAC.0000023440.82735.ba PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811GZ UT WOS:000220761700003 ER PT S AU Basinger, SA Redding, DC AF Basinger, SA Redding, DC BE Peterson, LD Guyer, RC TI Terrestrial planet finder coronagraph optical modeling SO SPACE SYSTEMS ENGINEERING AND OPTICAL ALIGNMENT MECHANISMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Systems Engineering and Optical Alignment Mechanisms CY AUG 04-06, 2004 CL Denver, CO SP SPIE DE Terrestrial Planet Finder; coronagraph; modeling; optics; space telescopes AB The Terrestrial Planet Finder Coronagraph will rely heavily on modeling and analysis throughout its mission lifecycle. Optical modeling is especially important, since the tolerances on the optics as well as scattered light suppression are critical for the mission's success. The high contrast imaging necessary to observe a planet orbiting a distant star requires new and innovative technologies to be developed and tested, and detailed optical modeling provides predictions for evaluating design decisions. It also provides a means to develop and test algorithms designed to actively suppress scattered light via deformable mirrors and other techniques. The optical models are used in conjunction with structural and thermal models to create fully integrated optical/structural/thermal models that are used to evaluate dynamic effects of disturbances on the overall performance of the coronagraph. The optical models we have developed have been verified on the High Contrast Imaging Testbed. Results of the optical modeling verification and the methods used to perform full three-dimensional near-field diffraction analysis are presented. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Basinger, SA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 306-451, Pasadena, CA 91109 USA. NR 8 TC 2 Z9 2 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5466-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5528 BP 1 EP 9 DI 10.1117/12.560507 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BBC27 UT WOS:000224727800001 ER PT S AU Kissil, A Kwack, E Ho, T Liu, A Blaurock, C AF Kissil, A Kwack, E Ho, T Liu, A Blaurock, C BE Peterson, LD Guyer, RC TI Structural modeling for the terrestrial planet finder mission SO SPACE SYSTEMS ENGINEERING AND OPTICAL ALIGNMENT MECHANISMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Systems Engineering and Optical Alignment Mechanisms CY AUG 04-06, 2004 CL Denver, CO SP SPIE DE coronagraph; planet finder; telescope; deployable; sun-shield; large-optics AB The Coronagraph version of the Terrestrial Planet Finder (TPF) mission relies on a large-optics, space-born observatory, which requires extreme stability of the optics in the presence of thermal and dynamic disturbances. The structural design requires balancing of stringent constraints on launch packaging with unusually tight response requirements for thermal and dynamic environments. The minimum-mission structural model (pre-phase A, point design) includes a deployable, pre-tensioned membrane sun-shield and solar-sail, a 10m long deployable secondary support structure, and a light-weighted 6m diameter monolithic glass primary mirror. We performed thermal distortion and dynamic response analyses in order to demonstrate feasibility, quantify critical sensitivities, and to identify potential problems that might need to be addressed early on. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kissil, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 4 TC 0 Z9 0 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5466-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5528 BP 10 EP 21 DI 10.1117/12.560516 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BBC27 UT WOS:000224727800002 ER PT S AU Shaklan, S Marchen, L Zhao, F Peters, RD Ho, T Holmes, B AF Shaklan, S Marchen, L Zhao, F Peters, RD Ho, T Holmes, B BE Peterson, LD Guyer, RC TI Metrology system for the Terrestrial Planet Finder coronagraph SO SPACE SYSTEMS ENGINEERING AND OPTICAL ALIGNMENT MECHANISMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Systems Engineering and Optical Alignment Mechanisms CY AUG 04-06, 2004 CL Denver, CO SP SPIE ID FREQUENCY STABILIZATION; LASER AB The Terrestrial Planet Finder (TPF) employs an aggressive coronagraph designed to obtain better than 1e-10 contrast inside the third Airy ring. Minute changes in low-order aberration content scatter significant light at this position. One implication is the requirement to control low-order aberrations induced by motion of the secondary mirror relative to the primary mirror; sub-nanometer relative positional stability is required. We propose a 6-beam laser truss to monitor the relative positions of the two mirrors. The truss is based on laser metrology developed for the Space Interferometry Mission. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Shaklan, S (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 18 TC 2 Z9 2 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5466-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5528 BP 22 EP 31 DI 10.1117/12.559998 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BBC27 UT WOS:000224727800003 ER PT S AU Peng, CY Levine, M Shido, L Leland, R AF Peng, CY Levine, M Shido, L Leland, R BE Peterson, LD Guyer, RC TI Experimental observations on material damping at cryogenic temperatures SO SPACE SYSTEMS ENGINEERING AND OPTICAL ALIGNMENT MECHANISMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Systems Engineering and Optical Alignment Mechanisms CY AUG 04-06, 2004 CL Denver, CO SP SPIE AB This paper describes a unique experimental facility designed to measure damping of materials at cryogenic temperatures for the Terrestrial Planet Finder (TPF) mission at the Jet Propulsion Laboratory. The test facility removes other sources of damping in the measurement by avoiding frictional interfaces, decoupling the test specimen from the support system, and by using a non-contacting measurement device. Damping data reported herein are obtained for materials (Aluminum, Aluminum/Terbium/Dysprosium, Titanium, Composites) vibrating in free-free bending modes with low strain levels (< 10(-6) ppm). The fundamental frequencies of material samples are ranged from 14 to 202 Hz. To provide the most beneficial data relevant to TPF-like precision optical space missions, the damping data are collected from room temperatures (around 293 K) to cryogenic temperatures (below 40 K) at unevenly-spaced intervals. More data points are collected over any region of interest. The test data shows a significant decrease in viscous damping at cryogenic temperatures. The cryogenic damping can be as low as 10(-4)%, but the amount of the damping decrease is a function of frequency and material. However, Titanium 15-3-3-3 shows a remarkable increase in damping at cryogenic temperatures. It demonstrates over one order of magnitude increase in damping in comparison to Aluminum 6061-T6. Given its other properties (e.g., good stiffness and low conductivity) this may prove itself to be a good candidate for the application on TPF. At room temperatures, the test data are correlated well with the damping predicted by the Zener theory. However, large discrepancies at cryogenic temperatures between the Zener theory and the test data are observed. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Peng, CY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 15 TC 1 Z9 1 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5466-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5528 BP 44 EP 62 DI 10.1117/12.561173 PG 19 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BBC27 UT WOS:000224727800005 ER PT S AU Karlmann, PB Dudik, MJ Halverson, PG Levine, M Marcin, M Peters, RD Shaklan, S Van Buren, D AF Karlmann, PB Dudik, MJ Halverson, PG Levine, M Marcin, M Peters, RD Shaklan, S Van Buren, D BE Peterson, LD Guyer, RC TI Continued development of a precision cryogenic dilatometer for the James Webb Space Telescope SO SPACE SYSTEMS ENGINEERING AND OPTICAL ALIGNMENT MECHANISMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Systems Engineering and Optical Alignment Mechanisms CY AUG 04-06, 2004 CL Denver, CO SP SPIE DE coefficient of thermal expansion; dilatometer; thermal strain; fused silica; zerodur AB As part of the James Webb Space Telescope (JWST) materials working group, a novel cryogenic dilatometer was designed and built at NASA Jet Propulsion Laboratory to help address stringent coefficient of thermal expansion (CTE) knowledge requirements. Previously reported results and error analysis have estimated a CTE measurement accuracy for ULE of 1.7 ppb/K with a 20K/thermal load and 0.1 ppb/K with a 280K thermal load.(1) Presented here is a further discussion of the cryogenic dilatometer system and a description of recent work including system modifications and investigations. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Karlmann, PB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 4 TC 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5466-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5528 BP 63 EP 71 DI 10.1117/12.561342 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BBC27 UT WOS:000224727800006 ER PT S AU Mosier, GE Howard, JM Johnston, JD Parrish, KA Hyde, TT McGinnis, MA Bluth, M Kim, K Ha, KQ AF Mosier, GE Howard, JM Johnston, JD Parrish, KA Hyde, TT McGinnis, MA Bluth, M Kim, K Ha, KQ BE Peterson, LD Guyer, RC TI The role of integrated modeling in the design and verification of the James Webb Space Telescope SO SPACE SYSTEMS ENGINEERING AND OPTICAL ALIGNMENT MECHANISMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Systems Engineering and Optical Alignment Mechanisms CY AUG 04-06, 2004 CL Denver, CO SP SPIE DE JWST; optics; integrated modeling; image quality; telescope; verification; validation AB The James Web Space Telescope (JWST) is a large, infrared-optimized space telescope scheduled for launch in 2011. System-level verification of critical optical performance requirements will rely on integrated modeling to a considerable degree. In turn, requirements for accuracy of the models are significant. The size of the lightweight observatory structure, coupled with the need to test at cryogenic temperatures, effectively precludes validation of the models and verification of optical performance with a single test in 1-g. Rather, a complex series of steps are planned by which the components of the end-to-end models are validated at various levels of subassembly, and the ultimate verification of optical performance is by analysis using the assembled models. This paper describes the critical optical performance requirements driving the integrated modeling activity, shows how the error budget is used to allocate and track contributions to total performance, and presents examples of integrated modeling methods and results that support the preliminary observatory design. Finally, the concepts for model validation and the role of integrated modeling in the ultimate verification of observatory are described. C1 NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Mosier, GE (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5466-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5528 BP 96 EP 107 DI 10.1117/12.564452 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BBC27 UT WOS:000224727800009 ER PT S AU Moore, G Chainyk, M Schiermeier, J AF Moore, G Chainyk, M Schiermeier, J BE Peterson, LD Guyer, RC TI Multidisciplinary analysis for large-scale optical design SO SPACE SYSTEMS ENGINEERING AND OPTICAL ALIGNMENT MECHANISMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Systems Engineering and Optical Alignment Mechanisms CY AUG 04-06, 2004 CL Denver, CO SP SPIE DE finite element analysis; multidisciplinary analysis; thermal analysis; structural analysis; optical aberrations AB Accurately predicting optical performance for any of the near-term concepts proposed under NASA's Origins missions is a uniquely challenging task, and one that has served to highlight a number of areas of necessary advancement in the field of computer-aided engineering analysis. The strongly coupled nature of these classes of problems combined with unprecedented levels of required optical precision demand a solution approach that is itself fundamentally integrated if accurate, efficient analyses, capable of pointing the way towards improved designs are to be achieved. Recent development efforts have served to lay the foundation for an entirely new finite element-based analytical capability; one that is open, highly extensible, is Matlab-hosted, and which utilizes NASTRAN syntax to describe common-model multidisciplinary analyis tasks. Capabilities currently under development, a few of which will be highlighted here, will soon capture behavioural aspects of coupled nonlinear radiative heat transfer, structures, and optics problems to a level of accuracy and performance not yet achieved for these classes of problems, in an environment that will greatly facilitate future research, development, and technical oversight efforts. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Moore, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5466-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5528 BP 108 EP 117 DI 10.1117/12.561096 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BBC27 UT WOS:000224727800010 ER PT S AU Milman, MH Korechoff, RE Zhang, LD AF Milman, MH Korechoff, RE Zhang, LD BE Peterson, LD Guyer, RC TI Error modeling of multibaseline optical truss, part 1: Modeling of system level performance SO SPACE SYSTEMS ENGINEERING AND OPTICAL ALIGNMENT MECHANISMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Systems Engineering and Optical Alignment Mechanisms CY AUG 04-06, 2004 CL Denver, CO SP SPIE ID SPACE-INTERFEROMETRY-MISSION; ASTROMETRY AB Global astrometry is the measurement of stellar positions and motions. These are typically characterized by five parameters, including two position parameters, two proper motion parameters, and parallax. The Space Interferometry Mission (SIM) will derive these parameters for a grid of approximately 1300 stars covering the celestial sphere to an accuracy of approximately 4uas, representing a two orders of magnitude improvement over the most precise current star catalogues. Narrow angle astrometry will be performed to a 1uas accuracy. A wealth of scientific information will be obtained from these accurate measurements encompassing many aspects of both galactic and extragalactic science. SIM will be subject to a number of instrument errors that can potentially degrade performance. Many of these errors are systematic in that they are relatively static and repeatable with respect to the time frame and direction of the observation. This paper and its companion define the modeling of the contributing factors to these errors and the analysis of how they impact SIM's ability to perform astrometric science. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Milman, MH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 7 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5466-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5528 BP 118 EP 125 DI 10.1117/12.557202 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BBC27 UT WOS:000224727800011 ER PT S AU Ha, KQ Femiano, MD Mosier, GE AF Ha, KQ Femiano, MD Mosier, GE BE Peterson, LD Guyer, RC TI Minimum-time and vibration avoidance attitude maneuver for spacecraft with torque and momentum limit constraints in redundant reaction wheel configuration SO SPACE SYSTEMS ENGINEERING AND OPTICAL ALIGNMENT MECHANISMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Systems Engineering and Optical Alignment Mechanisms CY AUG 04-06, 2004 CL Denver, CO SP SPIE DE minimum-time slew maneuver; flexible body dynamics; reaction wheel momentum and torque limits; attitude control AB In this paper, we present an optimal open-loop slew trajectory algorithm developed at GSFC for the so-called "Yardstick design" [1] of the James Webb Space Telescope (JWST). JWST is an orbiting infrared observatory featuring a lightweight, segmented primary mirror approximately 6 meters in diameter and a sunshield approximately the size of a tennis court. This large, flexible structure will have significant number of lightly damped, dominant flexible modes. With very stringent requirements on pointing accuracy and image quality, it is important that slewing be done within the required time constraint and with minimal induced vibration in order to maximize observing efficiency. With reaction wheels as control actuators, initial wheel speeds as well as individual wheel torque and momentum limits become dominant constraints in slew performance. These constraints must be taken into account when performing slews to ensure that unexpected reaction wheel saturation does not occur, since such saturation leads to control failure in accurately tracking commanded motion and produces high frequency torque components capable of exciting structural modes. A minimum-time constraint is also included and coupled with reaction wheel limit constraints in the optimization to minimize both the effect of the control torque on the flexible body motion and the maneuver time. The optimization is on slew command parameters, such as maximum slew velocity and acceleration, for a given redundant reaction wheel configuration and is based on the dynamic interaction between the spacecraft and reaction wheel motion. Analytical development of the slew algorithm to generate desired slew position, rate, and acceleration profiles to command a feedback/feed forward control system is described. High-fidelity simulation and experimental results are presented to show that the developed slew law achieves the objectives. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ha, KQ (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. NR 3 TC 0 Z9 0 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5466-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5528 BP 126 EP 137 DI 10.1117/12.558456 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BBC27 UT WOS:000224727800012 ER PT S AU Maghami, PG Hsu, OC Markley, FL O'Donnell, JR AF Maghami, PG Hsu, OC Markley, FL O'Donnell, JR BE Peterson, LD Guyer, RC TI Control modes of the ST7 disturbance reduction system flight validation experiment SO SPACE SYSTEMS ENGINEERING AND OPTICAL ALIGNMENT MECHANISMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Systems Engineering and Optical Alignment Mechanisms CY AUG 04-06, 2004 CL Denver, CO SP SPIE AB The Space Technology 7 (ST7) experiment will perform an on-orbit system-level validation of two specific Disturbance Reduction System technologies: a gravitational reference sensor employing a free-floating test mass and a set of micronewton colloidal thrusters. The ST7 Disturbance Reduction System (DRS) is designed to maintain the spacecraft's position with respect to a free-floating test mass to less than 10 nm/rootHz over the frequency range of 1 to 30 mHz. This paper presents the overall design and analysis of the spacecraft drag-free and attitude controllers. These controllers close the loop between the gravitational sensors and the micronewton colloidal thrusters. There are five control modes in the operation of the ST7 DRS, starting with the attitude-only mode and leading to the science mode. The design and analysis of each of the control modes as well as the mode transition strategy are presented. C1 NASA, Goddard Space Flight Ctr, Miss Engn & Syst Anal Div, Greenbelt, MD 20771 USA. RP Maghami, PG (reprint author), NASA, Goddard Space Flight Ctr, Miss Engn & Syst Anal Div, Code 661, Greenbelt, MD 20771 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5466-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5528 BP 138 EP 149 DI 10.1117/12.559523 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BBC27 UT WOS:000224727800013 ER PT S AU Ford, V Parks, R Coleman, M AF Ford, V Parks, R Coleman, M BE Peterson, LD Guyer, RC TI Passive thermal compensation of the optical bench of the galaxy evolution explorer SO SPACE SYSTEMS ENGINEERING AND OPTICAL ALIGNMENT MECHANISMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Systems Engineering and Optical Alignment Mechanisms CY AUG 04-06, 2004 CL Denver, CO SP SPIE DE ultraviolet; passive athermalization; space telescope; optomechanical design AB The Galaxy Evolution Explorer is an orbiting space telescope that will collect information on star formation by observing galaxies and stars in ultraviolet wavelengths. The optical bench supporting detectors and related optical components used an interesting and unusual passive thermal compensation technique to accommodate thermally-induced focal length changes in the optical system. The proposed paper will describe the optical bench thermal compensation design including concept, analysis, assembly and testing results. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ford, V (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5466-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5528 BP 171 EP 180 DI 10.1117/12.560247 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BBC27 UT WOS:000224727800016 ER PT S AU Zhang, LD Milman, M Korechoff, R AF Zhang, LD Milman, M Korechoff, R BE Peterson, LD Guyer, RC TI Error modeling of multi-baseline optical truss, part II: Application to SIM metrology truss field dependent error SO SPACE SYSTEMS ENGINEERING AND OPTICAL ALIGNMENT MECHANISMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Systems Engineering and Optical Alignment Mechanisms CY AUG 04-06, 2004 CL Denver, CO SP SPIE DE modeling; interferometer; metrology; corner cube retro-reflector; instrument systematic error ID SPACE INTERFEROMETRY MISSION AB The current design of the Space Interferometry Mission (SIM) employs a 19 laser-metrology-beam system (also called L19 external metrology truss) to monitor changes of distances between the fiducials of the flight system's multiple baselines. The function of the external metrology truss is to aid in the determination of the time-variations of the interferometer baseline. The largest contributor to truss error occurs in SIM wide-angle observations when the articulation of the siderostat mirrors (in order to gather starlight from different sky coordinates) brings to light systematic errors due to offsets at levels of instrument components (which include corner cube retro-reflectors, etc.). This is the external metrology wide-angle field-dependent error. Physics-based model of field-dependent error at single metrology gauge level is developed and linearly propagated to errors in interferometer delay. General formulation of delay error sensitivity to various error parameters is developed. The essence of the linear error model is contained in an error-mapping matrix. A corresponding Zernike component matrix approach is developed in parallel with its advantages discussed. As a first example, dihedral error model is developed for the corner cubes (CC) attached to the siderostat mirrors. Average and worst case residual errors are computed when various orders of field-dependent terms are removed from the delay error. These serve as guidelines for arriving at system requirements given the error budget allocation. Highlights of the non-common vertex error (NCVE) model are shown as a second example followed by discussions. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zhang, LD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 9 TC 2 Z9 2 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5466-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5528 BP 245 EP 254 DI 10.1117/12.557138 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BBC27 UT WOS:000224727800023 ER PT S AU Toland, R Leviton, D Koterba, S AF Toland, R Leviton, D Koterba, S BE Peterson, LD Guyer, RC TI Theoferometer for high accuracy optical alignment and metrology SO SPACE SYSTEMS ENGINEERING AND OPTICAL ALIGNMENT MECHANISMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Systems Engineering and Optical Alignment Mechanisms CY AUG 04-06, 2004 CL Denver, CO SP SPIE AB The accurate measurement of the orientation of optical parts and systems is a pressing problem for upcoming space missions, such as stellar interferometers, requiring the knowledge and maintenance of positions to the sub-arcsecond level. Theodolites, the devices commonly used to make these measurements, cannot provide the needed level of accuracy. This paper describes the design, construction, and testing of an interferometer system to fill the widening gap between future requirements and current capabilities. A Twyman-Green interferometer mounted on a 2 degree of freedom rotation stage is able to obtain sub-arcsecond, gravity-referenced tilt measurements of a sample alignment cube. Dubbed a 'theoferometer,' this device offers greater ease-of-use, accuracy, and repeatability than conventional methods, making it a suitable 21st-century replacement for the theodolite. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Toland, R (reprint author), NASA, Goddard Space Flight Ctr, Code 551 Opt, Greenbelt, MD 20771 USA. NR 9 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5466-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5528 BP 305 EP 315 DI 10.1117/12.559969 PG 11 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BBC27 UT WOS:000224727800029 ER PT S AU Tsuyuki, G Ganapathi, G Bame, D Patzold, J Fisher, R Theriault, L AF Tsuyuki, G Ganapathi, G Bame, D Patzold, J Fisher, R Theriault, L BE ElGenk, MS TI The hardware challenges for the Mars Exploration Rover heat rejection system SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB The primary objective of the Mars Exploration Rover (MER) 2003 Project focused on the search for evidence of water on Mars. The launch of two identical flight systems occurred in June and July of 2003. The roving science vehicles are expected to land on the Martian surface in early and late January of 2004, respectively. The flight system design inherited many successfully features and approaches from the Mars Pathfinder Mission. This included the use of a mechanically-pumped fluid loop, known as the Heat Rejection System (HRS), to transport heat from the Rover to radiators on the Cruise Stage during the quiescent trek to Mars. While the heritage of the HRS was evident, application of this system for MER presented unique and difficult challenges with respect to hardware implementation. We will discuss these hardware challenges in each HRS hardware element: the integrated pump assembly, cruise stage HRS, lander HRS, and Rover HRS. These challenges span the entire development cycle including fabrication, assembly, and test. We will conclude by citing the usefulness of this system during launch operations, where in particular, the flight hardware inside the Rover was thermally conditioned by the HRS since there was no other effective means of maintaining its temperature. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tsuyuki, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 59 EP 70 PG 12 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600008 ER PT S AU Jaworske, DA AF Jaworske, DA BE ElGenk, MS TI A review of textured surfaces, paints, and coatings for space radiator applications SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB Future space nuclear power systems will require large radiators to dissipate excess thermal energy. Such radiators may be composed of carbon-carbon composite fins made from high thermal conductivity graphite fibers or may be a more traditional honeycomb structure with face sheets composed of a suitable high temperature metal. In either case, the surface of the radiator must have a high emittance at the desired operating temperature, envisioned to be in the range of 400 to 900 K, and must be durable for the length of the mission, envisioned to be ten years. Existing thermal control paints and coatings may be applicable at the low end of the envisioned temperature range, but may not be applicable at elevated temperatures. Hence, other avenues of emittance enhancement need to be explored, Previous work has identified a number of promising technologies that may be useful for enhancing the emittance of candidate surfaces, including texturing the radiator surface via sand blasting, oxidation at elevated temperature, and exposure to atomic oxygen. This paper will review existing candidate thermal control paints and coatings to identify their strengths and weaknesses and will review other promising technologies that have been proposed in the past few years to enhance the emittance of radiator surfaces. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Jaworske, DA (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA. NR 10 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 71 EP 75 PG 5 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600009 ER PT S AU Baker, CL Grob, EW McCarthy, TV Nikitkin, MN Ancarrow, WC AF Baker, CL Grob, EW McCarthy, TV Nikitkin, MN Ancarrow, WC BE ElGenk, MS TI Geoscience Laser Altimetry System (GLAS) on-orbit flight report on the propylene Loop Heat Pipes (LHPs) SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB The Geoscience Laser Altimetry System (GLAS) instrument which is the sole instrument on ICESat was launched on January 12, 2003. GLAS utilizes the very first actively controlled propylene Loop Heat Pipes (LHPs) as the core of its thermal system that are tightly controlled (to +/- 0.1 degreesC.) The LHPs started quickly when the Dale Ohm starter heaters were powered and have started, as designed, several additional times in the mission. The low control heater power and on-orbit tight temperature control appear independent of gravity effects when comparing ground testing to flight data. The use of coupling blocks was also unique to these LHPs. Their application reduced control heater power by reducing the subcooling from the radiator. The effectiveness in reducing subcooling of the coupler blocks decreased during flight from ground testing, but internal thermal isolation in the compensation chamber between the subcooled returning liquid increased in flight resulting in no net increase in control heater power versus ground measurements. Overall the application of LHPs in the thermal system for GLAS met instrument requirements and provided flexibility for the overall system as last minute requirements became known. C1 NASA, Goddard Space Flight Ctr, Dept Thermal Engn, Greenbelt, MD 20771 USA. RP Baker, CL (reprint author), NASA, Goddard Space Flight Ctr, Dept Thermal Engn, Code 545, Greenbelt, MD 20771 USA. NR 5 TC 3 Z9 3 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 88 EP 95 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600011 ER PT S AU Reinarts, TR Ford, DA AF Reinarts, TR Ford, DA BE ElGenk, MS TI Corrections for heat flux measurements taken on launch vehicles SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB Knowledge of aerothermally induced convective heat transfer and plume induced radiative heat transfer loads is essential to the design of thermal protection systems (TPS) for launch vehicles. Aerothermal and radiative models are typically calibrated via the data from cylindrical, in-flight, flush-mounted surface heat flux gauges that are exposed to the external thermal and velocity boundary layers as well as thermal radiation. Typically, Schmidt-Boelter gauges, taking advantage of the I-Dimensional Fourier's law, measure the incident heat flux. This instrumentation, when surrounded by low-conductivity insulation, has an exposed surface temperature significantly lower than the insulation. As a result of this substantial disturbance to the thermal boundary layer, the heat flux incident on the gauge tends to be considerably higher (potentially by factors of 2 or more) than it would have been on the insulation had the calorimeter not been there. In addition, the gauge can receive energy radially from the hotter insulation, contributing to the increase of the indicated heat flux. This paper will present an overview of an effort to model the heat flux gauge under typical flight conditions that includes an installation surrounded by high temperature insulation. The goal is to correct the measurements to reflect the local heat flux on the insulation had the instrument not been present. The three major components of this effort include: 1) a three-dimensional computational thermal math model including the internal conduction heat transfer details of a Schmidt-Boelter gauge, 2) a two-dimensional Navier-Stokes computational fluid dynamics (CFD) analysis to determine the effects on measurement of the rapidly changing thermal boundary layer over the near step changes in wall temperature, and 3) testing performed on flat plates exposed to an aerothermal environment in the Marshall Space Flight Center (MSFC) Improved Hot Gas Facility (IHGF). A brief summary of calibration issues will be presented, followed by the analytical efforts, as well as an update on testing results and preliminary model calibration results. Finally, recommendations will be made for installation and flight data corrections. C1 NASA, Expendable Launch Vehicles Miss Anal Branch, Kennedy Space Ctr, FL 32899 USA. RP Reinarts, TR (reprint author), NASA, Expendable Launch Vehicles Miss Anal Branch, VA-F3, Kennedy Space Ctr, FL 32899 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 133 EP 139 PG 7 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600017 ER PT S AU Martin, J Salvail, P AF Martin, J Salvail, P BE ElGenk, MS TI Sodium heat pipe module processing for the SAFE-100 reactor concept SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE ID SUPPORT AB To support development and hardware-based testing of various space reactor concepts, the Early Flight Fission-Test Facility (EFF-TF) team established a specialized glove box unit with ancillary systems to handle/process alkali metals. Recently, these systems have been commissioned with sodium supporting the fill of stainless steel heat pipe modules for use with a 100 kW thermal heat pipe reactor design. As part of this effort, procedures were developed and refined to govern each segment of the process covering: fill, leak check, vacuum processing, weld closeout, and final "wet in". A series of 316 stainless steel modules, used as precursors to the actual 321 stainless steel modules, were filled with 35 +/-1 grams of sodium using a known volume canister to control the dispensed mass. Each module was leak checked to <10(-10) std cc/sec helium and vacuum conditioned at 250 degreesC to assist in the removal of trapped gases. A welding procedure was developed to close out the fill stem preventing external gases from entering the evacuated module. Finally the completed modules were vacuum fired at 750 degreesC allowing the sodium to fully wet the internal surface and wick structure of the heat pipe module. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP NASA, George C Marshall Space Flight Ctr, TD40, Huntsville, AL 35812 USA. EM jim.j.martin@nasa.gov NR 7 TC 1 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 148 EP 155 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600019 ER PT S AU Gavert, RB AF Gavert, RB BE ElGenk, MS TI Market driven space exploration SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB Market driven space exploration will have the opportunity to develop to new levels with the coming of space nuclear power and propulsion. NASA's recently established Prometheus program is expected to receive several billion dollars over the next five years for developing nuclear power and propulsion systems for future spacecraft. Not only is nuclear power and propulsion essential for long distance Jupiter type missions, but it also important for providing greater access to planets and bodies nearer to the Earth. NASA has been working with industrial partners since 1987 through its Research Partnerships Centers (RPCs) to utilize the attributes of space in Low Earth Orbit (LEO). Plans are now being made to utilize the RPCs and industrial partners in extending the duration and boundaries of human space flight to create new opportunities for exploration and discovery. Private investors are considering setting up shops in LEO for commercial purposes. The trend is for more industrial involvement in space. Nuclear power and propulsion will hasten the progress. The objective of this paper is to show the progression of space market driven research and its potential for supporting space exploration given nuclear power and propulsion capabilities. C1 NASA Headquarters, Space Prod Dev Div, Washington, DC 20546 USA. RP Gavert, RB (reprint author), NASA Headquarters, Space Prod Dev Div, Washington, DC 20546 USA. NR 8 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 183 EP 188 PG 6 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600023 ER PT S AU Lueck, DE Immer, CD AF Lueck, DE Immer, CD BE ElGenk, MS TI Closed end launch tube (CELT) SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB A small-scale test apparatus has been built and tested for the CELT pneumatic launch assist concept presented at STAIF 2001. The 7.5 cm (3-inch) diameter x 305 M (1000 feet) long system accelerates and pneumatically brakes a 6.35 cm diameter projectile with variable weight (1.5 - 5 Kg). The acceleration and braking tube has been instrumented with optical sensors and pressure transducers at 14 stations to take data throughout the runs. Velocity and pressure profiles for runs with various accelerator pressures and projectile weights are given. This test apparatus can serve as an important experimental tool for verifying this concept. C1 NASA, Spaceport Engn & Technol Directorate, Spaceport Technol Dev Off, Technol Implementat Branch, Kennedy Space Ctr, FL 32899 USA. RP Lueck, DE (reprint author), NASA, Spaceport Engn & Technol Directorate, Spaceport Technol Dev Off, Technol Implementat Branch, YA-C3, Kennedy Space Ctr, FL 32899 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 189 EP 196 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600024 ER PT S AU Fiehler, D Oleson, S AF Fiehler, D Oleson, S BE ElGenk, MS TI Mission steering profiles of outer planetary orbiters using Radioisotope Electric Propulsion SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB Radioisotope Electric Propulsion (REP) has the potential to enable small spacecraft to orbit outer planetary targets with trip times comparable to flyby missions. The ability to transition from a flyby to an orbiter mission lies in the availability of continuous low power electric propulsion along the entire trajectory. The electric propulsion system's role is to add and remove energy from the spacecraft's trajectory to bring it in and out of a heliocentric hyperbolic escape trajectory for the outermost target bodies. Energy is added and the trajectory is reshaped to rendezvous with the closer-in target bodies. Sample REP trajectories will be presented for missions ranging for distances from Jupiter orbit to the Pluto-Kuiper Belt. C1 QSS Grp Inc, NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Fiehler, D (reprint author), QSS Grp Inc, NASA Glenn Res Ctr, 21000 Brookpk Rd,MS 301-3, Cleveland, OH 44135 USA. NR 17 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 248 EP 255 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600031 ER PT S AU Roach, PR Kittel, P Feller, J Helvensteijir, B AF Roach, PR Kittel, P Feller, J Helvensteijir, B BE ElGenk, MS TI Thermal isolator with strong mechanical support for a radioisotope heating unit SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB We have developed a suspension system using pre-tensioned titanium alloy wires to support a 1 Watt Radioisotope Heating Unit (RHU) for a mission to Mars. This suspension is very strong in all directions and has quite low thermal conduction between the RHU and its colder surroundings. This will allow the RHU to operate at 250 degreesC for generating electrical power from an attached thermoelectric converter (TEC) after surviving multiple 300 G impacts on the Martian surface. We have tested the Suspension under impact loads that have the same duration as the impacts expected from the air-bag cushions planned for the Mars mission. The suspension survives impacts of 500 G with the RHU canister at room temperature and at 250 degreesC. We calculate that with the RHU at 250 degreesC there will be only 86 mW of heat conducted through the support structure. This design in intended for use with multilayer insulation in a good vacuum. We estimate that the conduction through such insulation would be 75 mW. This leaves more than 800 mW of the heat from the RHU to flow through the TEC. yielding more than 40 mW of electrical power. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Roach, PR (reprint author), NASA, Ames Res Ctr, MS 244-10, Moffett Field, CA 94035 USA. NR 6 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 264 EP 269 PG 6 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600033 ER PT S AU Juhasz, AJ Sawicki, JT AF Juhasz, AJ Sawicki, JT BE ElGenk, MS TI High temperature fusion reactor cooling using Brayton cycle based partial energy conversion SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB For some future space power systems using high temperature nuclear heat sources most of the output energy will be used in other than electrical form, and only a fraction of the total thermal energy generated will need to be converted to electrical work. The paper describes the conceptual design of such a "partial energy conversion" system, consisting of a high temperature fusion reactor operating in series with a high temperature radiator and in parallel with dual closed cycle gas turbine (CCGT) power systems, also referred to as closed Brayton cycle (CBC) systems, which are supplied with a fraction of the reactor thermal energy for conversion to electric power. Most of the fusion reactor's output is in the form of charged plasma which is expanded through a magnetic nozzle of the interplanetary propulsion system. Reactor heat energy is ducted to the high temperature series radiator utilizing the electric power generated to drive a helium gas circulation fan. In addition to discussing the thermodynamic aspects of the system design the authors include a brief overview of the gas turbine and fan rotor-dynamics and proposed bearing support technology along with performance characteristics of the three phase AC electric power generator and fan drive motor. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Juhasz, AJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 347 EP 353 PG 7 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600042 ER PT S AU Thieme, LG Schreiber, JG AF Thieme, LG Schreiber, JG BE ElGenk, MS TI Advanced technology development for Stirling convertors SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB A high-efficiency Stirling Radioisotope Generator (SRG) for use on potential NASA Space Science missions is being developed by the Department of Energy, Lockheed Martin, Stirling Technology Company, and NASA Glenn Research Center (GRC). These missions may include providing spacecraft onboard electric power for deep space missions or power for unmanned Mars rovers. GRC is also developing advanced technology for Stirling convertors, aimed at substantially improving the specific power and efficiency of the convertor and the overall power system. Performance and mass improvement goals have been established for second- and third-generation Stirling radioisotope power systems. Multiple efforts are underway to achieve these goals, both in-house at GRC and under various grants and contracts. The status and results to date for these efforts will be discussed in this paper. Cleveland State University (CSU) is developing a multi-dimensional Stirling computational fluid dynamics code, capable of modeling complete convertors. A 2-D version of the code is now operational, and validation efforts at both CSU and the University of Minnesota are complementing the code development. A screening of advanced superalloy, refractory metal alloy, and ceramic materials has been completed, and materials have been selected for creep and joining characterization as part of developing a high-temperature heater head. A breadboard characterization is underway for an advanced controller using power electronics for active power factor control with a goal of eliminating the heavy tuning capacitors that are typically needed to achieve near unity power factors. Key Stirling developments just initiated under recent NRA (NASA Research Announcement) awards will also be discussed. These include a lightweight convertor to be developed by Sunpower Inc. and an advanced microfabricated regenerator to be done by CSU. C1 NASA, Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA. RP Thieme, LG (reprint author), NASA, Glenn Res Ctr Lewis Field, MS 301-2,21000 Brookpk Rd, Cleveland, OH 44135 USA. NR 11 TC 7 Z9 7 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 432 EP 439 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600053 ER PT S AU Barrett, MJ Reid, BM AF Barrett, MJ Reid, BM BE ElGenk, MS TI System mass variation and entropy generation in 100-kWe closed-Brayton-cycle space power systems SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB State-of-the-art closed-Brayton-cycle (CBC) space power systems were modeled to study performance trends in a trade space characteristic of interplanetary orbiters. For working-fluid molar masses of 48.6, 39.9 and 11.9 kg/kmol, peak system pressures of 1.38 and 3.0 MPa and compressor pressure ratios ranging from 1.6 to 2.4, total system masses were estimated. System mass increased as peak operating pressure increased for all compressor pressure ratios and molar mass values examined. Minimum mass point comparison between 72% He at 1.38 MPa peak and 94% He at 3.0 MPa peak showed an increase in system mass of 14%. Converter flow loop entropy generation rates were calculated for 1.38 and 3.0 MPa peak pressure cases. Physical system behavior was approximated using a pedigreed NASA-Glenn modeling code, Closed Cycle Engine Program (CCEP), which included realistic performance prediction for heat exchangers, radiators and turbomachinery. C1 NASA, Glenn Res Ctr, Power & On Board Prop Technol Div, Cleveland, OH 44135 USA. RP Barrett, MJ (reprint author), NASA, Glenn Res Ctr, Power & On Board Prop Technol Div, Cleveland, OH 44135 USA. NR 14 TC 11 Z9 11 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 445 EP 452 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600055 ER PT S AU Tew, R Ibrahim, M Simon, T Mantell, S Gedeon, D Qiu, SG Wood, JG AF Tew, R Ibrahim, M Simon, T Mantell, S Gedeon, D Qiu, SG Wood, JG BE ElGenk, MS TI Overview 2003 of NASA multi-D Stirling convertor code development and DOE and NASA Stirling regenerator R&D efforts SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB This paper will report on (1) continuation through the 3(rd) year of a NASA grant for multi-dimensional Stirling CFD code development and validation, (2) continuation through the 3(rd) and final year of a Department of Energy, Golden Field Office (DOE), regenerator research effort and a NASA grant for continuation of the effort through two additional years, and (3) a new NASA Research Award for design, microfabrication and testing of a "Next Generation Stirling Engine Regenerator." Cleveland State University (CSU) is the lead organization for all three efforts, with the University of Minnesota (UMN) and Gedeon Associates as subcontractors. The Stirling Technology Co. and Sunpower, Inc. acted as unfunded consultants or participants through the 3(rd) years of both the NASA multi-D code development and DOE regenerator research efforts; they will both be subcontractors on the new regenerator microfabrication contract. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Roy.C.Tew@nasa.gov NR 16 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 473 EP 482 PG 10 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600058 ER PT S AU Kimnach, GL Soltis, JV AF Kimnach, GL Soltis, JV BE ElGenk, MS TI Power management and distribution trades studies for a deep-space mission scientific spacecraft SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB As part of NASA's Project Prometheus, the Nuclear Systems Program, NASA GRC performed trade studies on the various Power Management and Distribution (PMAD) options for a deep-space scientific spacecraft, which would have a nominal electrical power requirement of 100 kWe. These options included AC (1000Hz and 1500Hz) and DC primary distribution at various voltages. The distribution system efficiency, reliability, mass, thermal, corona, space radiation levels, and technology readiness of devices and components were considered. The final proposed system consisted of two independent power distribution channels, sourced by two 3-phase, 110 kVA alternators nominally operating at half-rated power. Each alternator nominally supplies 50 kWe to one-half of the ion thrusters and science modules, but is capable of supplying the total power requirements in the event of loss of one alternator. This paper is an introduction to the methodology for the trades done to arrive at the proposed PMAD architecture. Any opinions expressed are those of the author(s) and do not necessarily reflect the views of Project Prometheus. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Kimnach, GL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 301-5, Cleveland, OH 44135 USA. NR 2 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 590 EP 597 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600070 ER PT S AU Birchenough, AG AF Birchenough, AG BE ElGenk, MS TI A high efficiency DC bus regulator/RPC for spacecraft applications SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB DC bus voltage regulation may be required in future high powered spacecraft due to the length of the busses or because they are not generated at precise voltage levels. In these cases the regulation range is often only a few percent increase or decrease, but conventional DC voltage regulators switch all the power passing through them, and this level of power switched determines the size and losses in the regulator. A recently developed concept uses a low power DC-DC converter in series with the bus to raise or lower the bus voltage over a small range. This partial power processing technique combines the small size and power losses of the low power converter with the ability to regulate, (over a small range) a high power bus. The Series Connected Buck Boost Regulator (SCBBR) described herein provides bus regulation with an efficiency of 98%. The circuit also provides bus switching and overcurrent limiting functions of a Remote Power Controller (RPC). This paper describes the circuit design and performance of a breadboard SCBBR configured as a bus voltage regulator providing +/- 40% voltage regulation range, bus switching, and overload limiting. C1 NASA, Glenn Res Ctr Lewis Field, Power & On Board Prop Technol Div, Cleveland, OH 44135 USA. RP Birchenough, AG (reprint author), NASA, Glenn Res Ctr Lewis Field, Power & On Board Prop Technol Div, Cleveland, OH 44135 USA. NR 3 TC 3 Z9 3 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 606 EP 613 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600072 ER PT S AU Van Dyke, M AF Van Dyke, M BE ElGenk, MS TI Early flight fission test facilities (EFF-TF) to support near-term space fission systems SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE ID ELECTRIC PROPULSION AB Through hardware based design and testing, the EFF-TF investigates fission power and propulsion component, subsystems, and integrated system design and performance. Through demonstration of systems concepts (designed by Sandia and Los Alamos National Laboratories) in relevant environments, previous non-nuclear tests in the EFF-TF have proven to be a highly effective method (from both cost and performance standpoint) to identify and resolve integration issues. Ongoing research at the EFF-TF is geared towards facilitating research, development, system integration, and system utilization via cooperative efforts with DOE labs, industry, universities, and other NASA centers. This paper describes the current efforts for 2003. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Van Dyke, M (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NR 6 TC 7 Z9 7 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 713 EP 719 PG 7 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600084 ER PT S AU Godfroy, TJ Kapernick, RJ Bragg-Sitton, SM AF Godfroy, TJ Kapernick, RJ Bragg-Sitton, SM BE ElGenk, MS TI Thermally simulated 32kW direct-drive gas-cooled reactor: Design, assembly, and test SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB One of the power systems under consideration for nuclear electric propulsion is a direct-drive gas-cooled reactor coupled to a Brayton cycle. In this system, power is transferred from the reactor to the Brayton system via a circulated closed loop gas. To allow early utilization, system designs must be relatively simple, easy to fabricate, and easy to test using non-nuclear heaters to closely mimic heat from fission. This combination of attributes will allow pre-prototypic systems to be designed, fabricated, and tested quickly and affordably. The ability to build and test units is key to the success of a nuclear program, especially if an early flight is desired. The ability to perform very realistic non-nuclear testing increases the success probability of the system. In addition, the technologies required by a concept will substantially impact the cost, time, and resources required to develop a successful space reactor power system. This paper describes design features, assembly, and test matrix for the testing of a thermally simulated 32kW direct-drive gas-cooled reactor in the Early Flight Fission-Test Facility (EFF-TF) at Marshall Space Flight Center. The reactor design and test matrix are provided by Los Alamos National Laboratories. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Godfroy, TJ (reprint author), NASA, George C Marshall Space Flight Ctr, TD40, Huntsville, AL 35812 USA. NR 5 TC 6 Z9 6 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 757 EP 763 PG 7 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600090 ER PT S AU Bowman, R Ritzert, F Freedman, M AF Bowman, R Ritzert, F Freedman, M BE ElGenk, MS TI Evaluation of candidate materials for a high-temperature Stirling convertor heater head SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB The Department of Energy (DOE) and NASA have identified Stirling Radioisotope Generators (SRG) as a candidate power system for use on long-duration, deep-space science missions and Mars rovers. One of the developments planned for an upgraded version of the current SRG design is to achieve higher efficiency by increasing the overall operating temperature of the system. Currently, the SRG operates with a heater head temperature of 650 degreesC and is fabricated from the nickel base superalloy 718. This temperature is at the limit of Alloy 718's capability, and any planned increase in temperature will be contingent on identifying a more capable material from which to fabricate the heater head. To this end, an assessment of material candidates was performed assuming a range of heater head temperatures. The chosen alternative material candidates will be discussed, along with the development efforts needed to ensure that these materials can meet the demanding system requirements of long-duration operation in hostile environments. C1 NASA, Glenn Res Ctr, Div Mat, Cleveland, OH 44135 USA. RP Bowman, R (reprint author), NASA, Glenn Res Ctr, Div Mat, Cleveland, OH 44135 USA. NR 7 TC 4 Z9 4 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 821 EP 828 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600097 ER PT S AU Cohen, MM AF Cohen, MM BE ElGenk, MS TI Mobile lunar base concepts SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB This paper describes three innovative concepts for a mobile lunar base. These concept combine design research for habitat architecture, mobility systems, habitability, radiation protection, human factors, and living and working environments on the lunar surface. The mobile lunar base presents several key advantages over conventional static base notions. These advantages concern landing zone safety, the requirement to move modules over the lunar surface, and the ability to stage mobile reconnaissance with effective systemic redundancy. All of these concerns lead to the consideration of a mobile walking habitat module and base design. The key issues involve landing zone safety, the ability to transport habitat modules across the surface, and providing reliability and redundancy to exploration traverses in pressurized vehicles. With self-ambulating lunar base modules, it will be feasible to have each module separate itself from its retro-rocket thruster unit, and walk five to ten kin away from the LZ to a pre-selected site. These mobile modules can operate in an autonomous or teleoperated mode to navigate the lunar surface. At the site of the base, the mobile modules can combine together; make pressure port connections among themselves, to create a multi-module pressurized lunar base. C1 NASA, Ames Res Ctr, Space Projects Div, Adv Projects Branch, Moffett Field, CA 94035 USA. RP Cohen, MM (reprint author), NASA, Ames Res Ctr, Space Projects Div, Adv Projects Branch, Moffett Field, CA 94035 USA. NR 10 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 845 EP 853 PG 9 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600099 ER PT S AU Watson, JK Robbins, WW AF Watson, JK Robbins, WW BE ElGenk, MS TI Preliminary analysis of ISS maintenance history and implications for supportability of future missions SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE AB The International Space Station (ISS) enables the study of supportability issues associated with long-duration human spaceflight. The ISS is a large, complex spacecraft that must be maintained by its crew. In contrast to the Space Shuttle Orbiter vehicle, but similar to spacecraft that will be component elements of future missions beyond low-Earth orbit, ISS does not return to the ground for servicing and provisioning of spares is severely constrained by transportation limits. Although significant technical support is provided by ground personnel, all hands-on maintenance tasks are performed by the crew. Data accumulated over the first several years of ISS operations have been analyzed to gain a better understanding of maintenance-related workload. This analysis addresses both preventive and corrective maintenance and includes all US segment core systems. Systems and tasks that are major contributors to workload are identified. As further experience accrues, lessons will be learned that will influence future system designs so that they require less maintenance and, when maintenance is required, it can be performed more efficiently. By heeding the lessons of ISS it will be possible to identify system designs that should be more robust and point towards advances in both technology and design that will offer the greatest return on investment. C1 NASA, Lyndon B Johnson Space Ctr, Adv Dev Off, Houston, TX 77058 USA. RP Watson, JK (reprint author), NASA, Lyndon B Johnson Space Ctr, Adv Dev Off, Houston, TX 77058 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 905 EP 912 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600105 ER PT S AU Wilson, JW Cucinotta, FA Schimmerling, W AF Wilson, JW Cucinotta, FA Schimmerling, W BE ElGenk, MS TI Emerging radiation health-risk mitigation technologies SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE ID SPACE RADIATION; TRACK STRUCTURE; ISSUES; INACTIVATION; PROTECTION; DESIGN; CELLS AB Past space missions beyond the confines of the Earth's protective magnetic field have been of short duration and protection from the effects of solar particle events was of primary concern. The extension of operational infrastructure beyond low-Earth orbit to enable routine access to more interesting regions of space will require protection from the hazards of the accumulated exposures of Galactic Cosmic Rays (GCR). There are significant challenges in providing protection from the long-duration exposure to GCR: the human risks to the exposures are highly uncertain and safety requirements places unreasonable demands in supplying sufficient shielding materials in the design, A vigorous approach to future radiation health-risk mitigation requires a triage of techniques (using biological and technical factors) and reduction of the uncertainty in radiation risk models. The present paper discusses the triage of factors for risk mitigation with associated materials issues and engineering design methods. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM john.w.wilson@larc.nasa.gov NR 38 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 913 EP 924 PG 12 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600106 ER PT S AU Robertson, T Nordley, GD AF Robertson, T Nordley, GD BE ElGenk, MS TI A review of past insights by Robert L. Forward, PhD: Emerging technologies and future concepts SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM-STAIF 2004 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2004) CY FEB 08-11, 2004 CL Albuquerque, NM SP Boeing Co, Gen Autom, Lockheed Martin, Los Alamos Natl Lab, Northrop Grumman Space Technol, Sandia Natl Labs, US DOE ID SUPERCONDUCTORS; FIELD AB A review of various technologies discussed by Dr. Robert Forward is presented as a tribute to Dr. Forward, and is based on selections from his writings and those of subsequent investigators. Some emphasis is placed on the new frontiers of space propulsion, power and communication. Many of these concepts and technologies are presented within the STAIF 2004 "1st Symposium on New Frontiers and Future Concepts." These range from highly speculative notions to hardware that has now been demonstrated in space flight. Among these concepts and technologies to be discussed are future communications, antimatter propulsion, space elevators and tethers, beamed energy propulsion, and emerging gravity theories and concepts. C1 NASA, George C Marshall Space Flight Ctr, Propuls Res Ctr, Huntsville, AL 35812 USA. RP Robertson, T (reprint author), NASA, George C Marshall Space Flight Ctr, Propuls Res Ctr, Huntsville, AL 35812 USA. NR 50 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0171-3 J9 AIP CONF PROC PY 2004 VL 699 BP 1247 EP 1254 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology; Physics, Applied SC Engineering; Nuclear Science & Technology; Physics GA BY68D UT WOS:000189437600147 ER PT S AU Habib, S Zukor, D Ambrose, S AF Habib, S Zukor, D Ambrose, S BE Habbit, RD Tchoryk, P TI Using science driven technologies for the defense and security applications SO SPACEBORNE SENSORS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Spaceborne Sensors CY APR 13, 2004 CL Orlando, FL SP SPIE DE landsat; NASA; soil moisture; calcium; synchronous; UARS AB For the last three decades, space science remote sensing technologies have been providing enormous amounts of useful data and information in broadening our understanding of the solar system including our home planet. This research, as it has expanded our learning process, has generated additional questions. This has further resulted in establishing new science requirements, which have culminated in defining and pushing the state-of-the-art technology needs. NASAs Earth Science exploration has deployed about 18 highly complex satellites so far and is in a process of defining and launching multiple observing systems in the next decade. Due to the heightened security alert of our Nation, researchers and technologists are paying serious attention to make use of these science driven technologies for dual use. In other words, how such sophisticated observing and measuring systems can be used in detecting multiple types of security concerns with substantial lead time so that the appropriate law enforcement agencies and decision makers can take adequate steps to defuse any potential risks and protect society. This paper examines numerous NASA technologies such as laser/lidar systems, microwave and millimeter wave technologies, optical observing systems, high performance computational techniques for rapid analyses, and imaging products that can have a tremendous pay off for security applications. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Habib, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 3 TC 0 Z9 0 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5341-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5418 BP 1 EP 9 DI 10.1117/12.543672 PG 9 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BAX93 UT WOS:000224146900001 ER PT S AU Briscoe, JM Broderick, DJ Howard, R Corder, EL AF Briscoe, JM Broderick, DJ Howard, R Corder, EL BE Habbit, RD Tchoryk, P TI Machine vision applied to navigation of confined spaces SO SPACEBORNE SENSORS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Spaceborne Sensors CY APR 13, 2004 CL Orlando, FL SP SPIE DE miniature; vision; robotics; inspection; laser AB The reliability of space related assets has been emphasized after the second loss of a Space Shuttle. The intricate nature of the hardware being inspected often requires a complete disassembly to perform a thorough inspection which can be difficult as well as costly. Furthermore, it is imperative that the hardware under inspection not be altered in any other manner than that which is intended. In these cases the use of machine vision can allow for inspection with greater frequency using less intrusive methods. Such systems can provide feedback to guide, not only manually controlled instrumentation, but autonomous robotic platforms as well. This paper serves to detail a method using machine vision to provide such sensing capabilities in a compact package. A single camera is used in conjunction with a projected reference grid to ascertain precise distance measurements. The design of the sensor focuses on the use of conventional components in an unconventional manner with the goal of providing a solution for systems that do not require or cannot accommodate more complex vision systems. C1 NASA, George C Marshall Space Flight Ctr, Imaging Team, Huntsville, AL 35812 USA. RP Briscoe, JM (reprint author), NASA, George C Marshall Space Flight Ctr, Imaging Team, ED12, Huntsville, AL 35812 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5341-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5418 BP 30 EP 37 DI 10.1117/12.542079 PG 8 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BAX93 UT WOS:000224146900004 ER PT S AU Howard, RT Johnston, ASN Bryan, TC Book, ML AF Howard, RT Johnston, ASN Bryan, TC Book, ML BE Habbit, RD Tchoryk, P TI Advanced Video Guidance Sensor (AVGS) development testing SO SPACEBORNE SENSORS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Spaceborne Sensors CY APR 13, 2004 CL Orlando, FL SP SPIE DE Automated Rendezvous and Capture; Video Guidance Sensor; AR&C; AR&D; VGS; AVGS AB NASA's Marshall Space Flight Center was the driving force behind the development of the Advanced Video Guidance Sensor, an active sensor system that provides near-range sensor data as part of an automatic rendezvous and docking system. The sensor determines the relative positions and attitudes between the active sensor and the passive target at ranges up to 300 meters. The AVGS uses laser diodes to illuminate retro-reflectors in the target, a solid-state camera to detect the return from the target, and image capture electronics and a digital signal processor to convert the video information into the relative positions and attitudes. The AVGS will fly as part of the Demonstration of Autonomous Rendezvous Technologies (DART) in October, 2004. This development effort has required a great deal of testing of various sorts at every phase of development. Some of the test efforts included optical characterization of performance with the intended target, thermal vacuum testing, performance tests in long range vacuum facilities, EMI/EMC tests, and performance testing in dynamic situations. The sensor has been shown to track a target at ranges of up to 300 meters, both in vacuum and ambient conditions, to survive and operate during the thermal vacuum cycling specific to the DART mission, to handle EMI well, and to perform well in dynamic situations. C1 NASA, George C Marshall Space Flight Ctr, Simulat Grp, Huntsville, AL 35812 USA. RP Howard, RT (reprint author), NASA, George C Marshall Space Flight Ctr, Simulat Grp, ED19, Huntsville, AL 35812 USA. NR 6 TC 8 Z9 9 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5341-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5418 BP 50 EP 60 DI 10.1117/12.542475 PG 11 WC Engineering, Aerospace; Remote Sensing SC Engineering; Remote Sensing GA BAX93 UT WOS:000224146900006 ER PT S AU Fredrickson, SE Duran, S Howard, N Wagenknecht, JD AF Fredrickson, SE Duran, S Howard, N Wagenknecht, JD BE Tchoryk, P Wright, M TI Application of the Mini AERCam free flyer for orbital inspection SO SPACECRAFT PLATFORMS AND INFRASTRUCTURE SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Spacecraft Platforms and Infrastructure CY APR 14, 2004 CL Orlando, FL SP SPIE DE AERCam; free flyer; docking; magnetic; navigation; inspection; nanosatellite; spacecraft; servicing; autonomy AB The Engineering Directorate of NASA Johnson Space Center has developed a nanosatellite-class free-flyer intended for future external inspection and remote viewing of human spacecraft. The Miniature Autonomous Extravehicular Robotic Camera (Mini AERCam) technology demonstration unit has been integrated into the approximate form and function of a flight system. The spherical Mini AERCam free flyer is 7.5 inches in diameter and weighs approximately 10 pounds, yet it incorporates significant additional capabilities compared to the 35 pound, 14 inch AERCam Sprint that flew as a Shuttle flight experiment in 1997. Mini AERCam hosts a full suite of miniaturized avionics, instrumentation, communications, navigation, imaging, power, and propulsion subsystems, including two digital video cameras and a high resolution still image camera. The vehicle is designed for either remotely piloted operations or supervised autonomous operations including automatic stationkeeping and point-to-point maneuvering. Free-flyer testing has been conducted on an air-bearing table and in a six degree-of-freedom closed-loop orbital simulation. Ibis paper describes recent enhancements to the Mini AERCam system aimed at providing a more autonomous system for space inspection, including docking mechanisms and on-board docking navigation for autonomous deployment and retrieval of the free flyer. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Wagenknecht, JD (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 2 TC 2 Z9 2 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5342-0 J9 P SOC PHOTO-OPT INS PY 2004 VL 5419 BP 26 EP 35 DI 10.1117/12.542810 PG 10 WC Engineering, Aerospace SC Engineering GA BAX95 UT WOS:000224149300003 ER PT J AU Greenleaf, JE Rehrer, NJ Mohler, SR Quach, DT Evans, DG AF Greenleaf, JE Rehrer, NJ Mohler, SR Quach, DT Evans, DG TI Airline chair-rest deconditioning - Induction of immobilisation thromboemboli? SO SPORTS MEDICINE LA English DT Review ID DEEP-VEIN THROMBOSIS; LONG-HAUL FLIGHTS; ECONOMY CLASS SYNDROME; PROLONGED AIR-TRAVEL; ACTIVATED PROTEIN-C; ALTITUDE PULMONARY-EDEMA; ACUTE MOUNTAIN-SICKNESS; COACH CLASS THROMBOSIS; VENOUS THROMBOSIS; BED-REST AB Air passenger miles will likely double by year 2020. The altered and restrictive environment in an airliner cabin can influence haematological homeostasis in passengers and crew. Flight-related deep venous thromboemboli (DVT) have been associated with at least 577 deaths on 42 of 120 airlines from 1977 to 1984 (25 deaths/million departures), whereas many such cases go unreported. However, there are four major factors that could influence formation of possible flight-induced DVT: sleeping accommodations (via sitting immobilisation); travellers' medical history (via tissue injury); cabin environmental factors (via lower partial pressure,of oxygen and lower relative humidity); and the more encompassing chair-rest deconditioning (C-RD) syndrome. There is ample evidence that recent injury and surgery (especially in deconditioned hospitalised patients) facilitate thrombophlebitis acid formation of DVT that may be exacerbated by the immobilisation of prolonged air travel. In the healthy flying population, immobilisation factors associated with prolonged (>5 hours) C-RD such as total body dehydration, hypovolaemia and increased blood viscosity, and reduced venous blood flow (pooling) in the legs may facilitate formation of DVT. However, data from at least four case-controlled epidemiological studies did not confirm a direct causative relationship. between air travel and DVT, but factors such as a history of vascular thromboemboli, venous insufficiency, chronic heart failure, obesity, immobile standing position, more than three pregnancies, infectious disease, long-distance travel, muscular trauma and violent physical effort were significantly more frequent in DVT patients than in controls. Thus, there is no clear, direct evidence yet that prolonged sitting in airliner seats, or prolonged experimental chair-rest or bed-rest deconditioning. treatments cause DVT in healthy people. C1 NASA, Ames Res Ctr, Gravitat Res Branch, Stanford, CA 94305 USA. NASA, Ames Res Ctr, Lab Human Environm Physiol, Stanford, CA 94305 USA. Univ Otago, Sch Phys Educ, Dunedin, New Zealand. Wright State Univ, Dept Community Hlth, Dayton, OH USA. RP Greenleaf, JE (reprint author), NASA, Ames Res Ctr, Gravitat Res Branch, 239-11, Stanford, CA 94305 USA. NR 156 TC 3 Z9 3 U1 1 U2 6 PU ADIS INT LTD PI AUCKLAND PA 41 CENTORIAN DR, PRIVATE BAG 65901, MAIRANGI BAY, AUCKLAND 1311, NEW ZEALAND SN 0112-1642 J9 SPORTS MED JI Sports Med. PY 2004 VL 34 IS 11 BP 705 EP 725 DI 10.2165/00007256-200434110-00002 PG 21 WC Sport Sciences SC Sport Sciences GA 860VS UT WOS:000224372400002 PM 15456346 ER PT S AU Yorke, HW AF Yorke, HW BE Burton, MG Jayawardhana, R Bourke, TL TI Theory of formation of massive stars via accretion SO STAR FORMATION AT HIGH ANGULAR RESOLUTION SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 221st Symposium of the International-Astronomical-Union CY JUL 22-25, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID PROTOSTELLAR DISKS; STELLAR EVOLUTION; GROWING ACCRETION; MAIN-SEQUENCE; GRAINS AB The collapse of massive molecular clumps can produce high mass stars, but the evolution is not simply a scaled-up version of low mass star formation. Outflows and radiative effects strongly hinder the formation of massive stars via, accretion. A necessary condition for accretion growth of a hydrostatic object up to high masses M greater than or similar to 20M(circle dot) (rather than coalescence of optically thick objects) is the formation of, and accretion through, a circumstellar disk. Once the central object has accreted approximately 10 M-circle dot it has already evolved to core hydrogen-burning; the resultant main sequence star continues to accrete material as it begins to photoevaporate its circurnstellar disk (and any nearby disks) on a timescale of similar to10(5) yr, similar to the accretion timescale. Until the disk(s) is (are) completely photoevaporated, this configuration is observable as an ultra-compact HII region (UCHII). The final mass of the central star (and any nearby neighboring systems) is determined by the interplay between radiation acceleration, UV photoevaporation, stellar winds and outflows, and the accretion through the disk. Several aspects of this evolutionary sequence have been simulated numerically, resulting in a "proof of concept". This scenario places strong constraints on the accretion rate necessary to produce high mass stars and offers an opportunity to test the accretion hypothesis. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Yorke, HW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-506, Pasadena, CA 91109 USA. NR 27 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-161-3 J9 IAU SYMP PY 2004 IS 221 BP 141 EP 152 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBB15 UT WOS:000224473800015 ER PT S AU Greene, T AF Greene, T BE Burton, MG Jayawardhana, R Bourke, TL TI Infrared studies of protostellar binaries SO STAR FORMATION AT HIGH ANGULAR RESOLUTION SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 221st Symposium of the International-Astronomical-Union CY JUL 22-25, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID STAR-FORMING REGIONS; MU-M SURVEY; MULTIPLICITY; EVOLUTION; SYSTEMS; CLUSTER AB Although much progress has been made in studying the multiplicity properties of pre-main-sequence T Tauri stars over the past decade, younger and more embedded protostellar systems are just now being surveyed for multiplicity. I examine several recent infrared imaging and spectroscopic studies which reveal the multiplicity properties of embedded protostars for the first time. The overall binary / multiplicity fraction of protostars is statistically indistinguishable from that of premain-sequence stars when measured over similar separation distances. Some individual components of protostellar binaries appear to be coeval from their spectral energy distributions or spectra. However, there are some systems which appear to consist of both a protostar and a pre-main-sequence star, and the coevality of these systems is very uncertain. There is much yet to be learned about the multiplicity properties of protostars, and future high resolution near-IR imaging surveys will likely make much headway. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Greene, T (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. NR 17 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-161-3 J9 IAU SYMP PY 2004 IS 221 BP 223 EP 228 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBB15 UT WOS:000224473800023 ER PT S AU Clampin, M Krist, J Ardila, DR Illingworth, G AF Clampin, M Krist, J Ardila, DR Illingworth, G BE Burton, MG Jayawardhana, R Bourke, TL TI ACS coronagraphic observations of optically thin debris disks SO STAR FORMATION AT HIGH ANGULAR RESOLUTION SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 221st Symposium of the International-Astronomical-Union CY JUL 22-25, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID CIRCUMSTELLAR DISK; DYNAMICS AB The Advanced Camera for Surveys (ACS) offers a coronagraphic imaging mode with angular resolution of 0.026" pixel(-1). In combination with with the appropriate subtraction of reference star point spread functions (PSF) the coronagraph is capable of achieving contrast ratios of similar to1000. We present some of the first ACS observations of the optically thin debris disk HD141569A and discuss new results from these observations. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Clampin, M (reprint author), NASA, Goddard Space Flight Ctr, 8077 Greenbelt Rd, Greenbelt, MD 20771 USA. RI Clampin, mark/D-2738-2012 NR 14 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-161-3 J9 IAU SYMP PY 2004 IS 221 BP 449 EP 457 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBB15 UT WOS:000224473800050 ER PT B AU Hollenbach, D Adams, FC AF Hollenbach, D Adams, FC BE Johnstone, D Adams, FC Lin, DNC Neufeld, DA Ostriker, EC TI The disruption of planet-forming disks SO STAR FORMATION IN THE INTERSTELLAR MEDIUM: IN HONOR OF DAVID HOLLENBACH, CHRIS MCKEE AND FRANK SHU SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Star Formation in the Interstellar Medium held in honor of David Hollenbach, Chris McKee and Frank Shu CY JUN 30-JUL 03, 2003 CL Lake Tahoe, CA ID HERBIG AE/BE STARS; GIANT PLANETS; SOLAR NEBULA; ORION NEBULA; MASSIVE STARS; GAS; MODELS; HYADES; PHOTOEVAPORATION; PROTOPLANET AB Photoevaporation is likely the dominant dispersal mechanism for the outer regions of dusty disks around young stars. The gas in disk surfaces is often heated by ultraviolet photons from either the central star or from a luminous nearby massive star in the star-forming cluster; this heated gas evaporates into interstellar space, dragging along small dust particles. In this paper, we focus on photo evaporation caused by nearby massive stars and study whether photo evaporation can remove the outer disk material before the gas giant planets can form or before the dust there coagulates into large particles (greater than about 1 cm in size) which resist entrainment in the evaporating gas and remain in orbit to form Kuiper Belt objects. We show how photoevaporation can explain the difference in hydrogen content of the giant planets in our solar system, and may suppress gas giant planet formation in large clusters such as the Hyades, 47 Tuc, or the Trapezium. Photoevaporation in medium-sized and large clusters may also suppress the formation of Kuiper Belt Objects beyond about 100 AU. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Hollenbach, D (reprint author), NASA, Ames Res Ctr, MS245-3, Moffett Field, CA 94035 USA. NR 49 TC 5 Z9 5 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-185-0 J9 ASTR SOC P PY 2004 VL 323 BP 3 EP 18 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBQ04 UT WOS:000227011700001 ER PT S AU Phillips, KJH Sylwester, J Sylwester, B Landi, E AF Phillips, K. J. H. Sylwester, J. Sylwester, B. Landi, E. BA Dupree, AK BF Dupree, AK TI Abundances of potassium, argon, and sulphur in solar flares SO Stars as Suns: Activity, Evolution and Planets SE IAU SYMPOSIA LA English DT Proceedings Paper CT 219th IAU Symposium on Stars as Suns - Activity, Evolution, and Planets CY JUL 21-25, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union ID ELEMENT ABUNDANCES; ATOMIC DATABASE; EMISSION-LINES; CHIANTI; SUN AB Observations of the 3.3-6.1 A X-ray line and continuous spectrum during four long-duration flares with the RESIK crystal spectrometer on the Coronas-F spacecraft have been analyzed to get the absolute abundances of potassium, argon, and sulphur. A differential emission measure of the form DEM alpha exp(-T-e/T-0) was found to give the most consistent results of three models including an isothermal model. We obtained K/H = (3.7 +/- 1.0) X 10(-7), a factor 3 times photospheric; Ar/H (2.8 +/- 0.2) X 10(-6), slightly lower than photospheric; and S/H = (2.2 +/- 0.4) x 10(-5), approximately equal to photospheric. These measurements are consistent with a pattern in which elements with low (< 10 eV) first ionization potential are enriched in the corona by a factor of about 3 and elements of high first ionization potential have abundances approximately equal to photospheric. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Polish Acad Sci, Ctr Space Res, PL-51622 Wroclaw, Poland. Artep Inc, Ellicott City, MD 21042 USA. USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. RP Phillips, KJH (reprint author), NASA, Goddard Space Flight Ctr, Code 682, Greenbelt, MD 20771 USA. RI Landi, Enrico/H-4493-2011 NR 9 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-163-X J9 IAU SYMP PY 2004 VL 2004 IS 219 BP 176 EP 180 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFN67 UT WOS:000243338300019 ER PT S AU Fludra, A Ireland, J AF Fludra, A. Ireland, J. BA Dupree, AK BF Dupree, AK TI Diagnostics of coronal heating in solar active regions SO STARS AS SUNS: ACTIVITY, EVOLUTION AND PLANETS SE IAU SYMPOSIA LA English DT Proceedings Paper CT 219th IAU Symposium on Stars as Suns - Activity, Evolution, and Planets CY JUL 21-25, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union ID MAGNETIC-FIELD AB We study the relationship between EUV spectral line intensities and the photospheric magnetic field in solar active regions, using magnetograms from SOHO-MDI and EUV spectra of the Fe XVI 360.8 A line (2 x 10(6) K) and the O V 629.7 A line (220,000 K) from the Coronal Diagnostic Spectrometer on SOHO, recorded for several active regions. We overlay and compare spatial patterns of the O V emission and the magnetic flux concentrations, with a 4" x 4" spatial resolution, and search for a relationship between the local O V line intensity and the photospheric magnetic flux density in each active region. While this dependence exhibits a certain amount of scatter, it can be represented by a power law fit. The average power index from all regions is 0.7 +/- 0.2. Applying static loop models, we derive the dependence of the heating rate on the magnetic flux density, E(h) proportional to B(0.8), and compare it to the dependence predicted by the coronal heating models. C1 Rutherford Appleton Lab, CCLRC, Didcot OX11 0QX, Oxon, England. NASA, Goddard Space Flight Ctr, Analyt Corp, L3com, Greenbelt, MD 20771 USA. RP Fludra, A (reprint author), Rutherford Appleton Lab, CCLRC, Didcot OX11 0QX, Oxon, England. NR 12 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-163-X J9 IAU SYMP PY 2004 VL 2004 IS 219 BP 478 EP 482 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFN67 UT WOS:000243338300058 ER PT S AU Harra, LK Sterling, AC AF Harra, Louise K. Sterling, Alphonse C. BA Dupree, AK BF Dupree, AK TI Solar "EIT waves" - What are they? SO Stars as Suns: Activity, Evolution and Planets SE IAU SYMPOSIA LA English DT Proceedings Paper CT 219th IAU Symposium on Stars as Suns - Activity, Evolution, and Planets CY JUL 21-25, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union ID CORONAL MASS EJECTION AB There has been substantial interest in the coronal wave phenomena since its discovery several years ago using the EUV Imaging Telescope onboard SOHO (Thompson et al. 1999). One of the first explanations was that finally the coronal part of the Moreton wave had been discovered. Since then, there have been a number of results giving different explanations. We will discuss these in this paper along with the latest results on coronal waves from a spectroscopic perspective. C1 Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. RP Harra, LK (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. NR 13 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-163-X J9 IAU SYMP PY 2004 VL 2004 IS 219 BP 498 EP 502 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFN67 UT WOS:000243338300062 ER PT S AU Habbal, SR Woo, R AF Habbal, Shadia Rifai Woo, Richard BA Dupree, AK BF Dupree, AK TI Origin of the solar wind and open coronal magnetic structures SO Stars as Suns: Activity, Evolution and Planets SE IAU SYMPOSIA LA English DT Proceedings Paper CT 219th IAU Symposium on Stars as Suns - Activity, Evolution, and Planets CY JUL 21-25, 2003 CL Sydney, AUSTRALIA SP Int Astronom Union ID EMISSION-LINE POLARIZATION; SPECTROMETER; FIELD; GAS; SUN AB Identifying the regions of open magnetic structures in the corona, namely regions where field lines expand outwards into interplanetary space, is equivalent to establishing the origin of the solar wind at the Sun. A review of recent studies, based on the comparison of the distribution, as a function of latitude, of density and velocity in the inner corona and in interplanetary space, is presented. It is shown how, at solar minimum, this comparison leads to the unexpected result that the fast solar wind expands indiscriminately from a significant fraction of the solar surface, not limited to polar coronal holes, as has been believed for the past three decades. It is also shown how polarization measurements of coronal forbidden lines, which yield the direction of the coronal magnetic field, lend further support to this result. The implications of these findings are that a significant fraction of the solar magnetic field is primarily open, expanding almost radially into interplanetary space, carrying with it the imprint of the distribution of density in the corona, while the 'closed' structures contribute a small fraction to the overall filling factor of coronal density structures. Furthermore, the solar wind particle flux is found to be correlated with density, implying a higher mass loss rate from the higher density quiet Sun regions, and the likelihood of a solar cycle dependence in the mass loss rate, as the are of polar coronal holes decreases with increased solar activity. C1 Univ Wales, Inst Math & Phys Sci, Aberystwyth SY23 3BZ, Dyfed, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Habbal, SR (reprint author), Univ Wales, Inst Math & Phys Sci, Aberystwyth SY23 3BZ, Dyfed, Wales. NR 18 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-163-X J9 IAU SYMP PY 2004 VL 2004 IS 219 BP 587 EP 597 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFN67 UT WOS:000243338300072 ER PT B AU Yang, RQ Hill, CJ Wong, CM AF Yang, RQ Hill, CJ Wong, CM BE Buckley, DN Chang, PC Fox, PD Chan, WK Shiojima, K TI Recent progress in the development of antimonide-based mid-IR interband cascade lasers SO STATE-OF-THE-ART PROGRAM ON COMPOUND SEMICONDUCTORS XL (SOTAPOCS XL) AND NARROW BANDGAP OPTOELECTRONIC MATERIALS AND DEVICES II SE ELECTROCHEMICAL SOCIETY SERIES LA English DT Proceedings Paper CT 40th State-of-the-Art Program on Compound Semiconductors (SOTAPOCS XL)/2nd Narrow Bandgap Optoelectronic Materials and Devices Symposium CY MAY 09-14, 2004 CL San Antonio, TX SP Electrochem Soc, Electron Div ID DISTRIBUTED-FEEDBACK LASERS; HEAT-SINKING; OPERATION; TEMPERATURE AB Antimonide-based type-II interband cascade lasers are promising in becoming efficient and compact mid-infrared (3-5 mum) light sources for many applications such as gas sensing and environmental monitoring. Significant progress toward such a goal has recently been made in terms of achieving low threshold current densities (e.g. similar to9 A/cm(2) at 80 K), high temperature operation (e.g. 325 K in pulsed and 200 K in cw modes), and continuous wave operation of single-mode distributed feedback lasers. We review the recent progress of Sb-based mid-IR IC lasers and address the requirements for further improvements in their performance. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Yang, RQ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 25 TC 0 Z9 0 U1 0 U2 0 PU ELECTROCHEMICAL SOCIETY INC PI PENNINGTON PA 65 S MAIN ST, PENNINGTON, NJ 08534-2839 USA BN 1-56677-407-1 J9 ELEC SOC S PY 2004 VL 2004 IS 2 BP 179 EP 190 PG 12 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Optics; Physics, Condensed Matter SC Engineering; Materials Science; Optics; Physics GA BAH42 UT WOS:000222222800026 ER PT S AU Yunck, TP Hajj, GA AF Yunck, TP Hajj, GA BE Sparks, RSJ Hawkesworth, CJ TI Global navigation satellite sounding of the atmosphere and GNSS altimetry: Prospects for geosciences SO STATE OF THE PLANET: FRONTIERS AND CHALLENGES IN GEOPHYSICS SE Geophysical Monograph Book Series LA English DT Proceedings Paper CT 23rd General Assembly of the International-Union-of-Geodesy-and Geophysics CY JUL, 2003 CL Sapporo, JAPAN SP Int Union Geodesy & Geophys ID RADIO OCCULTATION MEASUREMENTS; GPS SIGNAL; POSITIONING SYSTEM; LOWER TROPOSPHERE; OCEAN ALTIMETRY; SCATTERING; SURFACE; INTERFEROMETRY; TEMPERATURE AB The vast illuminating power of the Global Positioning System (GPS), which transformed space geodesy in the 1990s, is now serving to probe the earth's fluid envelope in unique ways. Three distinct techniques have emerged: ground-based sensing of the integrated atmospheric moisture; space-based profiling of atmospheric refractivity, pressure, temperature, moisture, and other properties by active limb sounding; and surface (ocean and ice) altimetry and scatterometry with reflected signals detected from space. Ground-based GPS moisture sensing is already in provisional use for numerical weather prediction. Limb sounding, while less mature, offers a bevy of attractions, including high accuracy, stability, and vertical resolution; all-weather operation; and exceptionally low cost. GPS bistatic radar, or "reflectometry," is the least advanced but shows promise for a number of niche applications. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 126-347, Pasadena, CA 91109 USA. NR 57 TC 1 Z9 1 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0065-8448 BN 0-87590-415-7 J9 GEOPHYS MONOGR SER PY 2004 VL 150 BP 161 EP 176 DI 10.1029/150GM14 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA BBO48 UT WOS:000226692700013 ER PT S AU Fu, LL Rodriguez, E AF Fu, LL Rodriguez, E BE Sparks, RSJ Hawkesworth, CJ TI High-resolution measurement of ocean surface topography by radar interferometry for oceanographic and geophysical applications SO STATE OF THE PLANET: FRONTIERS AND CHALLENGES IN GEOPHYSICS SE Geophysical Monograph Book Series LA English DT Proceedings Paper CT 23rd General Assembly of the International-Union-of-Geodesy-and Geophysics CY JUL, 2003 CL Sapporo, JAPAN SP Int Union Geodesy & Geophys ID NORTH-ATLANTIC; TOPEX/POSEIDON; CIRCULATION; VARIABILITY; ACCURACIES; SATELLITE; ENERGY AB This paper describes a new approach to making altimeter measurements from off-nadir radar signal returns and its oceanographic and geophysical applications. The approach is based on the technique of radar interferomety and the new instrument is called the Wide-Swath Ocean Altimeter (WSOA). WSOA is designed to be flown with a Jason class conventional dual-frequency altimeter system, including a multi-frequency radiometer for the correction of the effects of water vapor in the troposphere. WSOA will extend the measurement from a line along the nadir to a swath of 200 kin centered on the nadir track. The most important application of WSOA is to provide the first synoptic maps of the global oceanic eddy field with a spatial resolution of 15 km x 15 km. The strong currents and water property anomalies (in temperature, salinity, oxygen, etc.) associated with ocean eddies are a major factor affecting the oceanic general circulation and the biogeochemical cycles of the ocean. WSOA will also provide measurements that allow the monitoring and study of coastal currents and tides that affect the lives of half of the world's population. The intrinsic resolution of WSOA in the look direction of the interferometric radar is about 1 km, allowing the estimation of sea surface slope with an accuracy of 1 micro radian down to a wavelength of 20 km for a 2-year mission (15 km for a 5-year mission). This capability will make contributions to the mapping of the details of the sea floor topography. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-323, Pasadena, CA 91109 USA. NR 31 TC 18 Z9 18 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0065-8448 BN 0-87590-415-7 J9 GEOPHYS MONOGR SER PY 2004 VL 150 BP 209 EP 224 DI 10.1029/150GM17 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA BBO48 UT WOS:000226692700016 ER PT S AU Venet, A AF Venet, A BE Giacobazzi, R TI A scalable nonuniform pointer analysis for embedded programs SO STATIC ANALYSIS, PROCEEDINGS SE LECTURE NOTES IN COMPUTER SCIENCE LA English DT Article; Proceedings Paper CT 11th International Static Analysis Symposium (SAS 2004) CY AUG 26-28, 2004 CL Vernona, ITALY AB In this paper we present a scalable pointer analysis for embedded applications that is able to distinguish between instances of recursively defined data structures and elements of arrays. The main contribution consists of an efficient yet precise algorithm that can handle multithreaded programs. We first perform an inexpensive flow-sensitive analysis of each function in the program that generates semantic equations describing the effect of the function on the memory graph. These equations bear numerical constraints that describe nonuniform points-to relationships. We then iteratively solve these equations in order to obtain an abstract storage graph that describes the shape of data structures at every point of the program for all possible thread interleavings. We bring experimental evidence that this approach is tractable and precise for real-size embedded applications. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Venet, A (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM arnaud@email.arc.nasa.gov NR 25 TC 6 Z9 6 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-22791-1 J9 LECT NOTES COMPUT SC PY 2004 VL 3148 BP 149 EP 164 PG 16 WC Computer Science, Theory & Methods SC Computer Science GA BAU83 UT WOS:000223655800013 ER PT S AU van Belle, GT Ciardi, DR Thompson, RR Akeson, RL AF van Belle, GT Ciardi, DR Thompson, RR Akeson, RL BE Maeder, A Eenens, P TI Direct observations of rotationally distorted stars SO STELLAR ROTATION SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 215th International-Astronomical-Union Symposium on Stellar Rotation CY NOV 11-15, 2002 CL Cancun, MEXICO SP Int Astron Union, Univ Guanajuato, UNAM, CLAFM ID ANGULAR SIZE MEASUREMENTS; A-TYPE STARS; EFFECTIVE TEMPERATURES; CONTINUUM EMISSION; STELLAR ATMOSPHERE; MIRA VARIABLES; LINE-PROFILES; VELOCITIES; OBLATENESS; DIAMETERS AB We present infrared interferometric angular size measurements for rapidly rotating stars which indicate non-circular projected disk brightness distributions. For the A7IV-V star Altair, assuming that the apparent oblateness of the photosphere is due to the star's rapid rotation, a rigorous evaluation of the observation data in the context of a rigidly rotating Roche model shows that. an estimate of v sin i = 210 +/- 13 km s(-1) can be derived that is independent of spectroscopic techniques. Altair is the first main sequence star for which direct. observations of an oblate photosphere have been reported: and the first star for which v sin i has been established from observations of the stars photospheric geometry. Future prospects for this technique are considered, and a prospective catalog of 67 rotationally oblate targets is presented. C1 CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP van Belle, GT (reprint author), CALTECH, Michelson Sci Ctr, 770 S Wilson Ave MS 100-22, Pasadena, CA 91125 USA. EM vdberg@merate.mi.astro.it NR 35 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-180-X J9 IAU SYMP PY 2004 IS 215 BP 177 EP 186 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBM41 UT WOS:000226161500045 ER PT S AU Heap, SR Lanz, T AF Heap, SR Lanz, T BE Maeder, A Eenens, P TI Effects of rotation in low-metallicity stars SO STELLAR ROTATION SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 215th International-Astronomical-Union Symposium on Stellar Rotation CY NOV 11-15, 2002 CL Cancun, MEXICO SP Int Astron Union, Univ Guanajuato, UNAM, CLAFM ID EVOLUTION; BLUE AB We have carried out a spectral analysis of 17 O-type stars in the Small Magellanic Cloud (SMC). We find several lines of evidence that rotation plays an important role in massive stars in this low-metallicity galaxy (Z = 0.2 Zcircle dot): (1) strong enrichment of nitrogen in half the program stars due to rotational mixing of processed material in the core up to the surface; (2) reduction of the effective gravity by the centrifugal force; (3) apparent anomalies in cluster isochrones that imply some stars are rotating at critical velocities. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, College Pk, MD 20742 USA. EM heap@srh.gsfc.nasa.gov NR 5 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-180-X J9 IAU SYMP PY 2004 IS 215 BP 220 EP 221 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBM41 UT WOS:000226161500052 ER PT S AU Borucki, W Koch, D Boss, A Dunham, E Dupree, A Geary, J Gilliland, R Howell, S Jenkins, J Kondo, Y Latham, D Lissauer, J Reitsema, H AF Borucki, W Koch, D Boss, A Dunham, E Dupree, A Geary, J Gilliland, R Howell, S Jenkins, J Kondo, Y Latham, D Lissauer, J Reitsema, H BE Favata, F Aigrain, S Wilson, A TI The Kepler mission: a technical overview SO STELLAR STRUCTURE AND HABITABLE PLANET FINDING SE ESA SPECIAL PUBLICATIONS LA English DT Proceedings Paper CT 2nd Eddington Workshop on Stellar Structure and Habitable Planet Finding CY APR 09-11, 2003 CL Palermo, ITALY SP European Space Agcy, INAF DE Kepler mission : Discovery-class mission to detect the transit of Earth-size and larger planets ID PLANETS AB The Kepler mission is a NASA Discovery-class mission designed to continuously monitor the brightness of 100 000 main sequence stars to detect the transits of Earth-size and larger planets. It is a wide field of view photometer with a Schmidt-type telescope and an array of 42 CCDs covering the 100 sq. deg. Field of View (FOV). It has a 0.95 m aperture and a 1.4 m primary and is designed to attain a photometric precision of 2 parts in 10(5) for V = 12 solar-like stars for a 6-hour transit duration. It will continuously observe 100000 stars from V = 9 to V = 15 in the Cygnus constellation for a period of four years with a cadence of 4 per hour. An additional 250 stars can be monitored at a cadence of once per minute to address asteroseismology of stars brighter than V = 11.5. The photometer is scheduled to be launched into heliocentric orbit in 2007. A ground-based program to classify all 450 000 stars to V = 15 in the FOV and to conduct a detailed examination of a subset of the stars that show planetary companions is also planned. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Borucki, W (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 3 TC 25 Z9 25 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-848-4 J9 ESA SP PUBL PY 2004 VL 538 BP 177 EP 182 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAD67 UT WOS:000221678200021 ER PT S AU Suess, ST Nerney, S AF Suess, ST Nerney, S BE VonSteiger, R Lui, ATY Newell, PT Troshhichev, OA TI Flow in streamer boundaries, and streamer stability SO STREAMERS, SLOW SOLAR WIND, AND THE DYNAMICS OF THE MAGNETOSPHERE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE solar wind; solar corona; streamers ID REGION; CORONA; MODEL; BETA AB Streamers can extend to many solar radii but the closed field regions, or helmets, reach no higher than 2-4 solar radii. The brightness boundary defining streamers is therefore, a boundary between different flow regimes rather than between static plasma and expanding solar wind. It is reasonable to assume that, this boundary divides fast coronal hole wind from slow wind. Flow inside this boundary can be studied using MHD models and is a type of stagnation flow. We describe such a model that is essentially analytic and show examples of flow solutions within the context and assumptions of the model. The flow affects the stability of the underlying helmet, which can be subject to a leakage out of the cusp that is similar to the small mass releases observed with the SOHO/LASCO coronagraph. It can also cause the helmet to be susceptible to being carried away in a coronal mass ejection. The model therefore, also offers a way to study streamer stability. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Ohio Univ, Lancaster, OH 43130 USA. RP Suess, ST (reprint author), NASA, George C Marshall Space Flight Ctr, Mail Stop SD50, Huntsville, AL 35812 USA. EM steve.suess@msfc.nasa.gov NR 16 TC 9 Z9 9 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 33 IS 5 BP 668 EP 675 DI 10.1016/S0273-1177(03)00237-0 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAD22 UT WOS:000221642000001 ER PT S AU Gopalswamy, N Shimojo, M Lu, W Yashiro, S Shibasaki, K Howard, RA AF Gopalswamy, N Shimojo, M Lu, W Yashiro, S Shibasaki, K Howard, RA BE VonSteiger, R Lui, ATY Newell, PT Troshhichev, OA TI On coronal streamer changes SO STREAMERS, SLOW SOLAR WIND, AND THE DYNAMICS OF THE MAGNETOSPHERE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE coronal mass ejections; coronal streamers; prominence eruptions; solar eruptions ID MASS EJECTION; PROMINENCE; EVOLUTION AB Coronal streamer represents one of the pre-eruption configurations of coronal mass ejections (CMEs), because they overlie prominences and often possess all the substructures of CMEs. In this paper, we report on a study of streamer changes associated with prominence eruptions. The prominence eruptions and streamer changes were observed by the Nobeyama radioheliograph and Solar and Heliospheric Observatory (SOHO), respectively. Multiwavelength data showed that at least one of the streamer events involved heating and small-scale material ejection that subsequently stalled. After presenting illustrative examples, we compare the properties of the streamer-related events with those of general population of prominence events. We find that the properties of streamer-related prominence events are closer to those of prominence eruptions with transverse trajectories. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. Catholic Univ Amer, Washington, DC 20064 USA. USN, Res Lab, Washington, DC 20064 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Mailcode 695-0,Bldg 21,Room 260, Greenbelt, MD 20771 USA. EM gopals@fugee.gsfc.nasa.gov RI Gopalswamy, Nat/D-3659-2012; OI Shimojo, Masumi/0000-0002-2350-3749 NR 10 TC 6 Z9 6 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 33 IS 5 BP 676 EP 680 DI 10.1016/S0273-1177(03)00236-9 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAD22 UT WOS:000221642000002 ER PT S AU Ofman, L AF Ofman, L BE VonSteiger, R Lui, ATY Newell, PT Troshhichev, OA TI The origin of the slow solar wind in coronal streamers SO STREAMERS, SLOW SOLAR WIND, AND THE DYNAMICS OF THE MAGNETOSPHERE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE sun; corona; solar wind; MHD; multi-fluid equations; satellite observations ID MHD MODEL; MAGNETOHYDRODYNAMIC MODEL; HELMET STREAMERS; ACCELERATION; HOLES; SPECTROMETER; SIMULATION; VELOCITIES; SPEEDS; BELT AB The highly variable slow solar wind has been associated with low-latitude regions of the heliosphere most clearly by the Ulysses spacecraft. Although, it is evident today that the slow solar wind originates in coronal helmet streamers, the mechanism of the slow solar wind acceleration, and the origin of the variability are still being debated. The combination of new observations and numerical modeling are beginning to address these questions. I will discuss how recent in-situ observations by Ulysses, white light and EUV observations by the LASCO and UVCS instruments on SOHO advanced our understanding of the streamer structure, dynamics, and stability. I will briefly review the current state of numerical MHD modeling of streamers, and the possible mechanisms that may produce the highly variable slow wind. I will present the results of recent heat-conductive MHD modeling of multiple streamer slow solar wind with heating function constrained by observations. I will show how multi-fluid numerical modeling of the slow solar wind in streamers helps to identify the regions of the slow solar wind outflow. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ofman, L (reprint author), Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Mail Code 682, Greenbelt, MD 20771 USA. EM ofman@waves.gsfc.nasa.gov NR 39 TC 16 Z9 16 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 33 IS 5 BP 681 EP 688 DI 10.1016/S0273-1177(03)00235-7 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAD22 UT WOS:000221642000003 ER PT J AU Venter, G Sobieszczanski-Sobieski, J AF Venter, G Sobieszczanski-Sobieski, J TI Multidisciplinary optimization of a transport aircraft wing using particle swarm optimization SO STRUCTURAL AND MULTIDISCIPLINARY OPTIMIZATION LA English DT Article; Proceedings Paper CT AIAA/ISSMO 9th Symposium on Multidisciplinary Analysis and Optimization CY SEP 04-06, 2002 CL ATLANTA, GA SP Amer Inst Aeronaut & Astronaut, ISSMO DE particle swarm optimization; discrete optimization; multidisciplinary optimization; numerical noise; aircraft wing design AB The purpose of this paper is to demonstrate the application of particle swarm optimization to a realistic multidisciplinary optimization test problem. The paper's new contributions to multidisciplinary optimization are the application of a new algorithm for dealing with the unique challenges associated with multidisciplinary optimization problems, and recommendations for the utilization of the algorithm in future multidisciplinary optimization applications. The selected example is a bi-level optimization problem that demonstrates severe numerical noise and has a combination of continuous and discrete design variables. The use of traditional gradient-based optimization algorithms is thus not practical. The numerical results presented indicate that the particle swarm optimization algorithm is able to reliably find the optimum design for the problem presented. The algorithm is capable of dealing with the unique challenges posed by multidisciplinary optimization, as well as the numerical noise and discrete variables present in the current example problem. C1 Vanderplaats Res & Dev Inc, Colorado Springs, CO 80906 USA. NASA, Langley Res Ctr, Analyt & Computat Methods Branch, Hampton, VA 23681 USA. RP Vanderplaats Res & Dev Inc, 1797 S 8th St,Suite 200, Colorado Springs, CO 80906 USA. EM gventer@vrand.com; j.sobieski@larc.nasa.gov OI Venter, Gerhard/0000-0001-9513-9774 NR 13 TC 98 Z9 107 U1 5 U2 23 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1615-147X EI 1615-1488 J9 STRUCT MULTIDISCIP O JI Struct. Multidiscip. Optim. PD JAN PY 2004 VL 26 IS 1-2 BP 121 EP 131 DI 10.1007/s00158-003-0318-3 PG 11 WC Computer Science, Interdisciplinary Applications; Engineering, Multidisciplinary; Mechanics SC Computer Science; Engineering; Mechanics GA 774RG UT WOS:000188997800011 ER PT B AU Telesman, J Kantzos, P Gayda, J Bonacuse, PJ Prescenzi, A AF Telesman, J Kantzos, P Gayda, J Bonacuse, PJ Prescenzi, A BE Green, KA Pollock, TM Harada, H Howson, TE Reed, RC Schirra, JJ Walston, S TI Microstructural variables controlling time-dependent crack growth in a P/M superalloy SO Superalloys 2004 LA English DT Proceedings Paper CT 10th International Symposium on Superalloys CY SEP 19-23, 2004 CL Champion, PA SP TMS Seven Springs Int Symp Comm, TMS High Temp Alloys Comm, ASM Int DE hold time crack growth; microstructure; P/M superalloys ID BEHAVIOR; FATIGUE; CREEP AB A study was performed to determine the variables which influence hold time crack growth resistance of Alloy 10, a new powder metallurgy (P/M) superalloy. In a well controlled study, both the effect of compositional changes and variation in heat treatments were investigated. The results indicate that significant changes in the alloy's niobium, tantalum and cobalt content did not have an appreciable effect on hold time crack growth resistance. In contrast to the composition study, the heat treatments evaluated produced up to an order of magnitude changes in the crack growth resistance. Quantitative image analysis was performed to analyze the microstructural features produced by each heat treatment. It was found that the cooling gamma' precipitate size distribution is closely related to the measured hold time crack growth behavior. The larger the mean size of the cooling precipitates, the better is the resistance to hold time crack growth. It is proposed that the size and distribution of the precipitates might play an important role in determining the extent of crack tip relaxation which occurs through creep-type processes. The differences in the stress relaxation rate influence the crack driving forces and thus crack growth resistance. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Telesman, J (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 8 TC 25 Z9 26 U1 0 U2 0 PU MINERALS, METALS & MATERIALS SOC PI WARRENDALE PA 184 THORN HILL RD, WARRENDALE, PA 15086-7514 USA BN 0-87339-576-X PY 2004 BP 215 EP 224 PG 10 WC Metallurgy & Metallurgical Engineering; Materials Science, Characterization & Testing SC Metallurgy & Metallurgical Engineering; Materials Science GA BBX42 UT WOS:000228231000024 ER PT B AU Gabb, TP Telesman, J Kantzos, PT Smith, JW Browning, PF AF Gabb, TP Telesman, J Kantzos, PT Smith, JW Browning, PF BE Green, KA Pollock, TM Harada, H Howson, TE Reed, RC Schirra, JJ Walston, S TI Effects of high temperature exposures on fatigue life of disk superalloys SO Superalloys 2004 LA English DT Proceedings Paper CT 10th International Symposium on Superalloys CY SEP 19-23, 2004 CL Champion, PA SP TMS Seven Springs Int Symp Comm, TMS High Temp Alloys Comm, ASM Int DE disk; superalloys; low cycle fatigue; environment ID LOW-CYCLE FATIGUE AB The effects on fatigue life of high temperature exposures simulating service conditions were considered for two disk superalloys. Powder metallurgy processed, supersolvus heat treated Udimet (R) 720 and ME3 fatigue specimens were exposed in air at temperatures of 650 to 704 degrees C, for times of 100 h to over 1000 h. They were then tested using conventional fatigue tests at 650 and 704 degrees C, to determine the effects of exposure on fatigue resistance. Cyclic dwell verification tests were also performed to contrast the effects of intermixed exposures and fatigue cycles. The prior exposures reduced life by up to 70% and increased the scatter in life, compared to unexposed levels. Cyclic dwell tests reduced lives even more. Fractographic evaluations indicated the failure mode was shifted by the exposures and cyclic dwells from predominantly internal to often surface crack initiations. The increased scatter in life was related to the competition between internal crack initiations at inclusions or large grains producing longer lives, and surface crack initiations at an environmentally affected surface layer producing shorter lives. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Gabb, TP (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. NR 12 TC 15 Z9 17 U1 0 U2 1 PU MINERALS, METALS & MATERIALS SOC PI WARRENDALE PA 184 THORN HILL RD, WARRENDALE, PA 15086-7514 USA BN 0-87339-576-X PY 2004 BP 269 EP 274 PG 6 WC Metallurgy & Metallurgical Engineering; Materials Science, Characterization & Testing SC Metallurgy & Metallurgical Engineering; Materials Science GA BBX42 UT WOS:000228231000030 ER PT B AU Gayda, J Gabb, TP Kantzos, PT AF Gayda, J Gabb, TP Kantzos, PT BE Green, KA Pollock, TM Harada, H Howson, TE Reed, RC Schirra, JJ Walston, S TI The effect of dual microstructure heat treatment on an advanced nickel-base disk alloy SO Superalloys 2004 LA English DT Proceedings Paper CT 10th International Symposium on Superalloys CY SEP 19-23, 2004 CL Champion, PA SP TMS Seven Springs Int Symp Comm, TMS High Temp Alloys Comm, ASM Int DE nickel-base superalloy; disk; heat treatment AB Five heat treat options for an advanced nickel-base disk alloy, LSHR, have been investigated. These included two conventional solution heat treat cycles, subsolvus/oil quench and supersolvus/fan cool, which yield fine grain and coarse grain microstructure disks respectively, as well as three advanced dual microstructure heat treat (DMHT) options. The DMHT options produce disks with a fine grain bore and a coarse grain rim. Based on an overall evaluation of the mechanical property data, it was evident that the three DMHT options achieved a desirable balance of properties in comparison to the conventional solution heat treatments for the LSHR alloy. However, one of the DMHT option, SUB/DMHT, produced the best set of proper-ties, largely based on dwell crack growth data. Further evaluation of the SUB/DMHT option in spin pit experiments on a generic disk shape demonstrated the advantages and reliability of a dual grain structure at the component level. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Gayda, J (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 11 TC 20 Z9 23 U1 1 U2 4 PU MINERALS, METALS & MATERIALS SOC PI WARRENDALE PA 184 THORN HILL RD, WARRENDALE, PA 15086-7514 USA BN 0-87339-576-X PY 2004 BP 323 EP 329 PG 7 WC Metallurgy & Metallurgical Engineering; Materials Science, Characterization & Testing SC Metallurgy & Metallurgical Engineering; Materials Science GA BBX42 UT WOS:000228231000037 ER PT B AU Nathal, MV Whittenberger, JD Hebsur, MG Kantzos, PT Krause, DL AF Nathal, MV Whittenberger, JD Hebsur, MG Kantzos, PT Krause, DL BE Green, KA Pollock, TM Harada, H Howson, TE Reed, RC Schirra, JJ Walston, S TI Superalloy lattice block structures SO Superalloys 2004 LA English DT Proceedings Paper CT 10th International Symposium on Superalloys CY SEP 19-23, 2004 CL Champion, PA SP TMS Seven Springs Int Symp Comm, TMS High Temp Alloys Comm, ASM Int DE lattice block; truss structures; honey comb; casting; superalloy ID BEHAVIOR AB Initial investigations of investment cast superalloy lattice block suggest that this technology will yield a low cost approach to utilize the high temperature strength and environmental resistance of superalloys in lightweight, damage tolerant structural configurations. Work to date has demonstrated that relatively large superalloy lattice block panels can be successfully investment cast from both IN-718 and Mar-M247. These castings exhibited mechanical properties consistent with the strength of the same superalloys measured from more conventional castings. The lattice block structure also accommodates significant deformation without failure, and is defect tolerant in fatigue. The potential of lattice block structures opens new opportunities for the use of superalloys in future generations of aircraft applications that demand strength and environmental resistance at elevated temperatures along with low weight. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Nathal, MV (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 14 TC 5 Z9 5 U1 0 U2 1 PU MINERALS, METALS & MATERIALS SOC PI WARRENDALE PA 184 THORN HILL RD, WARRENDALE, PA 15086-7514 USA BN 0-87339-576-X PY 2004 BP 431 EP 439 PG 9 WC Metallurgy & Metallurgical Engineering; Materials Science, Characterization & Testing SC Metallurgy & Metallurgical Engineering; Materials Science GA BBX42 UT WOS:000228231000048 ER PT J AU Tangborn, A AF Tangborn, A TI Wavelet approximation of error covariance propagation in data assimilation SO TELLUS SERIES A-DYNAMIC METEOROLOGY AND OCEANOGRAPHY LA English DT Article ID SUBSPACE STATISTICAL ESTIMATION; SEQUENTIAL DATA ASSIMILATION; KALMAN FILTER; SUPPORTED WAVELETS; DYNAMICS; SCHEMES; SYSTEM AB Estimation of the state of the atmosphere with the Kalman filter remains a distant goal in part because of high computational cost of evolving the error covariance for both linear and non-linear systems (in this case, the extended Kalman filter). Wavelet approximation is presented here as a possible solution that efficiently compresses both global and local covariance information. We demonstrate the compression characteristics by implementing a wavelet approximation scheme on the assimilation of the one-dimensional Burgers' equation. The discrete linearized equations (tangent linear model) and analysis covariance are projected onto a wavelet basis and truncated to just 6% of the coefficients. A nearly optimal forecast is achieved and we show that errors due to truncation of the dynamics are no greater than the errors due to covariance truncation. C1 NASA, Goddard Space Flight Ctr, Data Assimilat Off, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, JCET, Baltimore, MD 21228 USA. RP Tangborn, A (reprint author), NASA, Goddard Space Flight Ctr, Data Assimilat Off, Code 910-3, Greenbelt, MD 20771 USA. EM tangborn@dao.gsfc.nasa.gov NR 27 TC 8 Z9 8 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0280-6495 J9 TELLUS A JI Tellus Ser. A-Dyn. Meteorol. Oceanol. PD JAN PY 2004 VL 56 IS 1 BP 16 EP 28 DI 10.1111/j.1600-0870.2004.00034.x PG 13 WC Meteorology & Atmospheric Sciences; Oceanography SC Meteorology & Atmospheric Sciences; Oceanography GA 773RV UT WOS:000188937300002 ER PT S AU Brown, LR Naumenko, OV Polovtseva, ER Sinitsa, LN AF Brown, LR Naumenko, OV Polovtseva, ER Sinitsa, LN BE Matvienko, GG Krekov, GM TI Absorption spectrum of H2S between 7200 and 7890 cm(-1) SO TENTH JOINT INTERNATIONAL SYMPOSIUM ON ATMOSPHERIC AND OCEAN OPTICS/ATMOSPHERIC PHYSICS, PT 1: RADIATION PROPAGATION IN THE ATMOSPHERE AND OCEAN SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT 10th Joint International Symposium on Atmospheric and Ocean Optics/Atmospheric Physics CY JUN 24-28, 2003 CL Tomsk, RUSSIA SP Inst Atmospher Opt, Inst Solar-Terrestrial Phys, Russian Acad Sci, Siberian Branch, SPIE Russia Chapter, Opt Soc Amer, SPIE DE high resolution spectra; effective Hamiltonians; spectra assignment and modeling ID INFRARED-SPECTRUM; (H2S)-S-32 AB The high resolution absorption spectra of H2S have been recorded in the region 7200 - 7890 cm(-1) with the McMath Fourier transform spectrometer located at Kitt Peak National Observatory. A careful analysis of the spectra led to derivation of 1080 precise energy levels for the 1st decade interacting states of (H2S)-S-32, (H2S)-S-32, and (H2S)-S-34 isotope species. The energy levels were introduced into a least squares fit using a Hamiltonian which takes into account Coriolis, Darling-Dennison and Fermi-resonance interactions. Precise rotational and coupling parameters have been determined which reproduce the experimental energy levels within 0.0015 cm(-1) for the main isotope species. The experimental band origin E-v = 7419.9162 cm(-1) for the super weak (220)-(000) band was obtained for the first time from the simultaneous analysis of cold (220)-(000) and hot (220)-(010) bands. Detailed and accurate H,S absorption line list was generated in the HITRAN format for the first decade spectral region. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Brown, LR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. NR 9 TC 4 Z9 5 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5315-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5396 BP 42 EP 48 DI 10.1117/12.548211 PG 7 WC Instruments & Instrumentation; Meteorology & Atmospheric Sciences; Oceanography; Optics SC Instruments & Instrumentation; Meteorology & Atmospheric Sciences; Oceanography; Optics GA BY79P UT WOS:000189465000006 ER PT S AU Siegel, PH Dengler, RJ AF Siegel, PH Dengler, RJ BE Hwu, RJ TI Terahertz heterodyne imager for biomedical applications SO TERAHERTZ AND GIGAHERTZ ELECTRONICS AND PHOTONICS III SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Terahertz and Gigahertz Electronics and Photonics III CY JAN 25-26, 2004 CL San Jose, CA SP SPIE ID GAAS C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Siegel, PH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NR 15 TC 11 Z9 11 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5262-9 J9 P SOC PHOTO-OPT INS PY 2004 VL 5354 BP 1 EP 9 DI 10.1117/12.540027 PG 9 WC Optics; Physics, Applied SC Optics; Physics GA BAE26 UT WOS:000221795200001 ER PT S AU Pike, L Maddalon, J Miner, P Geser, A AF Pike, L Maddalon, J Miner, P Geser, A BE Slind, K Bunker, A Gopalakrishnan, G TI Abstractions for fault-tolerant distributed system verification SO THEOREM PROVING IN HIGHER ORDER LOGICS, PROCEEDINGS SE LECTURE NOTES IN COMPUTER SCIENCE LA English DT Article; Proceedings Paper CT 17th International Conference on Theorem Proving in Higher Order Logics CY SEP 14-17, 2004 CL Pk City, UT SP INTEL, Natl Sci Fdn ID FORMAL VERIFICATION AB Four kinds of abstraction for the design and analysis of fault-tolerant distributed systems are discussed. These abstractions concern system messages, faults, fault-masking voting, and communication. The abstractions are formalized in higher-order logic, and are intended to facilitate specifying and verifying such systems in higher-order theorem-provers. C1 NASA, Langley Res Ctr, Formal Methods Grp, Hampton, VA 23681 USA. Natl Inst Aerosp, Hampton, VA 23666 USA. RP Pike, L (reprint author), NASA, Langley Res Ctr, Formal Methods Grp, M-S 130, Hampton, VA 23681 USA. EM lee.s.pike@nasa.gov; j.m.maddalon@nasa.gov; paul.s.miner@nasa.gov; geser@nianet.org NR 26 TC 9 Z9 9 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-23017-3 J9 LECT NOTES COMPUT SC PY 2004 VL 3223 BP 257 EP 270 PG 14 WC Computer Science, Theory & Methods SC Computer Science GA BAX12 UT WOS:000224025900019 ER PT S AU Snyder, GJ Caillat, T AF Snyder, GJ Caillat, T BE Nolas, GS Yang, J Hogan, TP Johnson, DC TI Using the compatibility factor to design high efficiency segmented thermoelectric generators SO THERMOELECTRIC MATERIALS 2003-RESEARCH AND APPLICATIONS SE MATERIALS RESEARCH SOCIETY SYMPOSIUM PROCEEDINGS LA English DT Proceedings Paper CT Symposium on Thermoelectric Materials held at the 2003 MRS Fall Meeting CY DEC 01-03, 2003 CL Boston, MA SP Mat Res Soc AB Using thermoelectric compatibility, efficient thermoelectric generators are rationally designed. With examples, compatible and incompatible systems are explained and materials proposed for targeted development. The compatibility factor explains why segmentation of TAGS with SnTe or PbTe produces little extra power, while filled skutterudite increases the efficiency from 10.5% to 13.6%. High efficiency generators are designed with compatible n-type La2Te3, and similar p-type material, while incompatible SiGe alloys actually reduce the efficiency. A refractory metal with high p-type thermopower (>100 V/K) is required for development. The Chevrel compound Cu4Mo6Se8 is a compatible p-type metal that provides a modest increase in efficiency. A fully segmented generator using Bi2Te3-type, PbTe, TAGS, Zn4Sb3, skutterudite, La2Te3, and Chevrel compounds between 25 degreesC and 1000 degreesC will achieve 18.1% conversion efficiency. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Snyder, GJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 277-207, Pasadena, CA 91109 USA. RI Snyder, G. Jeffrey/E-4453-2011; Snyder, G/I-2263-2015 OI Snyder, G. Jeffrey/0000-0003-1414-8682; NR 10 TC 8 Z9 8 U1 1 U2 10 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 USA SN 0272-9172 BN 1-55899-731-8 J9 MATER RES SOC SYMP P PY 2004 VL 793 BP 37 EP 42 PG 6 WC Instruments & Instrumentation; Materials Science, Multidisciplinary; Materials Science, Characterization & Testing; Materials Science, Composites SC Instruments & Instrumentation; Materials Science GA BY84H UT WOS:000189476400005 ER PT S AU Huang, CK Herman, JA Myung, N Lim, JR Fleurial, JP AF Huang, CK Herman, JA Myung, N Lim, JR Fleurial, JP BE Nolas, GS Yang, J Hogan, TP Johnson, DC TI Investigation of the properties of electrochemically deposited semiconductor materials for thermoelectric applications SO THERMOELECTRIC MATERIALS 2003-RESEARCH AND APPLICATIONS SE MATERIALS RESEARCH SOCIETY SYMPOSIUM PROCEEDINGS LA English DT Proceedings Paper CT Symposium on Thermoelectric Materials held at the 2003 MRS Fall Meeting CY DEC 01-03, 2003 CL Boston, MA SP Mat Res Soc AB At JPL, it is our desire to fabricate thermoelectric micro-devices for power generation and cooling applications using an electrochemical deposition (ECD) technique. We believe that the performance of our current micro-device developed is limited by the properties of the ECD materials. Therefore, the objective of this study is to develop ECD methods, for obtaining n-type Bi2Te3 and p-type Bi2-xSbxTe3 thermoelectric materials with near bulk properties, as well as optimizing morphology and transport properties. The films of Bi2Te3 and Bi2-xSbxTe3 were initially obtained under various ECD conditions. Seebeck coefficients and transport properties were then measured along the direction parallel to the substrates before and after annealing at 250 degreesC for 2 hrs. From the data obtained, ECD n-Bi2Te3 material can achieve a high Seebeck coefficient (-189 muV/K) when it is deposited at -200 mV vs. SCE. The in-plane resistivity, in-plane mobility, and carrier concentration are 3.0 mohm-cm, 31 cm(2) V-1S-1, and 6.79 x 10(19) cm(-3), respectively. As for the p-type Bi2-xSbxTe3, it is possible to achieve a high Seebeck coefficient (+295 muV/K) when it is deposited at 0.3 mA/cm(2). The in-plane resistivity, in-plane mobility, and carrier concentration are 9.8374 mohm-cm, 66.58 cm(2)V(-1)S(-1), and 9.54 x 10(18) cm(-3), respectively. From the results of our preliminary study, we have found the conditions for depositing high quality Bi2Te3 and Bi2-xSbxTe3 materials with thermoelectric properties comparable to those of their state-of-the-art bulk samples. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Huang, CK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 7 TC 2 Z9 2 U1 0 U2 0 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DRIVE, WARRENDALE, PA 15088-7563 USA SN 0272-9172 BN 1-55899-731-8 J9 MATER RES SOC SYMP P PY 2004 VL 793 BP 311 EP 316 PG 6 WC Instruments & Instrumentation; Materials Science, Multidisciplinary; Materials Science, Characterization & Testing; Materials Science, Composites SC Instruments & Instrumentation; Materials Science GA BY84H UT WOS:000189476400044 ER PT S AU Wilt, DM Wehrer, RJ Maurer, WF Jenkins, PP Wernsman, B Schultz, RW AF Wilt, DM Wehrer, RJ Maurer, WF Jenkins, PP Wernsman, B Schultz, RW BE Gopinath, A Coutts, TJ Luther, J TI Buffer layer effects on tandem InGaAs TPV devices SO THERMOPHOTOVOLTAIC GENERATION OF ELECTRICITY SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 6th International Conference on Thermophotovoltaic Generation of Electricity CY JUN 14-16, 2004 CL Freiburg, GERMANY SP Naval Sea Syst Command, NASA Glenn Res Ctr, USN Off Naval Res Int Field Off, UK, Natl Renewable Energy Lab, Fraunhofer Inst Solar Energy Syst ISE, Aixtron AG, Akzo Nobel, Wafer Technol Ltd, Epichem Grp AB Tandem thermophotovoltaic (TPV) cells have the potential to demonstrate efficiencies exceeding those of single junction devices. Fabricating TPV tandem devices utilizing indium gallium arsenide (InGaAs) for all of the component cells in a two cell tandem necessitates the inclusion of an optically transparent buffer structure in-between the high bandgap device (In0.53Ga0.47As - 0.74eV) and the low bandgap device (In0.66Ga0.34As - 0.63eV) to accommodate the similar to1% lattice strain generated due to the change in InGaAs composition. The impact of the buffer structure on the underlying lattice-matched InGaAs device has been examined by producing 0.74eV InGaAs devices both with and without buffer layers grown on top of them. All structures were characterized by reciprocal space x-ray diffraction to determine epilayer composition and residual strain. Electrical characterization of the devices was performed to examine the effect of the buffer on the device performance. The electrical impact of the buffer structure depends upon where it is positioned. When near the emitter region, a 260% increase in dark current was measured, whereas no change in dark current was observed when it was near the base region. C1 NASA, Glenn Res Ctr, Cleveland, OH USA. RP Wilt, DM (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. NR 8 TC 3 Z9 3 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0222-1 J9 AIP CONF PROC PY 2004 VL 738 BP 453 EP 461 PG 9 WC Engineering, Electrical & Electronic; Physics, Applied; Physics, Condensed Matter SC Engineering; Physics GA BBM16 UT WOS:000226110600051 ER PT S AU Zalameda, JN Winfree, WP AF Zalameda, JN Winfree, WP BE Burleigh, DD Cramer, KE Peacock, GR TI Improved sampling of thermal transients using focal plane array infrared imagers SO THERMOSENSE XXVI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Thermosense XXVI CY APR 13-15, 2004 CL Orlando, FL SP SPIE DE thermal nondestructive evaluation; defect contrast; corrosion detection and thermal diffusivity AB Quantitative thermal diffusivity and thickness images can be obtained by minimizing the squared difference between the data and a thermal model. This requires the transient portion of the thermal response to be adequately sampled. For fixed infrared camera frame rates (typically 60 hertz) this may be difficult for very fast thermal transients. The focus of this effort is to investigate a technique where the application of the flash heat is controlled by a variable delay. By cycling the flash heating and implementing a linearly increasing delay, thermal transients faster than the frame rate of the thermal camera can be successfully sampled. Detection of subsurface defects with improved defect contrast and spatial resolution on samples with fabricated defects is presented. C1 USA, NASA, Langley Res Ctr,Vehicle Technol Directorate, Nondestruct Evaluat Sci Branch, Hampton, VA 23681 USA. RP Zalameda, JN (reprint author), USA, NASA, Langley Res Ctr,Vehicle Technol Directorate, Nondestruct Evaluat Sci Branch, MS 231, Hampton, VA 23681 USA. NR 5 TC 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5328-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5405 BP 374 EP 381 DI 10.1117/12.547453 PG 8 WC Optics; Imaging Science & Photographic Technology SC Optics; Imaging Science & Photographic Technology GA BAL28 UT WOS:000222663600043 ER PT S AU Gyekenyesi, AL Morscher, GN AF Gyekenyesi, AL Morscher, GN BE Burleigh, DD Cramer, KE Peacock, GR TI Evaluating the mechanical behavior of notched SiC/SiC composites using thermoelastic stress analysis SO THERMOSENSE XXVI SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Thermosense XXVI CY APR 13-15, 2004 CL Orlando, FL SP SPIE DE Thermoelastic Stress Analysis; TSA; SPATE; Ceramic matrix composites; mechanical behavior; notch sensitivity; stress concentration factor ID CERAMIC-MATRIX COMPOSITES; SENSITIVITY AB Ceramic matrix composites (CMCs) are potential materials for high temperature applications in gas turbines. Currently, the main areas of consideration include combustor liners and turbine vanes. Because these components contain stress concentrations, it is imperative that candidate materials be fully assessed concerning behavior related to stress risers. In this study, the stress fields adjacent to machined notch roots were examined for woven SiC fiber reinforced, melt infiltrated SiC matrix composites with a BN interphase, utilizing either Hi-Nicalon(TM) fibers or the stiffer Sylramic(R) fibers. The double-edge notched tensile test approach was used for multiple notch sizes. In addition, the materials ability to diffuse stress concentrations by inelastic damage mechanisms was considered. The damage was induced by applying predetermined tensile stresses known to cause matrix cracking. The thermoelastic stress analysis technique (TSA, also recognized as SPATE: Stress Pattern Analysis by Thermal Emission) was utilized to define the stress profile on the specimen surface. TSA is based on the fact that materials experience small temperature changes when compressed or expanded. When subjecting a structure to a cyclic load, a related cyclic temperature profile results. The surface temperature profile, measured with an infrared camera, is directly related to the surface stresses on the structure. The amplitude of the TSA signal is defined to be linearly dependent on the cyclic stress amplitude. Here, results were provided concerning the stress concentration behavior as a function of notch length, damage level, as well as the mean stress during TSA measurements. C1 NASA, Glenn Res Ctr, OAI, Cleveland, OH 44135 USA. RP Gyekenyesi, AL (reprint author), NASA, Glenn Res Ctr, OAI, 21000 Brookpk Rd MS 6-1, Cleveland, OH 44135 USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5328-5 J9 P SOC PHOTO-OPT INS PY 2004 VL 5405 BP 456 EP 465 DI 10.1117/12.544544 PG 10 WC Optics; Imaging Science & Photographic Technology SC Optics; Imaging Science & Photographic Technology GA BAL28 UT WOS:000222663600052 ER PT B AU Reeves, J Watson, D Osborne, J O'Brien, P Pounds, K AF Reeves, J Watson, D Osborne, J O'Brien, P Pounds, K BE Feroci, M Frontera, F Masetti, N Piro, L TI XMM-Newton observations of GRB afterglows SO THIRD ROME WORKSHOP ON GAMMA-RAY BURSTS IN THE AFTERGLOW ERA SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 3rd Workshop on Gamma-Ray Bursts CY SEP 17-20, 2002 CL CNR, Rome, ITALY HO CNR ID GAMMA-RAY BURSTS AB The properties of all 4 GRB X-ray afterglows, observed to date with XMM-Newton, are presented. GRB 011211, GRB010220 and GRB 001025A all appear to show X-ray line emission features, whilst a fourth, GRB 020322, shows soft X-ray absorption. The line emission from GRB 011211, observed at 11 hours after the initial burst, appears to decay with time, the rest-energies of the lines indicate an outflow of similar to 0.1 c, implying a moderate (days/weeks) time delay between any supernova event and the burst itself. The X-ray spectrum of GRB01025A exhibits a soft excess, which may also be attributable to a blend of emission lines. Overall the observations are supportive of stellar collapse models for GRBs, implying that long GRBs occur in a rich, high density environment. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Reeves, J (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. EM jnr@star.le.ac.uk NR 12 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-165-6 J9 ASTR SOC P PY 2004 VL 312 BP 181 EP 184 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAM85 UT WOS:000222873300039 ER PT B AU Kazanas, D Contopoulos, J AF Kazanas, D Contopoulos, J BE Feroci, M Frontera, F Masetti, N Piro, L TI The MHD origin of GRBs: A new view at the GRB proper - Afterglow correlations SO THIRD ROME WORKSHOP ON GAMMA-RAY BURSTS IN THE AFTERGLOW ERA SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 3rd Workshop on Gamma-Ray Bursts CY SEP 17-20, 2002 CL CNR, Rome, ITALY HO CNR ID GAMMA-RAY BURSTS; DISCOVERY AB Based on the exact solution of the axisymmetric dipole magnetosphere and its asymptotic split-monopole configuration we propose a model for the GRB central engine along the lines suggested sometime ago by Usov, namely a highly magnetized (B similar to 10(15) G), rapidly spinning (P similar to 1 msec) neutron star. As discussed by us (Contopoulos & Kazanas 2002), the asymptotic solution of a spinning axisymmetric dipole leads to a quasispherical MHD wind which gradually converts its Poynting flux to relativistic motion, with its Lorentz factor Gamma proportional to the wind radius R. The acceleration saturates at a value Gamma(0) at radius R-0, when its inertial energy density becomes comparable to that of the magnetic field. Further increase in the Lorentz factor is averted by a change in the wind geometry which collimates away from its initial conical shape. We propose that the ensuing development of this wind through the ISM constitutes the GRB and its afterglow. We speculate that the variety of GRB properties depends, mainly, on the magnitude of the cross section pi R-0(2) of the collimated winds, with the broader ones having the larger Lorentz factors Gamma(0). Since larger Gamma(0) leads to a brighter GRB, while larger pi R-0(2) to a shorter afterglow break time, the correlations between the properties of the GRB proper and their afterglows are qualitatively obtained. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kazanas, D (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-165-6 J9 ASTR SOC P PY 2004 VL 312 BP 369 EP 372 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAM85 UT WOS:000222873300076 ER PT B AU Kazanas, D Georganopoulos, M Mastichiadis, A AF Kazanas, D Georganopoulos, M Mastichiadis, A BE Feroci, M Frontera, F Masetti, N Piro, L TI The "supercritical pile" model for GRBs: Tapping the proton energy and getting the F-v(v) peak at 1 MeV SO THIRD ROME WORKSHOP ON GAMMA-RAY BURSTS IN THE AFTERGLOW ERA SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 3rd Workshop on Gamma-Ray Bursts CY SEP 17-20, 2002 CL CNR, Rome, ITALY HO CNR ID BATSE; EMISSION; BLAZARS; ORIGIN AB We propose a process by which the kinetic energy of the protons, that carry most of the energy of GRB relativistic blast waves (RBW), is converted explosively into relativistic electrons of the same Lorentz factor, which subsequently produce the observed prompt gamma-ray emission of the burst. This conversion is the result of the combined effects of the reflection of photons produced within the flow by upstream located matter, their re-interception and conversion into E(+)e(-)-pairs on the RBW by the pgamma --> pe(+) e(-) reaction. This process depends on kinematic and dynamic thresholds; the former depends on the RBW Lorentz factor Gamma while the second on the column density of the post shock matter to the pgamma --> e(+) e(-) reaction; this latter condition is in effect that of the criticality of a nuclear pile, hence the terminology. It is shown that, when operating near threshold, the resulting GRB spectrum produces its peak luminosity at energy (in the lab frame) E similar or equal to m(e)c(2), thereby providing an answer to this outstanding question of GRBs. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kazanas, D (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-165-6 J9 ASTR SOC P PY 2004 VL 312 BP 437 EP 440 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAM85 UT WOS:000222873300092 ER PT B AU Gehrels, N AF Gehrels, N BE Feroci, M Frontera, F Masetti, N Piro, L TI The swift GRB MIDEX mission SO THIRD ROME WORKSHOP ON GAMMA-RAY BURSTS IN THE AFTERGLOW ERA SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 3rd Workshop on Gamma-Ray Bursts CY SEP 17-20, 2002 CL CNR, Rome, ITALY HO CNR ID GAMMA-RAY BURSTS; 28 FEBRUARY 1997; OPTICAL-EMISSION; AFTERGLOW; REDSHIFT AB Swift is a first-of-its-kind multiwavelength transient observatory for gamma-ray burst astronomy. It has the optimum capabilities for the next breakthroughs in determining the origin of gamma-ray bursts and their afterglows, as well as using bursts to probe the early Universe. Swift will also perform the first sensitive hard X-ray survey of the sky. The mission is being developed by an international collaboration and consists of three instruments, the Burst Alert Telescope (BAT), the X-ray Telescope (XRT), and the Ultraviolet and Optical Telescope (UVOT). The BAT, a wide-field gamma-ray detector, will detect > 100 gamma-ray bursts per year with a sensitivity 5 times that of BATSE. The sensitive narrow-field XRT and UVOT will be autonomously slewed to the burst location in 20 to 70 seconds to determine 0.3 - 5.0 arcsec positions and perform optical, UV, and X-ray spectrophotometry. Strong education/public outreach and follow-up programs will help to engage the public and astronomical community. The Swift launch is planned for December 2003. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gehrels, N (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-165-6 J9 ASTR SOC P PY 2004 VL 312 BP 495 EP 501 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAM85 UT WOS:000222873300104 ER PT B AU Cline, TL Barthelmy, SD Hurley, KC Anfimov, D Mitrofanov, I Golenetskii, S Mazets, E Crew, G Ricker, G Atteia, JL AF Cline, TL Barthelmy, SD Hurley, KC Anfimov, D Mitrofanov, I Golenetskii, S Mazets, E Crew, G Ricker, G Atteia, JL BE Feroci, M Frontera, F Masetti, N Piro, L TI The interplanetary gamma-ray burst network in 2002-3 SO THIRD ROME WORKSHOP ON GAMMA-RAY BURSTS IN THE AFTERGLOW ERA SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 3rd Workshop on Gamma-Ray Bursts CY SEP 17-20, 2002 CL CNR, Rome, ITALY HO CNR AB The interplanetary gamma-ray burst network (IPN) has been reconstituted with the successful addition of the Mars Odyssey mission, compensating for the loss in 2001 of the NEAR mission at the asteroid Eros. The interplanetary array now consists of Ulysses at 5-6 AU, Odyssey in Martian orbit, and GGS-Wind beyond the Moon, augmented with HETE-2, RHESSI and INTEGRAL in Earth orbit. This IPN, with its several-arc-minute localization accuracy, is enabling a continuing supply of GRB sources for counterpart searches and afterglow studies. In addition, the IPN, as it had with BeppoSAX, assisted the GRB checkouts of HETE-2, RHESSI, and INTEGRAL with confirming localizations. Other transients have also been observed, including several SGRs and a source that is neither a GRB nor an SGR. The high (up to 9/month) rate of precise but delayed IPN localizations complements the less frequent but more prompt HETE-2 and INTEGRAL localizations. This IPN is expected to operate until at least 2004, hopefully until well after the launch of the Swift mission. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Cline, TL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Barthelmy, Scott/D-2943-2012; Golenetskii, Sergey/B-3818-2015 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-165-6 J9 ASTR SOC P PY 2004 VL 312 BP 517 EP 519 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BAM85 UT WOS:000222873300108 ER PT B AU Gilliam, D AF Gilliam, D GP ieee computer society TI WETICE 2004 - Ninth Enterprise Security (ES) Workshop report SO THIRTEENTH IEEE INTERNATIONAL WORKSHOPS ON ENABLING TECHNOLOGIES: INFRASTRUCTURE FOR COLLABORATIVE ENTERPRISES, PROCEEDINGS LA English DT Proceedings Paper CT 13th IEEE International Workshop on Enabling Technologies - Infrastructure for Collaborative Enterprises (WET ICE 2004) CY JUN 14-16, 2004 CL Univ Modena & Reggio Emilia, Modena, ITALY SP IEEE Comp Soc, Tech Comm Data Engn, W Virginia Univ, Concurrent Engn Res Ctr HO Univ Modena & Reggio Emilia C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP Gilliam, D (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2183-5 PY 2004 BP 195 EP 197 DI 10.1109/ENABL.2004.82 PG 3 WC Computer Science, Theory & Methods SC Computer Science GA BBB51 UT WOS:000224553100031 ER PT B AU Gilliam, DP AF Gilliam, DP GP ieee computer society TI Security risks: Management and mitigation in the software life cycle SO THIRTEENTH IEEE INTERNATIONAL WORKSHOPS ON ENABLING TECHNOLOGIES: INFRASTRUCTURE FOR COLLABORATIVE ENTERPRISES, PROCEEDINGS LA English DT Proceedings Paper CT 13th IEEE International Workshop on Enabling Technologies - Infrastructure for Collaborative Enterprises (WET ICE 2004) CY JUN 14-16, 2004 CL Univ Modena & Reggio Emilia, Modena, ITALY SP IEEE Comp Soc, Tech Comm Data Engn, W Virginia Univ, Concurrent Engn Res Ctr HO Univ Modena & Reggio Emilia AB A formal approach to managing and mitigating security risks in the software life cycle is requisite to developing software that has a higher degree of assurance that it is free of security defects which pose risk to the computing environment and the organization. Due to its criticality, security should be integrated as a formal approach in the software life cycle. Both a software security checklist and assessment tools should be incorporated into this life cycle process and integrated with a security risk assessment and mitigation tool. The current research at JPL addresses these areas through the development of a Software Security Assessment Instrument (SSAI) and integrating it with a Defect Detection and Prevention (DDP) risk management tool. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. EM david.p.gailliam@jpl.nasa.gov NR 21 TC 1 Z9 1 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2183-5 PY 2004 BP 211 EP 216 DI 10.1109/ENABL.2004.55 PG 6 WC Computer Science, Theory & Methods SC Computer Science GA BBB51 UT WOS:000224553100035 ER PT S AU Richardson, JD Wang, C Burlaga, LF AF Richardson, JD Wang, C Burlaga, LF BE Cairns, IH Genta, G Scherer, K TI The solar wind in the outer heliosphere SO TO THE EDGE OF THE SOLAR SYSTEM AND BEYOND SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE outer heliosphere; solar wind; magnetic field; transient events ID COSMIC-RAY MODULATION; TERMINATION SHOCK; MAGNETIC-FIELDS; DISTANT HELIOSPHERE; CYCLE VARIATIONS; PICKUP IONS; VOYAGER 1; AU; FLOW; FLUCTUATIONS AB We review recent plasma and magnetic field results stemming from Voyager 1 and 2 observations of the solar wind in the outer heliosphere. The solar wind speed profiles in 2002 are dominated by shock-related speed increases followed by long ramps of decreasing speed. Significant variability in the density and temperature are seen on all time scales. Transient events near solar maxima drive the formation of MIRs which are increasingly important at large radial distances. Both the density and magnetic field magnitude are consistent with the predictions of Parker's solar wind model. The solar wind pressure changes at all latitudes over the solar cycle, resulting in an oscillation of the heliospheric boundary positions. As the Voyagers move farther out, the effect of the interstellar medium on the solar wind increases. Observed speeds at Voyager 2 are about 60 km/s lower than those in the inner heliosphere due to interaction with the interstellar neutrals. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 MIT, Space Res Ctr, Cambridge, MA 02139 USA. Chinese Acad Sci, Lab Space Weather, Beijing, Peoples R China. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Richardson, JD (reprint author), MIT, Space Res Ctr, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM jdr@space.mit.edu NR 30 TC 9 Z9 9 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2004 VL 34 IS 1 BP 150 EP 156 DI 10.1016/j.asr.2003.03.066 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAS46 UT WOS:000223368400023 ER PT S AU Collier, MR Moore, TE Simpson, D Roberts, A Szabo, A Fuselier, S Wurz, P Lee, MA Tsurutani, BT AF Collier, MR Moore, TE Simpson, D Roberts, A Szabo, A Fuselier, S Wurz, P Lee, MA Tsurutani, BT BE Cairns, IH Genta, G Scherer, K TI An unexplained 10-40 degrees shift in the location of some diverse neutral atom data at 1 AU SO TO THE EDGE OF THE SOLAR SYSTEM AND BEYOND SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE neutral atom environment; neutral solar wind; interstellar neutral atom data; plasma wave data ID LOCAL INTERSTELLAR-MEDIUM; SOLAR-WIND; HYDROGEN; CLOUD; GAS; HELIOSPHERE; ENVIRONMENT; HELIUM; ORIGIN; FIELD AB Four different data sets pertaining to the neutral atom environment at 1 AU are presented and discussed. These data sets include neutral solar wind and interstellar neutral atom data from IMAGE/LENA, energetic hydrogen atom data from SOHO/HSTOF and plasma wave data from the magnetometer on ISEE-3. Surprisingly, these data sets are centered between 262degrees and 292degrees ecliptic longitude, similar to10-40degrees from the upstream interstellar neutral (ISN) flow direction at 254degrees resulting from the motion of the Sun relative to the local interstellar cloud (LIC). Some possible explanations for this offset, none of which is completely satisfactory, are discussed. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Lockheed Adv Technol Ctr, Palo Alto, CA 94304 USA. Univ Bern, CH-3012 Bern, Switzerland. Univ New Hampshire, Durham, NH 03824 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Collier, MR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM mcollier@pop600.gsfc.nasa.gov RI Moore, Thomas/D-4675-2012; Collier, Michael/I-4864-2013 OI Moore, Thomas/0000-0002-3150-1137; Collier, Michael/0000-0001-9658-6605 NR 28 TC 24 Z9 24 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2004 VL 34 IS 1 BP 166 EP 171 DI 10.1016/j.asr.2003.03.068 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BAS46 UT WOS:000223368400026 ER PT S AU Lindsey, AE Pecheur, C AF Lindsey, AE Pecheur, C BE Jensen, K Podelski, A TI Simulation-based verification of autonomous controllers via Livingstone PathFinder SO TOOLS AND ALGORITHMS FOR THE CONSTRUCTION AND ANALYSIS OF SYSTEMS, PROCEEDINGS SE Lecture Notes in Computer Science LA English DT Article; Proceedings Paper CT 10th International Conference on Tools and Algorithms for the Construction and Analysis of Systems CY MAR 29-APR 02, 2004 CL Barcelona, SPAIN SP Catalonia Tech Univ, LSI Dept, European Assoc Theoret Comp Sci, European Assoc Programming Languages & System, European Assoc Software & Technol, ACM SIGACT, SIGSOFT, SIGPLAN AB AI software is often used as a means for providing greater autonomy to automated systems, capable of coping with harsh and unpredictable environments. Due in part to the enormous space of possible situations that they aim to address, autonomous systems pose a serious challenge to traditional test-based verification approaches. Efficient verification approaches need to be perfected before these systems can reliably control critical applications. This publication describes Livingstone PathFinder (LPF), a verification tool for autonomous control software. LPF applies state space exploration algorithms to an instrumented testbed, consisting of the controller embedded in a simulated operating environment. Although LPF has focused on NASA's Livingstone model-based diagnosis system applications, the architecture is modular and adaptable to other systems. This article presents different facets of LPF and experimental results from applying the software to a Livingstone model of the main propulsion feed subsystem for a prototype space vehicle. C1 NASA, Ames Res Ctr, QSS Grp, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, RIACS, Moffett Field, CA 94035 USA. RP NASA, Ames Res Ctr, QSS Grp, Moffett Field, CA 94035 USA. EM tlindsey@ptolemy.arc.nasa.gov; pecheur@ptolemy.arc.nasa.gov NR 11 TC 4 Z9 4 U1 0 U2 2 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-21299-X J9 LECT NOTES COMPUT SC PY 2004 VL 2988 BP 357 EP 371 PG 15 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BY92R UT WOS:000189496900028 ER PT B AU McGlynn, T Accomazzi, A Berriman, B Borne, K Eichhorn, G Good, J Kimball, T Mazzerella, J Rots, A Thomas, B AF McGlynn, T Accomazzi, A Berriman, B Borne, K Eichhorn, G Good, J Kimball, T Mazzerella, J Rots, A Thomas, B BE Quinn, PJ Gorski, KM TI Building interoperable NASA archives SO TOWARD AN INTERNATIONAL VIRTUAL OBSERVATORY SE ESO ASTROPHYSICS SYMPOSIA LA English DT Proceedings Paper CT Conference on Toward and International Virtual Observatory CY JUN 10-14, 2002 CL Garching, GERMANY SP ESO, ESA, NASA, NSF AB Over the past decades NASA has developed an extensive set of archives for space astronomy data. These archives are organized along mission, wavelength regime and information domains. Interlinking of these archives is essential to enable the fullest use of NASA's data resources. These archives will form key elements of the VO and include many advanced archive systems. Understanding the issues that arise in linking these systems together will be important in understanding how to build the full Virtual Observatory. C1 NASA, HEASARC, Greenbelt, MD 20771 USA. RP McGlynn, T (reprint author), NASA, HEASARC, Code 660-1, Greenbelt, MD 20771 USA. RI Eichhorn, Guenther/C-9480-2009 OI Eichhorn, Guenther/0000-0002-3032-1978 NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-21001-6 J9 ESO ASTROPHY SYMP PY 2004 BP 294 EP 295 DI 10.1007/10857598_58 PG 2 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BAV00 UT WOS:000223659000058 ER PT J AU Lam, CW James, JT McCluskey, R Hunter, RL AF Lam, CW James, JT McCluskey, R Hunter, RL TI Pulmonary toxicity of single-wall carbon nanotubes in mice 7 and 90 days after intratracheal instillation SO TOXICOLOGICAL SCIENCES LA English DT Article; Proceedings Paper CT 42nd Annual Meeting of the Society-of-Toxicology CY MAR 09-13, 2003 CL SALT LAKE CITY, UTAH SP Soc Toxicol DE carbon nanotubes; pulmonary toxicity; epithelioid granulomas; nanotube toxicity ID GRAPHITE PNEUMOCONIOSIS; SIMULATED LUNAR; MARTIAN DUSTS; INHALATION; RATS; SILICOSIS; RESPONSES; EXPOSURE; QUARTZ AB Nanomaterials are part of an industrial revolution to develop lightweight but strong materials for a variety of purposes. Single-wall carbon nanotubes are an important member of this class of materials. They structurally resemble rolled-up graphite sheets, usually with one end capped; individually they are about 1 nm in diameter and several microns long, but they often pack tightly together to form rods or ropes of microscopic sizes. Carbon nanotubes possess unique electrical, mechanical, and thermal properties and have many potential applications in the electronics, computer, and aerospace industries. Unprocessed nanotubes are very light and could become airborne and potentially reach the lungs. Because the toxicity of nanotubes in the lung is not known, their pulmonary toxicity was investigated. The three products studied were made by different methods and contained different types and amounts of residual catalytic metals. Mice were intratracheally instilled with 0, 0.1, or 0.5 mg of carbon nanotubes, a carbon black negative control, or a quartz positive control and euthanized 7 d or 90 d after the single treatment for histopathological study of the lungs. All nanotube products induced dose-dependent epithelioid granulomas and, in some cases, interstitial inflammation in the animals of the 7-d groups. These lesions persisted and were more pronounced in the 90-d groups; the lungs of some animals also revealed peribronchial inflammation and necrosis that had extended into the alveolar septa. The lungs of mice treated with carbon black were normal, whereas those treated with high-dose quartz revealed mild to moderate inflammation. These results show that, for the test conditions described here and on an equal-weight basis, if carbon nanotubes reach the lungs, they are much more toxic than carbon black and can be more toxic than quartz, which is considered a serious occupational health hazard in chronic inhalation exposures. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Wyle Labs, Houston, TX 77058 USA. Univ Texas, Sch Med, Dept Pathol & Lab Med, Houston, TX 77030 USA. RP Lam, CW (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM Chiu-wing.Lam@jsc.nasa.gov NR 40 TC 1166 Z9 1270 U1 27 U2 182 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1096-6080 J9 TOXICOL SCI JI Toxicol. Sci. PD JAN PY 2004 VL 77 IS 1 BP 126 EP 134 DI 10.1093/toxsci/kfg243 PG 9 WC Toxicology SC Toxicology GA 762NJ UT WOS:000187988800016 PM 14514958 ER PT S AU Crisp, D Atlas, RM Breon, FM Brown, LR Burrows, JP Ciais, P Connor, BJ Doney, SC Fung, IY Jacob, DJ Miller, CE O'Brien, D Pawson, S Randerson, JT Rayner, P Salawitch, RJ Sander, SP Sen, B Stephens, GL Tans, PP Toon, GC Wennberg, PO Wofsy, SC Yung, YL Kuang, ZM Chudasama, B Sprague, G Weiss, B Pollock, R Kenyon, D Schroll, S AF Crisp, D Atlas, RM Breon, FM Brown, LR Burrows, JP Ciais, P Connor, BJ Doney, SC Fung, IY Jacob, DJ Miller, CE O'Brien, D Pawson, S Randerson, JT Rayner, P Salawitch, RJ Sander, SP Sen, B Stephens, GL Tans, PP Toon, GC Wennberg, PO Wofsy, SC Yung, YL Kuang, ZM Chudasama, B Sprague, G Weiss, B Pollock, R Kenyon, D Schroll, S BE Burrows, JP Thompson, AM TI The orbiting carbon observatory (OCO) mission SO TRACE CONSTITUENTS IN THE TROPOSPHERE AND LOWER STRATOSPHERE SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE orbiting carbon observatory; atmospheric carbon dioxide ID ATMOSPHERIC CO2; INTERANNUAL VARIABILITY; LATITUDINAL DISTRIBUTION; SEASONAL CYCLE; TRACE GASES; WATER-VAPOR; DIOXIDE; ABSORPTION; SINKS; LAND AB The Orbiting Carbon Observatory (OCO) mission will make the first global, space-based measurements of atmospheric carbon dioxide (CO(2)) with the precision, resolution, and coverage needed to characterize CO(2) sources and sinks on regional scales. The measurement approach and instrument specifications were determined through an analysis of existing carbon cycle data and a series of observing system simulation experiments. During its 2-year mission, OCO will fly in a 1: 15 PM sun-synchronous orbit with a 16-day ground-track repeat time, just ahead of the EOS Aqua platform. It will carry a single instrument that incorporates three bore-sighted high-resolution spectrometers designed to measure reflected sunlight in the 0.76-mum O(2) A-band and in the CO(2) bands at 1.61 and 2.06 mum. Soundings recorded in these three bands will be used to retrieve the column-averaged CO(2) dry air mole fraction (X(CO2)). A comprehensive validation program was included in the mission to ensure that the space-based X(CO2) measurements have precisions of similar to0.3% (1 ppm) on regional scales. OCO measurements will be used in global synthesis inversion and data assimilation models to quantify CO(2) sources and sinks. While OCO will have a nominal lifetime of only 2 years, it will serve as a pathfinder for future long-term CO(2) monitoring missions. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Lab Sci Climat Environm, UMR 1572, CE Orme Merisies, F-1191 Gif Sur Yvette, France. Univ Bremen, Inst Umweltphys, D-28334 Bremen, Germany. Univ Bremen, Inst Fernerkundung, D-28334 Bremen, Germany. Natl Inst Water & Atmospher Res, Omakau 9182, New Zealand. Woods Hole Oceanog Inst, Marine Chem & Geochem Dept, Woods Hole, MA 02543 USA. Univ Calif Berkeley, Berkeley Atmospher Sci Ctr, Berkeley, CA 94720 USA. Harvard Univ, Cambridge, MA 02138 USA. Haverford Coll, Dept Chem, Haverford, PA 19041 USA. CSIRO, Aspendale, Vic 3195, Australia. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. Climate Monitoring & Diagnost Lab, Boulder, CO 80305 USA. Hamilton Sundstrand Sensor Syst, Pomona, CA 91767 USA. Orbital Sci Corp, Dulles, VA USA. RP Crisp, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM david.crisp@jpl.nasa.gov RI Salawitch, Ross/B-4605-2009; Atlas, Robert/A-5963-2011; Wennberg, Paul/A-5460-2012; Doney, Scott/F-9247-2010; Pawson, Steven/I-1865-2014; Breon, Francois-Marie/M-4639-2016; Burrows, John/B-6199-2014 OI Salawitch, Ross/0000-0001-8597-5832; Atlas, Robert/0000-0002-0706-3560; Doney, Scott/0000-0002-3683-2437; Pawson, Steven/0000-0003-0200-717X; Breon, Francois-Marie/0000-0003-2128-739X; Burrows, John/0000-0002-6821-5580 NR 45 TC 340 Z9 363 U1 5 U2 53 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES-SERIES PY 2004 VL 34 IS 4 SI 2004 BP 700 EP 709 DI 10.1016/j.asr.2003.08.062 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Remote Sensing SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences; Remote Sensing GA BAU49 UT WOS:000223618200004 ER PT S AU Savtchenko, A Ouzounov, D Ahmad, S Acker, J Leptoukh, G Koziana, J Nickless, D AF Savtchenko, A Ouzounov, D Ahmad, S Acker, J Leptoukh, G Koziana, J Nickless, D BE Burrows, JP Thompson, AM TI Terra and aqua MODIS products available from NASA GES DAAC SO TRACE CONSTITUENTS IN THE TROPOSPHERE AND LOWER STRATOSPHERE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE NASA GES DAAC; earth observing system data gateway; Terra and aqua MODIS products ID WATER-VAPOR; AEROSOL; CLOUD AB The NASA Goddard Earth Sciences Distributed Active Archive Center (GES DAAC), known as GSFC-ECS in the Earth Observing System Data Gateway, distributes three major groups of MODIS products: Level 1 Radiometric and Geolocation data, and Level 2 and higher level of Atmosphere and Ocean products. The Atmosphere data types are aerosol, water vapor, cloud, temperature and moisture profiles, and cloud mask. The 107 (at present) Ocean data types include such parameters as normalized water-leaving radiances, chlorophyll and pigment concentrations ("ocean color"), total absorptions, sea surface temperatures, and ocean primary productivity. GES DAAC provides a broad spectrum of MODIS support, covering; data access, visualization tools, tools for search and order of the aforementioned data, documentation, data content, troubleshooting, and science and software support for the Earth Observing System Core System (ECS). The Web gateway for MODIS data products and services is http:// daac.gsfc.nasa.gov/MODIS/. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Goddard Space Flight Ctr, GES DACC, Greenbelt, MD 20771 USA. RP Savtchenko, A (reprint author), NASA, Goddard Space Flight Ctr, GES DACC, Greenbelt, MD 20771 USA. EM savtche@eosdata.gsfc.nasa.gov NR 7 TC 61 Z9 66 U1 5 U2 22 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 4 SI 2004 BP 710 EP 714 DI 10.1016/j.asr.2004.03.012 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Remote Sensing SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences; Remote Sensing GA BAU49 UT WOS:000223618200005 ER PT S AU Beirle, S Platt, U Wenig, M Wagner, T AF Beirle, S Platt, U Wenig, M Wagner, T BE Burrows, JP Thompson, AM TI NOx production by lightning estimated with GOME SO TRACE CONSTITUENTS IN THE TROPOSPHERE AND LOWER STRATOSPHERE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE GOME; NOx-production by lightning; nitrogen oxides; atmospheric chemistry; satellite remote sensing; free troposphere ID UPPER TROPOSPHERE; LOWER STRATOSPHERE; EMISSIONS; OZONE; NO(X); DISTRIBUTIONS; MODEL; SOILS AB Nitrogen oxides (NO + NO2 = NOx) are important trace gases in the troposphere with impact on human health, climate and atmospheric chemistry, e.g. through their role in ozone production. Therefore a better understanding of the strength of the various sources (fossil fuel combustion, biomass burning, soil emissions, lightning) is desirable. NOx produced by lightning contributes approx. 12%, i.e. 5 (2-20) T-g [N]/year [Atmos. Environ. 31 (1997) 1735; EULINOX - The European Lightning Nitrogen Oxides Project. DLR - Forschungsbericht 2000-28, 2000], of the totally produced nitrogen oxides. An uncertainty of one order of magnitude remains. Here we present an estimation of lightning produced NOx using satellite data. Lightning activity is monitored by the Lightning Imaging Sensor since November 1997. The same time span is also covered by NO2 measurements from the Global Ozone Monitoring Experiment. This allows a statistical approach. In this study we relate lightning frequency and the tropospheric vertical column densities of NO2 over Central Australia, where other NOx sources have only minor contribution. By analyzing the correlation of lightning activity with the vertical column densities of NO2 we estimate the globally produced lightning NOx to be similar to2.8 (0.8-14) T-g [N]/year. Despite the many uncertainties involved in NO2 retrieval (e.g. profile information, cloud influence), this value shows a good agreement with literature. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Inst Umweltphys, INF 229, D-69120 Heidelberg, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Beirle, S (reprint author), Inst Umweltphys, INF 229, D-69120 Heidelberg, Germany. EM beirle@iup.uni-heidelberg.de RI Wenig, Mark/K-7279-2012 NR 25 TC 38 Z9 40 U1 0 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 4 SI 2004 BP 793 EP 797 DI 10.1016/j.asr.2003.07.069 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Remote Sensing SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences; Remote Sensing GA BAU49 UT WOS:000223618200020 ER PT S AU Hollwedel, J Wenig, M Beirle, S Kraus, S Kuhl, S Wilms-Grabe, W Platt, U Wagner, T AF Hollwedel, J Wenig, M Beirle, S Kraus, S Kuhl, S Wilms-Grabe, W Platt, U Wagner, T BE Burrows, JP Thompson, AM TI Year-to-year variations of spring time polar tropospheric BrO as seen by GOME SO TRACE CONSTITUENTS IN THE TROPOSPHERE AND LOWER STRATOSPHERE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE GOME; global ozone monitoring; springtime polar tropospheric BrO; year-to-year variations ID OPTICAL-ABSORPTION SPECTROSCOPY; OZONE DESTRUCTION; BROMINE OXIDE; SUNRISE; DOAS; DEPLETION; RELEASE AB In this paper we present data on the variation of tropospheric BrO, that is connected with the spring time ozone depletion in polar regions. For this study we use data derived from the Global Ozone Monitoring Experiment (GOME) for the years 1996-2001. We especially focus on the possible detection of trends in the extent of coverage of polar regions by BrO and on the time series of BrO abundances. For this purpose we calculated monthly means during polar spring of the areas that are covered with BrO exceeding certain thresholds. It turns out that in the timeseries of total, i.e. tropospheric and stratospheric, BrO column densities there is, up to now, no clear trend identifiable. In contrast, the analysis of areas covered by high concentrations of tropospheric BrO (columns > 5.5 x 10(13) molecules/cm(2)) is considerably expanding (about 10% per year during 1996-2000) in the northern hemisphere in the comparison of monthly means during polar spring, which is possibly due to an anthropogenic effect on the climate system. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Univ Heidelberg, Inst Umweltphys, D-69120 Heidelberg, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hollwedel, J (reprint author), Univ Heidelberg, Inst Umweltphys, Neuenheimer Feld 229, D-69120 Heidelberg, Germany. EM jens.hollwedel@iup.uni-heidelberg.de RI Wenig, Mark/K-7279-2012 NR 25 TC 24 Z9 25 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 4 SI 2004 BP 804 EP 808 DI 10.1016/j.asr.2003.08.060 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Remote Sensing SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences; Remote Sensing GA BAU49 UT WOS:000223618200022 ER PT S AU Ichoku, C Kaufman, YJ Remer, LA Levy, R AF Ichoku, C Kaufman, YJ Remer, LA Levy, R BE Burrows, JP Thompson, AM TI Global aerosol remote sensing from MODIS SO TRACE CONSTITUENTS IN THE TROPOSPHERE AND LOWER STRATOSPHERE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT 2nd World Space Congress/34th COSPAR Scientific Assembly CY OCT 10-19, 2002 CL HOUSTON, TX SP Comm Space Res DE aerosol remote sensing; MODIS; aerosol concentration and size parameters; regional aerosol radiative forcing ID TROPOSPHERIC AEROSOL; AERONET; OCEANS AB Global aerosol concentration and size parameters derived from MODIS sensors onboard the Terra and Aqua satellites are continuously being evaluated with ground-based measurements and used for various aerosol studies. These parameters have enabled a two-year assessment of aerosol loading and seasonal trends over several important regions on land and ocean, based on 5 x 5degrees monthly averages. Similar studies were conducted at higher spatial (50 x 50-km) and temporal (daily) resolutions over selected sites representative of pollution, smoke, dust, and sea-salt aerosol types. Also, a two parameter clustering technique has been employed successfully for categorizing the predominant aerosol types and events affecting selected locations over the Atlantic and Pacific Oceans. In addition, results of regional aerosol radiative forcing calculations over a few regions are reported. (C) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Sci Syst & Applicat Inc, Lanham, MD 20706 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Ichoku, C (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd, Lanham, MD 20706 USA. EM ichoku@climate.gsfc.nasa.gov RI Ichoku, Charles/E-1857-2012; Levy, Robert/M-7764-2013 OI Ichoku, Charles/0000-0003-3244-4549; Levy, Robert/0000-0002-8933-5303 NR 16 TC 63 Z9 72 U1 3 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI KIDLINGTON PA THE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND SN 0273-1177 J9 ADV SPACE RES PY 2004 VL 34 IS 4 SI 2004 BP 820 EP 827 DI 10.1016/j.asr.2003.07.071 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences; Remote Sensing SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences; Remote Sensing GA BAU49 UT WOS:000223618200025 ER PT S AU Ramachandran, N Mazuruk, K AF Ramachandran, N Mazuruk, K BE Sadhal, SS TI Magnetic microspheres and tissue model studies for therapeutic applications SO TRANSPORT PHENOMENA IN MICROGRAVITY SE Annals of the New York Academy of Sciences LA English DT Article; Proceedings Paper CT Conference on Microgravity Transport Processes in Fluid, Thermal, Materials and Biological Sciences CY SEP 14-18, 2003 CL Davos, SWITZERLAND SP Engn Conf Int, NASA, US Natl Sci Fdn DE hyperthermia; cancer therapy; magnetic particles and microspheres; magnetic fluids; Curie temperature; thermoregulating particles ID IN-VITRO; FLUID HYPERTHERMIA; CANCER-TREATMENT; PARTICLES; NANOPARTICLES; TOXICITY; SYSTEM AB The use of magnetic fluids and magnetic particles in combinatorial hyperthermia therapy for cancer treatment is reviewed. The investigation approach adopted for producing thermoregulating particles and tissue model studies for studying particle retention and heating characteristics is discussed. C1 BAE SYST Analyt Serv Inc, NASA Marshall Space Flight Ctr, Huntsville, AL USA. Univ Alabama, Huntsville, AL 35899 USA. RP Ramachandran, N (reprint author), BAE SYST Analyt Serv Inc, NASA Marshall Space Flight Ctr, SD 46, Huntsville, AL USA. EM narayanan.ramachandran@msfc.nasa.gov NR 31 TC 8 Z9 8 U1 0 U2 3 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-563-X J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1027 BP 99 EP 109 DI 10.1196/annals.1324.010 PG 11 WC Biophysics; Mechanics; Multidisciplinary Sciences SC Biophysics; Mechanics; Science & Technology - Other Topics GA BBP91 UT WOS:000226975400010 PM 15644349 ER PT S AU Tucker, DS Ethridge, EC Smith, GA Workman, G AF Tucker, DS Ethridge, EC Smith, GA Workman, G BE Sadhal, SS TI Effects of gravity on ZBLAN glass crystallization SO TRANSPORT PHENOMENA IN MICROGRAVITY SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Microgravity Transport Processes in Fluid, Thermal, Materials and Biological Sciences CY SEP 14-18, 2003 CL Davos, SWITZERLAND SP Engn Conf Int, NASA, US Natl Sci Fdn DE non-oxide glass; microgravity; ZBLAN; crystallization ID NUCLEATION; FLOW; MELT AB The effects of gravity on the crystallization of ZrF4-BaF2-LaF(3)AIF(3)-NaF glasses have been studied using the NASA KC-135 and a sounding rocket. Fibers and cylinders of ZBLAN glass were heated to the crystallization temperature in unit and reduced gravity. When processed in unit gravity the glass crystallized, but when processed in reduced gravity, crystallization was suppressed. A possible explanation involving shear thinning is presented to explain these results. C1 NASA, NSSTC, SD71, Huntsville, AL 35805 USA. Marshall Space Flight Ctr, SD46, Huntsville, AL USA. Univ Alabama, Huntsville, AL 35899 USA. RP Tucker, DS (reprint author), NASA, NSSTC, SD71, 320 Sparkman Dr, Huntsville, AL 35805 USA. EM dr.dennis.tucker@nasa.gov NR 20 TC 6 Z9 6 U1 0 U2 9 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-563-X J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1027 BP 129 EP 137 DI 10.1196/annals.1324.012 PG 9 WC Biophysics; Mechanics; Multidisciplinary Sciences SC Biophysics; Mechanics; Science & Technology - Other Topics GA BBP91 UT WOS:000226975400012 PM 15644351 ER PT S AU Kaul, RK Barghouty, AF Dahche, HM AF Kaul, RK Barghouty, AF Dahche, HM BE Sadhal, SS TI Space radiation transport properties of polyethylene-based composites SO TRANSPORT PHENOMENA IN MICROGRAVITY SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Microgravity Transport Processes in Fluid, Thermal, Materials and Biological Sciences CY SEP 14-18, 2003 CL Davos, SWITZERLAND SP Engn Conf Int, NASA, US Natl Sci Fdn DE ionizing radiation; space radiation; shielding; shielding effectiveness; HZE; transport; simulation; transmission; polyethylene; hybrid materials; polyethylene-based composites; composites; galactic cosmic rays; solar energetic particles; deep-space missions; micrometeorite shields; Mars missions; multi-functional materials; fluences; dose; dose-equivalent; linear energy transfer ID SOLAR ENERGETIC PARTICLES; PARTIAL CROSS-SECTIONS; NUCLEUS REACTIONS; IONIC CHARGE; EVENT AB Composite materials that can serve as both effective shielding materials against cosmic-ray and energetic solar particles in deep space, as well as structural materials for habitat and spacecraft, remain a critical and mission enabling component in mission planning and exploration. Polyethylene is known to have excellent shielding properties due to its low density, coupled with high hydrogen content. Polyethylene-fiber reinforced composites promise to combine this shielding effectiveness with the required mechanical properties of structural materials. Samples of polyethylene-fiber reinforced epoxy matrix composite 1-5cm thick Were prepared at the NASA Marshall Space Flight Center and tested against a 500 MeV/nucleon Fe beam at the HIMAC facility of NIRS in Chiba, Japan. This paper presents measured and calculated results for the radiation transport properties of these samples. C1 NASA, George C Marshall Space Flight Ctr, SD46, Huntsville, AL 35812 USA. Roanoke Coll, Dept Chem, Salem, VA 24153 USA. RP Kaul, RK (reprint author), NASA, George C Marshall Space Flight Ctr, SD46, Huntsville, AL 35812 USA. EM nasser.barghouty@msfc.nasa.gov NR 23 TC 3 Z9 3 U1 1 U2 5 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-563-X J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1027 BP 138 EP 149 DI 10.1196/annals.1324.013 PG 12 WC Biophysics; Mechanics; Multidisciplinary Sciences SC Biophysics; Mechanics; Science & Technology - Other Topics GA BBP91 UT WOS:000226975400013 PM 15644352 ER PT S AU Balasubramaniam, R Subramanian, RS AF Balasubramaniam, R Subramanian, RS BE Sadhal, SS TI Thermocapillary migration of a drop - An exact solution with Newtonian interfacial rheology and stretching/shrinkage of interfacial area elements for small Marangoni numbers SO TRANSPORT PHENOMENA IN MICROGRAVITY SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Microgravity Transport Processes in Fluid, Thermal, Materials and Biological Sciences CY SEP 14-18, 2003 CL Davos, SWITZERLAND SP Engn Conf Int, NASA, US Natl Sci Fdn DE thermocapillary migration; Newtonian interfacial rheology; small Marangoni numbers; drop; stretching and shrinking of interface ID MOTION; BUBBLES; TEMPERATURE; ENERGY AB In this paper we analyze the effects of the following phenomena associated with the thermocapillary migration of a drop. The first is the influence of Newtonian surface rheology of the interface and the second is that of the energy changes associated with stretching and shrinkage of the interfacial area elements, when the drop is in motion. The former occurs because of dissipative processes in the interfacial region, such as when surfactant molecules are adsorbed at the interface in sufficient concentration. The interface is typically modeled in this instance by ascribing to it a surface viscosity. This is a different effect from that of interfacial tension gradients arising from surfactant concentration gradients. The stretching and shrinkage of interfacial area elements leads to changes in the internal energy of these elements that affects the transport of energy in the fluids adjoining the interface. When an element on the interface is stretched, its internal energy increases because of the increase in its area. This energy is supplied by the neighboring fluids that are cooled as a consequence. Conversely, when an element on the interface shrinks, the adjoining fluids are warmed. In the case of a moving drop, elements of interfacial area are stretched in the forward half of the drop, and are shrunk in the rear half. Consequently, the temperature variation on the surface of the drop and its migration speed are modified. The analysis of the motion of a drop including these effects was first performed by LeVan in 1981, in the limit when convective transport of momentum and energy are negligible. We extend the analysis of LeVan to include the convective transport of momentum by demonstrating that an exact solution of the momentum equation is obtained for an arbitrary value of the Reynolds number. This solution is then used to calculate the slightly deformed shape of the drop from a sphere. C1 NASA, Glenn Res Ctr, Natl Ctr Micrograv Res, Cleveland, OH 44135 USA. Clarkson Univ, Dept Chem Engn, Potsdam, NY USA. RP Balasubramaniam, R (reprint author), NASA, Glenn Res Ctr, Natl Ctr Micrograv Res, Mail Stop 110-3, Cleveland, OH 44135 USA. EM bala@grc.nasa.gov NR 10 TC 5 Z9 5 U1 0 U2 3 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-563-X J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1027 BP 303 EP 310 DI 10.1196/annals.1324.024 PG 8 WC Biophysics; Mechanics; Multidisciplinary Sciences SC Biophysics; Mechanics; Science & Technology - Other Topics GA BBP91 UT WOS:000226975400024 PM 15644363 ER PT S AU Rashidnia, N Balasubramaniam, R Schroer, RT AF Rashidnia, N Balasubramaniam, R Schroer, RT BE Sadhal, SS TI The formation of spikes in the displacement of miscible fluids SO TRANSPORT PHENOMENA IN MICROGRAVITY SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Microgravity Transport Processes in Fluid, Thermal, Materials and Biological Sciences CY SEP 14-18, 2003 CL Davos, SWITZERLAND SP Engn Conf Int, NASA, US Natl Sci Fdn DE spikes; displacement; miscible fluids ID VISCOUS-FLUID; CAPILLARY TUBES AB We report on experiments in which a more viscous fluid displaces a less viscous one in a vertical cylindrical tube. These experiments were performed using silicone oils in a vertical pipette of small diameter. The more viscous fluid also had a slightly larger density than the less viscous fluid. In the initial configuration, the fluids were at rest, and the interface was nominally flat. A dye was added to the more viscous fluid for ease of observation of the interface between the fluids. The How was initiated by pumping the more viscous fluid into the less viscous one. The displacement velocity was such that the Reynolds number was smaller than unity and the Peclet number for mass transfer between the fluids was large compared to unity. For upward displacement of the more viscous fluid from an initially stable configuration, an axisymmetric ringer was observed under all conditions. However, a needle-shaped spike was seen to propagate from the main finger in many cases, similar to that observed by Petitjeans and Maxworthy for the displacement of a more viscous fluid by a less viscous one. C1 NASA, Glenn Res Ctr, Natl Ctr Micrograv Res, Cleveland, OH 44135 USA. RP Rashidnia, N (reprint author), NASA, Glenn Res Ctr, Natl Ctr Micrograv Res, 21000 Brookpk Rd,MS-110-3, Cleveland, OH 44135 USA. EM nasser.rashidnia@grc.nasa.gov NR 10 TC 3 Z9 3 U1 0 U2 1 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-563-X J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1027 BP 311 EP 316 DI 10.1196/annals.1324.025 PG 6 WC Biophysics; Mechanics; Multidisciplinary Sciences SC Biophysics; Mechanics; Science & Technology - Other Topics GA BBP91 UT WOS:000226975400025 PM 15644364 ER PT S AU Kassemi, M Deserranno, D Oas, JG AF Kassemi, M Deserranno, D Oas, JG BE Sadhal, SS TI Effect of gravity on the caloric stimulation of the inner ear SO TRANSPORT PHENOMENA IN MICROGRAVITY SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Microgravity Transport Processes in Fluid, Thermal, Materials and Biological Sciences CY SEP 14-18, 2003 CL Davos, SWITZERLAND SP Engn Conf Int, NASA, US Natl Sci Fdn DE fluid structural interaction; inner ear; vestibular system; CFD; caloric test; microgravity ID SPACE; MODEL AB Robert Barany won the 1914 Nobel Prize in medicine for his convection hypothesis for caloric stimulation. Microgravity caloric tests aboard the 1983 SpaceLab1 mission produced nystagmus results that contradicted the basic premise of Barany's convection theory. In this paper, we present a fluid structural analysis of the caloric stimulation of the lateral semicircular canal. Direct numerical simulations indicate that on earth, natural convection is the dominant mechanism for endolymphatic now. However, in the microgravity environment of orbiting spacecraft, where buoyancy effects are mitigated, an expansive convection becomes the sole mechanism for producing endolymph motion and cupular displacement. Transient 1 g and microgravity case studies are presented to delineate the different dynamic behaviors of the 1 g and microgravity endolymphatic flows. The associated fluid-structural interactions are also analyzed based on the time evolution of cupular displacements. C1 NASA, Glenn Res Ctr, Natl Ctr Micrograv Res, Cleveland, OH 44135 USA. Case Western Reserve Univ, Dept Biomed Engn, Cleveland, OH 44106 USA. Cleveland Clin Fdn, Dept Otolaryngol, Cleveland, OH USA. RP Kassemi, M (reprint author), NASA, Glenn Res Ctr, Natl Ctr Micrograv Res, 21000 Brookpk Rd,MS110-3, Cleveland, OH 44135 USA. EM mohammad.kassemi@grc.nasa.gov NR 24 TC 1 Z9 1 U1 0 U2 3 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-563-X J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1027 BP 360 EP 370 DI 10.1196/annals.1324.030 PG 11 WC Biophysics; Mechanics; Multidisciplinary Sciences SC Biophysics; Mechanics; Science & Technology - Other Topics GA BBP91 UT WOS:000226975400029 PM 15644368 ER PT S AU Niederhaus, CE Jacobs, JW AF Niederhaus, CE Jacobs, JW BE Sadhal, SS TI An experimental study of the Richtmyer-Meshkov instability in microgravity SO TRANSPORT PHENOMENA IN MICROGRAVITY SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Microgravity Transport Processes in Fluid, Thermal, Materials and Biological Sciences CY SEP 14-18, 2003 CL Davos, SWITZERLAND SP Engn Conf Int, NASA, US Natl Sci Fdn DE Richtmyer-Meshkov instability; microgravity; fluid dynamics; interface stability; Taylor instability ID GAS INTERFACE; SINGLE-MODE; DRIVEN; FLUIDS; PERTURBATIONS; GROWTH; FUSION; LASER; NOVA AB Richtmyer-Meshkov (RM) instability occurs when a planar interface separating two fluids of different density is impulsively accelerated in the direction of its normal. It is one of the most fundamental fluid instabilities and is of importance to the fields of astrophysics and inertial confinement fusion. Because RM instability experiments are normally carried out in shock tubes, where the generation of a sharp, well-controlled interface between gases is difficult, there is a scarcity of good experimental results. The experiments presented here use a novel technique that circumvents many of the experimental difficulties that have previously limited the study of RM instability in shock tubes. In these experiments, the instability is generated incompressibly, by bouncing a rectangular tank containing two liquids off of a fixed spring. These experiments, which utilize PLIF flow visualization, yield time-motion image sequences of the nonlinear development and transition to turbulence of the instability that are of a quality unattainable in shock tube experiments. Measurements obtained from these images, therefore, provide benchmark data for the evaluation of nonlinear models for the late-time growth of the instability. Because the run time in these experiments is limited, new experiments in the NASA Glenn 2.2 second drop tower, capable of achieving longer run times, are currently under way. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Univ Arizona, Tucson, AZ USA. RP Niederhaus, CE (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-5, Cleveland, OH 44135 USA. EM charles.niederhaus@nasa.gov RI Jacobs, Jeffrey/B-1339-2013 OI Jacobs, Jeffrey/0000-0003-0193-7105 NR 28 TC 0 Z9 0 U1 0 U2 5 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-563-X J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1027 BP 403 EP 413 DI 10.1196/annals.1324.033 PG 11 WC Biophysics; Mechanics; Multidisciplinary Sciences SC Biophysics; Mechanics; Science & Technology - Other Topics GA BBP91 UT WOS:000226975400032 PM 15644371 ER PT S AU Matson, DM Fair, DJ Hyers, RW Rogers, JR AF Matson, DM Fair, DJ Hyers, RW Rogers, JR BE Sadhal, SS TI Contrasting electrostatic and electromagnetic levitation experimental results for transformation kinetics of steel alloys SO TRANSPORT PHENOMENA IN MICROGRAVITY SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Microgravity Transport Processes in Fluid, Thermal, Materials and Biological Sciences CY SEP 14-18, 2003 CL Davos, SWITZERLAND SP Engn Conf Int, NASA, US Natl Sci Fdn DE containerless processing; steel transformation; rapid solidification AB The delay between conversion of metastable ferrite to stable austenite during ternary Fe-Cr-Ni alloy double recalescence is seen to differ by over an order of magnitude for tests conducted using electrostatic and electromagnetic levitation. Several possible reasons for this deviation are proposed. Thermodynamic calculations on evaporation rates indicate that potential composition shifts during testing are minimized by limiting test time and thermal history. Simulation indicates that deviation would be limited to a factor of 1.5 under worst-case conditions. Possible effects due to differences in sample size are also eliminated since the metastable array, where stable phase nucleation must occur, is significantly smaller than the sample. Differences in internal convection are seen to be the most probable reason for the observed deviation. C1 Tufts Univ, Dept Mech Engn, Medford, MA 02155 USA. Univ Massachusetts, Amherst, MA 01003 USA. George C Marshall Space Flight Ctr, Huntsville, AL USA. RP Matson, DM (reprint author), Tufts Univ, Dept Mech Engn, 200 Coll Ave,025 Anderson Hall, Medford, MA 02155 USA. EM douglas.matson@tufts.edu RI Hyers, Robert/G-3755-2010; Matson, Douglas/I-7860-2015 NR 13 TC 15 Z9 16 U1 2 U2 6 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-563-X J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1027 BP 435 EP 446 DI 10.1196/annals.1324.035 PG 12 WC Biophysics; Mechanics; Multidisciplinary Sciences SC Biophysics; Mechanics; Science & Technology - Other Topics GA BBP91 UT WOS:000226975400034 PM 15644373 ER PT S AU Hyers, RW Matson, DM Kelton, KF Rogers, JR AF Hyers, RW Matson, DM Kelton, KF Rogers, JR BE Sadhal, SS TI Convection in containerless processing SO TRANSPORT PHENOMENA IN MICROGRAVITY SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Microgravity Transport Processes in Fluid, Thermal, Materials and Biological Sciences CY SEP 14-18, 2003 CL Davos, SWITZERLAND SP Engn Conf Int, NASA, US Natl Sci Fdn DE electromagnetic levitation; electrostatic levitation; convection; containerless processing; quasicrystals; stainless steel ID THERMOPHYSICAL PROPERTIES; STAINLESS-STEEL; SURFACE-TENSION; ALLOYS; NI; VISCOSITY AB Different containerless processing techniques have different strengths and weaknesses. Applying more than one technique allows various parts of a problem to be solved separately. For two research projects, one on phase selection in steels and the other on nucleation and growth of quasicrystals, a combination of experiments using electrostatic levitation (ESL) and electromagnetic levitation (EML) is appropriate. In both experiments, convection is an important variable. The convective conditions achievable with each method are compared for two very different materials: a low-viscosity, high-temperature stainless steel, and a high-viscosity, low-temperature quasierystal-forming alloy. It is clear that the techniques are complementary when convection is a parameter to be explored in the experiments. For a number of reasons, including the sample size, temperature, and reactivity, direct measurement of the convective velocity is not feasible. Therefore, we must rely on computation techniques to estimate convection in these experiments. These models are an essential part of almost any microgravity investigation. The methods employed and results obtained for the projects levitation observation of dendrite evolution in steel ternary alloy rapid solidification (LODESTARS) and quasicrystalline undercooled alloys for space investigation (QUASI) are explained. C1 Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA. Tufts Univ, Medford, MA 02155 USA. Washington Univ, St Louis, MO 63130 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Hyers, RW (reprint author), Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA. EM hyers@ecs.umass.edu RI Hyers, Robert/G-3755-2010; Matson, Douglas/I-7860-2015 NR 20 TC 23 Z9 25 U1 0 U2 4 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-563-X J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1027 BP 474 EP 494 DI 10.1196/annals.1324.038 PG 21 WC Biophysics; Mechanics; Multidisciplinary Sciences SC Biophysics; Mechanics; Science & Technology - Other Topics GA BBP91 UT WOS:000226975400037 PM 15644376 ER PT S AU Kassemi, M Panzarella, CH AF Kassemi, M Panzarella, CH BE Sadhal, SS TI Ventless pressure control of two-phase propellant tanks in microgravity SO TRANSPORT PHENOMENA IN MICROGRAVITY SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Microgravity Transport Processes in Fluid, Thermal, Materials and Biological Sciences CY SEP 14-18, 2003 CL Davos, SWITZERLAND SP Engn Conf Int, NASA, US Natl Sci Fdn DE pressure control; two-phase storage; microgravity; propellant tanks; computational fluid dynamics; space cryogenic tanks AB This work studies pressurization and pressure control of a large liquid hydrogen storage tank. A finite element model is developed that couples a lumped thermodynamic formulation for the vapor region with a complete solution of the Navier-Stokes and energy equations for the flow and temperature fields in the liquid. Numerical results show that buoyancy effects are strong, even in microgravity, and can reposition a vapor bubble that is initially at the center of the tank to a region near the tank wall in a relatively short time. Long-term tank pressurization with the vapor bubble at the tank wall shows that after an initial transient lasting about a week, the final rate of pressure increase agrees with a purely thermodynamic analysis of the entire tank. However, the final pressure levels are quite different from thermodynamic predictions. Numerical results also show that there is significant thermal stratification in the liquid due to the effects of natural convection. A subcooled jet is used to provide simultaneous cooling and mixing in order to bring the tank pressure back down to its initial value. Three different jet speeds are examined. Although the lowest jet speed is ineffective at controlling the pressure because of insufficient penetration into the liquid region, the highest jet speed is shown to be quite effective at disrupting thermal stratification and reducing the tank pressure in reasonable time. C1 NASA, Glenn Res Ctr, Natl Ctr Micrograv Res, Cleveland, OH 44135 USA. Ohio Aerosp Inst, Cleveland, OH USA. RP Kassemi, M (reprint author), NASA, Glenn Res Ctr, Natl Ctr Micrograv Res, 21000 Brookpk Rd,MS110-3, Cleveland, OH 44135 USA. EM mohammad.kassemi@grc.nasa.gov NR 28 TC 0 Z9 0 U1 0 U2 2 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-563-X J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1027 BP 511 EP 528 DI 10.1196/annals.1324.040 PG 18 WC Biophysics; Mechanics; Multidisciplinary Sciences SC Biophysics; Mechanics; Science & Technology - Other Topics GA BBP91 UT WOS:000226975400039 PM 15644378 ER PT S AU Trolinger, JD L'Esperance, D Rangel, RH Coimbra, CFM Witherow, WK AF Trolinger, JD L'Esperance, D Rangel, RH Coimbra, CFM Witherow, WK BE Sadhal, SS TI Design and preparation of a particle dynamics space flight experiment, SHIVA SO TRANSPORT PHENOMENA IN MICROGRAVITY SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Microgravity Transport Processes in Fluid, Thermal, Materials and Biological Sciences CY SEP 14-18, 2003 CL Davos, SWITZERLAND SP Engn Conf Int, NASA, US Natl Sci Fdn DE particle dynamics; Stokes flow; microgravity; holography ID IMAGE VELOCIMETRY; MOTION; EQUATION AB This paper describes the flight experiment, supporting ground science, and the design rationale for a project on spaceflight holography investigation in a virtual apparatus (SHIVA). SHIVA is a fundamental study of particle dynamics in fluids in microgravity. Gravitation effects and steady Stokes drag often dominate the equations of motion of a particle in a fluid and consequently microgravity provides an ideal environment in which to study the other forces, such as the pressure and viscous drag and especially the Basset history force. We have developed diagnostic recording methods using holography to save all of the particle field optical characteristics, essentially allowing the experiment to be transferred from space back to Earth in what we call the "virtual apparatus" for microgravity experiments on Earth. We can quantify precisely the three-dimensional motion of sets of particles, allowing us to test and apply new analytic solutions developed by members of the team. In addition to employing microgravity to augment the fundamental study of these forces, the resulting data will allow us to quantify and understand the ISS environment with great accuracy. This paper shows how we used both experiment and theory to identify and resolve critical issues and to produce an optimal experimental design that exploits microgravity for the study. We examined the response of particles of specific gravity from 0.1 to 20, with radii from 0.2 to 2mm, to fluid oscillation at frequencies up to 80Hz with amplitudes up to 200microns. To observe some of the interesting effects predicted by the new solutions requires the precise location of the position of a particle in three dimensions. To this end we have developed digital holography algorithms that enable particle position location to a small fraction of a pixel in a CCD array. The spaceflight system will record holograms both on film and electronically. The electronic holograms can be downlinked providing real-time data, essentially acting like a remote window into the ISS experimental chamber. Ground experiments have provided input to a night system design that can meet the requirements for a successful experiment on ISS. Moreover the ground experiments have provided a definitive, quantitative observation of the Basset history force over a wide range of conditions. Results of the ground experiments, the flight experiment design, preliminary night hardware design, and data analysis procedures are reported. C1 MetroLaser Inc, Res, Irvine, CA 92614 USA. Univ Calif Irvine, Irvine, CA USA. Univ Hawaii, Honolulu, HI 96822 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Trolinger, JD (reprint author), MetroLaser Inc, Res, 2572 White Rd, Irvine, CA 92614 USA. EM jtrolinger@metrolaserinc.com RI Coimbra, Carlos/A-3036-2008 NR 12 TC 3 Z9 3 U1 0 U2 1 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-563-X J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1027 BP 550 EP 566 DI 10.1196/annals.1324.042 PG 17 WC Biophysics; Mechanics; Multidisciplinary Sciences SC Biophysics; Mechanics; Science & Technology - Other Topics GA BBP91 UT WOS:000226975400041 PM 15644380 ER PT J AU DellaCorte, C AF DellaCorte, C TI Looking into the future SO TRIBOLOGY & LUBRICATION TECHNOLOGY LA English DT Editorial Material C1 NASA, Glenn Res Ctr, Cleveland, OH USA. RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. EM cdellacorte@stle.org NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS PI PARK RIDGE PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA SN 0024-7154 J9 TRIBOL LUBR TECHNOL JI Tribol. Lubr. Technol. PD JAN PY 2004 VL 60 IS 1 BP 8 EP 8 PG 1 WC Engineering, Mechanical SC Engineering GA 763DA UT WOS:000188056600002 ER PT S AU Hall, NR Mackey, JR Matula, TJ AF Hall, NR Mackey, JR Matula, TJ BE Batchelor, BG Hugli, H TI Sonoluminescence bubble measurements using vision-based algorithms SO TWO- AND THREE-DIMENSIONAL VISION SYSTEMS FOR INSPECTION, CONTROL, AND METROLOGY SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Two- and Three-Dimensional Vision Systems for Inspection, Control and Metrology CY OCT 29-30, 2003 CL Providence, RI SP SPIE DE sonolurninescence; bubble; machine vision; algorithms; centroid position ID SINGLE; LIGHT AB Vision-based measurement methods were used to measure bubble sizes in this sonoluminescence experiment. Bubble imaging was accomplished by placing the bubble between a bright light source and a microscope-CCD camera system. A collimated light-emitting diode was operated in a pulsed mode with an adjustable time delay with respect to the piezo-electric transducer drive signal. The light-emitting diode produced a bubble shadowgraph consisting of a multiple exposure made by numerous light pulses imaged onto a charge-couple device camera. Each image was transferred from the camera to a computer-controlled machine vision system via a frame grabber. The frame grabber was equipped with on-board memory to accommodate sequential image buffering while images were transferred to the host processor and analyzed. This configuration allowed the host computer to perform diameter measurements, centroid position measurements and shape estimation in "real-time" as the next image was being acquired. Bubble size measurement accuracy with an uncertainty of 3 microns was achieved using standard lenses and machine vision algorithms. Bubble centroid position accuracy was also within the 3 micron tolerance of the vision system. This uncertainty estimation accounted for the optical spatial resolution, digitization errors and the edge detection algorithm accuracy. The vision algorithms include camera calibration, thresholding, edge detection, edge position determination, distance between two edges computations and centroid position computations. C1 NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA. RP NASA, John H Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM nancy.r.hall@grc.nasa.gov; jeff.mackey@mkoptics.com; matula@apl.washington.edu NR 14 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5153-3 J9 PROC SPIE PY 2004 VL 5265 BP 90 EP 97 DI 10.1117/12.516150 PG 8 WC Computer Science, Artificial Intelligence; Instruments & Instrumentation; Optics SC Computer Science; Instruments & Instrumentation; Optics GA BY76S UT WOS:000189458100010 ER PT S AU Lavelle, JP Schuet, SR Schuet, DJ AF Lavelle, JP Schuet, SR Schuet, DJ BE Batchelor, BG Hugli, H TI High-speed 3D scanner with real-time 3D processing SO TWO- AND THREE-DIMENSIONAL VISION SYSTEMS FOR INSPECTION, CONTROL, AND METROLOGY SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Two- and Three-Dimensional Vision Systems for Inspection, Control and Metrology CY OCT 29-30, 2003 CL Providence, RI SP SPIE DE 3D Scanner; real time; laser triangulation AB A novel 3D sensing system with real-time 3D processing has been developed which is capable of scanning an object at very high speeds (greater than 500,000 3D points/second) and creating high-resolution 3D surface maps. Laser triangulation is used in conjunction with a high-resolution camera, a laser diode, and processing electronics all incorporated into a small sensor package that traverses linearly or rotates from a fixed position to scan an object. Processing is done on board the instrument and the resultant 3D data is transmitted to a PC. This results in rapid scans, with 3D images produced as the instrument is scanning. The sensing system was developed for the NASA Mars rover program and for the inspection of Shuttle Thermal Protection System (tiles), radiator, and structures. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lavelle, JP (reprint author), NASA, Ames Res Ctr, Code SFT, Moffett Field, CA 94035 USA. NR 4 TC 2 Z9 2 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5153-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5265 BP 179 EP 188 DI 10.1117/12.519660 PG 10 WC Computer Science, Artificial Intelligence; Instruments & Instrumentation; Optics SC Computer Science; Instruments & Instrumentation; Optics GA BY76S UT WOS:000189458100020 ER PT B AU Simpkins, P AF Simpkins, Patrick BE Kelly, TK Butz, WP Carroll, S Adamson, DM Bloom, G TI What data do STEM agency policymakers need? Workforce planning for the future: The NASA perspective SO U.S. SCIENFIFIC AND TECHNICAL WORKFORCE: IMPRIVING DATA FOR DECISIONMAKING SE RAND CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 140th Meeting of the National-Academy-of-Sciences CY APR 28, 2003 CL Washington, DC SP Nat Acad Sci C1 NASA, Management Syst Div, Informat Technol Syst Integrat Unit, Washington, DC 20546 USA. NR 9 TC 0 Z9 0 U1 1 U2 1 PU RAND PI SANTA MONICA PA PUBLICATIONS DEPT, 1700 MAIN ST PO BOX 2138, SANTA MONICA, CA 90407-2138 USA BN 0-8330-3651-3 J9 RAND CONF PROC PY 2004 BP 60 EP 68 PG 9 WC Industrial Relations & Labor; Public Administration SC Business & Economics; Public Administration GA BEV79 UT WOS:000239653900008 ER PT S AU Ning, CZ Li, J AF Ning, CZ Li, J BE Tsen, KT Song, JJ Jiang, HX TI Effects of collective excitations and scatterings in quantum well intersubband transitions SO ULTRAFAST PHENOMENA IN SEMICONDUCTORS AND NANOSTRUCTURE MATERIALS VIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Ultrafast Phenomena in Semiconductors and Nanostructure Materials VIII CY JAN 26-29, 2004 CL San Jose, CA SP SPIE DE intersubband transition; linewidth; electron scattering; phonon scattering; collective excitation; many-body effects; quantum wells; nanostructures ID INVERSION LAYERS; TEMPERATURE-DEPENDENCE; ABSORPTION LINEWIDTH; INTERFACE ROUGHNESS; GAAS; ACCUMULATION; DENSITY; SI; ENERGY; BAND AB Quantum well intersubband transitions display some of the most interesting many-body effects including various collective excitations, such as intersubband plasmon and Fermi-edge singularity (repellon). To describe these various excitations and to study the effects of scatterings on the intersubband lineshape, we have performed a systematic microscopic theoretical investigation of intersubband transitions. The theory leads to a set of intersubband semiconductor Bloch equations (ISBEs) at the first order of Coulomb interaction. The extension to include the second order Coulomb interaction and LO-phonon interaction leads to optical dephasing or linewidth broadening. Using this theory, we have studied systematically the interplay of collective excitations in quantum well intersubband transitions. Our results show that such interplay leads to dramatic changes in spectral features, such as absorption peak positions and lineshape, compared with a free-particle theory. We will also show that the typical usage of the dephasing rate approximation is generally invalid for intersubband transitions. There is a strong cancellation effects between the in- (off-diagonal) and out(diagonal) scattering terms at the second order and the out-scattering alone overestimates the linewidth significantly. Such a cancellation is much stronger for intersubband transitions than for interband case, because of the much smaller inhomogeneous broadening in the intersubband case. We also show that there is a cancellation of electron-electron and electron-phonon scatterings in their contributions to the linewidth. Finally we will show that our theory agrees very well with recent infrared absorption experiments. C1 NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Ning, CZ (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Mail Stop N229-1, Moffett Field, CA 94035 USA. NR 30 TC 2 Z9 2 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5260-2 J9 P SOC PHOTO-OPT INS PY 2004 VL 5352 BP 284 EP 298 DI 10.1117/12.529574 PG 15 WC Physics, Condensed Matter SC Physics GA BAL08 UT WOS:000222660600030 ER PT S AU Krotkov, NA Bhartia, PK Herman, JR Slusser, J Scott, G Labow, G Vasilkov, A Eck, T Dubovik, O Holben, B AF Krotkov, NA Bhartia, PK Herman, JR Slusser, J Scott, G Labow, G Vasilkov, A Eck, T Dubovik, O Holben, B BE Slusser, JR Herman, JR Gao, W Bernhard, G TI Measuring aerosol UV absorption optical thickness by combining use of shadowband and almucantar techniques SO ULTRAVIOLET GROUND- AND SPACE-BASED MEASUREMENTS, MODELS, AND EFFECTS IV SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Ultraviolet Ground- and Space-based Measurements, Models and Effects IV CY AUG 05-06, 2004 CL Denver, CO SP SPIE DE ultraviolet radiation; aerosol absorption; single scattering albedo; CIMEL sun photometer; AERONET network; UV multi-filter rotating shadow band radiometer; UV MFRSR; diffuse fraction measurements ID SINGLE-SCATTERING ALBEDO; SOLAR ULTRAVIOLET-RADIATION; PHOTOLYSIS RATE COEFFICIENT; SKY RADIANCE MEASUREMENTS; BIOMASS BURNING AEROSOLS; BAND RADIOMETER; GROUND ALBEDO; AERONET; SURFACE; DEPTH AB We report final results of an aerosol UV absorption closure experiment where a UV-shadow-band radiometer (UV-MFRSR, USDA UVB Monitoring and Research Network) and 4 rotating sun-sky radiometers (CIMEL. NASA AERONET network) were run side-by-side continuously for 17 months at NASA/GSFC site in Greenbelt, MD. The aerosol extinction optical thickness, Text, was measured by the CIMEL direct-sun technique in the visible and at two UV wavelengths 340 and 380 nm. These results were used for UV-MFRSR daily on-site calibration and 3-min measurements of tau(ext) at 325nm, 332nm and 368nm. The tau(ext) measurements were used as input to the radiative transfer model along with AERONET retrievals of the column-integrated particle size distribution (PSD) to infer an effective imaginary part of the UV aerosol refractive index, k, by fitting MFRSR measured voltage ratios. Using all cases for cloud-free days, we derive diurnal and seasonal dependence of the aerosol absorption optical thickness, tau(abs),, with an uncertainty 0.01-0.02. At our site tau(abs) follows pronounced seasonal dependence with maximum values similar to0.07 at 368nm (similar to0.15 at 325nm) occurring in summer hazy conditions and <0.02 in winter-fall seasons, when aerosol loadings are small. Inferred values of k allow calculation of the single scattering albedo, omega, in UVA and comparisons with AERONET almucantar omega(440) retrievals at 440nm. Overall, omega was slightly lower in UV than in the visible: case average =0.93 compared to =0.95. However, the differences (omega(440) - omega(368)> similar to0.02, rms difference similar to0.016) are smaller than uncertainties of both retrievals (deltaomegasimilar to0.03). Low values are consistent with higher values for imaginary refractive index, k: similar to0.01 compare to similar to0.006. However, mean differences in k(similar to0.004) were only slightly larger than AERONET retrieval uncertainty deltak similar to0.003(27). We also found that a) decreases with decrease in zero, suggesting different aerosol composition in summer and winter months. So far, our results do not allow explaining the causes of apparent larger aerosol absorption in UV. Continuing co-located measurements at GFSC is important to improve the comparison statistics, but conducting aerosol absorption measurements at different sites with varying conditions is also desirable. C1 NASA, Goddard Space Flight Ctr, GEST Ctr, Univ Maryland Baltimore Cty, Greenbelt, MD 20771 USA. RP Krotkov, NA (reprint author), NASA, Goddard Space Flight Ctr, GEST Ctr, Univ Maryland Baltimore Cty, Code 916, Greenbelt, MD 20771 USA. RI Dubovik, Oleg/A-8235-2009; ECK, THOMAS/D-7407-2012; Krotkov, Nickolay/E-1541-2012; Bhartia, Pawan/A-4209-2016; OI Dubovik, Oleg/0000-0003-3482-6460; Krotkov, Nickolay/0000-0001-6170-6750; Bhartia, Pawan/0000-0001-8307-9137; Herman, Jay/0000-0002-9146-1632 NR 41 TC 1 Z9 1 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5483-4 J9 P SOC PHOTO-OPT INS PY 2004 VL 5545 BP 17 EP 27 DI 10.1117/12.559557 PG 11 WC Instruments & Instrumentation SC Instruments & Instrumentation GA BBD68 UT WOS:000225039800003 ER PT S AU Ansar, A Huertas, A Matthies, LH Goldberg, S AF Ansar, A Huertas, A Matthies, LH Goldberg, S BE Gerhart, GR Shoemaker, CM Gage, DW TI Enhancement of stereo at range discontinuities SO UNMANNED GROUND VEHICLE TECHNOLOGY VI SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Unmanned Ground Vehicle Technology VI CY APR 13-15, 2004 CL Orlando, FL SP SPIE DE real-time stereo; stereo pre-process; edge-assisted stereo ID IMPLEMENTATION AB Stereo is a key component in many autonomous navigation tasks. These applications demand real-time performance and consequently, the state-of-the-art uses local correlation-based algorithms that lend themselves to algorithmic and hardware optimization. These systems perform well in simple terrain or on open ground. However, when discrete objects such as trees are present in the scene, correlation-based approaches exhibit inherent difficulties. Some of these difficulties are introduced during the preprocessing stage that attempts to compensate for photometric variations between the cameras. Other difficulties occur during the correlation stage due to occlusion. As a result, object portions appear enlarged, contracted, or missing, as the range data bleeds between the foreground object and the background. This complicates subsequent obstacle detection, representation and modeling. These problems have been addressed by more sophisticated stereo algorithms based on energy minimization and global optimization schemes. Such complex algorithms, however, are computationally demanding and not amenable to real-time implementation. Our solution uses a better preprocessing method, intelligent use of edge cues, and a variation of the traditional shiftable window approach to enhance the stereo correlation at and near depth discontinuities. There is additional computational overhead involved, but we are able to maintain real-time performance. We present details of our new algorithm and several results in complex natural environments. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP CALTECH, Jet Propuls Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. NR 16 TC 2 Z9 2 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5345-5 J9 PROC SPIE PY 2004 VL 5422 BP 24 EP 35 DI 10.1117/12.547774 PG 12 WC Automation & Control Systems; Robotics; Transportation Science & Technology SC Automation & Control Systems; Robotics; Transportation GA BAX98 UT WOS:000224151200003 ER PT S AU Solecki, WD Rosenzweig, C AF Solecki, WD Rosenzweig, C BE AlfsenNorodom, C Lane, BD Corry, M TI Biodiversity, biosphere reserves, and the big apple - A study of the New York Metropolitan Region SO URBAN BIOSPHERE AND SOCIETY: PARTNERSHIP OF CITIES SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Urban Biosphere and Society - Partnership of Cities CY OCT 29-30, 2003 CL New York Acad Sci, New York, NY SP Columbia Univ, Earth Inst, UNESCO HO New York Acad Sci DE urban biodiversity; biosphere reserve; New York Metropolitan Region; environmental change; ecological footprint AB The objectives of this article were to assess the dimensions of biodiversity-urban society interactions within the New York Metropolitan Region, a 31-county area with a population of 21.5 million, and to explore pathways to reconcile dysfunctional relationships between these two ever-entwined systems. The article builds on the premise that urban biodiversity exists at a crucial nexus of ecological and societal interactions, linking local, regional, and global scales, and that urban ecologies are projected to become even more dynamic in the future, particularly as a result of global climate change. The pathway proposed to reconcile the biodiversity-urban society relationships is the incorporation of biosphere reserve strategies into regional environmental planning efforts focused on the New York/New Jersey Harbor/Estuary specifically and on the greater New York Metropolitan Region in general. The concepts of the "ecological footprint" and vulnerability to global environmental change are used to analyze the current interactions between biodiversity and urban society, and to evaluate the efficacy of adopting biosphere reserve strategies in the region. New York has long been at the forefront of American environmentalism and landscape planning. Coupled with this history is a still small but growing interest in regional environmental planning efforts (e.g., the U.S. EPA Harbor Estuary Program) and green infrastructure (e.g., the 2002 Humane Metropolis Conference organized by the Ecological Cities Project). The research presented here aims to contribute to these nascent activities. As a megacity, New York may serve as a model for other major cities of the world. C1 CUNY Hunter Coll, Dept Geog, New York, NY 10021 USA. Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY USA. RP Solecki, WD (reprint author), CUNY Hunter Coll, Dept Geog, 695 Pk Ave, New York, NY 10021 USA. EM wsolecki@hunter.cuny.edu NR 29 TC 9 Z9 11 U1 3 U2 37 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-553-2 J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1023 BP 105 EP 124 DI 10.1196/annals.1319.004 PG 20 WC Environmental Sciences; Environmental Studies; Multidisciplinary Sciences; Urban Studies SC Environmental Sciences & Ecology; Science & Technology - Other Topics; Urban Studies GA BAN79 UT WOS:000223006800006 PM 15253901 ER PT S AU Alfsen-Norodom, C Boehme, SE Clemants, S Corry, M Imbruce, V Lane, BD Miller, RB Padoch, C Panero, M Peters, CM Rosenzweig, C Solecki, W Walsh, D AF Alfsen-Norodom, C Boehme, SE Clemants, S Corry, M Imbruce, V Lane, BD Miller, RB Padoch, C Panero, M Peters, CM Rosenzweig, C Solecki, W Walsh, D BE AlfsenNorodom, C Lane, BD Corry, M TI Managing the megacity for global sustainability - The New York Metropolitan Region as an urban biosphere reserve SO URBAN BIOSPHERE AND SOCIETY: PARTNERSHIP OF CITIES SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Urban Biosphere and Society - Partnership of Cities CY OCT 29-30, 2003 CL New York Acad Sci, New York, NY SP Columbia Univ, Earth Inst, UNESCO HO New York Acad Sci DE biosphere reserves; world network of biosphere reserves; urban ecosystems; industrial ecology; ecological footprint; urban agriculture; megacities; environmental governance AB The UNESCO World Network of Biosphere Reserves (WNBR), while not originally conceived to include urban areas, was intended to include sites representing all significant ecosystems with the goal of support for sustainable development locally and globally. Drawing on the example of the New York Metropolitan Region (NYMR), which has a population of 21.4 million, it is argued here that the eventual inclusion of the largest of the world's cities in WNBR not only is within the logic of the biosphere reserve concept, but would also benefit the network and its goals. The ecological significance of the NYMR, its role as a driver for global environmental change, as well as the efforts under way in the city to improve urban environmental management and governance are all examined. Potential added value to the WNBR of including megacities such as the NYMR is considered, in particular, regarding the sharing of best practices, lessons learned, and the strengthening of links between megacities and their global natural resource bases. C1 Columbia Univ, Earth Inst, CUBES, Columbia Univ UNESCO Joint Program Biosphere & Soc, New York, NY 10027 USA. New York Acad Sci, Harbor Project, New York, NY USA. Brooklyn Bot Garden, Brooklyn, NY USA. New York Bot Garden, New York, NY USA. Columbia Univ, CIESIN, New York, NY USA. Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY USA. CUNY Hunter Coll, Dept Geog, New York, NY 10021 USA. RP Lane, BD (reprint author), Columbia Univ, Earth Inst, CUBES, Columbia Univ UNESCO Joint Program Biosphere & Soc, 2910 Broadway,Hogan Hall B-16, New York, NY 10027 USA. EM ben2002@columbia.edu; ben2002@columbia.edu NR 25 TC 5 Z9 6 U1 2 U2 31 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-553-2 J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2004 VL 1023 BP 125 EP 141 DI 10.1196/annals.1319.005 PG 17 WC Environmental Sciences; Environmental Studies; Multidisciplinary Sciences; Urban Studies SC Environmental Sciences & Ecology; Science & Technology - Other Topics; Urban Studies GA BAN79 UT WOS:000223006800007 PM 15253902 ER PT B AU Potsdam, MA Silva, MJ AF Potsdam, MA Silva, MJ GP ieee computer society TI Tilt rotor aeromechanics phenomena in low speed flight SO USERS GROUP CONFERENCE, PROCEEDINGS LA English DT Proceedings Paper CT Users Group Conference CY JUN 07-11, 2004 CL Williamsburg, VA SP User Advocacy Grp, HPCMPO Outreach Team AB This work investigates important aeromechanics phenomena affecting the V-22 tilt rotor in low speed sideward flight or while hovering in quartering or crosswind conditions. These phenomena, such as pitch-up with sideslip and increased power required in sideward flight, were identified during V-22 critical azimuth flight testing and impacted handling qualities in this flight regime. High fidelity, dynamic, unsteady, Navier-Stokes computational fluid dynamics (CFD) calculations are presented and compared with flight test data CFD predicts the flight test trends as a function of wind direction, in good agreement with data. Detailed investigation clearly shows the interaction of the rotor wake with the airframe as the major cause of the aeromechanics phenomena seen on the V-22. Identification of the underlying flow field physics allows investigation of options for alleviation anti prediction of future tilt rotor configurations. C1 NASA, Rotorcraft Div, USA, AMRDEC,Aeroflightdynam Directorate, Moffett Field, CA USA. RP Potsdam, MA (reprint author), NASA, Rotorcraft Div, USA, AMRDEC,Aeroflightdynam Directorate, Moffett Field, CA USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2259-9 PY 2004 BP 151 EP 157 PG 7 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering; Engineering, Electrical & Electronic; Mechanics SC Computer Science; Engineering; Mechanics GA BBP31 UT WOS:000226863200022 ER PT S AU Weisskopf, MC AF Weisskopf, MC BE Hasinger, G Turner, MJL TI Five years of operation of the Chandra X-ray Observatory SO UV AND GAMMA-RAY SPACE TELESCOPE SYSTEMS, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on UV and Gamma-Ray Space Telescope Systems CY JUN 21-24, 2004 CL Glasgow, SCOTLAND SP SPIE DE X-ray imaging; grazing-incidence optics; X-ray astronomy ID CRAB-NEBULA; GALAXY; CLUSTER; DISCOVERY; EMISSION; BINARY; LETGS; FIELD AB The on-orbit performance of the Chandra X-ray Observatory over its first five years of operation is reviewed. The Observatory is naming smoothly and the scientific return continues to be outstanding. C1 NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Greenbelt, MD 20771 USA. RP Weisskopf, MC (reprint author), NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Greenbelt, MD 20771 USA. NR 30 TC 6 Z9 6 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5420-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5488 BP 25 EP 39 DI 10.1117/12.561489 PN 1-2 PG 15 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA BBD21 UT WOS:000224987100003 ER PT S AU Content, D Colella, D Hadjimichael, T Lehan, JP McMann, J Reid, P Saha, T Zhang, W AF Content, D Colella, D Hadjimichael, T Lehan, JP McMann, J Reid, P Saha, T Zhang, W BE Hasinger, G Turner, MJL TI Optical metrology for the segmented optics on the Constellation-X Spectroscopy X-ray telescope SO UV AND GAMMA-RAY SPACE TELESCOPE SYSTEMS, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on UV and Gamma-Ray Space Telescope Systems CY JUN 21-24, 2004 CL Glasgow, SCOTLAND SP SPIE DE optical metrology; x-ray optics; constellation-X AB We present the metrology requirements and metrology implementation necessary to optically characterize the reflector technology for the Constellation-X (C-X) spectroscopy x-ray telescope (SXT). This segmented, 1.6m diameter highly nested telescope presents many metrology and alignment challenges. In particular, these mirrors have a stringent imaging error budget as compared to their intrinsic stiffness. The low stiffness is seen to be implied by the required effective area and the required weight. The low mirror stiffness has implications for the metrology that can be used. A variety of contact and non-contact optical profiling and interferometric methods are combined to test the formed glass substrates before replication and the replicated reflector segments. The reflectors are tested both stand-alone and in-situ in an alignment tower. Some of these methods have not been used on prior x-ray telescopes and some are feasible only because of the segmented approach used on the SXT. Methods to be discussed include high precision coordinate measurement machines using very low force or optical probes, axial interferometric profiling, azimuthal circularity profiling, and use of advanced null optics such as conical computer generated hologram (CGHs). C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Content, D (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 13 TC 6 Z9 6 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5420-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5488 BP 272 EP 282 DI 10.1117/12.553231 PN 1-2 PG 11 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA BBD21 UT WOS:000224987100026 ER PT S AU White, NE Tananbaum, H Weaver, K Petre, R Bookbinder, J AF White, NE Tananbaum, H Weaver, K Petre, R Bookbinder, J BE Hasinger, G Turner, MJL TI The science goals of the Constellation-X mission SO UV AND GAMMA-RAY SPACE TELESCOPE SYSTEMS, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on UV and Gamma-Ray Space Telescope Systems CY JUN 21-24, 2004 CL Glasgow, SCOTLAND SP SPIE DE observatories; X-rays; spectroscopy; dark energy; black holes ID BLACK-HOLE; ACCRETION; LINES AB The Constellation-X mission will address the questions: "What happens to matter close to a black hole?" and "What is Dark Energy?" These questions are central to the NASA Beyond Einstein Program, where Constellation-X plays a central role. The mission will address these questions by using high throughput X-ray spectroscopy to observe the effects of strong gravity close to the event horizon of black holes, and to observe the formation and evolution of clusters of galaxies in order to precisely determine Cosmological parameters. To achieve these primary science goals requires a factor of 25-100 increase in sensitivity for high resolution spectroscopy. The mission will also perform routine high-resolution X-ray spectroscopy of faint and extended X-ray source populations. This will provide diagnostic information such as density, elemental abundances, velocity, and ionization state for a wide range of astrophysical problems. This has enormous potential for the discovery of new unexpected phenomena. The Constellation-X mission is a high priority in the National Academy of Sciences McKee-Taylor Astronomy and Astrophysics Survey of new Astrophysics Facilities for the first decade of the 21st century. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP White, NE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI White, Nicholas/B-6428-2012 OI White, Nicholas/0000-0003-3853-3462 NR 8 TC 6 Z9 6 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5420-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5488 BP 382 EP 387 DI 10.1117/12.550799 PN 1-2 PG 6 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA BBD21 UT WOS:000224987100037 ER PT S AU Gendreau, K Cash, W Gorenstein, P Windt, D Kaaret, P Reynolds, C AF Gendreau, K Cash, W Gorenstein, P Windt, D Kaaret, P Reynolds, C BE Hasinger, G Turner, MJL TI MAXIM: The black hole imager SO UV AND GAMMA-RAY SPACE TELESCOPE SYSTEMS, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on UV and Gamma-Ray Space Telescope Systems CY JUN 21-24, 2004 CL Glasgow, SCOTLAND SP SPIE DE X-rays; interferometry; X-ray astronomy; X-ray optics; grazing incidence optics ID HIGH-ENERGY ASTRONOMY; OPTICS; INTERFEROMETER; TELESCOPE AB The Beyond Einstein Program in NASA's Office of Space Science Structure and Evolution of the Universe theme spells out the top level scientific requirements for a Black Hole Imager in its strategic plan. The MAXIM mission will provide better than one tenth of a microarcsecond imaging in the X-ray band in order to satisfy these requirements. We will overview the driving requirements to achieve these goals and ultimately resolve the event horizon of a supermassive black hole. We will present the current status of this effort that includes a study of a baseline design as well as two alternative approaches. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gendreau, K (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 16 TC 7 Z9 7 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5420-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5488 BP 394 EP 402 DI 10.1117/12.551250 PN 1-2 PG 9 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA BBD21 UT WOS:000224987100039 ER PT S AU Petre, R Content, D Lehan, J O'Dell, S Owens, S Podgorsky, W Stewart, J Zhang, W AF Petre, R Content, D Lehan, J O'Dell, S Owens, S Podgorsky, W Stewart, J Zhang, W BE Hasinger, G Turner, MJL TI The Constellation-X Spectroscopy X-ray Telescope SO UV AND GAMMA-RAY SPACE TELESCOPE SYSTEMS, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on UV and Gamma-Ray Space Telescope Systems CY JUN 21-24, 2004 CL Glasgow, SCOTLAND SP SPIE DE X-ray mirrors; constellation-X ID ALIGNMENT; SXT AB The status of technology development for the Constellation-X Spectroscopy X-ray Telescope (SXT) mirror is presented. The SXT mirror combines a large (1.6 in) aperture with modest (12 arc see half power diameter) angular resolution and low mass (750 kg). The overall collecting area, larger than 9,600 square cm at 0.25 keV, requires high throughput, and thus nesting of a substantial number of thin reflectors. A phased development program is underway to develop reflectors, mounting and alignment approaches, and metrology techniques for components and the mirror has a whole. The latest results in all these areas are summarized, along with an overview of results of optical testing of reflector performance. C1 NASA, Goddard Space Flight Ctr, Xray Astrophys Branch, Greenbelt, MD 20771 USA. RP Petre, R (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Branch, Code 662, Greenbelt, MD 20771 USA. OI O'Dell, Stephen/0000-0002-1868-8056 NR 8 TC 5 Z9 5 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5420-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5488 BP 505 EP 514 DI 10.1117/12.552062 PN 1-2 PG 10 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA BBD21 UT WOS:000224987100050 ER PT S AU Leitch, JW Lieber, MD Gallagher, DJ Gendreau, KC Cash, WC Shipley, AF AF Leitch, JW Lieber, MD Gallagher, DJ Gendreau, KC Cash, WC Shipley, AF BE Hasinger, G Turner, MJL TI System performance model and error budget for MAXIM SO UV AND GAMMA-RAY SPACE TELESCOPE SYSTEMS, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on UV and Gamma-Ray Space Telescope Systems CY JUN 21-24, 2004 CL Glasgow, SCOTLAND SP SPIE DE grazing incidence; MAXIM; error budget; tolerance; x-ray; wavefront error AB The proposed Micro-Arcsecond X-ray Imaging Mission (MAXIM) uses an array of spacecraft containing grazing incidence optics to create and acquire an image on a distant detector spacecraft. Among the technical challenges facing the mission, maintaining an acceptably small wavefront error in the optical system is addressed in this paper. Starting with a performance model for the observatory and both analytically- and raytrace-based optical sensitivities to misalignment and figure error, an error budget is constructed that includes the effects of the individual optical surfaces, the alignment of the optical elements within the 4-mirror periscope sub-assemblies, and the relative alignment of the many periscopes that make up the MAXIM optical imaging system. At this stage of conceptual development, the allocations to different sub-systems that affect wavefront error is based on the philosophy of "spreading the pain" associated with performance requirements of the contributing elements. The performance model and error budget become tools with which to explore different architectures and requirements allocations as the mission concept develops. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Leitch, JW (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. NR 6 TC 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5420-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5488 BP 593 EP 600 DI 10.1117/12.552358 PN 1-2 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA BBD21 UT WOS:000224987100058 ER PT S AU Thomas, RJ AF Thomas, RJ BE Hasinger, G Turner, MJL TI Elliptical varied line-space (EVLS) gratings SO UV AND GAMMA-RAY SPACE TELESCOPE SYSTEMS, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on UV and Gamma-Ray Space Telescope Systems CY JUN 21-24, 2004 CL Glasgow, SCOTLAND SP SPIE DE UV; EUV; stigmatic; imaging spectrograph; varied line-space; aspheric grating; optical design AB Imaging spectroscopy at wavelengths below 2000 Angstrom offers an especially powerful method for studying many extended high-temperature astronomical objects, like the Sun and its outer layers. But the technology to make such measurements is also especially challenging, because of the poor reflectance of all standard materials at these wavelengths, and because the observations must be made from above the absorbing effects of the Earth's atmosphere. To solve these problems, single-reflection stigmatic spectrographs for XUV wavelengths have been flown on several space missions based on designs with toroidal uniform line-space (TULS) or spherical varied line-space (SVLS) gratings that operate at near normal-incidence. More recently, three solar EUV/UV instruments have been selected that use toroidal varied line-space (TVLS) gratings; these are SUMI and RAISE, both sounding rocket payloads, and NEXUS, a SMEX satellite-mission. The next logical extension to such designs is the use of elliptical surfaces for varied line-space (EVLS) rulings. In fact, EVLS designs are found to provide superior imaging even at very large spectrograph magnifications and beam-speeds, permitting extremely high-quality performance in remarkably compact instrument packages. In some cases, such designs may be optimized even further by using a hyperbolic surface for the feeding telescope. The optical characteristics of two solar EUV spectrometers based on these concepts are described: EUS and EUI, both being developed as possible instruments for ESA's Solar Orbiter mission by consortia led by RAL and by MSSL, respectively. C1 NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. RP Thomas, RJ (reprint author), NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Code 661, Greenbelt, MD 20771 USA. NR 4 TC 0 Z9 0 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5420-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5488 BP 755 EP 762 DI 10.1117/12.552131 PN 1-2 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA BBD21 UT WOS:000224987100075 ER PT S AU Walyus, KD Pepe, J Prior, M AF Walyus, KD Pepe, J Prior, M BE Hasinger, G Turner, MJL TI Life extension activities for the hubble space telescope SO UV AND GAMMA-RAY SPACE TELESCOPE SYSTEMS, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on UV and Gamma-Ray Space Telescope Systems CY JUN 21-24, 2004 CL Glasgow, SCOTLAND SP SPIE AB Without an additional Hubble Space Telescope (HST) Servicing Mission (SM4), the HST Project will face numerous challenges to keep the telescope operating for as long as possible. As part of SM4, the HST Project planned to install various upgrades to the telescope including the installation of new batteries and new rate integrating gyros. Without these upgrades, reliability analyses and trend projections indicate that the spacecraft will lose the capability to conduct science operations later this decade. The HST team is being challenged to maximize the telescope's remaining operational lifetime, and also maximize its science output and quality. The two biggest areas of concern are the age and condition of the batteries and gyros. Together they comprise the largest risk to telescope productivity and safety and present the biggest challenges to the HST team. The six nickel-hydrogen (NiH2) batteries on HST are the original batteries from launch. With fourteen years of operational fife, these batteries have lasted longer than those on any comparable mission. Yet as with all batteries, their capacity has been declining. Engineers are examining various methods to prolong the life of these mission critical batteries, and retard the rate of degradation. In addition to the batteries, the National Aeronautics and Space Administration (NASA) scheduled all six gyros to be replaced on SM4. Two of the six gyros have already failed, leaving four available for operational use. To be able to conduct science operations, the telescope currently needs three gyros. Efforts are underway to enable a guiding mode that will require only two gyros. In this mode, however, science target scheduling will be strongly driven by new factors (such as star tracker availability), which may ultimately reduce science gathering efficiency. The status on this effort and its potential impact on science operations will be discussed. This paper will focus on these and other efforts to prolong the life of the HST, thus enabling it to remain a world-class observatory for as long as possible. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Walyus, KD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5420-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5488 BP 781 EP 788 DI 10.1117/12.551953 PN 1-2 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA BBD21 UT WOS:000224987100078 ER PT S AU West, EA Porter, JG Davis, JM Gary, GA Noble, MW Lewis, M Thomas, RJ AF West, EA Porter, JG Davis, JM Gary, GA Noble, MW Lewis, M Thomas, RJ BE Hasinger, G Turner, MJL TI The Marshall Space Flight Center solar ultraviolet magnetograph SO UV AND GAMMA-RAY SPACE TELESCOPE SYSTEMS, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on UV and Gamma-Ray Space Telescope Systems CY JUN 21-24, 2004 CL Glasgow, SCOTLAND SP SPIE ID LINE; GRATINGS; REGION AB This paper will describe the objectives of the Marshall Space Flight Center (MSFC) Solar Ultraviolet Magnetograph Investigation (SUMI) and the optical components that have been developed to meet those objectives. In order to test the scientific feasibility of measuring magnetic fields in the UV, a sounding rocket payload is being developed. This paper will discuss: (1) the scientific measurements that will be made by the SUMI sounding rocket program, (2) how the optics have been optimized for simultaneous measurements of two magnetic lines CIV (1550Angstrom) and MgII (2800Angstrom), and (3) the optical, reflectance, transmission and polarization measurements that have been made on the SUMI telescope mirrors and polarimeter. C1 NASA, George C Marshall Space Flight Ctr, NSSTC, Greenbelt, MD 20771 USA. RP West, EA (reprint author), NASA, George C Marshall Space Flight Ctr, NSSTC, Greenbelt, MD 20771 USA. NR 12 TC 8 Z9 8 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5420-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5488 BP 801 EP 812 DI 10.1117/12.563524 PN 1-2 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA BBD21 UT WOS:000224987100080 ER PT S AU Zhang, WW Content, DA Henderson, SJ Lehan, JP Petre, R Saha, TT AF Zhang, WW Content, DA Henderson, SJ Lehan, JP Petre, R Saha, TT BE Hasinger, G Turner, MJL TI Development of lightweight X-ray mirrors for the constellation-X mission SO UV AND GAMMA-RAY SPACE TELESCOPE SYSTEMS, PTS 1 AND 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on UV and Gamma-Ray Space Telescope Systems CY JUN 21-24, 2004 CL Glasgow, SCOTLAND SP SPIE DE X-ray optics; lightweight optics; Constellation-X AB Constellation-X is NASA's next major X-ray astronomical observatory. Its salient features are its very large effective X-ray collecting area (about 30,000 cm(2) at 1 keV) and high resolution gratings and cryogenic detector systems. The large mirror effective area presents unique and unprecedented challenges in optical fabrication and metrology. In this paper we report on the development of very lightweight X-ray mirrors that address these challenges. We use a two-step mirror fabrication process: (1) slumping thin (0.4mm) flat glass sheets to generate high quality substrates that may have mid-frequency figure errors, and (2) reducing or eliminating the mid-frequency errors using an epoxy replication process. We discuss problems and the potential associated with each of these two steps. Based on our work to date, we expect that this technology to be able to meet the baseline Constellation-X requirements, Le, 15" HPD (half-power diameter) at the observatory level. In the next few years, we will further advance this technology and expect it to reach the Constellation-X goal: 5" HPD at the observatory level. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zhang, WW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. OI O'Dell, Stephen/0000-0002-1868-8056 NR 5 TC 18 Z9 18 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5420-6 J9 P SOC PHOTO-OPT INS PY 2004 VL 5488 BP 820 EP 828 DI 10.1117/12.552250 PN 1-2 PG 9 WC Engineering, Aerospace; Instruments & Instrumentation; Optics SC Engineering; Instruments & Instrumentation; Optics GA BBD21 UT WOS:000224987100082 ER PT S AU Artho, C Havelund, K AF Artho, C Havelund, K BE Steffen, B Levi, G TI Applying Jlint to space exploration software SO VERIFICATION, MODEL CHECKING, AND ABSTRACT INTERPRETATION, PROCEEDINGS SE Lecture Notes in Computer Science LA English DT Article; Proceedings Paper CT 5th International Conference on Verification, Model Checking and Abstract Interpretation CY JAN 11-13, 2004 CL VENICE, ITALY SP Ca Foscari Univ, Dept Comp Sci, ACM, EAPLS ID JAVA PROGRAMS/; MODEL-CHECKING AB yJava is a very successful programming language which is also becoming widespread in embedded systems, where software correctness is critical. flint is a simple but highly efficient static analyzer that checks a Java program for several common errors, such as null pointer exceptions, and overflow errors. It also includes checks for multi-threading problems, such as deadlocks and data races. The case study described here shows the effectiveness of Jlint in finding certain faults, including multi-threading problems. Analyzing the reasons for false positives in the multi-threading warnings gives an insight into design patterns commonly used in multi-threaded code. The results show that a few analysis techniques are sufficient to avoid almost all false positives. These techniques include investigating all possible callers and a few code idioms. Verifying the correct application of these patterns is still crucial, because their correct usage is not trivial. C1 ETH, Inst Comp Syst, Zurich, Switzerland. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP ETH, Inst Comp Syst, Zurich, Switzerland. NR 23 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-20803-8 J9 LECT NOTES COMPUT SC PY 2004 VL 2937 BP 297 EP 308 PG 12 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BY43B UT WOS:000189213100023 ER PT S AU Hines, G Rahman, ZU Jobson, D Woodell, G AF Hines, G Rahman, ZU Jobson, D Woodell, G BE Rahman, ZU Schowengerdt, RA Reichenbach, SE TI DSP implementation of the retinex image enhancement algorithm SO VISUAL INFORMATION PROCESSING XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Visual Information Processing XIII CY APR 15-16, 2004 CL Orlando, FL SP SPIE DE image enhancement; digital signal processing; retinex AB The Retinex is a general-purpose image enhancement algorithm that is used to produce good visual representations of scenes. It performs a non-linear spatial/spectral transform that synthesizes strong local contrast enhancement and color constancy. A real-time, video frame rate implementation of the Retinex is required to meet the needs of various potential users. Retinex processing contains a relatively large number of complex computations, thus to achieve real-time performance using current technologies requires specialized hardware and software. In this paper we discuss the design and development of a digital signal processor (DSP) implementation of the Retinex. The target processor is a Texas Instruments TMS320C6711 floating point DSP. NTSC video is captured using a dedicated frame-grabber card, Retinex processed, and displayed on a standard monitor. We discuss the optimizations used to achieve real-time performance of the Retinex and also describe our future plans on using alternative architectures. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Hines, G (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 20 TC 14 Z9 14 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5361-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5438 BP 13 EP 24 DI 10.1117/12.544500 PG 12 WC Imaging Science & Photographic Technology SC Imaging Science & Photographic Technology GA BAS06 UT WOS:000223341800002 ER PT S AU Jobson, DJ Rahman, ZU Woodell, GA Hines, GD AF Jobson, DJ Rahman, ZU Woodell, GA Hines, GD BE Rahman, ZU Schowengerdt, RA Reichenbach, SE TI Automatic assessment and reduction of noise using edge pattern analysis in non-linear image enhancement SO VISUAL INFORMATION PROCESSING XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Visual Information Processing XIII CY APR 15-16, 2004 CL Orlando, FL SP SPIE ID VISUAL-CORTEX; RETINEX; MONKEY AB Noise is the primary visibility limit in the process of non-linear image enhancement, and is no longer a statistically stable additive noise in the post-enhancement image. Therefore novel approaches are needed to both assess and reduce spatially variable noise at this stage in overall image processing. Here we will examine the use of edge pattern analysis both for automatic assessment of spatially variable noise and as a foundation for new noise reduction methods. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Jobson, DJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 8 TC 2 Z9 2 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5361-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5438 BP 141 EP 149 DI 10.1117/12.539786 PG 9 WC Imaging Science & Photographic Technology SC Imaging Science & Photographic Technology GA BAS06 UT WOS:000223341800015 ER PT B AU Divsalar, D Dolinar, S Thorpe, J AF Divsalar, D Dolinar, S Thorpe, J GP IEEE TI Accumulate-Repeat-Accumulate-Accumulate-codes SO VTC2004-FALL: 2004 IEEE 60TH VEHICULAR TECHNOLOGY CONFERENCE, VOLS 1-7: WIRELESS TECHNOLOGIES FOR GLOBAL SECURITY LA English DT Proceedings Paper CT 60th IEEE Vehicular Technology Conference CY SEP 26-29, 2004 CL Los Angeles, CA SP IEEE Vehicular Technol Soc, Aerosp Corp, Cisco Syst, Motorola, Raytheon, TaconicElektrobit, Qualcomm, Wiley ID DESIGN AB Inspired by recently proposed Accumulate-RepeatAccumulate (ARA) codes [15], in this paper we propose a channel coding scheme called Accumulate-Repeat-Accumulate-Accumulate (ARAA) codes. These codes can he seen as serial turbo-like codes or as a subclass of Low Density Parity Check (LDPC) codes, and they have a projected graph or protograph representation; this allows for a high-speed iterative decoder implementation using belief propagation. An ARAA code can be viewed as a precoded Repeat-and-Accumulate (RA) code with puncturing in concatenation with another accumulator, where simply an accumulator is chosen as the precoder; thus ARAA codes have a very fast encoder structure. Using density evolution on their associated protographs, we find examples of rate-1/2 ARAA codes with maximum variable node degree 4 for which a minimum bit-SNR as low as 0.21 dB from the channel capacity limit can be achieved as the block size goes to infinity. Such a low threshold cannot be achieved by RA or Irregular RA (IRA) or unstructured irregular LDPC codes with the same constraint on the maximum variable node degree. Furthermore by puncturing the accumulators we can construct families of higher rate ARAA codes with thresholds that stay close to their respective channel capacity thresholds uniformly. Iterative decoding simulation results show comparable performance with the best-known LDPC codes but with very low error floor even at moderate block sizes. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Divsalar, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-8521-7 PY 2004 BP 2292 EP 2296 PG 5 WC Telecommunications SC Telecommunications GA BBU82 UT WOS:000227931902158 ER PT S AU Atlas, R AF Atlas, R BE VonderHaar, TH Huang, HLA TI Impact of satellite surface-wind data on weather prediction SO WEATHER AND ENVIRONMENTAL SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Weather and Environmental Satellites CY AUG 02-03, 2004 CL Denver, CO SP SPIE, Colorado Photon Ind Assoc AB One of the important applications of satellite surface wind observations is to increase the accuracy of weather analyses and forecasts. The first satellite to measure surface wind over the oceans was Seasat in 1978. On board was a scatterometer, which measured radar backscatter from centimeter-scale capillary waves, from which surface wind speed and direction could be deduced. In more recent years, passive microwave remote sensing of the ocean surface has provided extensive observations of surface wind speed, and advanced scatterometers have been providing surface wind velocity data over the oceans. The initial impact of satellite surface wind data on weather analysis and forecasting was very small, but extensive research has been conducted since the early days of Seasat to improve the data accuracy and the utilization of these data in atmospheric models. Current satellite surface wind data are used to improve the detection of intense storms over the ocean, as well as to improve the overall representation of the wind field in numerical weather prediction models. As a result, these data are contributing to improved warnings for ships at sea and to improved global weather forecasts. Recent experiments conducted with data from the SeaWinds scatterometers aboard both Quikscat and ADEOS 2 indicate that increased coverage of scatterometer data can lead to even larger impacts than are routinely obtained now. C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Atlas, R (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 910, Greenbelt, MD 20771 USA. RI Vonder Haar, Thomas/F-2048-2011 NR 1 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5487-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5549 BP 134 EP 144 DI 10.1117/12.558447 PG 11 WC Engineering, Aerospace; Environmental Sciences; Meteorology & Atmospheric Sciences; Remote Sensing SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences; Remote Sensing GA BBC32 UT WOS:000224730100015 ER PT S AU Minnis, P Smith, WL Nguyen, L Spangenberg, DA Heck, PW Palikonda, R Ayers, JK Wolff, C Murray, JJ AF Minnis, P Smith, WL Nguyen, L Spangenberg, DA Heck, PW Palikonda, R Ayers, JK Wolff, C Murray, JJ BE VonderHaar, TH Huang, HLA TI Near-real time cloud properties and aircraft icing indices from GEO and LEO satellites SO WEATHER AND ENVIRONMENTAL SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Weather and Environmental Satellites CY AUG 02-03, 2004 CL Denver, CO SP SPIE, Colorado Photon Ind Assoc DE aircraft icing; clouds; remote sensing; cloud microphysics; GOES; MODIS; AVHRR; air safety AB Imagers on many of the current and future operational meteorological satellites in geostationary Earth orbit (GEO) and lower Earth orbit (LEO) have enough spectral channels to derive cloud microphysical properties useful for a variety of applications. The products include cloud amount, phase, optical depth, temperature, height and pressure, thickness, effective particle size, and ice or liquid water path, shortwave albedo, and outgoing longwave radiation for each imager pixel. Because aircraft icing depends on cloud temperature, droplet size, and liquid water content as well as aircraft variables, it is possible to estimate the potential icing conditions from the cloud phase, temperature, effective droplet size, and liquid water path. A prototype icing index is currently being derived over the contiguous USA in near-real time from Geostationary Operational Environmental Satellite (GOES-10 and 12) data on a half-hourly basis and from NOAA-16 Advanced Very High Resolution (AVHRR) data when available. Because the threshold-based algorithm is sensitive to small errors and differences in satellite imager and icing is complex process, a new probability based icing diagnosis technique is developed from a limited set of pilot reports. The algorithm produces reasonable patterns of icing probability and intensities when compared with independent model and pilot report data. Methods are discussed for improving the technique for incorporation into operational icing products.Imagers on many of the current and future operational meteorological satellites in geostationary Earth orbit (GEO) and lower Earth orbit (LEO) have enough spectral channels to derive cloud microphysical properties useful for a variety of applications. The products include cloud amount, phase, optical depth, temperature, height and pressure, thickness, effective particle size, and ice or liquid water path, shortwave albedo, and outgoing longwave radiation for each imager pixel. Because aircraft icing depends on cloud temperature, droplet size, and liquid water content as well as aircraft variables, it is possible to estimate the potential icing conditions from the cloud phase, temperature, effective droplet size, and liquid water path. A prototype icing index is currently being derived over the contiguous USA in near-real time from Geostationary Operational Environmental Satellite (GOES-10 and 12) data on a half-hourly basis and from NOAA-16 Advanced Very High Resolution (AVHRR) data when available. Because the threshold-based algorithm is sensitive to small errors and differences in satellite imager and icing is complex process, a new probability based icing diagnosis technique is developed from a limited set of pilot reports. The algorithm produces reasonable patterns of icing probability and intensities when compared with independent model and pilot report data. Methods are discussed for improving the technique for incorporation into operational icing products. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Minnis, P (reprint author), NASA, Langley Res Ctr, MS 420, Hampton, VA 23681 USA. RI Vonder Haar, Thomas/F-2048-2011 NR 28 TC 2 Z9 2 U1 0 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5487-7 J9 P SOC PHOTO-OPT INS PY 2004 VL 5549 BP 145 EP 155 DI 10.1117/12.560488 PG 11 WC Engineering, Aerospace; Environmental Sciences; Meteorology & Atmospheric Sciences; Remote Sensing SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences; Remote Sensing GA BBC32 UT WOS:000224730100016 ER PT J AU Flom, Y Wang, L AF Flom, Y Wang, L TI Flaw tolerance in lap shear brazed joints - Part 1 SO WELDING JOURNAL LA English DT Article DE aerospace; brazement; brazing; furnace brazing; lap joints AB Furnace brazing is a joining process used in the aerospace and other industries to produce strong permanent and hermetic structural joints. As in any joining process, brazed joints have various imperfections and defects. At the present time, our understanding of the influence of the internal defects on the strength of the brazed joints is not adequate. The goal of this three-part investigation is to better understand the properties and failure mechanisms of the brazed joints containing defects. This study focuses on the behavior of brazed lap shear joints because of their importance in manufacturing aerospace structures. In Part 1, an average shear strength capability and failure modes of the single lap joints are explored. Stainless steel specimens brazed with pure silver are tested in accordance with the AWS C3.2 standard. Comparison of the failure loads and the ultimate shear strength with the finite element analysis (FEA) of the same specimens as a function of the overlap widths shows excellent correlation between the experimental and calculated values for the defect-free lap joints. A damage zone criterion is shown to work quite well in understanding the failure of the braze joints. In Part 2, the findings of Part 1 will be verified on the larger test specimens. Also, various flaws will be introduced in the test specimens to simulate incomplete braze coverage in the lap joints. Mechanical testing and FEA will be performed on these joints to verify that behavior of the flawed ductile lap joints is similar to joints with a reduced braze area. Finally, in Part 3, the results obtained in Parts 1 and 2 will be applied to the actual brazed structure to evaluate the load-carrying capability of a structural lap joint containing discontinuities. In addition, a simplified engineering procedure will be offered for the laboratory testing of the lap shear specimens. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. SWALES Aerosp, Beltsville, MD USA. RP Flom, Y (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 18 TC 5 Z9 5 U1 0 U2 1 PU AMER WELDING SOC PI MIAMI PA 550 N W LEJEUNE RD, MIAMI, FL 33126 USA SN 0043-2296 J9 WELD J JI Weld. J. PD JAN PY 2004 VL 83 IS 1 BP 32S EP 38S PG 7 WC Metallurgy & Metallurgical Engineering SC Metallurgy & Metallurgical Engineering GA 759TV UT WOS:000187753700012 ER PT S AU Gubarev, M Ramsey, B Apple, J AF Gubarev, M Ramsey, B Apple, J BE Flanagan, KA Siegmund, OHW TI Gas scintillation proportional counters for high-energy x-ray astronomy SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE DE x-ray astronomy instrumentation; x-ray detectors; proportional counters ID BOARD AB A focal plane array of high-pressure gas scintillation proportional counters (GSPC) for a balloon-borne hard-x-ray telescope is under development at the Marshall Space Flight Center. These detectors each have an active area of similar to 20 cm(2), and are filled with a high pressure (10(6) Pa) xenon-helium mixture. Imaging is via crossed-grid position-sensitive phototubes sensitive in the UV region. The performance of the GSPC is well matched to that of the telescope's x-ray optics which have response to 75 keV and a focal spot size of similar to 500 mum. The detector's energy resolution, 4% FWHM at 60 keV, is adequate for resolving the broad spectral lines of astrophysical importance and for accurate continuum measurements. Full details of the instrument and its performance will be provided. C1 NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. RP Gubarev, M (reprint author), NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, SD 70, Huntsville, AL 35812 USA. NR 3 TC 3 Z9 3 U1 1 U2 4 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 151 EP 157 DI 10.1117/12.506464 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700017 ER PT S AU Barthelmy, SD AF Barthelmy, SD BE Flanagan, KA Siegmund, OHW TI The Burst Alert telescope (BAT) on the swift MIDEX mission SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE DE gamma-ray; GRB; hard x-ray; survey; burst; afterglow; CZT; coded aperture; astrophysics; cosmology ID GAMMA-RAY BURST; 28 FEBRUARY 1997 AB The Burst Alert telescope (BAT) is one of 3 instruments on the Swift MIDEX spacecraft to study gamma-ray bursts (GRBs). The BAT instrument is the instrument that first detects the GRB and localizes the burst direction to an accuracy of 1-4 arcmin within 20 see after the start of the event. These locations cause the spacecraft to autonomously slew to point the two narrow-FOV instruments at the burst location within 20-70 sec to make follow-up x-ray and optical observations. BAT is a wide-FOV coded-aperture instrument with a CdZnTe detector plane. The detector plane is composed of 32,768 pieces of CdZnTe (4x4x2mm), and the coded-aperture mask is composed of similar to52,000 pieces of lead (5x5x1mm) with a 1-m separation between mask and detector plane. The BAT operates over the 15-150 keV energy range with similar to6 keV resolution, a sensitivity of 0.2 ph/cm(2)-sec, and a 1.4 sr (half-coded) FOV. We expect to detect >100 GRBs/yr for a 2-year mission. The BAT also performs an all-sky hard x-ray survey with a sensitivity of similar to2 mCrab (systematic limit) and as a hard x-ray transient monitor. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Barthelmy, SD (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. RI Barthelmy, Scott/D-2943-2012 NR 9 TC 44 Z9 44 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 175 EP 189 DI 10.1117/12.506779 PG 15 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700020 ER PT S AU Parsons, A Tueller, J Krimm, H Barthelmy, S Cummings, J Markwardt, C Hullinger, D Gehrels, N Fenimore, E Palmer, D Sato, G Nakazawa, K Takahashi, T Watanabe, S Okada, Y Takahashi, H Suzuki, M Tashiro, M AF Parsons, A Tueller, J Krimm, H Barthelmy, S Cummings, J Markwardt, C Hullinger, D Gehrels, N Fenimore, E Palmer, D Sato, G Nakazawa, K Takahashi, T Watanabe, S Okada, Y Takahashi, H Suzuki, M Tashiro, M BE Flanagan, KA Siegmund, OHW TI Swift/BAT calibration and the estimated BAT hard x-ray survey sensitivity SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE DE Swift; BAT; hard x-ray survey; CZT; gamma-ray; GRB; burst; coded aperture; astrophysics AB In addition to providing the initial gamma-ray burst trigger and location, the Swift Burst Alert Telescope (BAT) will also perform an all-sky hard x-ray survey based on serendipitous pointings resulting from the study of gamma-ray bursts. BAT was designed with a very wide field-of-view (FOV) so that it can observe roughly 1/7 of the sky at any time. Since gamma-ray bursts are uniformly distributed over the sky, the final BAT survey coverage is expected to be nearly uniform. BAT's large effective area and long sky exposures will produce a 15 - 150 keV survey with up to 30 times better sensitivity than any previous hard x-ray survey (e.g. HEAO A4). Since the sensitivity of deep exposures in this energy range is systematics limited, the ultimate survey sensitivity depends on the relative sizes of the statistical and systematic errors in the data. Many careful calibration experiments were performed at NASA/Goddard Space Flight Center to better understand the BAT instrument's response to 15-150 keV gamma-rays incident from any direction within the FOV. Using radioactive sources of gamma-rays with known locations and energies, the Swift team can identify potential systematic errors in the telescope's performance and estimate the actual Swift hard x-ray survey sensitivity in flight. These calibration results will be discussed and a preliminary parameterization of the BAT instrument response will be presented. While the details of the individual BAT CZT detector response will be presented elsewhere in these proceedings, this talk will focus on the translation of the calibration experimental data into overall hard x-ray survey sensitivity. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Parsons, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Barthelmy, Scott/D-2943-2012; Tueller, Jack/D-5334-2012; Parsons, Ann/I-6604-2012 NR 5 TC 4 Z9 4 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 190 EP 200 DI 10.1117/12.506309 PG 11 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700021 ER PT S AU Bloser, PF Hunter, SD Depaola, GO Longo, F AF Bloser, PF Hunter, SD Depaola, GO Longo, F BE Flanagan, KA Siegmund, OHW TI A concept for a high-energy gamma-ray polarimeter SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE DE polarimetry; gamma-ray astronomy; pair production; gas detectors; Monte Carlo simulations ID MICRO-WELL DETECTORS; X-RAY; LINEAR-POLARIZATION; PAIR PRODUCTION; VELA PULSAR; LARGE-AREA; TELESCOPE; ASTRONOMY; EMISSION AB We present a concept for an imaging gamma-ray polarimeter operating from similar to 50 MeV to similar to 1 GeV. Such an instrument would be valuable for the study of high-energy pulsars, active galactic nuclei, supernova remnants, and gamma-ray bursts. The concept makes use of pixelized gas micro-well detectors, under development at Goddard Space Flight Center, to record the electron-positron tracks from pair-production events in a large gas volume. Pixelized micro-well detectors have the potential to form large-volume 3-D track imagers with similar to 100 mum (rms) position resolution at moderate cost. The combination of high spatial resolution and a continuous low-density gas medium permits many thousands of measurements per radiation length, allowing the particle tracks to be imaged accurately before multiple scattering masks their original directions. The polarization of the incoming radiation may then be determined from the azimuthal distribution of the electron-positron pairs. We have performed Geant4 simulations of these processes to estimate the polarization sensitivity of a simple telescope geometry at 100 MeV. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bloser, PF (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. RI Hunter, Stanley/D-2942-2012 NR 36 TC 8 Z9 8 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 322 EP 333 DI 10.1117/12.505838 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700032 ER PT S AU Black, JK Deines-Jones, P Jahoda, K Ready, SE Street, RA AF Black, JK Deines-Jones, P Jahoda, K Ready, SE Street, RA BE Flanagan, KA Siegmund, OHW TI High-sensitivity X-ray polarimetry with amorphous silicon active-matrix pixel proportional counters SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE DE X-ray polarimetry; particle tracking; proportional counter; GEM; pixel readout ID MICRO-WELL DETECTORS; GAS DETECTORS; GEM AB Photoelectric X-ray polarimeters based on pixel micropattern gas detectors (MPGDs) offer order-of-magnitude improvement in sensitivity over more traditional techniques based on X-ray scattering. This new technique places some of the most interesting astronomical observations within reach of even a small, dedicated mission. The most sensitive instrument would be a photoelectric polarimeter at the focus of a very large mirror, such as the planned XEUS. Our efforts are focused on a smaller pathfinder mission, which would achieve its greatest sensitivity with large-area, low-background, collimated polarimeters. We have recently demonstrated a MPGD polarimeter using amorphous silicon thin-film transistor (TFT) readout suitable for the focal plane of an X-ray telescope. All the technologies used in the demonstration polarimeter are scalable to the areas required for a high-sensitivity collimated polarimeter. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Black, JK (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. RI Jahoda, Keith/D-5616-2012 NR 17 TC 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 346 EP 353 DI 10.1117/12.504862 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700034 ER PT S AU Weisskopf, MC AF Weisskopf, MC BE Flanagan, KA Siegmund, OHW TI Four years of operation of the Chandra X-ray observatory SO X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on X-Ray and Gamma-Ray Instrumentation for Astronomy XIII CY AUG 03-05, 2003 CL San Diego, CA SP SPIE DE x-ray imaging; grazing-incidence optics; x-ray astronomy ID GALAXY; DISCOVERY; CLUSTER; FIELD; JET; M87 AB The Chandra X-Ray Observatory is the X-ray component of NASA's Great Observatory Program. The facility provides scientific data to the international astronomical community in response to proposals for its use. Data becomes public at most one year after the observation. The Observatory is the product of the efforts of many commercial, academic, and government organizations in the United States and Europe. NASA's Marshall Space Flight Center (MSFC) manages the Project and provides Project Science; NGST (formerly TRW) served as prime contractor responsible for providing the spacecraft, the telescope, and assembling and testing the observatory; and the Smithsonian Astrophysical Observatory (SAO) provides technical support and is responsible for ground operations including the Chandra X-Ray Center (CXC). C1 NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. RP Weisskopf, MC (reprint author), NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. NR 20 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-5038-3 J9 P SOC PHOTO-OPT INS PY 2004 VL 5165 BP 387 EP 401 DI 10.1117/12.510236 PG 15 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BY69W UT WOS:000189441700038 ER PT S AU Meier, DL AF Meier, DL BE Kaaret, P Lamb, FK Swank, JH TI Understanding x-ray timing and radio observations of jet sources SO X-RAY TIMING 2003: ROSSI AND BEYOND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Timing 2003 - Rossi and Beyond CY NOV 03-05, 2003 CL Cambridge, MA SP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, NASA, Goddard Space Sfight Ctr, Lab High Energy Astrophys, Rossi X Ray Timing Explorer Project ID BLACK-HOLE ACCRETION; DOMINATED ACCRETION; NEUTRON-STAR; GX 339-4; FLOWS; BINARY; DISKS; EMISSION; FLARES; REGION AB Time-dependent x-ray and radio observations of accreting sources give considerable insight into how jets might be produced, both in low-luminosity and high-luminosity situations. I discuss recent observations of binary x-ray sources and AGN that may have a direct bearing on jet production, and I review the theoretical efforts that have been made to understand them. While it is certainly true that jet production can be understood only with a good accretion model, I also argue that accretion onto compact objects cannot be understood without fully taking into account the production of a jet. Jets are probably a fundamental aspect of some accretion modes. In a quest for an integrated model for accretion and jet production I introduce a new accretion concept, the magnetically-dominated accretion flow or MDAF, as an alternative to current models for the low/hard/plateau state of accreting black holes (and the atoll source island state). Although much quantitative work needs to be performed before the concept can evolve into a true model, MDAFs have a number of phenomenological advantages. In addition to providing explanations for several X-ray timing and radio properties of accreting sources, the MDAF suggests a model for the infrared flares in the Galactic center. C1 JPL, Pasadena, CA 91109 USA. RP Meier, DL (reprint author), JPL, MS 238-332,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 36 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0193-4 J9 AIP CONF PROC PY 2004 VL 714 BP 135 EP 142 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAP36 UT WOS:000223117800024 ER PT S AU Kazanas, D Titarchuk, L Becker, PA AF Kazanas, D Titarchuk, L Becker, PA BE Kaaret, P Lamb, FK Swank, JH TI Broad red-shifted lines as a signature of outflow SO X-RAY TIMING 2003: ROSSI AND BEYOND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Timing 2003 - Rossi and Beyond CY NOV 03-05, 2003 CL Cambridge, MA SP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, NASA, Goddard Space Sfight Ctr, Lab High Energy Astrophys, Rossi X Ray Timing Explorer Project ID CONVERGING FLUID-FLOW; COMPTON-SCATTERING; SPHERICAL FLOWS; BLACK-HOLES; ACCRETION AB We formulate and solve the diffusion problem of line photon propagation in a bulk outflow from a compact object (black hole or neutron star) using a generic assumption regarding the distribution of line photons within the outflow. Thomson scattering of the line photons within the expanding flow leads to a decrease of their energy which is of first order in v/c, where v is the outflow velocity and c the speed of light. We demonstrate that the emergent line profile is closely related to the time distribution of photons diffusing through the flow (the light curve) and consists of a broad redshifted feature. We analyzed the line profiles for the general case of outflow density distribution. We emphasize that the redshifted lines are intrinsic properties of the powerful outflow that are supposed to be in many compact objects. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kazanas, D (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0193-4 J9 AIP CONF PROC PY 2004 VL 714 BP 154 EP 156 PG 3 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAP36 UT WOS:000223117800028 ER PT S AU Strohmayer, TE AF Strohmayer, TE BE Kaaret, P Lamb, FK Swank, JH TI Future probes of the neutron star equation of state using X-ray bursts SO X-RAY TIMING 2003: ROSSI AND BEYOND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Timing 2003 - Rossi and Beyond CY NOV 03-05, 2003 CL Cambridge, MA SP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, NASA, Goddard Space Sfight Ctr, Lab High Energy Astrophys, Rossi X Ray Timing Explorer Project ID BRIGHTNESS OSCILLATIONS; COHERENT OSCILLATIONS; ABSORPTION-LINES; KS 1731-260; COMPACTNESS; FREQUENCY; EVOLUTION; PULSARS; BOUNDS; MATTER AB Observations with NASA's Rossi X-ray Timing Explorer (RXTE) have resulted in the discovery of fast (200 - 600 Hz), coherent X-ray intensity oscillations (hereafter, "burst oscillations") during thermonuclear X-ray bursts from 12 low mass X-ray binaries (LMXBs). Although many of their detailed properties remain to be fully understood, it is now beyond doubt that these oscillations result from spin modulation of the thermonuclear burst flux from the neutron star surface. Among the new timing phenomena revealed by RXTE the burst oscillations are perhaps the best understood, in the sense that many of their properties can be explained in the framework of this relatively simple model. Because of this, detailed modelling of burst oscillations can be an extremely powerful probe of neutron star structure, and thus the equation of state (EOS) of supranuclear density matter. Both the compactness parameter beta = GM/c(2)R, and the surface velocity, v(rot) = Omega(spin)R, are encoded in the energy-dependent amplitude and shape of the modulation pulses. The new discoveries have spurred much new theoretical work on thermonuclear burning and propagation on neutron stars, so that in the near future it is not unreasonable to think that detailed physical models of the time dependent flux from burning neutron stars will be available for comparison with the observed pulse profiles from a future, large collecting area X-ray timing observatory. In addition, recent high resolution burst spectroscopy with XMM/Newton suggests the presence of redshifted absorption lines from the neutron star surface during bursts. This leads to the possibility of using large area, high spectral resolution measurements of X-ray bursts as a precise probe of neutron star structure. In this work I will explore the precision with which constraints on neutron star structure, and hence the dense matter EOS, can be made with the implementation of such programs. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Strohmayer, TE (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 661, Greenbelt, MD 20771 USA. NR 39 TC 16 Z9 16 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0193-4 J9 AIP CONF PROC PY 2004 VL 714 BP 245 EP 252 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAP36 UT WOS:000223117800045 ER PT S AU Ibrahim, AI Markwardt, CB Swank, JH Ransom, S Roberts, M Kaspi, V Woods, PM Safi-Harb, S Balman, S Parke, WC Kouveliotou, C Hurley, K Cline, T AF Ibrahim, AI Markwardt, CB Swank, JH Ransom, S Roberts, M Kaspi, V Woods, PM Safi-Harb, S Balman, S Parke, WC Kouveliotou, C Hurley, K Cline, T BE Kaaret, P Lamb, FK Swank, JH TI The discovery of a Transient magnetar SO X-RAY TIMING 2003: ROSSI AND BEYOND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Timing 2003 - Rossi and Beyond CY NOV 03-05, 2003 CL Cambridge, MA SP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, NASA, Goddard Space Sfight Ctr, Lab High Energy Astrophys, Rossi X Ray Timing Explorer Project ID X-RAY PULSAR; CYCLOTRON-RESONANCE; NEUTRON-STARS; FIELD AB The newly discovered X-ray transient XTE J1810-197 exhibits almost all characteristics of magnetars. It possesses a relatively long spin period of 5.54 sand a rapid spin down rate of approximate to10(-11) s s(-1), while showing no evidence for Doppler shifts due to a binary companion. This yields a magnetar-strength dipole field B = 3 x 10(14) G and a young characteristic age tau less than or equal to 7600 yr. The spectrum of the source is notably soft (photon index approximate to 4) and optical observations with the 1.5 m Russian-Turkish Optical Telescope RTT150 revealed a limiting magnitude of R-c = 21.5, both consistent with those of Soft gamma repeaters and anomalous X-ray pulsars. However, the source shows a significant flux decline for over nine months and is present in archival ASCA and ROSAT observations at nearly two orders of magnitude fainter luminosity. Putting all evidence together shows that we have found the first confirmed transient magnetar. This suggests the presence of other unidentified transient magnetars in a state similar to XTE J1810-197 in its inactive phase. The detection of such sources is one of the important areas in which future X-ray timing missions can make a significant impact. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Ibrahim, AI (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RI Ibrahim, Alaa/A-6250-2008; OI Ibrahim, Alaa/0000-0002-8791-7270; Roberts, Mallory/0000-0002-9396-9720 NR 25 TC 2 Z9 2 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0193-4 J9 AIP CONF PROC PY 2004 VL 714 BP 294 EP 297 PG 4 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAP36 UT WOS:000223117800053 ER PT S AU Corbet, RHD Laycock, S Coe, MJ Marshall, FE Markwardt, CB AF Corbet, RHD Laycock, S Coe, MJ Marshall, FE Markwardt, CB BE Kaaret, P Lamb, FK Swank, JH TI Monitoring and discovering X-ray pulsars in the small magellanic cloud SO X-RAY TIMING 2003: ROSSI AND BEYOND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Timing 2003 - Rossi and Beyond CY NOV 03-05, 2003 CL Cambridge, MA SP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, NASA, Goddard Space Sfight Ctr, Lab High Energy Astrophys, Rossi X Ray Timing Explorer Project ID STAR-FORMATION; EVOLUTION; SMC AB Regular monitoring of the SMC with RXTE has revealed a huge number of X-ray pulsars. Together with discoveries from other satellites at least 45 SMC pulsars are now known. One of these sources, a pulsar with a period of approximately 7.8 seconds, was first detected in early 2002 and since discovery it has been found to be in outburst nine times. The outburst pattern clearly shows a period of 45.1 +/- 0.4 d which is thought to be the orbital period of this system. Candidate outburst periods have also been obtained for nine other pulsars and continued monitoring will enable us to confirm these. This large number of pulsars, all located at approximately the same distance, enables a wealth of comparative studies. In addition, the large number of pulsars found (which vastly exceeds the number expected simply by scaling the relative mass of the SMC and the Galaxy) reveals the recent star formation history of the SMC which has been influenced by encounters with both the LMC and the Galaxy. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Corbet, RHD (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. NR 15 TC 4 Z9 4 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0193-4 J9 AIP CONF PROC PY 2004 VL 714 BP 337 EP 341 PG 5 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAP36 UT WOS:000223117800061 ER PT S AU Swank, J AF Swank, J BE Kaaret, P Lamb, FK Swank, JH TI Quasi-periodic oscillations from low-mass X-ray binaries with neutron stars SO X-RAY TIMING 2003: ROSSI AND BEYOND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Timing 2003 - Rossi and Beyond CY NOV 03-05, 2003 CL Cambridge, MA SP Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, NASA, Goddard Space Sfight Ctr, Lab High Energy Astrophys, Rossi X Ray Timing Explorer Project ID 4U 1820-30; MILLISECOND OSCILLATIONS; MULTIWAVELENGTH CAMPAIGN; SPECTRAL PROPERTIES; CYGNUS X-2; AQUILA X-1; VARIABILITY; DISCOVERY; OUTBURST; PULSAR AB Before the launch of the Rossi X-ray Timing Explorer (RXTE) it was recognized that neutron star accretion disks could extend inward to very near the neutron star surface, and thus be governed by millisecond timescales. Previous missions lacked the sensitivity to detect them. The kilohertz quasi-periodic oscillations (QPO) that RXTE discovered are often, but not always, evident in the X-ray flux. In 8 years RXTE has found kilohertz signals in about a fourth of 100 low-mass X-ray binaries (LMXB) containing neutron stars. The observed power spectra have simple dominant features, the two kilohertz oscillations, a low frequency oscillation, and band-limited white noise. They vary systematically with changes in other source properties and offer the possibility of comparison with model predictions. New information from the millisecond pulsars resolves some questions about the relations of the QPO and the spin. Coherence, energy spectrum and time lag measurements have indicated systematic behaviors, which should constrain mechanisms. C1 Goddard Space Flight Ctr, Greenbelt, MD 20740 USA. RP Swank, J (reprint author), Goddard Space Flight Ctr, Greenbelt, MD 20740 USA. NR 34 TC 4 Z9 4 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0193-4 J9 AIP CONF PROC PY 2004 VL 714 BP 357 EP 364 PG 8 WC Astronomy & Astrophysics; Instruments & Instrumentation SC Astronomy & Astrophysics; Instruments & Instrumentation GA BAP36 UT WOS:000223117800065 ER PT S AU McLaughlin, MA Lorimer, DR Champion, DJ Xilouris, K Arzoumanian, Z Backer, DC Cordes, JM Fruchter, AS Lommen, AN AF McLaughlin, MA Lorimer, DR Champion, DJ Xilouris, K Arzoumanian, Z Backer, DC Cordes, JM Fruchter, AS Lommen, AN BE Camilo, F TI New pulsars from Arecibo drift-scan searches SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union AB We report on new pulsars discovered in Arecibo drift-scan data. Processing of 2200 deg(2) of data has resulted in the detection of 41 known and 12 new pulsars. New pulsars include two millisecond pulsars, one solitary and one binary recycled pulsar, and one pulsar with very unusual pulse profile morphology and complex drifting subpulse behavior. C1 Univ Manchester, Jodrell Bank Observ, Macclesfield, Cheshire, England. Univ Virginia, Charlottesville, VA 22903 USA. NASA, Goddard Space Flight Ctr, USRA, LHEA, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Berkeley, CA 94720 USA. Cornell Univ, Ithaca, NY 14853 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Franklin & Marshall Coll, Lancaster, PA 17604 USA. RP McLaughlin, MA (reprint author), Univ Manchester, Jodrell Bank Observ, Macclesfield, Cheshire, England. NR 4 TC 0 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 127 EP 128 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000031 ER PT S AU Petre, R Hwang, U Holt, SS Williams, RM AF Petre, R Hwang, U Holt, SS Williams, RM BE Camilo, F TI X-ray studies of the pulsar wind Nebula around PSR B0540-69 SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID SUPERNOVA REMNANT 0540-69.3 AB The pulsar wind nebula (PWN) surrounding the 50-ms pulsar B0540-69 in the Large Magellanic Cloud shares many properties with the Crab Nebula, the canonical Galactic PWN. We have used the ACIS instrument on the Chandra X-ray Observatory to perform spatially resolved spectroscopy of the PWN. The spectrum of the inner 10" is characterized by a simple power law, with a spectral index that steepens strongly with radius. Outside the central 10" the spectra also require a thermal component. This diameter corresponds to a shell detected in [0 111], suggesting that this shell represents a skin around the PWN, in analogy to the Crab. We infer the value of several key PWN parameters, including sigma, the average ratio of electromagnetic to particle flux. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. FW Olin Coll Engn, Needham, MA 02492 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. RP Petre, R (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 189 EP 192 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000048 ER PT S AU Harrus, I Bernstein, JP Slane, PO Gaensler, B Hughes, JP Moffett, D Dodson, R AF Harrus, I Bernstein, JP Slane, PO Gaensler, B Hughes, JP Moffett, D Dodson, R BE Camilo, F TI Chandra study of the central object associated with the supernova remnant MSH 11-62 SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID NEBULAE; PULSARS AB We present results from our analysis of Chandra data on the supernova remnant MSH 11-62 (also known as G291.0-0.1). Our previous ASCA analysis showed that MSH 11-62 is most likely a composite remnant whose strong non-thermal emission is powered by a compact object, most probably a pulsar. The present analysis confirms in a spectacular fashion the earlier detection of a compact source. The Chandra data reveal a small region with a hard non-thermal spectrum located at the tip of the central radio emission seen in data taken at the Australia Telescope Compact Array (ATCA). This source is likely the young rapidly rotating neutron star powering the synchrotron nebula in MSH 11-62. Compared to other young rotation-powered pulsars the Chandra spectrum of MSH 11-62 implies an energy loss rate of E similar to 5 x 10(36) ergs s(-1). C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rutgers State Univ, Piscataway, NJ 08854 USA. Furman Univ, Greenville, SC 29613 USA. Japan Aerosp Explorat Agcy, JAXA, Kanagawa 2298510, Japan. RP Harrus, I (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Gaensler, Bryan/F-8655-2010 NR 7 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 203 EP 206 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000052 ER PT S AU Israel, G Stella, L Covino, S Campana, S Angelini, L Mignani, R Mereghetti, S Marconi, G Perna, R AF Israel, G Stella, L Covino, S Campana, S Angelini, L Mignani, R Mereghetti, S Marconi, G Perna, R BE Camilo, F TI Unveiling the multi-wavelength phenomenology of anomalous X-ray pulsars SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID NEAR-INFRARED COUNTERPART; 1E 2259+586; DISCOVERY AB During 2002-2003 the number of IR-identified counterparts to the Anomalous X-ray Pulsars (AXPs) has grown to four (4U 0142+61, 1E 2259+586, 1E 1048.1-5937 and RXS J170849-400910) out of the six objects (plus two candidates) known in this class. More importantly, some new common characteristics have been identified, such as IR variability, IR flattening in the broad-band energy spectrum, X-ray spectral variability as a function of pulse phase (which are not predicted by the magnetar model), and X-ray bursts (which cannot be explained in terms of standard accretion models). We present the results obtained from an extensive multi-wavelength observational campaign carried out with the NTT and CFHT for the optical/IR bands, and XMM and Chandra (plus BeppoSAX axchival data) in X-rays. Based on these results and those reported in the literature, the IR-to-X-ray emission of AXPs is compared. C1 Osserv Astron Roma, INAF, I-00136 Rome, Italy. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. European So Observ, D-8046 Garching, Germany. Ist Astrofis Spaziale & Fis Cosm, CNR, Milan, Italy. European So Observ, Paranal, Chile. Princeton Univ, Princeton, NJ 08544 USA. RP Israel, G (reprint author), Osserv Astron Roma, INAF, I-00136 Rome, Italy. OI MEREGHETTI, SANDRO/0000-0003-3259-7801; Covino, Stefano/0000-0001-9078-5507 NR 16 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 247 EP 250 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000062 ER PT S AU Donovan, J Lommen, A Arzoumanian, Z Harding, A Strickman, M Gwinn, C Dodson, R McCulloch, P Moffett, D AF Donovan, J Lommen, A Arzoumanian, Z Harding, A Strickman, M Gwinn, C Dodson, R McCulloch, P Moffett, D BE Camilo, F TI Correlations between X-ray and radio pulses in Vela SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union AB Pulse-shape changes correlating with flux have been shown to exist in the Vela pulsar's radio emission (Krishnamohan P Downs 1983). The aim of this work was to look for correlations between radio and X-ray flux in Vela on a pulse-by-pulse basis. We found that Vela emits significantly more X-rays during radio pulses with strong flux than during weak radio flux pulses, which indicates that the mechanisms creating the Vela pulsar's X-ray and radio emission must be related. C1 Franklin & Marshall Coll, Lancaster, PA 17604 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. USN, Res Lab, Washington, DC USA. Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. Univ Tasmania, Hobart, Tas 7001, Australia. Furman Univ, Greenville, SC 29613 USA. RP Donovan, J (reprint author), Franklin & Marshall Coll, Lancaster, PA 17604 USA. NR 2 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 335 EP 336 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000085 ER PT S AU Dyks, J Harding, AK Rudak, B AF Dyks, J Harding, AK Rudak, B BE Camilo, F TI Two-pole caustic model for high-energy radiation from pulsars - Polarization SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union AB We present high-energy light curves and polarization properties of pulsars calculated within the recently proposed two-pole caustic model. The results are compared with the optical data for the Crab pulsar and with predictions of other high-energy pulsar models: the polar cap model, and the outer gap model. C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Nicolaus Copernicus Astron Ctr, PL-87100 Torun, Poland. RP Dyks, J (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 661, Greenbelt, MD 20771 USA. RI Harding, Alice/D-3160-2012 NR 5 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 373 EP 374 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000095 ER PT S AU Thompson, DJ AF Thompson, DJ BE Camilo, F TI Future facilities for gamma-ray pulsar studies SO YOUNG NEUTRON STARS AND THEIR ENVIRONMENTS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 218th Symposium of the International-Astronomical-Union on Yound Neutron Stars and Their Environments CY JUL 14-17, 2003 CL Sydney, AUSTRALIA SP Int Astron Union ID HIGH-ENERGY; MISSION; GEMINGA AB Pulsars seen at gamma-ray energies offer insight into particle acceleration to very high energies, along with information about the geometry and interaction processes in the magnetospheres of these rotating neutron stars. During the next decade, a number of new gamma-ray facilities will become available for pulsar studies. This brief review describes the motivation for gamma-ray pulsar studies, the opportunities for such studies, and some specific discussion of the capabilities of the Gamma-ray Large Area Space Telescope (GLAST) Large Area Telescope (LAT) for pulsar measurements. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Thompson, DJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RI Thompson, David/D-2939-2012 OI Thompson, David/0000-0001-5217-9135 NR 13 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-178-8 J9 IAU SYMP PY 2004 IS 218 BP 399 EP 406 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BBR59 UT WOS:000227426000103 ER PT J AU Zeng, T Wang, YH Chance, K Browell, EV Ridley, BA Atlas, EL AF Zeng, T Wang, YH Chance, K Browell, EV Ridley, BA Atlas, EL TI Widespread persistent near-surface ozone depletion at northern high latitudes in spring SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ARCTIC BOUNDARY-LAYER; POLAR SUNRISE; BRO CONCENTRATIONS; TROPOSPHERIC BRO; BROMINE; CHEMISTRY; MODEL; DESTRUCTION; RELEASE; EVENTS AB Springtime near-surface ozone depletion has been observed at northern high latitudes. Due to limited observations, the spatial and temporal extent of low O-3 concentrations near the surface is still unknown. A regional 3-D chemistry and transport model is applied to simulate surface O-3 depletion catalyzed by bromine radicals at northern high latitudes in March and April 2000. Satellite observations of BrO column by the ESA Global Ozone Monitoring Experiment (GOME) were processed to specify the BrO concentrations in the lower troposphere. In view of the GOME measurement and model uncertainties, the model results show an adequate agreement with the O-3 depletion events observed at two surface sites, Alert, Canada (82.5degreesN, 62.3degreesW) and Barrow, Alaska (71.3degreesN, 156.6degreesW), and by airborne in situ and DIAL instrument during the TOPSE experiments at northern high latitudes. Low O-3 events at Alert appear to be mostly driven by transport of O-3-poor air from high BrO regions. Model results indicate that low O-3 concentrations (<20 ppbv) near the surface cover similar to 60% of the northern high latitudes and that the depleted O-3 concentrations (<10 ppbv) cover similar to20% of the region in April. The high BrO events tend to be large-scale and persistent (1-2 weeks). We find that they are correlated with low temperature, a condition conducive for heterogeneous reactions on frozen snow or aerosol surfaces. C1 Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA. RP Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. EM ywang@eas.gatech.edu RI Wang, Yuhang/B-5578-2014; Atlas, Elliot/J-8171-2015 NR 28 TC 38 Z9 38 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 31 PY 2003 VL 30 IS 24 AR 2298 DI 10.1029/2003GL018587 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 761HZ UT WOS:000187896600005 ER PT J AU Chen, YH Miller, JR Francis, JA Russell, GL Aires, F AF Chen, YH Miller, JR Francis, JA Russell, GL Aires, F TI Observed and modeled relationships among Arctic climate variables SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Arctic; radiation; global climate model; feedback; validation; remote sensing ID SEA-ICE; SURFACE; OCEAN; RETRIEVALS; MULTIVARIATE; TEMPERATURE; PROJECT; FLUXES AB The complex interactions among climate variables in the Arctic have important implications for potential climate change, both globally and locally. Because the Arctic is a data-sparse region and because global climate models (GCMs) often represent Arctic climate variables poorly, significant uncertainties remain in our understanding of these processes. In addition to the traditional approach of validating individual variables with observed fields, we demonstrate that a comparison of covariances among interrelated parameters from observations and GCM output provides a tool to evaluate the realism of modeled relationships between variables. We analyze and compare a combination of conventional observations, satellite retrievals, and GCM simulations to examine some of these relationships. The three climate variables considered in this study are surface temperature, cloud cover, and downward longwave flux. Results show that the highest correlations between daily changes in pairs of variables for all three data sets occur between surface temperature and downward longwave flux, particularly in winter. There is less variability in GCM output, in part, because there is greater spatial averaging. Although the satellite products can be used to examine some of these relationships, additional work may be needed to ensure consistency between changes in radiative components of the energy budget and other retrieved quantities. The GCM's relationships between variables agree well with in situ observations, which provides some confidence that the GCM's representation of present-day climate is reasonable in high northern latitudes. C1 Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08901 USA. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Chen, YH (reprint author), Rutgers State Univ, Inst Marine & Coastal Sci, 71 Dudley Rd, New Brunswick, NJ 08901 USA. EM chen@imcs.rutgers.edu; miller@arctic.rutgers.edu; francis@imcs.rutgers.edu; grussell@giss.nasa.gov; filipe@sharki.giss.nasa.gov NR 32 TC 12 Z9 12 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 31 PY 2003 VL 108 IS D24 AR 4799 DI 10.1029/2003JD003824 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 761JT UT WOS:000187867300006 ER PT J AU Fujiwara, M Xie, SP Shiotani, M Hashizume, H Hasebe, F Vomel, H Oltmans, SJ Watanabe, T AF Fujiwara, M Xie, SP Shiotani, M Hashizume, H Hasebe, F Vomel, H Oltmans, SJ Watanabe, T TI Upper-tropospheric inversion and easterly jet in the tropics SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE easterly jet; temperature inversion; tropical upper troposphere ID WATER-VAPOR; PACIFIC; STRATOSPHERE; GREENHOUSE; TROPOPAUSE; AIRCRAFT; LAYERS; OZONE; WAVES AB Shipboard radiosonde measurements revealed a persistent temperature inversion layer with a thickness of similar to200 m at 12-13 km in a nonconvective region over the tropical eastern Pacific, along 2degreesN, in September 1999. Simultaneous relative humidity measurements indicated that the thin inversion layer was located at the top of a very wet layer with a thickness of 3-4 km, which was found to originate from the intertropical convergence zone (ITCZ) to the north. Radiative transfer calculations suggested that this upper tropospheric inversion (UTI) was produced and maintained by strong longwave cooling in this wet layer. A strong easterly jet stream was also observed at 12-13 km, centered around 4degrees-5degreesN. This easterly jet was in the thermal wind balance, with meridional temperature gradients produced by the cloud and radiative processes in the ITCZ and the wet outflow. Furthermore, the jet, in turn, acted to spread inversions further downstream through the transport of radiatively active water vapor. This feedback mechanism may explain the omnipresence of temperature inversions and layering structures in trace gases in the tropical troposphere. Examination of high-resolution radiosonde data at other sites in the tropical Pacific indicates that similar UTIs often appear around 12-15 km. The UTI around 12-15 km may thus be characterized as one of the "climatological" inversions in the tropical troposphere, forming the lower boundary of the so-called tropical tropopause layer, where the tropospheric air is processed photochemically and microphysically before entering the stratosphere. C1 Hokkaido Univ, Grad Sch Environm Earth Sci, Sapporo, Hokkaido 0600810, Japan. Univ Hawaii, Int Pacific Res Ctr, Honolulu, HI 96822 USA. Univ Hawaii, Dept Meteorol, Honolulu, HI 96822 USA. Kyoto Univ, Radio Sci Ctr Space & Atmosphere, Kyoto 6110011, Japan. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. NOAA, Climate Monitoring & Diagnost Lab, Boulder, CO 80305 USA. Natl Res Inst Fisheries sci, Fisheries Res Agcy, Kanagawa, Japan. RP Hokkaido Univ, Grad Sch Environm Earth Sci, Sapporo, Hokkaido 0600810, Japan. EM fuji@ees.hokudai.ac.jp RI Fujiwara, Masatomo/F-7852-2012; Xie, Shang-Ping/C-1254-2009 OI Xie, Shang-Ping/0000-0002-3676-1325 NR 32 TC 13 Z9 14 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 31 PY 2003 VL 108 IS D24 AR 2796 DI 10.1029/2003JD003928 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 761JT UT WOS:000187867300011 ER PT J AU Heald, CL Jacob, DJ Fiore, AM Emmons, LK Gille, JC Deeter, MN Warner, J Edwards, DP Crawford, JH Hamlin, AJ Sachse, GW Browell, EV Avery, MA Vay, SA Westberg, DJ Blake, DR Singh, HB Sandholm, ST Talbot, RW Fuelberg, HE AF Heald, CL Jacob, DJ Fiore, AM Emmons, LK Gille, JC Deeter, MN Warner, J Edwards, DP Crawford, JH Hamlin, AJ Sachse, GW Browell, EV Avery, MA Vay, SA Westberg, DJ Blake, DR Singh, HB Sandholm, ST Talbot, RW Fuelberg, HE TI Asian outflow and trans-Pacific transport of carbon monoxide and ozone pollution: An integrated satellite, aircraft, and model perspective SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE TRACE-P; MOPITT; Asian pollution; trans-Pacific transport; carbon monoxide; O-3 production ID TRACE-P EXPERIMENT; TROPOSPHERE MOPITT INSTRUMENT; CHEMICAL EVOLUTION; WESTERN PACIFIC; REACTIVE NITROGEN; AIR-POLLUTION; UNITED-STATES; CONTINENTAL OUTFLOW; NORTHEAST PACIFIC; EAST-ASIA AB Satellite observations of carbon monoxide (CO) from the Measurements of Pollution in the Troposphere (MOPITT) instrument are combined with measurements from the Transport and Chemical Evolution Over the Pacific (TRACE-P) aircraft mission over the northwest Pacific and with a global three-dimensional chemical transport model (GEOS-CHEM) to quantify Asian pollution outflow and its trans-Pacific transport during spring 2001. Global CO column distributions in MOPITT and GEOS-CHEM are highly correlated (R-2 = 0.87), with no significant model bias. The largest regional bias is over Southeast Asia, where the model is 18% too high. A 60% decrease of regional biomass burning emissions in the model (to 39 Tg yr(-1)) would correct the discrepancy; this result is consistent with TRACE-P observations. MOPITT and TRACE-P also give consistent constraints on the Chinese source of CO from fuel combustion (181 Tg CO yr(-1)). Four major events of trans- Pacific transport of Asian pollution in spring 2001 were seen by MOPITT, in situ platforms, and GEOS-CHEM. One of them was sampled by TRACE-P (26-27 February) as a succession of pollution layers over the northeast Pacific. These layers all originated from one single event of Asian outflow that split into northern and southern plumes over the central Pacific. The northern plume (sampled at 6-8 km off California) had no ozone enhancement. The southern subsiding plume (sampled at 2-4 km west of Hawaii) contained a 8-17 ppbv ozone enhancement, driven by decomposition of peroxyacetylnitrate (PAN) to nitrogen oxides (NOx). This result suggests that PAN decomposition in trans- Pacific pollution plumes subsiding over the United States could lead to significant enhancements of surface ozone. C1 Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Natl Ctr Atmospher Res, Boulder, CO 80303 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Sci Applicat Int Corp, Hampton, VA 23681 USA. Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA. RP Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. EM heald@fas.harvard.edu; djjacob@fas.harvard.edu; afiore@fas.harvard.edu; emmons@ucar.edu; gille@ucar.edu; mnd@ucar.edu; juying@ucar.edu; edwards@ucar.edu; j.h.crawford@larc.nasa.gov; ahamlin@mtu.edu; g.w.sachse@larc.nasa.gov; e.v.browell@larc.nasa.gov; m.a.avery@larc.nasa.gov; s.a.vay@larc.nasa.gov; d.j.westberg@larc.nasa.gov; drblake@uci.edu; hsingh@mail.arc.nasa.gov; scott.sandholm@eas.gatech.edu; robert.talbot@unh.edu; fuelberg@fsu.edu RI Heald, Colette/A-6813-2011; Crawford, James/L-6632-2013; Chem, GEOS/C-5595-2014; Deeter, Merritt/O-6078-2016; Emmons, Louisa/R-8922-2016 OI Crawford, James/0000-0002-6982-0934; Deeter, Merritt/0000-0002-3555-0518; Emmons, Louisa/0000-0003-2325-6212 NR 49 TC 137 Z9 137 U1 4 U2 33 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 31 PY 2003 VL 108 IS D24 AR 4804 DI 10.1029/2003JD003507 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 761JT UT WOS:000187867300002 ER PT J AU Smirnov, A Holben, BN Eck, TF Dubovik, O Slutsker, I AF Smirnov, A Holben, BN Eck, TF Dubovik, O Slutsker, I TI Effect of wind speed on columnar aerosol optical properties at Midway Island SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosol optical depth; maritime aerosol; wind speed; atmospheric correction; AERONET ID SEA-SALT AEROSOL; SKY RADIANCE MEASUREMENTS; TROPICAL INDIAN-OCEAN; MARINE BOUNDARY-LAYER; ATMOSPHERIC AEROSOL; NORTH-ATLANTIC; CAPE GRIM; DEPTH; AERONET; MODEL AB Aerosol optical properties over Midway Island in the central Pacific Ocean are considered in conjunction with the information on surface wind speed. In general, optical conditions over Midway resemble aerosol found over other maritime locations in the Pacific Ocean (Lanai, Tahiti, and Nauru). The most frequently occurring values of aerosol optical depth at 500-nm wavelength and Angstrom parameter are 0.06 and similar to0.40, respectively. Empirical relationships are established between columnar aerosol optical properties and surface wind speed. Increased emission of sea-salt aerosols at greater wind speeds primarily influenced aerosol optical depth at infrared wavelengths. The correlation coefficient between 24 hour average surface wind speed and aerosol optical depth, although not high (0.52 at a 1020 nm wavelength), is statistically significant at a 99% confidence level. Wind speed anticorrelates with the Angstrom parameter owing to an influx of large particles from the surface. Wind speed influences primarily the coarse fraction (radius >0.5 mum) concentration of the retrieved columnar size distribution (correlation coefficient 0.56). Effective radii of the retrieved fine and coarse modes are found to be independent of wind speed. Average size distributions for various wind speed bins can be very well simulated with the maritime aerosol component model. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. Sci Syst & Applicat Inc, Lanham, MD USA. RP Smirnov, A (reprint author), NASA, Goddard Space Flight Ctr, Code 923, Greenbelt, MD 20771 USA. EM asmirnov@aeronet.gsfc.nasa.gov; brent@aeronet.gsfc.nasa.gov; teck@aeronet.gsfc.nasa.gov; dubovik@aeronet.gsfc.nasa.gov; ilya@aeronet.gsfc.nasa.gov RI Dubovik, Oleg/A-8235-2009; Smirnov, Alexander/C-2121-2009; ECK, THOMAS/D-7407-2012 OI Dubovik, Oleg/0000-0003-3482-6460; Smirnov, Alexander/0000-0002-8208-1304; NR 41 TC 60 Z9 61 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 31 PY 2003 VL 108 IS D24 AR 4802 DI 10.1029/2003JD003879 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 761JT UT WOS:000187867300010 ER PT J AU Cravens, TE Waite, JH Gombosi, TI Lugaz, N Gladstone, GR Mauk, BH MacDowall, RJ AF Cravens, TE Waite, JH Gombosi, TI Lugaz, N Gladstone, GR Mauk, BH MacDowall, RJ TI Implications of Jovian X-ray emission for magnetosphere-ionosphere coupling SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE planetary magnetospheres; Jovian aurora; Jovian magnetosphere; X-rays; ion acceleration; field-aligned currents ID HUBBLE-SPACE-TELESCOPE; HOT PLASMA ENVIRONMENT; SOLAR-WIND; JUPITERS MAGNETOSPHERE; ULTRAVIOLET EMISSION; AURORAL PROCESSES; ENERGETIC OXYGEN; RADIO-BURSTS; HEAVY-IONS; UV AURORA AB The first observations of Jupiter made by the Chandra X-Ray Observatory revealed a powerful X-ray aurora located in the polar caps. The X-ray emission exhibited a 40-min periodicity. Such 40-min periodicities have previously been seen in energetic particle fluxes and in Jovian radio emission. This paper develops scenarios in which the X-ray emission is produced by energetic heavy ion precipitation, either on open field lines connecting to the solar wind or on closed field lines reaching to the outer magnetosphere. In order to produce enough X-ray power, both scenarios require the existence of field-aligned electric fields located somewhere between the ionosphere and the magnetosphere, most likely at a radial distance of a few Jovian radii. The potential needed for solar wind ions to produce the observed X-rays is about 200 kV and the potential needed for the magnetospheric ions is at least 8 MV. Protons and helium ions are also accelerated by the potential and should produce an intense ultraviolet aurora. Downward electrical current is carried by the precipitating ions and also by upwardly accelerated secondary electrons produced by the primary ion precipitation. The estimated downward Birkeland current is about 1000 MA for the solar wind case and is about 10 MA for the magnetospheric case. For the magnetosphere scenario, this observed current represents part of the "return'' current portion of the magnetospheric circuit associated with the departure of the mass-loaded magnetospheric plasma from corotation. The auroral X-ray emission maps at least part of this return current in the polar cap, whereas the main oval, produced by electron precipitation, is thought to map the region of upward Birkeland currents. The accelerated secondary electrons could be responsible for the periodic radio emission (i.e., QP-40 bursts). C1 Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Michigan, Space Phys Res Lab, AOSS Dept, Ann Arbor, MI 48109 USA. SW Res Inst, Dept Space Sci, San Antonio, TX 78228 USA. RP Cravens, TE (reprint author), Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. EM cravens@ukans.edu; hunterw@umich.edu; tamas@umich.edu; nlugaz@umich.edu; randy.gladstone@swri.org; barry.mauk@jhuap1.edu; robert.j.macdowall@nasa.gov RI Lugaz, Noe/C-1284-2008; MacDowall, Robert/D-2773-2012; Gombosi, Tamas/G-4238-2011; Mauk, Barry/E-8420-2017 OI Lugaz, Noe/0000-0002-1890-6156; Gombosi, Tamas/0000-0001-9360-4951; Mauk, Barry/0000-0001-9789-3797 NR 69 TC 46 Z9 46 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 31 PY 2003 VL 108 IS A12 AR 1465 DI 10.1029/2003JA010050 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 761JZ UT WOS:000187898400007 ER PT J AU Crider, DH Vignes, D Krymskii, AM Breus, TK Ness, NF Mitchell, DL Slavin, JA Acuna, MH AF Crider, DH Vignes, D Krymskii, AM Breus, TK Ness, NF Mitchell, DL Slavin, JA Acuna, MH TI A proxy for determining solar wind dynamic pressure at Mars using Mars Global Surveyor data SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE solar wind dynamic pressure; Mars Global Surveyor; magnetic pileup boundary; magnetic pileup region; Venus magnetic barrier ID MAGNETIC PILEUP BOUNDARY; BOW SHOCK; MARTIAN MAGNETOSPHERE; CRUSTAL MAGNETIZATION; MAG/ER EXPERIMENT; FIELD; PLASMA; IONOSPHERE; VENUS; MAGNETOPAUSE AB We develop a method to infer the upstream solar wind pressure at Mars using data from the Mars Global Surveyor (MGS) magnetometer instrument. The method assumes magnetic field pressure in the magnetic pileup region balances the incident solar wind dynamic pressure. Newtonian pressure balance conditions are imposed for positions off of the subflow point. Proof of concept exists from the mapping phase of the spacecraft mission, when the orbital geometry at a constant altitude allows fits to magnetic field data as a function of solar zenith angle. During the elliptical orbit phase of MGS, when the spacecraft passes through a large range of altitudes, such fits are not possible. However, the measured magnetic pressure in the magnetic pileup region is scaled by the same means as derived for the mapping orbits and reasonable upstream solar wind pressure is obtained. We compare the distribution of solar wind pressure calculated using MGS data with the solar wind pressure measured upstream of the Earth during the same time period and find good agreement, further supporting this algorithm as a valid proxy for the incident solar wind pressure. The response of the position of the Magnetic Pileup Boundary to the inferred solar wind pressure also validates the method. High solar wind ram pressure depresses the altitude of the Magnetic Pileup Boundary. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. Rostov State Univ, Space Phys Dept, Rostov Na Donu 344090, Russia. Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP 106 Driftwood Dr, Gibsonville, NC 27249 USA. EM dcrider@lepvax.gsfc.nasa.gov; didier_vignes@hotmail.com; amkrym@yahoo.com; breus@space.ru; nfness@udel.edu; mitchell@ssl.berkeley.edu; james.a.slavin@nasa.gov; mario.h.acuna@nasa.gov RI Slavin, James/H-3170-2012; Hurley, Dana/F-4488-2015 OI Slavin, James/0000-0002-9206-724X; Hurley, Dana/0000-0003-1052-1494 NR 47 TC 53 Z9 53 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 31 PY 2003 VL 108 IS A12 AR 1461 DI 10.1029/2003JA009875 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 761JZ UT WOS:000187898400002 ER PT J AU Numata, K Ando, M Yamamoto, K Otsuka, S Tsubono, K AF Numata, K Ando, M Yamamoto, K Otsuka, S Tsubono, K TI Wide-band direct measurement of thermal fluctuations in an interferometer SO PHYSICAL REVIEW LETTERS LA English DT Article ID GRAVITATIONAL-WAVE DETECTORS; THERMODYNAMICAL FLUCTUATIONS; LASER INTERFEROMETER; INTERNAL-FRICTION; MIRROR COATINGS; BROWNIAN-MOTION; MECHANICAL LOSS; NOISE; SENSITIVITY; RADIATION AB We directly measured mechanical thermal fluctuations in mirrors over three decades of frequency range using a short-length Fabry-Perot interferometer. This is the first such measurement at wide off-resonant frequency band that is much lower than mechanical resonant frequencies. Theoretically, the mechanical fluctuation in mirrors had been thought to become the principal noise in precise interferometry, such as in gravitational wave detection. We identified the thermally induced noises in the interferometer, the so-called substrate Brownian noise, substrate thermoelastic noise, and coating Brownian noise. C1 Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. Univ Tokyo, Inst Cosm Ray Res, Chiba 2778582, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Astron Observ, Tokyo, Japan. RP Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. EM numata@t-munu.phys.s.u-tokyo.ac.jp RI ANDO, MASAKI/G-4989-2014 OI ANDO, MASAKI/0000-0002-8865-9998 NR 32 TC 35 Z9 36 U1 2 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 31 PY 2003 VL 91 IS 26 AR 260602 DI 10.1103/PhysRevLett.91.260602 PG 4 WC Physics, Multidisciplinary SC Physics GA 759BY UT WOS:000187719300004 PM 14754033 ER PT J AU Lau, KM Wu, HT AF Lau, KM Wu, HT TI Warm rain processes over tropical oceans and climate implications SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CLOUDS; PRECIPITATION; CONVECTION; SHALLOW; MODEL AB From analysis of TRMM data, we find that warm rain accounts for 31% of the total rain amount and 72% of the total rain area in the tropics, and plays an important role in regulating the moisture content of the tropical atmosphere. There is a substantial increase in precipitation efficiency of light warm rain as the sea surface temperature increases, but precipitation efficiency of heavy rain associated with deep convection is independent of sea surface temperature. This implies that in a warmer climate, there may be more warm rain, at the expense of less cloud water available for middle and high level clouds. C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. Sci & Syst Applicat Inc, Lanham, MD USA. RP Lau, KM (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. EM william.k.lau@nasa.gov NR 16 TC 82 Z9 84 U1 1 U2 25 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 30 PY 2003 VL 30 IS 24 AR 2290 DI 10.1029/2003GL018567 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 761HX UT WOS:000187896400003 ER PT J AU Moore, JM Howard, AD Dietrich, WE Schenk, PM AF Moore, JM Howard, AD Dietrich, WE Schenk, PM TI Martian layered fluvial deposits: implications for Noachian climate scenarios SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID RIVER MEANDERS; EARLY MARS; WARM; WET AB Fluvial deposits in a basin north of Holden crater exhibiting a sinuous, anabranching pattern are of deltaic or fan origin. Channel width and meander wavelength indicate persistent flow magnitudes of about 700 m3/s. If these flows were produced by quasi-periodic climate episodes involving typical terrestrial-style precipitation, the deposit required thousands to millions of years to accumulate. However, a scenario of deposition during a few short episodes of constant heavy precipitation resulting from large impacts cannot be excluded. C1 NASA, Ames Res Ctr, Moffett Field, CA USA. Univ Virginia, Charlottesville, VA USA. Univ Calif Berkeley, Berkeley, CA USA. Lunar & Planetary Inst, Houston, TX USA. RP Moore, JM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA USA. EM jeff.moore@nasa.gov NR 19 TC 112 Z9 113 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 30 PY 2003 VL 30 IS 24 AR 2292 DI 10.1029/2003GL019002 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 761HX UT WOS:000187896400005 ER PT J AU Cabrol, NA Grin, EA Carr, MH Sutter, B Moore, JM Farmer, JD Greeley, R Kuzmin, RO DesMarais, DJ Kramer, MG Newsom, H Barber, C Thorsos, I Tanaka, KL Barlow, NG Fike, DA Urquhart, ML Grigsby, B Grant, FD de Goursac, O AF Cabrol, NA Grin, EA Carr, MH Sutter, B Moore, JM Farmer, JD Greeley, R Kuzmin, RO DesMarais, DJ Kramer, MG Newsom, H Barber, C Thorsos, I Tanaka, KL Barlow, NG Fike, DA Urquhart, ML Grigsby, B Grant, FD de Goursac, O TI Exploring Gusev Crater with Spirit: Review of science objectives and testable hypotheses SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review DE Gusev; lake; Apollinaris Patera; Spirit rover ID MARTIAN IMPACT CRATERS; ORBITER LASER ALTIMETER; MAADIM-VALLIS; EARLY MARS; CHEMICAL-COMPOSITION; WIND EROSION; ORIGIN; EJECTA; WATER; CHANNELS AB Gusev Crater was selected as the landing site for the Mars Exploration Rover (MER) Spirit mission. Located at the outlet of Ma'adim Vallis and 250 km south of the volcano Apollinaris Patera, Gusev is an outstanding site to achieve the goals of the MER mission. The crater could have collected sediments from a variety of sources during its 3.9 Ga history, including fluvial, lacustrine, volcanic, glacial, impact, regional and local aeolian, and global air falls. It is a unique site to investigate the past history of water on Mars, climate and geological changes, and the potential habitability of the planet, which are central science objectives of the MER mission. Because of its complex history and potential diversity, Gusev will allow the testing of a large spectrum of hypotheses with the complete suite of MER instruments. Evidence consistent with long-lived lake episodes exist in the landing ellipse area. They might offer a unique opportunity to study, for the first time, Martian aqueous sediments and minerals formed in situ in their geological context. We review the geological history and diversity of the landing site, the science hypotheses that can be tested during the MER mission, and the relevance of Gusev to the MER mission objectives and payload. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. US Geol Survey, Menlo Pk, CA 94025 USA. Arizona State Univ, Dept Geol, Tempe, AZ 85287 USA. Russian Acad Sci, Vernadsky Inst, Moscow 117975, Russia. Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. US Geol Survey, Flagstaff, AZ 86002 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. Univ Texas, Dept Sci & Math Educ, Richardson, TX 75083 USA. Schreder Planetarium, Redding, CA 96001 USA. Univ Mississippi, Dept Geol, Jackson, MS 39216 USA. Mars Soc France, F-92150 Suresnes, France. RP NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM ncabrol@mail.arc.nasa.gov; egrin@mail.arc.nasa.gov; carr@usgs.gov; bsutter@mail.arc.nasa.gov; jmoore@mail.arc.nasa.gov; jfarmer@asu.edu; greeley@asu.edu; rok@geokhi.ru; david_desmarais@qmgate.arc.nas; kramerm@fsl.orst.edu; newsom@unm.edu; ivan.e.thorsos@jpl.nasa.gov; ktanaka@usgs.gov; nadine.barlow@nau.edu; ngb@physics.ucf.edu; urquhart@utdallas.edu; brian@projectarise.org; goursac@club-internet.fr RI Fike, David/D-3634-2011 OI Fike, David/0000-0003-2848-0328 NR 100 TC 31 Z9 31 U1 4 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 30 PY 2003 VL 108 IS E12 AR 8076 DI 10.1029/2002JE002026 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 761JY UT WOS:000187898300001 ER PT J AU Sun, G Ranson, KJ Khairuk, VI Kovacs, K AF Sun, G Ranson, KJ Khairuk, VI Kovacs, K TI Validation of surface height from shuttle radar topography mission using shuttle laser altimeter SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE shuttle radar topography mission (SRTM); shuttle laser altimeter (SLA); interferometric SAR; DEM; lidar waveform; tree height ID WESTERN SAYANI MOUNTAINS; INTERFEROMETRIC RADAR; TROPICAL FOREST; SAR DATA; LIDAR; VEGETATION; GEOLOCATION; RETURNS; SIBERIA AB Spaceborne Interferometric SAR (InSAR) technology used in the Shuttle Radar Topography Mission (SRTM) and spaceborne lidar such as Shuttle Laser Altimeter-02 (SLA-02) are two promising technologies for providing global scale digital elevation models (DEMs). Each type of these systems has limitations that affect the accuracy or extent of coverage. These systems are complementary in developing DEM data. In this study, surface height measured independently by SRTM and SLA-02 was cross-validated. SLA data was first verified by field observations, and examinations of individual lidar waveforms. The geolocation accuracy of the SLA height data sets was examined by checking the correlation between the SLA surface height with SRTM height at 90 in resolution, while shifting the SLA ground track within its specified horizontal errors. It was found that the heights from the two instruments were highly correlated along the SLA ground track, and shifting the positions did not improve the correlation significantly. Absolute surface heights from SRTM and SLA referenced to the same horizontal and vertical datum (World Geodetic System (WGS) 84 Ellipsoid) were compared. The effects of forest cover and surface slope on the height difference were also examined. After removing the forest effect on SRTM height, the mean height difference with SLA-02 was near zero. It can be further inferred from the standard deviation of the height differences that the absolute accuracy of SRTM height at low vegetation area is better than the SRTM mission specifications (16 in). The SRTM height bias caused by forest cover needs to be further examined using future spaceborne lidar (e.g. GLAS) data. (C) 2003 Elsevier Inc. All rights reserved. C1 Univ Maryland, Dept Geog, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. VN Sukachev Inst Forest, Krasnoyarsk, Russia. Sci Syst & Applicat Inc, Lanham, MD 20706 USA. RP Sun, G (reprint author), Univ Maryland, Dept Geog, College Pk, MD 20742 USA. RI Ranson, Kenneth/G-2446-2012 OI Ranson, Kenneth/0000-0003-3806-7270 NR 28 TC 100 Z9 113 U1 2 U2 18 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC 30 PY 2003 VL 88 IS 4 BP 401 EP 411 DI 10.1016/j.rse.2003.09.001 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 754TF UT WOS:000187347100004 ER PT J AU Bewley, WW Kim, CS Kim, M Canedy, CL Lindle, JR Vurgaftman, I Meyer, JR Muller, RE Echternach, PM Kaspi, R AF Bewley, WW Kim, CS Kim, M Canedy, CL Lindle, JR Vurgaftman, I Meyer, JR Muller, RE Echternach, PM Kaspi, R TI Broad-stripe midinfrared photonic-crystal distributed-feedback lasers with laser-ablation confinement SO APPLIED PHYSICS LETTERS LA English DT Article ID BEAM QUALITY AB We investigate broad-stripe photonic-crystal distributed-feedback lasers emitting at lambda=4.4 mum. The beam quality improves dramatically when a laser ablation technique is used to eliminate parasitic Fabry-Perot-like modes, by inducing loss in the regions adjoining the pump stripe. Even though the peak of the gain spectrum never fully aligns with the grating resonance, for pulsed pumping the output beam is essentially diffraction limited up to a stripe width of 150 mum, and remains no worse than six times the diffraction limit for stripes as broad as 400 mum. (C) 2003 American Institute of Physics. C1 USN, Res Lab, Washington, DC 20375 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. USAF, Res Lab, Kirtland AFB, Albuquerque, NM 87110 USA. RP Bewley, WW (reprint author), USN, Res Lab, Washington, DC 20375 USA. RI Lindle, James/A-9426-2009 NR 13 TC 10 Z9 10 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD DEC 29 PY 2003 VL 83 IS 26 BP 5383 EP 5385 DI 10.1063/1.1637153 PG 3 WC Physics, Applied SC Physics GA 757ET UT WOS:000187536400013 ER PT J AU Jones, DBA Bowman, KW Palmer, PI Worden, JR Jacob, DJ Hoffman, RN Bey, I Yantosca, RM AF Jones, DBA Bowman, KW Palmer, PI Worden, JR Jacob, DJ Hoffman, RN Bey, I Yantosca, RM TI Potential of observations from the Tropospheric Emission Spectrometer to constrain continental sources of carbon monoxide SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE TES; carbon monoxide; inverse methods ID AIRCRAFT OBSERVATIONS; SPECTRAL RADIANCES; OZONE; CO; ASSIMILATION; SPACE; INSTRUMENT; SATELLITE; MODEL; SIMULATIONS AB We have conducted an observing system simulation experiment for the Tropospheric Emission Spectrometer (TES) satellite instrument to determine the potential of nadir retrievals of carbon monoxide (CO) from this instrument to constrain estimates of continental sources of CO. We use the GEOS-CHEM global chemical transport model to produce a pseudoatmosphere in which the relationship between sources and concentrations of CO is known. Linear profile retrievals of CO are calculated by sampling this pseudoatmosphere along the orbit of TES. These retrievals are used as pseudo-observations with a maximum a posteriori inverse algorithm to estimate the CO sources from the different continents. This algorithm accounts for the finite vertical resolution of the retrieval, instrument errors, and representation and transport errors in the GEOSCHEM simulation of CO. The structure of the transport error is estimated using the statistics of the difference between paired GEOS-CHEM forecasts of CO, and this structure is then scaled to match the model error in the GEOS-CHEM simulation of aircraft observations of Asian outflow over the NW Pacific. We show that with proper characterization of observation errors just 2 weeks of observations from TES have the potential to constrain estimates of continental sources of CO to within 10%. C1 Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Atmospher & Environm Res Inc, Lexington, MA 02421 USA. Swiss Fed Inst Technol EPFL, CH-1015 Lausanne, Switzerland. RP Jones, DBA (reprint author), Harvard Univ, Div Engn & Appl Sci, Pierce Hall,29 Oxford St, Cambridge, MA 02138 USA. EM dbj@io.harvard.edu RI Palmer, Paul/F-7008-2010; Yantosca, Robert/F-7920-2014; Jones, Dylan/O-2475-2014; Chem, GEOS/C-5595-2014 OI Yantosca, Robert/0000-0003-3781-1870; Jones, Dylan/0000-0002-1935-3725; NR 27 TC 45 Z9 47 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 26 PY 2003 VL 108 IS D24 AR 4789 DI 10.1029/2003JD003702 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 760ZQ UT WOS:000187865500002 ER PT J AU Hoge, FE Lyon, PE Mobley, CD Sundman, LK AF Hoge, FE Lyon, PE Mobley, CD Sundman, LK TI Radiative transfer equation inversion: Theory and shape factor models for retrieval of oceanic inherent optical properties SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE remote sensing; optical oceanography; inverse modeling; radiative transfer theory ID REMOTELY-SENSED REFLECTANCE; SATELLITE RETRIEVAL; THEORETICAL DERIVATION; RADIANCE MODEL; VARIABILITY; DEPENDENCE; WATERS; COLOR; NM AB It is shown that the in-water, shape factor formulation of the radiative transfer equation (RTE) (1) yields exact in-air expressions for the remote sensing reflectance R-rs and the equivalent remotely sensed reflectance RSRa and (2) can be configured for inherent optical property (IOP) retrievals using standard linear matrix inversion methods. Inversion of the shape factor RTE is exact in the sense that no approximations are made to the RTE. Thus errors in retrieved IOPs are produced only by uncertainties in (1) the models for the shape factors and related quantities and (2) the IOP models required for inversion. Hydrolight radiative transfer calculations are used to derive analytical models for the necessary backscattering shape factor, radiance shape factor, fractional forward scattering coefficient, ratio of air-to-water mean cosines, and diffuse attenuation coefficient for in-water upwelling radiance. These models predict the various shape factors with accuracies ranging typically from 2 to 20%. Using the modeled shape factors the in-air remotely sensed reflectance RSRa can be predicted to within 20% of the correct (Hydrolight-computed) values 96% of the time (or +/-0.0005 sr(-1) 86% of the time) for the synthetic data used to determine the shape factor models. Inversion of this shape factor RTE using field data is a comprehensive study to be published in a later paper. C1 NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. EG&G Inc, Wallops Flight Facil, Wallops Isl, VA 23337 USA. Sequoia Sci Inc, Westpk Tech Ctr, Redmond, WA 98052 USA. RP Hoge, FE (reprint author), NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA. NR 21 TC 3 Z9 4 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC 26 PY 2003 VL 108 IS C12 AR 3386 DI 10.1029/2000JC000447 PG 14 WC Oceanography SC Oceanography GA 760ZU UT WOS:000187865800001 ER PT J AU Gorevan, SP Myrick, T Davis, K Chau, JJ Bartlett, P Mukherjee, S Anderson, R Squyres, SW Arvidson, RE Madsen, MB Bertelsen, P Goetz, W Binau, CS Richter, L AF Gorevan, SP Myrick, T Davis, K Chau, JJ Bartlett, P Mukherjee, S Anderson, R Squyres, SW Arvidson, RE Madsen, MB Bertelsen, P Goetz, W Binau, CS Richter, L TI Rock Abrasion Tool: Mars exploration Rover mission SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE RAT; grinding; IDD; payload; rocks; instrument AB [1] The Rock Abrasion Tool (RAT) is an integral part of the Athena Science payload. Serving primarily as the geologist's rock hammer, the RAT will expose fresh surfaces of Martian rocks to other instruments on the payload. The RAT also brushes dust and debris from an excavated hole or unaltered rocks. To accomplish these tasks autonomously, the RAT, a sophisticated 3-axis precision-controlled device, was designed. Data products derived from RAT telemetry enable the RAT to also act as an important rock physical properties science instrument. The returned RAT grinding and penetration rate data will be inverted and compared to a rock library on the Earth. The design is also very compact and lightweight: the RAT is contained within a cylinder 128 mm long and 85 mm in diameter and has a mass of 687 g. C1 Honeybee Robot, New York, NY 10012 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Univ Copenhagen, Niels Bohr Inst Astron Phys & Geophys, Ctr Planetary Sci, DK-2100 Copenhagen, Denmark. DLR, German Aerosp Ctr, Inst Space Simulat, Cologne, Germany. Cornell Univ, Dept Astron, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. RP Honeybee Robot, 204 Elizabeth St, New York, NY 10012 USA. EM gorevan@honeybeerobotics.com RI Madsen, Morten/D-2082-2011 OI Madsen, Morten/0000-0001-8909-5111 NR 17 TC 69 Z9 69 U1 2 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 26 PY 2003 VL 108 IS E12 AR 8068 DI 10.1029/2003JE002061 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 760ZX UT WOS:000187866100001 ER PT J AU Squyres, SW Arvidson, RE Baumgartner, ET Bell, JF Christensen, PR Gorevan, S Herkenhoff, KE Klingelhofer, G Madsen, MB Morris, RV Rieder, R Romero, RA AF Squyres, SW Arvidson, RE Baumgartner, ET Bell, JF Christensen, PR Gorevan, S Herkenhoff, KE Klingelhofer, G Madsen, MB Morris, RV Rieder, R Romero, RA TI Athena Mars rover science investigation SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; Rover; payload ID MARTIAN ATMOSPHERE; DUST; PATHFINDER; MISSION; ANALOG; ROCKS; WATER AB [1] Each Mars Exploration Rover carries an integrated suite of scientific instruments and tools called the Athena science payload. The primary objective of the Athena science investigation is to explore two sites on the Martian surface where water may once have been present, and to assess past environmental conditions at those sites and their suitability for life. The remote sensing portion of the payload uses a mast called the Pancam Mast Assembly (PMA) that provides pointing for two instruments: the Panoramic Camera ( Pancam), and the Miniature Thermal Emission Spectrometer (Mini-TES). Pancam provides high-resolution, color, stereo imaging, while Mini-TES provides spectral cubes at mid-infrared wavelengths. For in-situ study, a five degree-of-freedom arm called the Instrument Deployment Device (IDD) carries four more tools: a Microscopic Imager (MI) for close-up imaging, an Alpha Particle X-Ray Spectrometer (APXS) for elemental chemistry, a Mossbauer Spectrometer (MB) for the mineralogy of Fe-bearing materials, and a Rock Abrasion Tool ( RAT) for removing dusty and weathered surfaces and exposing fresh rock underneath. The payload also includes magnets that allow the instruments to study the composition of magnetic Martian materials. All of the Athena instruments have undergone extensive calibration, both individually and using a set of geologic reference materials that are being measured with all the instruments. Using a MER-like rover and payload in a number of field settings, we have devised operations processes that will enable us to use the MER rovers to formulate and test scientific hypotheses concerning past environmental conditions and habitability at the landing sites. C1 Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ USA. Honeybee Robot, New York, NY 10012 USA. US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. Johannes Gutenberg Univ Mainz, Inst Anorgan Chem & Analyt Chem, D-55099 Mainz, Germany. Univ Copenhagen, Niels Bohr Inst, Orsted Lab, DK-2100 Copenhagen, Denmark. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Max Planck Inst Chem, D-55128 Mainz, Germany. RP Cornell Univ, Ctr Radiophys & Space Res, 428 Space Sci Bldg, Ithaca, NY 14853 USA. EM squyres@astro.cornell.edu RI de Souza, Paulo/B-8961-2008; Madsen, Morten/D-2082-2011 OI de Souza, Paulo/0000-0002-0091-8925; Madsen, Morten/0000-0001-8909-5111 NR 38 TC 152 Z9 153 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 26 PY 2003 VL 108 IS E12 AR 8062 DI 10.1029/2003JE002121 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 760ZX UT WOS:000187866100002 ER PT J AU Ansmann, A Bosenberg, J Chaikovsky, A Comeron, A Eckhardt, S Eixmann, R Freudenthaler, V Ginoux, P Komguem, L Linne, H Marquez, MAL Matthias, V Mattis, I Mitev, V Muller, D Music, S Nickovic, S Pelon, J Sauvage, L Sobolewsky, P Srivastava, MK Stohl, A Torres, O Vaughan, G Wandinger, U Wiegner, M AF Ansmann, A Bosenberg, J Chaikovsky, A Comeron, A Eckhardt, S Eixmann, R Freudenthaler, V Ginoux, P Komguem, L Linne, H Marquez, MAL Matthias, V Mattis, I Mitev, V Muller, D Music, S Nickovic, S Pelon, J Sauvage, L Sobolewsky, P Srivastava, MK Stohl, A Torres, O Vaughan, G Wandinger, U Wiegner, M TI Long-range transport of Saharan dust to northern Europe: The 11-16 October 2001 outbreak observed with EARLINET SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE mineral dust; lidar network ID AEROSOL SPATIAL-DISTRIBUTION; TO-BACKSCATTER RATIO; RAMAN LIDAR; OPTICAL-PROPERTIES; MULTIWAVELENGTH LIDAR; AIRCRAFT MEASUREMENTS; VERTICAL STRUCTURE; AIRBORNE LIDAR; INDIAN-OCEAN; EXTINCTION AB [1] The spread of mineral particles over southwestern, western, and central Europe resulting from a strong Saharan dust outbreak in October 2001 was observed at 10 stations of the European Aerosol Research Lidar Network (EARLINET). For the first time, an optically dense desert dust plume over Europe was characterized coherently with high vertical resolution on a continental scale. The main layer was located above the boundary layer ( above 1-km height above sea level (asl)) up to 3 - 5- km height, and traces of dust particles reached heights of 7 - 8 km. The particle optical depth typically ranged from 0.1 to 0.5 above 1-km height asl at the wavelength of 532 nm, and maximum values close to 0.8 were found over northern Germany. The lidar observations are in qualitative agreement with values of optical depth derived from Total Ozone Mapping Spectrometer ( TOMS) data. Ten-day backward trajectories clearly indicated the Sahara as the source region of the particles and revealed that the dust layer observed, e. g., over Belsk, Poland, crossed the EARLINET site Aberystwyth, UK, and southern Scandinavia 24 - 48 hours before. Lidar-derived particle depolarization ratios, backscatter- and extinction-related Angstrom exponents, and extinction-to-backscatter ratios mainly ranged from 15 to 25%, - 0.5 to 0.5, and 40 - 80 sr, respectively, within the lofted dust plumes. A few atmospheric model calculations are presented showing the dust concentration over Europe. The simulations were found to be consistent with the network observations. C1 Leibniz Inst Tropospharenforsch, D-04318 Leipzig, Germany. Max Planck Inst Meteorol, D-20146 Hamburg, Germany. Natl Acad Sci Belarus, Inst Phys, Minsk 220072, Byelarus. Univ Politecn Cataluna, Dept TSC, ES-08034 Barcelona, Spain. Tech Univ Munich, D-85354 Freising Weihenstephan, Germany. Leibniz Inst Atmospharenphys, D-18225 Kuhlungsborn, Germany. Univ Munich, Inst Meteorol, D-80333 Munich, Germany. NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08542 USA. Univ Wales, Dept Phys, Aberystwyth SY23 3BZ, Ceredigion, Wales. Observ Cantonal, Neuchatel, Switzerland. Univ Malta, Euromediterranean Ctr Insular Coastal Dynam, Valletta, Malta. Univ Paris 06, CNRS, Serv Aeron, F-75252 Paris, France. Inst Pierre Simon Laplace, Meteorol Dynam Lab, F-91128 Palaiseau, France. Polish Acad Sci, Inst Geophys, PL-01452 Warsaw, Poland. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Leibniz Inst Tropospharenforsch, Permoserstr 15, D-04318 Leipzig, Germany. EM albert@tropos.de; boesenberg@dkrz.de; chaikov@dragon.bas-net.by; comeron@tsc.upc.es; sabine@forst.tu-muenchen.de; eixmann@iap-kborn.de; volker.freudenthaler@meteo.physik.uni-muenchen.de; paul.ginoux@noaa.gov; llk@aber.ac.uk; linne@dkrz.de; malopez@tsc.upc.es; matthias@dkrz.de; ina@tropos.de; valentin.mitev@ne.ch; detlef@tropos.de; s.music@icod.org.mt; nicko@icod.org.mt; jacques.pelon@aero.jussieu.fr; laurent.sauvage@lmd.polytechnique.fr; pss@ra.onet.pl; manoj.srivastava@ne.ch; as@forst.tu-muenchen.de; torres@tparty.gsfc.nasa.gov; gxv@aber.ac.uk; ulla@tropos.de; m.wiegner@meteo.physik.uni-muenchen.de RI Stohl, Andreas/A-7535-2008; Ginoux, Paul/C-2326-2008; Comeron, Adolfo/M-5507-2013; Wandinger, Ulla/E-3348-2014; Linne, Holger/J-8510-2014; Wiegner, Matthias/F-8484-2011; Torres, Omar/G-4929-2013; MUELLER, DETLEF/F-1010-2015; Vaughan, Geraint/O-2459-2015; Eckhardt, Sabine/I-4001-2012 OI Stohl, Andreas/0000-0002-2524-5755; Ginoux, Paul/0000-0003-3642-2988; Comeron, Adolfo/0000-0001-6886-3679; Linne, Holger/0000-0003-3188-0429; MUELLER, DETLEF/0000-0002-0203-7654; Vaughan, Geraint/0000-0002-0885-0398; Eckhardt, Sabine/0000-0001-6958-5375 NR 44 TC 137 Z9 139 U1 1 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 24 PY 2003 VL 108 IS D24 AR 4783 DI 10.1029/2003JD003757 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 760ZP UT WOS:000187865400006 ER PT J AU Koch, D Park, J Del Genio, A AF Koch, D Park, J Del Genio, A TI Clouds and sulfate are anticorrelated: A new diagnostic for global sulfur models SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosol ID HIGH-FREQUENCY SEISMOGRAMS; AEROSOL; VARIABILITY; SENSITIVITY; ISCCP AB [1] We consider the correlation between clouds and sulfate in order to assess the relative importance of cloud aqueous-phase production of sulfate, precipatation scavenging of sulfate, and inhibition of gas-phase sulfate production beneath clouds. Statistical analysis of observed daily cloud cover and sulfate surface concentrations in Europe and North America indicates a significant negative correlation between clouds and sulfate. This implies that clouds remove sulfate via precipitation scavenging and/or inhibit sulfate gas-phase production more than they enhance sulfate concentration through aqueous-phase production. Persistent sulfate/cloud anticorrelations at long timescales (8 - 64 days) apparently result from large-scale dynamical influences on clouds, which in turn impact sulfate. A statistical analysis of output from the general circulation model (GCM) of the Goddard Institute for Space Studies (GISS) shows weak coherence between sulfate and cloud cover. However, there is stronger anticorrelation between the model's sulfate generated by gas-phase oxidation and cloud cover. Sulfate/cloud anticorrelation in the GCM strengthens if we extinguish gas-phase sulfate production beneath clouds, as should happen since the oxidant OH is photochemically generated. However the only way to achieve strong anticorrelation between total sulfate and clouds is by correcting our treatment of aqueous-phase sulfate production. Our model, like many other global tracer models, released dissolved species ( including sulfate) from clouds after each cloud time step rather than making release contingent upon cloud evaporation. After correcting this in the GISS model, more sulfate is rained out, the sulfate burden produced via the aqueous phase decreases to half its former amount, and the total sulfate burden is 25% lower. C1 Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Yale Univ, Dept Geol & Geophys, New Haven, CT 06520 USA. RP Koch, D (reprint author), Columbia Univ, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM dkoch@giss.nasa.gov; jeffrey.park@yale.edu RI Del Genio, Anthony/D-4663-2012 OI Del Genio, Anthony/0000-0001-7450-1359 NR 22 TC 31 Z9 31 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 24 PY 2003 VL 108 IS D24 AR 4781 DI 10.1029/2003JD003621 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 760ZP UT WOS:000187865400005 ER PT J AU Mills, FP Cageao, RP Sander, SP Allen, M Yung, YL Remsberg, EE Russell, JM Richter, U AF Mills, FP Cageao, RP Sander, SP Allen, M Yung, YL Remsberg, EE Russell, JM Richter, U TI OH column abundance over Table Mountain Facility, California: Intra-annual variations and comparisons to model predictions for 1997-2001 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE hydroxyl; mesosphere; photochemistry ID MIDDLE ATMOSPHERE; FRITZ-PEAK; DOPPLER DETECTION; STRATOSPHERIC OH; HYDROXYL; PHOTOCHEMISTRY; O-3; H2O; SPECTROSCOPY; SPECTROMETER AB [1] Measurements of the OH column abundance over the Jet Propulsion Laboratory's Table Mountain Facility (TMF) have been made since July 1997 at 10degrees - 80degrees solar zenith angle using a Fourier transform ultraviolet spectrometer. The measured OH column at any solar zenith angle is typically larger in the afternoon than in the morning. The variations observed in the OH column abundance appear to result from changes in atmospheric conditions on a daily or longer timescale. The larger observed variations are statistically significant. Sensitivity coefficients describing how the OH column abundance is expected to change in response to changes in the concentrations of H2O, O-3, NO, CO, and CH4 have been calculated on the basis of an analytic model. On the basis of these sensitivity coefficients and Halogen Occultation Experiment observations of O-3, the net sensitivity of the OH column abundance to variations in O-3 should be close to zero. The observed OH column abundance over TMF increased by about 25% from July 1997 to December 2001. This interannual trend in OH column abundance is not consistent with calculations that incorporate observed trends in H2O and O-3 and is at least a factor of 2 larger than the calculated difference between solar minimum and maximum. Comparisons between measured and calculated normalized OH column abundances suggest that the sensitivity of OH to variations in H2O may be a factor of 2 larger than predicted in present models and that there is some other major driver for the observed variability in the OH column abundance that was not included in the present analysis. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. RP Mills, FP (reprint author), Australian Natl Univ, Res Sch Phys Sci & Engn, Canberra, ACT 0200, Australia. EM frank.mills@anu.edu.au NR 36 TC 5 Z9 5 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 24 PY 2003 VL 108 IS D24 AR 4785 DI 10.1029/2003JD003481 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 760ZP UT WOS:000187865400003 ER PT J AU Comiso, JC Yang, JY Honjo, S Krishfield, RA AF Comiso, JC Yang, JY Honjo, S Krishfield, RA TI Detection of change in the Arctic using satellite and in situ data SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE Arctic Sea ice; climate change; surface temperature; wind; buoy; hydrography ID SEA-ICE COVER; BEAUFORT SEA; OCEAN; TEMPERATURE; SURFACE; WATER; VARIABILITY; GREENLAND; OSCILLATION; HYDROGRAPHY AB [1] The decade of the 1990s was the warmest decade of the last century, while the year 1998 was the warmest year ever observed by modern techniques, with 9 out of 12 months of the year being the warmest months. Satellite ice cover and surface temperature data, European Centre for Medium-Range Weather Forecasts (wind), and ocean hydrographic data are examined to gain insights into this warming phenomenon. Areas of ice-free water in both western and eastern regions of the Arctic are found to have followed a cyclical pattern with approximately decadal period but with a lag of about 3 years between the eastern and western regions. The pattern was interrupted by unusually large anomalies in 1993 and 1998 in the western region and in 1995 in the eastern region. The area of open water in 1998 was the largest ever observed in the western region and occurred concurrently with large surface temperature anomalies in the area and adjacent regions. This also occurred at a time when the atmospheric circulation changed from predominantly cyclonic in 1996 to anticyclonic in 1997 and 1998. Detailed hydrographic measurements over the same general area in April 1996 and April 1997 indicate a warming and significant freshening in the top layer of the ocean, suggesting increases in ice melt and/or river runoff. Continuous ocean temperature and salinity data from ocean buoys at depths of 8, 45, and 75 m confirm these results and show large interannual changes during the 1996-1998 period. Surface temperature data show a general warming in the region that is highly correlated with observed decline in summer sea ice, while hydrographic data suggest that in 1997 and 1998, the upper part of the ocean was unusually fresh and warm compared to available data between 1956 and 1996. C1 NASA, Goddard Space Flight Ctr, Lab Hydrospher Proc, Greenbelt, MD 20771 USA. Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. RP Comiso, JC (reprint author), NASA, Goddard Space Flight Ctr, Lab Hydrospher Proc, Greenbelt, MD 20771 USA. NR 46 TC 36 Z9 36 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC 24 PY 2003 VL 108 IS C12 AR 3384 DI 10.1029/2002JC001347 PG 24 WC Oceanography SC Oceanography GA 760ZT UT WOS:000187865700001 ER PT J AU Anderson, FS Haldemann, AFC Bridges, NT Golombek, MP Parker, TJ Neumann, G AF Anderson, FS Haldemann, AFC Bridges, NT Golombek, MP Parker, TJ Neumann, G TI Analysis of MOLA data for the Mars Exploration Rover landing sites SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars Exploration Rover; landing site; slope; roughness; Hurst; topography ID ORBITER LASER ALTIMETER; RADAR SCATTERING; ROUGHNESS; TOPOGRAPHY; SURFACE AB We have used Mars Orbiter Laser Altimeter (MOLA) data to demonstrate that selected landing sites meet the Mars Exploration Rover (MER) landing system topography and slope requirements at hectometer and kilometer scales. To provide a comprehensive analysis, we constrained slopes within each landing ellipse using four approaches: (1) measurements of local slopes at 1.2 km length scales using both an adirectional maximum gradient method and a higher-resolution bidirectional, along-track method, (2) predictions of 100 m slopes using self-affine statistics in conjunction with (3) calculations of both pulse width and slope corrected pulse width to constrain slopes at scales smaller than the MOLA spot size (<180 m), and (4) comparisons of simultaneously acquired MOLA data with Mars Orbiter Camera data to identify the geomorphologic features associated with variations in observed slopes, pulse width, and, for this analysis only, reflectivity. The results of the analysis indicate that the selected landing sites are consistent with the MER topography requirement of being below -1.3 km, as well as having slopes less than 5&DEG; at length scales of 100 m and <2degrees at length scales of 1.2 km. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Anderson, FS (reprint author), Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, 1680 East West Rd, Honolulu, HI 96822 USA. RI Neumann, Gregory/I-5591-2013; Bridges, Nathan/D-6341-2016 OI Neumann, Gregory/0000-0003-0644-9944; NR 29 TC 9 Z9 9 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 24 PY 2003 VL 108 IS E12 AR 8084 DI 10.1029/2003JE002125 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 760ZW UT WOS:000187866000002 ER PT J AU Christensen, PR Mehall, GL Silverman, SH Anwar, S Cannon, G Gorelick, N Kheen, R Tourville, T Bates, D Ferry, S Fortuna, T Jeffryes, J O'Donnell, W Peralta, R Wolverton, T Blaney, D Denise, R Rademacher, J Morris, RV Squyres, S AF Christensen, PR Mehall, GL Silverman, SH Anwar, S Cannon, G Gorelick, N Kheen, R Tourville, T Bates, D Ferry, S Fortuna, T Jeffryes, J O'Donnell, W Peralta, R Wolverton, T Blaney, D Denise, R Rademacher, J Morris, RV Squyres, S TI Miniature Thermal Emission Spectrometer for the Mars Exploration Rovers SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; IR spectroscopy; mineralogy; Mars surface ID PARTICULATE PLANETARY SURFACES; INFRARED-EMISSION; REFLECTANCE SPECTRA; MARTIAN SURFACE; PARTICLE-SIZE; MU-M; SEASONAL CAP; ICE CLOUDS; SPECTROSCOPY; ROCKS AB The Miniature Thermal Emission Spectrometer (Mini-TES) will provide remote measurements of mineralogy and thermophysical properties of the scene surrounding the Mars Exploration Rovers and guide the rovers to key targets for detailed in situ measurements by other rover experiments. The specific scientific objectives of the Mini-TES investigation are to (1) determine the mineralogy of rocks and soils, (2) determine the thermophysical properties of selected soil patches, and (3) determine the temperature profile, dust and water-ice opacity, and water vapor abundance in the lower atmospheric boundary layer. The Mini-TES is a Fourier Transform Spectrometer covering the spectral range 5-29 mum (339.50 to 1997.06 cm(-1)) with a spectral sample interval of 9.99 cm(-1). The Mini-TES telescope is a 6.35-cm-diameter Cassegrain telescope that feeds a flat-plate Michelson moving mirror mounted on a voice-coil motor assembly. A single deuterated triglycine sulfate (DTGS) uncooled pyroelectric detector with proven space heritage gives a spatial resolution of 20 mrad; an actuated field stop can reduce the field of view to 8 mrad. Mini-TES is mounted within the rover's Warm Electronics Box and views the terrain using its internal telescope looking up the hollow shaft of the Pancam Mast Assembly (PMA) to the fixed fold mirror and rotating elevation scan mirror in the PMA head located similar to1.5 m above the ground. The PMA provides a full 360degrees of azimuth travel and views from 30degrees above the nominal horizon to 50degrees below. An interferogram is collected every two seconds and transmitted to the Rover computer, where the Fast Fourier Transform, spectral summing, lossless compression, and data formatting are performed prior to transmission to Earth. Radiometric calibration is provided by two calibration V-groove blackbody targets instrumented with platinum thermistor temperature sensors with absolute temperature calibration of +/-0.1degreesC. One calibration target is located inside the PMA head; the second is on the Rover deck. The Mini-TES temperature is expected to vary diurnally from -10 to +30degreesC, with most surface composition data collected at scene temperatures >270 K. For these conditions the radiometric precision for two-spectra summing is +/-1.8x10(-8) W cm(-2) sr(-1)/cm(-1) between 450 and 1500 cm(-1), increasing to similar to4.2x10(-8) W cm(-2) sr(-1)/cm(-1) at shorter (300 cm(-1)) and longer (1800 cm(-1)) wave numbers. The absolute radiance error will be <5x10(-8) W cm(-2) sr(-1)/cm(-1), decreasing to similar to 1x10(-8) W cm(-2) sr(-1)/cm(-1) over the wave number range where the scene temperature will be determined (1200-1600 cm(-1)). The worst-case sum of these random and systematic radiance errors corresponds to an absolute temperature error of similar to 0.4 K for a true surface temperature of 270 K and similar to 1.5 K for a surface at 180 K. The Mini-TES will be operated in a 20-mrad panorama mode and an 8-mrad targeted mode, producing two-dimensional rasters and three-dimensional hyperspectral image cubes of varying sizes. The overall Mini-TES envelope size is 23.5 x 16.3 x 15.5 cm, and the mass is 2.40 kg. The power consumption is 5.6 W average. The Mini-TES was developed by Arizona State University and Raytheon Santa Barbara Remote Sensing. C1 Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Raytheon Santa Barbara Remote Sensing, Goleta, CA 93117 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Arizona State Univ, Dept Geol Sci, Campus Box 876305, Tempe, AZ 85287 USA. EM phil.christensen@asu.edu NR 68 TC 90 Z9 90 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 24 PY 2003 VL 108 IS E12 AR 8064 DI 10.1029/2003JE002117 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 760ZW UT WOS:000187866000001 ER PT J AU Fairfield, DH Farrugia, CJ Mukai, T Nagai, T Fedorov, A AF Fairfield, DH Farrugia, CJ Mukai, T Nagai, T Fedorov, A TI Motion of the dusk flank boundary layer caused by solar wind pressure changes and the Kelvin-Helmholtz instability: 10-11 January 1997 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE KH instability; dusk flank boundary; magnetopause motion; magnetopause waves; pressure discontinuity effects ID INTERPLANETARY MAGNETIC-FIELD; NEAR-EARTH MAGNETOTAIL; GEOTAIL OBSERVATIONS; NORTHWARD IMF; BOW SHOCK; MAGNETOSPHERIC RESPONSE; PLASMA SHEET; MAGNETOPAUSE; MAGNETOSHEATH; WAVES AB During an interval of steady northward IMF on 10-11 January 1997, Geotail and Interball spacecraft data at X = -5 to -15 R-E on the dusk flank reveal magnetopause boundary layer motions caused by both solar wind pressure discontinuities and the Kelvin-Helmholtz instability. Several large, sudden changes in solar wind density caused the magnetopause to move across both spacecraft. Relative timing of these crossings along with corresponding geosynchronous and ground magnetic field changes allow study of the propagation of pressure fronts in the magnetosheath and the associated wave propagation in the magnetosphere. The wave in the boundary layer propagates down the tail faster than the pressure front in the magnetosheath, producing boundary motion ahead of the magnetosheath front. This boundary layer wave can bulge out the magnetopause, causing a spacecraft in the magnetosheath to become immersed in the magnetosphere for as long as 2 or 3 min before the higher density magnetosheath plasma arrives and compresses the boundary. The tailward convecting magnetosheath pressure front moves more slowly near the magnetopause than it does further out in the magnetosheath, distorting the front and enhancing the likelihood that the boundary layer wave will outrun the magnetosheath front. Integrating the velocity perpendicular to the boundary shows that the boundary waves can have amplitudes of at least 1 or 2 Re. During periods of steady solar wind pressure, waves with periods of several minutes are observed in a boundary layer that are consistent with exitation of the Kelvin-Helmholtz instability. Magnetograms from five ground magnetometer chains show both pulsations initiated by the pressure discontinuities and ongoing wave trains probably related to the KH instability. C1 NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Greenbelt, MD 20771 USA. Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. Tokyo Inst Technol, Tokyo 1528551, Japan. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. RP NASA, Goddard Space Flight Ctr, Extraterr Phys Lab, Mail Code 695, Greenbelt, MD 20771 USA. EM donald.h.fairfield@nasa.gov; charlie.farrugia@unh.edu; mukai@stp.isas.ac.jp; nagai@geo.titech.ac.jp; andrei.federov@cesr.fr NR 46 TC 18 Z9 18 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 24 PY 2003 VL 108 IS A12 AR 1460 DI 10.1029/2003JA010134 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 761AB UT WOS:000187866500006 ER PT J AU Procopio, AS Remer, LA Artaxo, P Kaufman, YJ Holben, BN AF Procopio, AS Remer, LA Artaxo, P Kaufman, YJ Holben, BN TI Modeled spectral optical properties for smoke aerosols in Amazonia SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SKY RADIANCE MEASUREMENTS; BIOMASS-BURNING AEROSOLS; SINGLE SCATTERING ALBEDO; SAFARI 2000; SCAR-B; BRAZIL; SUN; IRRADIANCE; PARTICLES; RETRIEVAL AB The optical properties of aerosols from biomass burning in Brazil were derived from measurements by the AERONET sun photometer network in Amazonia. A dynamical aerosol model was constructed from Mie Theory calculations, using as input a constant complex refractive index and the average size distribution of aerosols for 12 ranges of aerosol optical thickness. The aerosol optical properties were described for 24 wavelengths in the spectral range of 0.20-3.00 mum. The model was used to simulate radiances and irradiances and the results agreed well with the measurements. The derived optical model is immediately applicable to estimate aerosol forcing by biomass burning aerosol emitted on the development frontier in Amazonia. C1 Univ Sao Paulo, Inst Fis, Dept Fis Aplicada, BR-05508900 Sao Paulo, Brazil. NASA, Goddard Space Flight Ctr, Terr Phys Lab, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Procopio, AS (reprint author), Univ Sao Paulo, Inst Fis, Dept Fis Aplicada, Rua Matao,Travessa R,187, BR-05508900 Sao Paulo, Brazil. RI Procopio, Aline/B-3367-2008; Procopio, Aline/L-7483-2013; Artaxo, Paulo/E-8874-2010 OI Procopio, Aline/0000-0002-2326-2500; Artaxo, Paulo/0000-0001-7754-3036 NR 30 TC 24 Z9 24 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 23 PY 2003 VL 30 IS 24 AR 2265 DI 10.1029/2003GL018063 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 760ZG UT WOS:000187864700001 ER PT J AU Trent, JD Kagawa, HK Paavola, CD McMillan, RA Howard, J Jahnke, L Lavin, C Embaye, T Henze, CE AF Trent, JD Kagawa, HK Paavola, CD McMillan, RA Howard, J Jahnke, L Lavin, C Embaye, T Henze, CE TI Intracellular localization of a group II chaperonin indicates a membrane-related function SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID HEAT-SHOCK PROTEINS; ARCHAEON SULFOLOBUS-SOLFATARICUS; T-COMPLEX POLYPEPTIDE-1; ACQUIRED THERMOTOLERANCE; SUBCELLULAR-LOCALIZATION; THERMOPHILIC ARCHAEBACTERIUM; HYPERTHERMOPHILIC ARCHAEON; MOLECULAR CHAPERONES; TETRAETHER LIPIDS; BINDING PROTEIN AB Chaperon ins are protein complexes that are believed to function as part of a protein folding system in the cytoplasm of the cell. We observed, however, that the group II chaperonins known as rosettasomes in the hyperthermophilic archaeon Sulfolobus shibatae, are not cytoplasmic but membrane associated. This association was observed in cultures grown at 60degreesC and 76degreesC or heat-shocked at 85degreesC by using immunofluorescence microscopy and in thick sections of rapidly frozen cells grown at 76degreesC by using immunogold electron microscopy. We observed that increased abundance of rosettasomes after heat shock correlated with decreased membrane permeability at lethal temperature (92degreesC). This change in permeability was not seen in cells heat-shocked in the presence of the amino acid analogue azetidine 2-carboxylic acid, indicating functional protein synthesis influences permeability. Azetidine experiments also indicated that observed heat-induced changes in lipid composition in S. shibatae could not account for changes in membrane permeability. Rosettasomes purified from cultures grown at 60degreesC and 76degreesC or heat-shocked at 85degreesC bind to liposomes made from either the bipolar tetraether lipids of Sulfolobus or a variety of artificial lipid mixtures. The presence of rosettasomes did not significantly change the transition temperature of liposomes, as indicated by differential scanning calorimetry, or the proton permeability of liposomes, as indicated by pyranine fluorescence. We propose that these group II chaperonins function as a structural element in the natural membrane based on their intracellular location, the correlation between their functional abundance and membrane permeability, and their potential distribution on the membrane surface. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. SETI Inst, Mountain View, CA 94043 USA. Univ Wisconsin, Integrated Microscopy Resource, Madison, WI 53706 USA. RP Trent, JD (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 54 TC 20 Z9 22 U1 0 U2 0 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD DEC 23 PY 2003 VL 100 IS 26 BP 15589 EP 15594 DI 10.1073/pnas.2136795100 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 757GL UT WOS:000187554600056 PM 14673104 ER PT J AU Sheard, BS Gray, MB McClelland, DE Shaddock, DA AF Sheard, BS Gray, MB McClelland, DE Shaddock, DA TI Laser frequency stabilization by locking to a LISA arm SO PHYSICS LETTERS A LA English DT Article DE LISA; gravitational wave detection; laser frequency stabilization AB We analyze a technique for suppressing laser frequency noise for the laser interferometer space antenna (LISA) gravitational wave detector. We demonstrate that the laser frequency can be stabilized to a LISA arm by high gain feedback. It is shown that the feedback bandwidth is not limited by the 33 second round-trip propagation time and example frequency controller designs are presented. (C) 2003 Elsevier B.V. All rights reserved. C1 Australian Natl Univ, Fac Sci, Dept Phys, Gravitat Wave Res Facil, Acton, ACT 0200, Australia. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sheard, BS (reprint author), Australian Natl Univ, Fac Sci, Dept Phys, Gravitat Wave Res Facil, Acton, ACT 0200, Australia. EM ben.sheard@anu.edu.au RI McClelland, David/E-6765-2010; Shaddock, Daniel/A-7534-2011 OI McClelland, David/0000-0001-6210-5842; Shaddock, Daniel/0000-0002-6885-3494 NR 13 TC 40 Z9 42 U1 2 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0375-9601 J9 PHYS LETT A JI Phys. Lett. A PD DEC 22 PY 2003 VL 320 IS 1 BP 9 EP 21 DI 10.1016/j.physleta.2003.10.076 PG 13 WC Physics, Multidisciplinary SC Physics GA 762ZP UT WOS:000188043100003 ER PT J AU Serjeant, S Farrah, D Geach, J Takagi, T Verma, A Kaviani, A Fox, M AF Serjeant, S Farrah, D Geach, J Takagi, T Verma, A Kaviani, A Fox, M TI The K-band Hubble diagram of submillimetre galaxies and hyperluminous galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : evolution; galaxies : formation; galaxies : starburst; cosmology : observations; infrared : galaxies; submillimetre ID ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMATION HISTORY; IRAS 1-JY SAMPLE; RADIO GALAXIES; HIGH-REDSHIFT; DEEP-FIELD; LUMINOSITY FUNCTION; SCUBA GALAXIES; QUASARS; IDENTIFICATIONS AB We present the K-band Hubble diagrams (K-z relations) of submillimetre-selected galaxies and hyperluminous galaxies (HLIRGs). We report the discovery of a remarkably tight K-z relation of HLIRGs, indistinguishable from that of the most luminous radio galaxies. Like radio galaxies, the HLIRG K-z relation at z less than or similar to 3 is consistent with a passively evolving similar to3L(*) instantaneous starburst starting from a redshift of z similar to 10 . In contrast, many submillimetre-selected galaxies are greater than or similar to2 mag fainter, and the population has a much larger dispersion. We argue that dust obscuration and/or a larger mass range may be responsible for this scatter. The galaxies so far proved to be hyperluminous may have been biased towards higher AGN bolometric contributions than submillimetre-selected galaxies due to the 60-mum selection of some, so the location on the K-z relation may be related to the presence of the most massive active galactic nucleus. Alternatively, a particular host galaxy mass range may be responsible for both extreme star formation and the most massive active nuclei. C1 Univ Kent, Sch Phys Sci, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NR, Kent, England. CALTECH, Jet Prop Lab, SIRTF Sci Ctr, Pasadena, CA 91125 USA. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2BW, England. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Serjeant, S (reprint author), Univ Kent, Sch Phys Sci, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NR, Kent, England. NR 65 TC 10 Z9 10 U1 0 U2 0 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 21 PY 2003 VL 346 IS 4 BP L51 EP L56 DI 10.1111/j.1365-2966.2003.07305.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753XK UT WOS:000187256700001 ER PT J AU Hoge, FE AF Hoge, FE TI Validation of satellite-retrieved oceanic inherent optical properties: proposed two-color elastic backscatter lidar and retrieval theory SO APPLIED OPTICS LA English DT Article ID REMOTELY-SENSED REFLECTANCE; THEORETICAL DERIVATION; VERTICAL STRUCTURE; VARIABILITY; DEPENDENCE; WATERS; MODEL; POC AB Recent radiative transfer models show that: (1) regardless of elastic lidar receiver field of view (FOV), at vanishing lidar depth the lidar-derived attenuation coefficient k(lidar) --> a, where a is the total absorption coefficient per meter of depth; and (2) for a wide FOV as the lidar sensing depth approaches some large value (depending on water type) k(lidar) --> K-d, where K-d is the diffuse attenuation for downwelling irradiance. As a result, it is shown that a time-resolved, dual-wavelength-laser, elastic-backscattering lidar can retrieve the three principal oceanic optical properties: (1) the absorption coefficient of phytoplankton a(ph), (2) the absorption coefficient of chromophoric dissolved organic matter (CDOM) a(CDOM), and (3) the nonwater total constituent backscattering coefficient b(bt). The lidar-retrieved a(ph), a(CDOM), and b(bt) inherent optical properties can be used to validate corresponding satellite-derived products such as those from terra moderate-resolution imaging spectroradiometer (MODIS), Aqua MODIS, Sea-viewing Wide Field-of-view Sensor, (SeaWiFS), and other ocean color sensors. (C) 2003 Optical Society of America. C1 NASA, Goddard Space Flight Ctr, Wallops Isl, VA 23337 USA. RP Hoge, FE (reprint author), NASA, Goddard Space Flight Ctr, Wallops Flight Facil,Bldg N-159, Wallops Isl, VA 23337 USA. EM frank.hoge@nasa.gov NR 22 TC 0 Z9 0 U1 0 U2 2 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD DEC 20 PY 2003 VL 42 IS 36 BP 7197 EP 7201 DI 10.1364/AO.42.007197 PG 5 WC Optics SC Optics GA 756KB UT WOS:000187463300016 PM 14717299 ER PT J AU Goldstein, JH Ade, PAR Bock, JJ Bond, JR Cantalupo, C Contaldi, CR Daub, MD Holzapfel, WL Kuo, C Lange, AE Lueker, M Newcomb, M Peterson, JB Pogosyan, D Ruhl, JE Runyan, MC Torbet, E AF Goldstein, JH Ade, PAR Bock, JJ Bond, JR Cantalupo, C Contaldi, CR Daub, MD Holzapfel, WL Kuo, C Lange, AE Lueker, M Newcomb, M Peterson, JB Pogosyan, D Ruhl, JE Runyan, MC Torbet, E TI Estimates of cosmological parameters using the cosmic microwave background angular power spectrum of ACBAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmological parameters; cosmology : observations ID ANISOTROPY; IMAGER; SIMULATIONS; SUPERNOVAE; UNIVERSE; CONSTANT; L=3500; ARRAY; MAPS AB We report an investigation of cosmological parameters based on the measurements of anisotropy in the cosmic microwave background radiation (CMB) made by the Arcminute Cosmology Bolometer Array Receiver (ACBAR). We use the ACBAR data in concert with other recent CMB measurements to derive Bayesian estimates of parameters in inflation-motivated adiabatic cold dark matter models. We apply a series of additional cosmological constraints on the shape and amplitude of the density power spectrum and the Hubble parameter and from supernovae to further re. ne our parameter estimates. Previous estimates of parameters are confirmed, with sensitive measurements of the power spectrum now ranging from l similar to 3 to 2800. Comparing individual best-fit models, we find that the addition of Omega(Lambda) as a parameter dramatically improves the fits. We also use the high-l data of ACBAR, along with similar data from the Cosmic Background Imager and Berkeley-Illinois-Maryland Association array, to investigate potential secondary anisotropies from the Sunyaev-Zel'dovich effect. We show that the results from the three experiments are consistent under this interpretation and use the data, combined and individually, to estimate sigma(8) from the Sunyaev-Zel'dovich component. C1 Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Toronto, Canadian Inst Theoret Astrophys, McLennan Labs, Toronto, ON M5S 3H8, Canada. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. CALTECH, Pasadena, CA 91125 USA. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Univ Alberta, Dept Phys, Edmonton, AB T6G 2J1, Canada. RP Case Western Reserve Univ, Dept Phys, 10900 Euclid Ave, Cleveland, OH 44106 USA. RI Peterson, Jeffrey/O-4794-2014; Holzapfel, William/I-4836-2015 OI Peterson, Jeffrey/0000-0003-1340-818X; NR 32 TC 106 Z9 106 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP 773 EP 785 DI 10.1086/379539 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756DX UT WOS:000187451500005 ER PT J AU Ruhl, JE Ade, PAR Bock, JJ Bond, JR Borrill, J Boscaleri, A Contaldi, CR Crill, BP de Bernardis, P De Troia, G Ganga, K Giacometti, M Hivon, E Hristov, VV Iacoangeli, A Jaffe, AH Jones, WC Lange, AE Masi, S Mason, P Mauskopf, PD Melchiorri, A Montroy, T Netterfield, CB Pascale, E Piacentini, F Pogosyan, D Polenta, G Prunet, S Romeo, G AF Ruhl, JE Ade, PAR Bock, JJ Bond, JR Borrill, J Boscaleri, A Contaldi, CR Crill, BP de Bernardis, P De Troia, G Ganga, K Giacometti, M Hivon, E Hristov, VV Iacoangeli, A Jaffe, AH Jones, WC Lange, AE Masi, S Mason, P Mauskopf, PD Melchiorri, A Montroy, T Netterfield, CB Pascale, E Piacentini, F Pogosyan, D Polenta, G Prunet, S Romeo, G TI Improved measurement of the angular power spectrum of temperature anisotropy in the cosmic microwave background from two new analyses of boomerang observations SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmological parameters; cosmology : observations ID GALACTIC DUST EMISSION; SCALE INTERFEROMETER; CONTINUUM SURVEY; MULTIPLE PEAKS; MAPS; RADIATION; SUPERNOVAE; TELESCOPE; CONSTANT; UNIVERSE AB We report the most complete analysis to date of observations of the cosmic microwave background (CMB) obtained during the 1998 flight of BOOMERANG. We use two quite different methods to determine the angular power spectrum of the CMB in 20 bands centered at l = 50 1000, applying them to similar to50% more data than has previously been analyzed. The power spectra produced by the two methods are in good agreement with each other and constitute the most sensitive measurements to date over the range 300 < l < 1000. The increased precision of the power spectrum yields more precise determinations of several cosmological parameters than previous analyses of BOOMERANG data. The results continue to support an inflationary paradigm for the origin of the universe, being well fitted by a similar to13.5 Gyr old,. at universe composed of approximately 5% baryonic matter, 30% cold dark matter, and 65% dark energy, with a spectral index of initial density perturbations n(s) similar to1. C1 Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. Cardiff Univ, Cardiff CF24 3YB, S Glam, Wales. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. Univ Calif Berkeley, Lawrence Berkeley Lab, Natl Energy Res Sci Comp Ctr, Computat Res Div, Berkeley, CA 94720 USA. CNR, IFAC, I-50127 Florence, Italy. CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. Calif State Univ Dominguez Hills, Dept Phys, Carson, CA 90747 USA. Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2BZ, England. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Univ Toronto, McLennan Labs, Dept Phys, Toronto, ON M5S 3H8, Canada. Univ Alberta, Dept Phys, Avadh Bhatia Phys Lab, Edmonton, AB T6G 2J1, Canada. CNRS, Inst Astrophys Paris, F-75014 Paris, France. Ist Nazl Geofis, I-00143 Rome, Italy. RP Case Western Reserve Univ, Dept Phys, Rockefeller Hall,10900 Evelid Ave, Cleveland, OH 44106 USA. RI Jaffe, Andrew/D-3526-2009; Piacentini, Francesco/E-7234-2010; OI Piacentini, Francesco/0000-0002-5444-9327; ROMEO, Giovanni/0000-0002-5535-7803; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Polenta, Gianluca/0000-0003-4067-9196; Hivon, Eric/0000-0003-1880-2733 NR 38 TC 101 Z9 101 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP 786 EP 805 DI 10.1086/379345 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756DX UT WOS:000187451500006 ER PT J AU Armstrong, JW Iess, L Tortora, P Bertotti, B AF Armstrong, JW Iess, L Tortora, P Bertotti, B TI Stochastic gravitational wave background: Upper limits in the 10(-6) to 10(-3) Hz band SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; gravitational waves; relativity ID BLACK-HOLE BINARIES; WATER-VAPOR; RADIATION; INTERFEROMETRY; SPACECRAFT; STABILITY; TRACKING; PULSARS; SEARCH AB We have used precision Doppler tracking of the Cassini spacecraft during its 2001-2002 solar opposition to derive improved observational limits to an isotropic background of low-frequency gravitational waves. Using the Cassini multilink radio system and an advanced tropospheric calibration system, the effects of heretofore leading noises-plasma and tropospheric scintillation-were, respectively, removed and calibrated to levels lower than other noises. The resulting data were used to construct upper limits to the strength of an isotropic background in the 10(-6) to 10(-3) Hz band. Our results are summarized as limits on the strain spectrum S-h(f), the characteristic strain (h(c) = the square root of the product of the frequency and the one-sided spectrum of strain at that frequency), and the energy density (Omega = energy density in bandwidth equal to center frequency assuming a locally white energy density spectrum, divided by the critical density). Our best limits are S-h(f) < 6 x 10(-27) Hz(-1) at several frequencies in the millihertz band, h(c) < 2 x 10(-15) at about 0.3 mHz, and Omega < 0.025 x h(75)(-2), where h(75) is the Hubble constant in units of 75 km s(-1) Mpc(-1), at 1.2 x 10(-6) Hz. These are the best observational limits in the low-frequency band, the bound on Omega, for example, being about 3 orders of magnitude better than previous constraints from Doppler tracking. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Roma La Sapienza, Dipartimento Ingn Aerospaziale & Astronaut, I-00184 Rome, Italy. Univ Bologna, Fac Ingn 2, I-47100 Forli, Italy. Univ Pavia, Dipartimento Fis Nucl & Teor, I-27100 Pavia, Italy. RP Armstrong, JW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI IESS, Luciano/F-4902-2011; Tortora, Paolo/J-6191-2012 OI IESS, Luciano/0000-0002-6230-5825; Tortora, Paolo/0000-0001-9259-7673 NR 38 TC 56 Z9 56 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP 806 EP 813 DI 10.1086/379505 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756DX UT WOS:000187451500007 ER PT J AU Perez, ID Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Celik, O Cui, W Dowdall, C Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, L Gaidos, JA Gibbs, K Gammell, S Hall, J Hall, TA Hillas, AM Holder, J Horan, D Jordan, M Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F LeBohec, S Linton, ET Lloyd-Evans, J Moriarty, P Muller, D Nagai, TN Ong, RA Page, M Pallassini, R Petry, D Power-Mooney, B Quinn, J Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Vassiliev, VV Wakely, SP Walker, G Weekes, TC AF Perez, ID Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Celik, O Cui, W Dowdall, C Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, L Gaidos, JA Gibbs, K Gammell, S Hall, J Hall, TA Hillas, AM Holder, J Horan, D Jordan, M Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F LeBohec, S Linton, ET Lloyd-Evans, J Moriarty, P Muller, D Nagai, TN Ong, RA Page, M Pallassini, R Petry, D Power-Mooney, B Quinn, J Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Vassiliev, VV Wakely, SP Walker, G Weekes, TC TI Search for high-energy gamma rays from an X-ray-selected blazar sample SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (RGB J0214+517, RGB J1117+202, RGB J1725+118, IES 0033+595, 1ES 0120+340; 1ES 0229+200, 1ES 0806+524, 1ES 1426+428, 1ES 1553+113, 1ES 1959+650); gamma rays : observations ID ACTIVE GALACTIC NUCLEI; BL LACERTAE OBJECTS; TEV ENERGIES; EMISSION; RADIATION; TELESCOPE; FLARE; MARKARIAN-501; ABSORPTION; DISCOVERY AB Our understanding of blazars has been greatly increased in recent years by extensive multiwavelength observations, particularly in the radio, X-ray, and gamma-ray regions. Over the past decade the Whipple 10 m telescope has contributed to this with the detection of five BL Lacertae objects at very high gamma-ray energies. The combination of multiwavelength data has shown that blazars follow a well-defined sequence in terms of their broadband spectral properties. Together with providing constraints on emission models, this information has yielded a means by which potential sources of TeV emission may be identified and predictions made as to their possible gamma-ray flux. We have used the Whipple telescope to search for TeV gamma-ray emission from eight objects selected from a list of such candidates. No evidence has been found for very high energy emission from the objects in our sample, and upper limits have been derived for the mean gamma-ray flux above 390 GeV. These flux upper limits are compared with the model predictions, and the implications of our results for future observations are discussed. C1 Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Galway Mayo Inst Technol, Sch Sci, Galway, Ireland. Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Natl Univ Ireland, Dept Phys, Dublin 4, Ireland. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT 84112 USA. Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. De Pauw Univ, Dept Phys, Greencastle, IN 46135 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Cork Inst Technol, Dept Phys, Cork, Ireland. RP Perez, ID (reprint author), Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. RI Hall, Jeter/F-6108-2013; Hall, Jeter/E-9294-2015; OI Cui, Wei/0000-0002-6324-5772; Knapp, Johannes/0000-0003-1519-1383 NR 48 TC 20 Z9 20 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP 909 EP 917 DI 10.1086/379544 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756DX UT WOS:000187451500015 ER PT J AU Netzer, H Kaspi, S Behar, E Brandt, WN Chelouche, D George, IM Crenshaw, DM Gabel, JR Hamann, FW Kraemer, SB Kriss, GA Nandra, K Peterson, BM Shields, JC Turner, TJ AF Netzer, H Kaspi, S Behar, E Brandt, WN Chelouche, D George, IM Crenshaw, DM Gabel, JR Hamann, FW Kraemer, SB Kriss, GA Nandra, K Peterson, BM Shields, JC Turner, TJ TI The ionized gas and nuclear environment in NGC 3783. IV. Variability and modeling of the 900 kilosecond Chandra spectrum SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 3783); galaxies : nuclei; galaxies : Seyfert; techniques : spectroscopic; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; REFLECTION GRATING SPECTROMETER; DUSTY WARM ABSORBER; X-RAY ABSORPTION; XMM-NEWTON; ULTRAVIOLET ABSORBER; GALAXY NGC-3783; EMISSION-LINES; SPECTROSCOPY; NGC-5548 AB We present a detailed spectral analysis of the data obtained from NGC 3783 during the period 2000-2001 using Chandra. The data were split in various ways to look for time- and luminosity-dependent spectral variations. This analysis, along with the measured equivalent widths of a large number of X-ray lines and photoionization calculations, lead us to the following results and conclusions. (1) NGC 3783 fluctuated in luminosity by a factor of similar to1.5 during individual observations (most of which were of 170 ks duration). These fluctuations were not associated with significant spectral variations. (2) On a longer timescale (20-120 days), we found the source to exhibit two very different spectral shapes. The main difference between these can be well-described by the appearance (in the "high state") and disappearance (in the "low state") of a spectral component that dominates the underlying continuum at the longest wavelengths. Contrary to the case in other objects, the spectral variations are not related to the brightening or the fading of the continuum at short wavelengths in any simple way. NGC 3783 seems to be the first active galactic nucleus (AGN) to show this unusual behavior. (3) The appearance of the soft continuum component is consistent with being the only spectral variation, and there is no need to invoke changes in the opacity of the absorbers lying along the line of sight. Indeed, we find that all the absorption lines that can be reliably measured have the same equivalent widths (within the observational uncertainties) during high and low states. (4) Photoionization modeling indicates that a combination of three ionized absorbers, each split into two kinematic components, can explain the strengths of almost all the absorption lines and bound-free edges. These three components span a large range of ionization and have total column of about 4 x 10(22) cm(-2). Moreover, all three components are thermally stable and seem to have the same gas pressure. Thus, all three may coexist in the same volume of space. This is the first detection of such a multicomponent, equilibrium gas in an AGN. (5) The only real discrepancy between our model and the observations concerns the range of wavelengths absorbed by the iron M-shell UTA feature. This most likely arises as the result of our underestimation of the poorly known dielectronic recombination rates appropriate for these ions. We also note a small discrepancy in the calculated column density of O vi and discuss its possible origin. (6) The lower limit on the distance of the absorbing gas in NGC 3783 is between 0.2 and 3.2 pc, depending on the component of ionized gas considered. The assumption of pressure equilibrium imposes an upper limit of about 25 pc on the distance of the least-ionized component from the central source. C1 Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, Baltimore, MD 21250 USA. Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. Johns Hopkins Univ, Dept Phys & Astron, Ctr Astrophys Sci, Baltimore, MD 21218 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Ohio Univ, Dept Phys & Astron, Clippinger Res Labs 251B, Athens, OH 45701 USA. RP Netzer, H (reprint author), Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. RI Brandt, William/N-2844-2015 OI Brandt, William/0000-0002-0167-2453 NR 35 TC 155 Z9 155 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP 933 EP 948 DI 10.1086/379508 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756DX UT WOS:000187451500017 ER PT J AU Neff, SG Ulvestad, JS Campion, SD AF Neff, SG Ulvestad, JS Campion, SD TI Radio emission associated with ultraluminous X-ray sources in the galaxy merger NGC 3256 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 3256); galaxies : interactions; galaxies : starburst; galaxies : star clusters; X-rays : binaries; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; SOURCE NGC-5204 X-1; CHANDRA OBSERVATIONS; OPTICAL COUNTERPART; BLACK-HOLES; STARS; NGC-6240; NGC-253; REGIONS; JETS AB We present new 6, 3.6, and 2 cm VLA radio observations of the nearby merger system NGC 3256, with resolutions of similar to100 pc, which reveal compact radio sources embedded in more diffuse emission at all three wavelengths. The two radio nuclei are partially resolved, but the two dominant compact sources that remain coincide with the two most powerful compact ultraluminous X-ray sources (ULXs) recently reported by Lira et al. The radio/X-ray ratios for these two sources are too high by factors of more than 100-1000 to be normal X-ray binaries. However, their radio and X-ray powers and ratios are consistent with low-luminosity active galactic nuclei (LLAGNs), and optical emission lines suggest the presence of a nuclear disk around the northern nucleus. If the two nuclear ULXs are LLAGNs, their associated black holes are separated by only similar to1 kpc, making them about 6 times closer to one another than those found recently in the merger galaxy NGC 6240. A third ULX on the outskirts of the merger is also a radio source and probably is a collection of supernova remnants. The remaining ULXs are not coincident with any source of compact radio emission and are consistent with expectations for beamed X-ray binaries or intermediate-mass black holes. C1 NASA, Astron & Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Sci Syst & Applicat Inc, Lanham, MD USA. RP Neff, SG (reprint author), NASA, Astron & Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 41 TC 28 Z9 28 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP 1043 EP 1048 DI 10.1086/379596 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756DX UT WOS:000187451500026 ER PT J AU Chuss, DT Davidson, JA Dotson, JL Dowell, CD Hildebrand, RH Novak, G Vaillancourt, JE AF Chuss, DT Davidson, JA Dotson, JL Dowell, CD Hildebrand, RH Novak, G Vaillancourt, JE TI Magnetic fields in cool clouds within the central 50 parsecs of the Galaxy SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; Galaxy : center; ISM : magnetic fields; submillimeter; techniques : polarimetric ID GALACTIC-CENTER REGION; FORMING MOLECULAR CLOUDS; SAGITTARIUS-A COMPLEX; FAR-INFRARED EMISSION; SUBMILLIMETER POLARIMETER; RADIO STRUCTURES; CENTER ARC; POLARIZATION; FILAMENT; ORIGIN AB We report the detection of polarized emission in the vicinity of the Galactic center for 158 positions within eight different pointings of the Hertz polarimeter operating on the Caltech Submillimeter Observatory. These pointings include locations 2' offset to the east, northeast, and northwest of M-0.02-0.07; locations to the southeast and northwest of the 20 km s(-1) cloud (M-0.13-0.08); CO 0.02-0.02, M0.07-0.08; and M0.11-0.08. We use these data in conjunction with previous far-infrared and submillimeter polarization results to find that the direction of the inferred magnetic field is related to the density of the molecular material in the following way: in denser regions, the projected field is generally parallel to the Galactic plane, whereas in regions of lower density, the field is generally perpendicular to the plane. One possible explanation for this result is that an initially poloidal field has been sheared into a toroidal configuration in regions that are dense enough such that the gravitational energy density is greater than the energy density of the magnetic field. Another possibility is that winds due to supernovae in the central molecular zone are responsible for deviations from a toroidal field outside of the densest molecular regions. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. CALTECH, Pasadena, CA 91125 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Univ Wisconsin, Madison, WI 53706 USA. RP Chuss, DT (reprint author), NASA, Goddard Space Flight Ctr, Code 685, Greenbelt, MD 20771 USA. RI Chuss, David/D-8281-2012; OI Vaillancourt, John/0000-0001-8916-1828 NR 37 TC 61 Z9 61 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP 1116 EP 1128 DI 10.1086/379538 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756DX UT WOS:000187451500030 ER PT J AU Sterling, AC Moore, RL AF Sterling, AC Moore, RL TI Tether-cutting energetics of a solar quiet-region prominence eruption SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : corona; Sun : flares; Sun : UV radiation ID CORONAL MASS-EJECTIONS; HOT PLASMA; FLUX ROPE; FLARES; EIT; TELESCOPE; MISSION; ONSET; WAVE AB We study the morphology and energetics of a slowly evolving quiet-region solar prominence eruption occurring on 1999 February 8-9 in the solar north polar crown region, using soft X-ray data from the soft X-ray telescope (SXT) on Yohkoh and Fe XV EUV 284 Angstrom data from the EUV Imaging Telescope (EIT) on the Solar and Heliospheric Observatory (SOHO). After rising at approximate to1 km s(-1) for about six hours, the prominence accelerates to a velocity of approximate to10 km s(-1), leaving behind EUV and soft X-ray loop arcades of a weak. are in its source region. Intensity dimmings occur in the eruption region cospatially in EUV and soft X-rays, indicating that the dimmings result from a depletion of material. Over the first two hours of the prominence's rapid rise, flarelike brightenings occur beneath the rising prominence that might correspond to "tether-cutting'' magnetic reconnection. These brightenings have heating requirements of up to similar to10(28)-10(29) ergs, and this is comparable to the mechanical energy required for the rising prominence over the same time period. If the ratio of mechanical energy to heating energy remains constant through the early phase of the eruption, then we infer that coronal signatures for the tether cutting may not be apparent at or shortly after the start of the fast phase in this or similar low-energy eruptions, since the plasma-heating energy levels would not exceed that of the background corona. C1 NASA, George C Marshall Space Flight Ctr, Dept Space Sci SD50, Huntsville, AL 35812 USA. RP Sterling, AC (reprint author), Inst Space & Astronaut Sci, Yoshinodai 3-1-1, Kanagawa 2298510, Japan. NR 24 TC 27 Z9 27 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP 1418 EP 1425 DI 10.1086/379164 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756DX UT WOS:000187451500053 ER PT J AU Meurer, GR Blakeslee, JP Sirianni, M Ford, HC Illingworth, GD Benitez, N Clampin, M Menanteau, F Tran, HD Kimble, RA Hartig, GF Ardila, DR Bartko, F Bouwens, RJ Broadhurst, TJ Brown, RA Burrows, CJ Cheng, ES Cross, NJG Feldman, PD Golimowski, DA Gronwall, C Infante, L Krist, JE Lesser, MP Martel, AR Miley, GK Postman, M Rosati, P Sparks, WB Tsvetanov, ZI White, RL Zheng, W AF Meurer, GR Blakeslee, JP Sirianni, M Ford, HC Illingworth, GD Benitez, N Clampin, M Menanteau, F Tran, HD Kimble, RA Hartig, GF Ardila, DR Bartko, F Bouwens, RJ Broadhurst, TJ Brown, RA Burrows, CJ Cheng, ES Cross, NJG Feldman, PD Golimowski, DA Gronwall, C Infante, L Krist, JE Lesser, MP Martel, AR Miley, GK Postman, M Rosati, P Sparks, WB Tsvetanov, ZI White, RL Zheng, W TI The discovery of globular clusters in the protospiral galaxy NGC 2915: Implications for hierarchical galaxy evolution SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : halos; galaxies : individual (NGC 2915); galaxies : star clusters ID STAR-FORMATION; DWARF GALAXY; LOCAL GROUP; SYSTEMS; HISTORY; ORIGIN; CORE; M31 AB We have discovered three globular clusters beyond the Holmberg radius in Hubble Space Telescope Advanced Camera for Surveys images of the gas-rich dark matter-dominated blue compact dwarf galaxy NGC 2915. The clusters, all of which start to resolve into stars, have M-V606 = -8.9 to -9.8 mag, significantly brighter than the peak of the luminosity function of Milky Way globular clusters. Their colors suggest a metallicity [Fe/H] approximate to -1.9 dex, typical of metal-poor Galactic globular clusters. The specific frequency of clusters is at a minimum normal, compared to spiral galaxies. However, since only a small portion of the system has been surveyed, it is more likely that the luminosity and mass normalized cluster content is higher, like that seen in elliptical galaxies and galaxy clusters. This suggests that NGC 2915 resembles a key phase in the early hierarchical assembly of galaxies-the epoch when much of the old stellar population has formed but little of the stellar disk. Depending on the subsequent interaction history, such systems could go on to build up larger elliptical galaxies, evolve into normal spirals, or in rare circumstances remain suspended in their development to become systems like NGC 2915. C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. WM Keck Observ, Kamuela, HI 96743 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Bartko Sci & Technol, Mead, CO 80542 USA. Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. European So Observ, D-85748 Garching, Germany. RP Meurer, GR (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. RI White, Richard/A-8143-2012; Clampin, mark/D-2738-2012; Kimble, Randy/D-5317-2012; OI Benitez, Narciso/0000-0002-0403-7455; Blakeslee, John/0000-0002-5213-3548 NR 30 TC 7 Z9 7 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP L83 EP L86 DI 10.1086/381317 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756EE UT WOS:000187452200008 ER PT J AU Sahai, R Kastner, JH Frank, A Morris, M Blackman, EG AF Sahai, R Kastner, JH Frank, A Morris, M Blackman, EG TI X-ray emission from the pre-planetary nebula Henize 3-1475 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM : jets and outflows; planetary nebulae : individual (He 3-1475); stars : AGB and post-AGB; stars : mass loss; X-rays : ISM ID PLANETARY-NEBULAE; MAGNETIC COLLIMATION; JETS; KILOMETER; HE-3-1475; NGC-7027; STELLAR; STARS; ANSAE AB We report the first detection of X-ray emission in a pre-planetary nebula, He 3-1475. Pre-planetary nebulae are rare objects in the short transition stage between the asymptotic giant branch (AGB) and planetary nebula evolutionary phases, and He 3-1475, characterized by a remarkable S-shaped chain of optical knots, is one of the most noteworthy members of this class. Observations with the Advanced CCD Imaging Spectrometer on board the Chandra X-Ray Observatory show the presence of compact emission coincident with the brightest optical knot in this bipolar object, which is displaced from the central star by 2."7 along the polar axis. Model fits to the X-ray spectrum indicate an X-ray temperature and luminosity, respectively, of K and 6 (4.3-5.7) x 10(6) K and (4 +/- 1.4) x 10(31) (D/5 kpc)(2) ergs s(-1), respectively. Our 3 sigma upper limit on the luminosity of compact X- ray emission from the central star in He 3-1475 is similar to5 x 10(31) (D/5 kpc)(2) ergs s(-1). The detection of X-rays in He 3-1475 is consistent with models in which fast collimated post-AGB outflows are crucial to the shaping of planetary nebulae; we discuss such models in the context of our observations. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Univ Calif Los Angeles, Div Astron & Astrophys, Los Angeles, CA 90095 USA. RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA. NR 28 TC 19 Z9 19 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP L87 EP L90 DI 10.1086/381316 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756EE UT WOS:000187452200009 ER PT J AU Stothers, RB AF Stothers, RB TI Radiative instability in stellar envelopes SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : interiors; stars : mass loss; stars : variables : other; stars : Wolf-Rayet; supergiants ID LUMINOUS BLUE VARIABLES; WOLF-RAYET STARS; MASS-LOSS RATES; S-DORADUS VARIABLES; WINDS; PARAMETERS; MODELS; OB AB A general analytic criterion for radiative instability in the envelope of a nonexplosive star is derived, based on a generalization of the Eddington limit for the star's luminosity, an expression for the stationary mass-loss acceleration, and an assumed universality of the critical mean density of the envelope. The derived criterion has been formulated as the minimum rate of mass loss needed to achieve a super-Eddington state. Expressed as a simple function of luminosity and effective temperature, it is applied to luminous blue variables (LBVs), Wolf-Rayet stars, and ordinary B-type supergiants. Assuming that the brightest LBVs as well as most of the Wolf-Rayet stars are post-main-sequence objects, these objects must have radiatively unstable envelopes. C1 NASA, Goddard Space Flight Ctr, Inst Space Studies, New York, NY 10025 USA. RP Stothers, RB (reprint author), NASA, Goddard Space Flight Ctr, Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. NR 24 TC 2 Z9 2 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2003 VL 599 IS 2 BP L103 EP L105 DI 10.1086/381192 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756EE UT WOS:000187452200013 ER PT J AU Farrell, WM Desch, MD Ogilvie, KW Kaiser, ML Goetz, K AF Farrell, WM Desch, MD Ogilvie, KW Kaiser, ML Goetz, K TI The role of upper hybrid waves in magnetic reconnection SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID WIND SPACECRAFT; PLASMA; MAGNETOSPHERE; ELECTRONS AB Wind observations of upper hybrid (UH) waves adjacent to a magnetic X-line are compared with simultaneous Wind electron observations to clarify wave-electron interactions. Electron beams and "football'' (T-parallel to>T-perpendicular to)distributions accompany the UH waves. The energy density of the inward-directed beams, at 10(-14) J/m(3), is sufficient to supply the free energy for the waves. The electron beams may be part of the larger Hall current system, and the UH wave/electron instability represent a Hall current dissipation process (i.e., an effective resistance) which removes energy as the currents travels along the separatrix. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA. EM william.farrell@gsfc.nasa.gov RI Farrell, William/I-4865-2013 NR 22 TC 12 Z9 13 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 20 PY 2003 VL 30 IS 24 AR 2259 DI 10.1029/2003GL017549 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 760WE UT WOS:000187857600002 ER PT J AU Gibson, SE Foster, DJ Guhathakurta, M Holzer, T St Cyr, OC AF Gibson, SE Foster, DJ Guhathakurta, M Holzer, T St Cyr, OC TI Three-dimensional coronal density structure: 1. Model SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE corona; streamers; coronal holes; large-scale coronal structure; coronal density; 3-D corona ID WHOLE SUN MONTH; SOLAR MINIMUM CORONA; MAGNETIC-FIELD AB The three-dimensional (3-D) density structure of the solar corona is a fundamental boundary condition on the solar wind. Most easily applied models of the global coronal density have been restricted to date to axisymmetric 2-D cases. We present here a 3-D model made up of a superposition of multiple streamers, having distinct gaussian widths in longitude and latitude and both longitudinal and latitudinal dependence of the neutral lines implicit beneath the streamer cores. Nonradiality of streamers and solar B-angle tilt are also explicitly treated. We show how this simple model can capture many of the general properties of coronal white light observations and demonstrate how such a model can assist in the interpretation of the multiple views on coronal structures such as will be provided by the upcoming STEREO mission. C1 Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Univ Colorado, Dept Phys, Boulder, CO 80309 USA. NASA Headquarters, Washington, DC USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. Catholic Univ, Dept Phys, Washington, DC USA. RP Natl Ctr Atmospher Res, High Altitude Observ, Pob 3000, Boulder, CO 80307 USA. EM sgibson@hao.ucar.edu; dafoster@hao.ucar.edu; madhulika.guhathakurta@hq.nasa.gov; holzer@hao.ucar.edu; chris.stcyr@gsfc.nasa.gov RI Gibson, Sarah/A-9189-2011 NR 19 TC 4 Z9 4 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 20 PY 2003 VL 108 IS A12 AR 1444 DI 10.1029/2003JA009994 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 760XD UT WOS:000187859800002 ER PT J AU Klingelhofer, G Morris, RV Bernhardt, B Rodionov, D de Souza, PA Squyres, SW Foh, J Kankeleit, E Bonnes, U Gellert, R Schroder, C Linkin, S Evlanov, E Zubkov, B Prilutski, O AF Klingelhofer, G Morris, RV Bernhardt, B Rodionov, D de Souza, PA Squyres, SW Foh, J Kankeleit, E Bonnes, U Gellert, R Schroder, C Linkin, S Evlanov, E Zubkov, B Prilutski, O TI Athena MIMOS II Mossbauer spectrometer investigation SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mossbauer spectroscopy; iron mineralogy; Mars; weathering; instrumentation; MIMOS II ID MAGNETIC-PROPERTIES EXPERIMENTS; HAWAIIAN PALAGONITIC SOIL; MARS EXPLORATION ROVERS; ANALOG MATERIALS; MAUNA-KEA; SPECTROSCOPY; HEMATITE; IRON; MINERALOGY; PATHFINDER AB Mossbauer spectroscopy is a powerful tool for quantitative mineralogical analysis of Fe-bearing materials. The miniature Mossbauer spectrometer MIMOS II is a component of the Athena science payload launched to Mars in 2003 on both Mars Exploration Rover missions. The instrument has two major components: (1) a rover-based electronics board that contains power supplies, a dedicated central processing unit, memory, and associated support electronics and (2) a sensor head that is mounted at the end of the instrument deployment device (IDD) for placement of the instrument in physical contact with soil and rock. The velocity transducer operates at a nominal frequency of similar to25 Hz and is equipped with two Co-57/Rh Mossbauer sources. The reference source (similar to5 mCi landed intensity), reference target (alpha-Fe2O3 plus alpha-Fe-0), and PIN-diode detector are configured in transmission geometry and are internal to the instrument and used for its calibration. The analysis Mossbauer source (similar to150 mCi landed intensity) irradiates Martian surface materials with a beam diameter of similar to1.4 cm. The backscatter radiation is measured by four PIN-diode detectors. Physical contact with surface materials is sensed with a switch-activated contact plate. The contact plate and reference target are instrumented with temperature sensors. Assuming similar to18% Fe for Martian surface materials, experiment time is 6-12 hours during the night for quality spectra (i.e., ood counting statistics); 1-2 hours is sufficient to identify and quantify the most abundant Fe-bearing phases. Data stored internal to the instrument for selectable return to Earth include Mossbauer and pulse-height analysis spectra (512 and 256 channels, respectively) for each of the five detectors in up to 13 temperature intervals (65 Mossbauer spectra), engineering data for the velocity transducer, and temperature measurements. The total data volume is similar to150 kB. The mass and power consumption are similar to500 g (similar to400 g for the sensor head) and similar to2 W, respectively. The scientific measurement objectives of the Mossbauer investigation are to obtain for rock, soil, and dust (1) the mineralogical identification of iron-bearing phases (e.g., oxides, silicates, sulfides, sulfates, and carbonates), (2) the quantitative measurement of the distribution of iron among these iron-bearing phases (e.g., the relative proportions of iron in olivine, pyroxenes, ilmenite, and magnetite in a basalt), (3) the quantitative measurement of the distribution of iron among its oxidation states (e.g., Fe2+, Fe3+, and Fe6+), and (4) the characterization of the size distribution of magnetic particles. Special geologic targets of the Mossbauer investigation are dust collected by the Athena magnets and interior rock and soil surfaces exposed by the Athena Rock Abrasion Tool and by trenching with rover wheels. C1 Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, Fachbereich Chem & Pharm, D-55099 Mainz, Germany. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Space Res Inst IKI, Moscow, Russia. Pelletizing Dept, Vitoria, Brazil. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Tech Univ Darmstadt, Inst Nucl Phys, D-64289 Darmstadt, Germany. RP Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, Fachbereich Chem & Pharm, Staudinger Weg 9, D-55099 Mainz, Germany. EM klingel@mail.uni-mainz.de RI de Souza, Paulo/B-8961-2008; Schroder, Christian/B-3870-2009 OI de Souza, Paulo/0000-0002-0091-8925; Schroder, Christian/0000-0002-7935-6039 NR 89 TC 124 Z9 125 U1 2 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 19 PY 2003 VL 108 IS E12 AR 8067 DI 10.1029/2003JE002138 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 760WY UT WOS:000187859300001 ER PT J AU Peterson, CH Rice, SD Short, JW Esler, D Bodkin, JL Ballachey, BE Irons, DB AF Peterson, CH Rice, SD Short, JW Esler, D Bodkin, JL Ballachey, BE Irons, DB TI Long-term ecosystem response to the Exxon Valdez oil spill SO SCIENCE LA English DT Review ID PRINCE-WILLIAM-SOUND; SALMON ONCORHYNCHUS-GORBUSCHA; SEA OTTERS; CRUDE-OIL; ALASKA; RECOVERY; MORTALITY; POPULATIONS; PERSISTENCE; COMMUNITY AB The ecosystem response to the 1989 spill of oil from the Exxon Valdez into Prince William Sound, Alaska, shows that current practices for assessing ecological risks of oil in the oceans and, by extension, other toxic sources should be changed. Previously, it was assumed that impacts to populations derive almost exclusively from acute mortality. However, in the Alaskan coastal ecosystem, unexpected persistence of toxic subsurface oil and chronic exposures, even at sublethal levels, have continued to affect wildlife. Delayed population reductions and cascades of indirect effects postponed recovery. Development of ecosystem-based toxicology is required to understand and ultimately predict chronic, delayed, and indirect long-term risks and impacts. C1 Univ N Carolina, Inst Marine Sci, Morehead City, NC 28557 USA. NOAA, Alaska Fisheries Sci Ctr, Auke Bay Lab, Natl Marine Fisheries Serv, Juneau, AK 99801 USA. Simon Fraser Univ, Dept Biol Sci, Ctr Wildlife Ecol, Burnaby, BC V5A 1S6, Canada. US Geol Survey, Alaska Sci Ctr, Anchorage, AK 99503 USA. US Fish & Wildlife Serv, US Dept Interior, Anchorage, AK 99503 USA. RP Peterson, CH (reprint author), Univ N Carolina, Inst Marine Sci, Morehead City, NC 28557 USA. NR 45 TC 457 Z9 486 U1 71 U2 574 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD DEC 19 PY 2003 VL 302 IS 5653 BP 2082 EP 2086 DI 10.1126/science.1084282 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 755CB UT WOS:000187385200032 PM 14684812 ER PT J AU Chylek, P Henderson, B Mishchenko, M AF Chylek, P Henderson, B Mishchenko, M TI Aerosol radiative forcing and the accuracy of satellite aerosol optical depth retrieval SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosol optical depth; satellite retrieval; radiative forcing ID TROPOSPHERIC AEROSOL; CLIMATE; ATSR-2; AVHRR; LAND; ATMOSPHERE; ABSORPTION; THICKNESS; BUDGET; CLOUDS AB The minimum acceptable accuracy of the top of the atmosphere radiative flux of DeltaF = 0.5 W/m(2) leads to the required accuracy in satellite based aerosol optical depth (AOD) retrieval of about Deltatau = 0.015 over the land and Deltatau = 0.010 over the ocean. None of the current operational satellite based instruments for AOD retrieval has been able to achieve this accuracy. The RMSE (Root Mean Square Error) of the AVHRR (Advanced Very High Resolution Radiometer) is typically between 0.06 and 0.15, while the RMSE of the MODIS (Moderate resolution Imaging Spectroradiometer) over the land has been estimated to be Deltatau = 0.05 + 0.2tau, which varies between Deltatau = 0.07 and Deltatau = 0.21 within the limit of usual aerosol optical depth between tau = 0.1 and tau = 0.8. The Department of Energy research satellite instrument, the Multispectral Thermal Imager (MTI), is capable of retrieving aerosol optical depth with an accuracy of Deltatau = 0.03 using an off nadir view at medium scattering angles. Theoretical analysis suggests that the uncertainties in aerosol phase function (due to uncertainties in aerosol shape, size distribution and optical properties) are the major obstacles for accurate aerosol optical depth retrieval. These uncertainties lead to a much larger error in aerosol optical depth retrieval at large scattering angles (usually at close to nadir view) than at off nadir views at medium scattering angles. On the basis of our theoretical analysis and on MTI experience, we suggest that in order to achieve the required accuracy in AOD retrieval, future satellite instruments using a single or dual-view AOD retrieval algorithm should use off-nadir views at medium scattering angles (between 50degrees and 100degrees). C1 Los Alamos Natl Lab, Los Alamos, NM 87545 USA. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. New Mexico State Univ, Dept Phys, Las Cruces, NM 88003 USA. RP Chylek, P (reprint author), Los Alamos Natl Lab, Mail Stop B244, Los Alamos, NM 87545 USA. EM chylek@lanl.gov; crmim@giss.nasa.gov RI Mishchenko, Michael/D-4426-2012 NR 31 TC 20 Z9 20 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 18 PY 2003 VL 108 IS D24 AR 4764 DI 10.1029/2003JD004044 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 760WN UT WOS:000187858400008 ER PT J AU Shenoy, DK Thomsen, DL Keller, P Ratna, BR AF Shenoy, DK Thomsen, DL Keller, P Ratna, BR TI Nonideal elasticity in liquid crystal elastomers SO JOURNAL OF PHYSICAL CHEMISTRY B LA English DT Letter ID POLYMER NETWORKS; MUSCLE AB Nematic elastomers undergo a phase change from an orientationally ordered nematic phase to a disordered isotropic phase when subjected to a temperature change. It is shown that such a phase change is both entropically and energetically driven. Isostrain data on a liquid crystal elastomer material is analyzed in terms of classical rubber elasticity theory. By separating the contributions to the total elastic restoring force into energetic and entropic components, the role of internal energy is assessed and shown to be significant. C1 USN, Res Lab, Ctr Biomol Sci & Engn, Washington, DC 20375 USA. USN, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. CNRS, UMR 168, Inst Curie, Sect Rech,Lab Phys Chem Curie, F-75231 Paris, France. RP Shenoy, DK (reprint author), USN, Res Lab, Ctr Biomol Sci & Engn, 4555 Overlook Ave SW, Washington, DC 20375 USA. NR 12 TC 8 Z9 8 U1 0 U2 5 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1520-6106 J9 J PHYS CHEM B JI J. Phys. Chem. B PD DEC 18 PY 2003 VL 107 IS 50 BP 13755 EP 13757 DI 10.1021/jp0359900 PG 3 WC Chemistry, Physical SC Chemistry GA 753ZX UT WOS:000187279200001 ER PT J AU Rundle, JB Turcotte, DL Shcherbakov, R Klein, W Sammis, C AF Rundle, JB Turcotte, DL Shcherbakov, R Klein, W Sammis, C TI Statistical physics approach to understanding the multiscale dynamics of earthquake fault systems SO REVIEWS OF GEOPHYSICS LA English DT Review DE earthquakes; critical phenomena; self-organization; forecasting ID TIME-TO-FAILURE; SELF-ORGANIZED CRITICALITY; DISCRETE-SCALE-INVARIANCE; MOMENT RELEASE MODEL; SLIDER-BLOCK MODEL; FOREST-FIRE MODEL; THRESHOLD SYSTEMS; CRITICAL-POINT; MECHANICAL BREAKDOWN; LIFETIME STATISTICS AB Earthquakes and the faults upon which they occur interact over a wide range of spatial and temporal scales. In addition, many aspects of regional seismicity appear to be stochastic both in space and time. However, within this complexity, there is considerable self-organization. We argue that the occurrence of earthquakes is a problem that can be attacked using the fundamentals of statistical physics. Concepts of statistical physics associated with phase changes and critical points have been successfully applied to a variety of cellular automata models. Examples include sandpile models, forest fire models, and, particularly, slider block models. These models exhibit avalanche behavior very similar to observed seismicity. A fundamental question is whether variations in seismicity can be used to successfully forecast the occurrence of earthquakes. Several attempts have been made to utilize precursory seismic activation and quiescence to make earthquake forecasts, some of which show promise. C1 Univ Calif Davis, Dept Phys, Ctr Computat Sci & Engn, Davis, CA 95616 USA. Univ Calif Davis, Dept Civil & Environm Engn, Davis, CA 95616 USA. Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. Jet Propuls Lab, Div Earth & Space Sci, Pasadena, CA USA. Boston Univ, Dept Phys, Boston, MA 02215 USA. Univ So Calif, Dept Geol & Geophys, Los Angeles, CA 90089 USA. RP Univ Calif Davis, Dept Phys, Ctr Computat Sci & Engn, Davis, CA 95616 USA. EM rundle@physics.ucdavis.edu; turcotte@geology.ucdavis.edu; roshch@physics.ucdavis.edu; klein@physics.bu.edu RI Shcherbakov, Robert/I-1036-2012 OI Shcherbakov, Robert/0000-0002-3057-0851 NR 168 TC 170 Z9 184 U1 0 U2 26 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 8755-1209 EI 1944-9208 J9 REV GEOPHYS JI Rev. Geophys. PD DEC 18 PY 2003 VL 41 IS 4 AR 1019 DI 10.1029/2003RG000135 PG 30 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 760XH UT WOS:000187860200001 ER PT J AU Giglio, L Pinzon, J Kasibhatla, P AF Giglio, L Pinzon, J Kasibhatla, P TI Comment on "Seasonal, intraseasonal, and interannual variability of global land fires and their effects on atmospheric aerosol distribution" SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Editorial Material DE fire; aerosol; remote sensing ID SOUTH-AMERICA; TRMM VIRS; SATELLITE; MODEL C1 Sci Syst & Applicat Inc, Lanham, MD USA. Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC 27708 USA. RP NASA, Goddard Space Flight Ctr, Code 923, Greenbelt, MD 20771 USA. EM giglio@hades.gsfc.nasa.gov; pinzon@negev.gsfc.nasa.gov; psk9@duke.edu RI Kasibhatla, Prasad/A-2574-2010 NR 10 TC 6 Z9 6 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 17 PY 2003 VL 108 IS D24 AR 4754 DI 10.1029/2003JD003548 PG 5 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 760WM UT WOS:000187858300004 ER PT J AU Ji, YM Stocker, E AF Ji, YM Stocker, E TI Reply to comment by L. Giglio et al. on "Seasonal, intraseasonal, and interannual variability of global land fires and their effects on atmospheric aerosol distribution" SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Editorial Material DE fire; aerosol; remote sensing C1 George Mason Univ, Sch Computat Sci, Fairfax, VA 22030 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP George Mason Univ, Sch Computat Sci, Fairfax, VA 22030 USA. EM yji@tsdis.gsfc.nasa.gov; stocker@tsdis.gsfc.nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 17 PY 2003 VL 108 IS D24 AR 4755 DI 10.1029/2003JD004115 PG 6 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 760WM UT WOS:000187858300015 ER PT J AU Menon, S Brenguier, JL Boucher, O Davison, P Del Genio, AD Feichter, J Ghan, S Guibert, S Liu, XH Lohmann, U Pawlowska, H Penner, JE Quaas, J Roberts, DL Schuller, L Snider, J AF Menon, S Brenguier, JL Boucher, O Davison, P Del Genio, AD Feichter, J Ghan, S Guibert, S Liu, XH Lohmann, U Pawlowska, H Penner, JE Quaas, J Roberts, DL Schuller, L Snider, J TI Evaluating aerosol/cloud/radiation process parameterizations with single-column models and Second Aerosol Characterization Experiment (ACE-2) cloudy column observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosol indirect effect; cloud microphysics; cloud optics ID GENERAL-CIRCULATION MODEL; LARGE-SCALE MODELS; MARINE STRATOCUMULUS CLOUDS; RADIATIVE PROPERTIES; CLIMATE MODEL; MICROPHYSICAL PROCESSES; FORECASTING SYSTEM; STRATIFORM CLOUDS; EFFECTIVE RADIUS; SOLAR-RADIATION AB The Second Aerosol Characterization Experiment (ACE-2) data set along with ECMWF reanalysis meteorological fields provided the basis for the single column model (SCM) simulations, performed as part of the PACE (Parameterization of the Aerosol Indirect Climatic Effect) project. Six different SCMs were used to simulate ACE-2 case studies of clean and polluted cloudy boundary layers, with the objective being to identify limitations of the aerosol/cloud/radiation interaction schemes within the range of uncertainty in in situ, reanalysis and satellite retrieved data. The exercise proceeds in three steps. First, SCMs are configured with the same fine vertical resolution as the ACE-2 in situ data base to evaluate the numerical schemes for prediction of aerosol activation, radiative transfer and precipitation formation. Second, the same test is performed at the coarser vertical resolution of GCMs to evaluate its impact on the performance of the parameterizations. Finally, SCMs are run for a 24-48 hr period to examine predictions of boundary layer clouds when initialized with large-scale meteorological fields. Several schemes were tested for the prediction of cloud droplet number concentration (N). Physically based activation schemes using vertical velocity show noticeable discrepancies compared to empirical schemes due to biases in the diagnosed cloud base vertical velocity. Prognostic schemes exhibit a larger variability than the diagnostic ones, due to a coupling between aerosol activation and drizzle scavenging in the calculation of N. When SCMs are initialized at a fine vertical resolution with locally observed vertical profiles of liquid water, predicted optical properties are comparable to observations. Predictions however degrade at coarser vertical resolution and are more sensitive to the mean liquid water path than to its spatial heterogeneity. Predicted precipitation fluxes are severely underestimated and improve when accounting for sub-grid liquid water variability. Results from the 24-48 hr runs suggest that most models have problems in simulating boundary layer cloud morphology, since the large-scale initialization fields do not accurately reproduce observed meteorological conditions. As a result, models significantly overestimate optical properties. Improved cloud morphologies were obtained for models with subgrid inversions and subgrid cloud thickness schemes. This may be a result of representing subgrid scale effects though we do not rule out the possibility that better large-forcing data may also improve cloud morphology predictions. C1 Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Columbia Univ, Ctr Climate Syst Res, New York, NY USA. Univ Calif Berkeley, Lawrence Berkeley Lab, EETD, Berkeley, CA 94720 USA. CNRS, Meteo France, CNRM, GAME, F-31057 Toulouse, France. Univ Sci & Technol Lille, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. Met Off, Hadley Ctr, Exeter EX1 3PB, Devon, England. Max Planck Inst Meteorol, D-20146 Hamburg, Germany. Pacific NW Natl Lab, Climate Phys Grp, Richland, WA 99352 USA. Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. Warsaw Univ, Inst Phys, PL-02093 Warsaw, Poland. CNRS, Meteorol Dynam Lab, F-75252 Paris, France. Free Univ Berlin, Inst Weltraumwissensch, D-1000 Berlin, Germany. Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA. RP Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM smenon@giss.nasa.gov RI Del Genio, Anthony/D-4663-2012; Boucher, Olivier/J-5810-2012; Boucher, Olivier/K-7483-2012; PAWLOWSKA, Hanna/C-9827-2013; Penner, Joyce/J-1719-2012; Liu, Xiaohong/E-9304-2011; Ghan, Steven/H-4301-2011; Quaas, Johannes/I-2656-2013; Lohmann, Ulrike/B-6153-2009 OI Del Genio, Anthony/0000-0001-7450-1359; Boucher, Olivier/0000-0003-2328-5769; Boucher, Olivier/0000-0003-2328-5769; PAWLOWSKA, Hanna/0000-0002-5345-778X; Liu, Xiaohong/0000-0002-3994-5955; Ghan, Steven/0000-0001-8355-8699; Quaas, Johannes/0000-0001-7057-194X; Lohmann, Ulrike/0000-0001-8885-3785 NR 75 TC 29 Z9 30 U1 2 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 17 PY 2003 VL 108 IS D24 AR 4762 DI 10.1029/2003JD003902 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 760WM UT WOS:000187858300013 ER PT J AU Nakamura, K Kondo, Y Chen, G Crawford, JH Takegawa, N Koike, M Kita, K Miyazaki, Y Shetter, RE Lefer, BL Avery, M Matsumoto, J AF Nakamura, K Kondo, Y Chen, G Crawford, JH Takegawa, N Koike, M Kita, K Miyazaki, Y Shetter, RE Lefer, BL Avery, M Matsumoto, J TI Measurement of NO2 by the photolysis conversion technique during the Transport and Chemical Evolution Over the Pacific (TRACE-P) campaign SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE NO2; O-3; photolytic conversion ID PHOTOSTATIONARY STATE ANALYSIS; INDUCED FLUORESCENCE DETECTION; WESTERN NORTH PACIFIC; AIRBORNE OBSERVATIONS; OZONE PHOTOCHEMISTRY; ATMOSPHERIC NO2; SOUTH-PACIFIC; PEM-TROPICS; SYSTEM; TROPOSPHERE AB An airborne instrument for in situ measurements of tropospheric nitrogen dioxide (NO2) was developed using the photolytic conversion technique followed by chemiluminescence detection of NO. This instrument was used for the measurements of NO2 on board the NASA P-3B aircraft during the Transport and Chemical Evolution Over the Pacific (TRACE-P) campaign. Comparison in the laboratory indicated less than 10% difference between our NO2 instrument and two independent laser-induced fluorescence instruments in the NO2 range of 30 parts per trillion by volume (pptv) to 50 ppbv. The magnitudes of potential errors in airborne tropospheric NO2 measurements were further assessed using the TRACE-P data set. The systematic errors estimated for the median NO2 mixing ratios, 70 pptv at 0-2 km (30 pptv at 2-8 km), were 19% (39%). The random errors for a 10 s integration time were estimated to be 5-10%, depending on altitude. The observed NO2 mixing ratios were compared to those calculated by a photochemical box model. Overall, the calculated NO2 values correlated very well with those observed (r(2)=0.97), although the calculations were systematically higher than the observations by about 30%, except for the highest flight levels. The calculated/observed NO2 ratio remained nearly constant, having values close to 1.3 at 0-4 km, and decreased with altitude. The difference between the observed and model-calculated values, however, was within the combined uncertainty in the measurement and model calculation. The underlying causes for this difference are to be determined in future studies. C1 Univ Tokyo, Adv Sci & Technol Res Ctr, Meguro Ku, Tokyo 1538904, Japan. Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. Ibaraki Univ, Fac Sci, Dept Environm Sci, Mito, Ibaraki 3108512, Japan. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80305 USA. Tokyo Metropolitan Univ, Grad Sch Engn, Dept Appl Chem, Hachioji, Tokyo 1920397, Japan. RP Univ Tokyo, Adv Sci & Technol Res Ctr, Meguro Ku, 4-6-1 Komaba, Tokyo 1538904, Japan. EM nakamura@atmos.rcast.u-tokyo.ac.jp; kondo@atmos.rcast.u-tokyo.ac.jp; g.chen@larc.nasa.gov; j.h.crawford@larc.nasa.gov; takegawa@atmos.rcast.u-tokyo.ac.jp; koike@eps.s.u-tokyo.ac.jp; kita@env.sci.ibaraki.ac.jp; yuzom@aos.eps.s.u-tokyo.ac.jp; shetter@ucar.edu; lefer@ucar.edu; m.a.avery@larc.nasa.gov; mjun@atmchem.apchem.metro-u.ac.jp RI Koike, Makoto/F-4366-2011; Kondo, Yutaka/D-1459-2012; Miyazaki, Yuzo/C-6920-2010; Crawford, James/L-6632-2013; Lefer, Barry/B-5417-2012 OI Crawford, James/0000-0002-6982-0934; Lefer, Barry/0000-0001-9520-5495 NR 28 TC 8 Z9 9 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 17 PY 2003 VL 108 IS D24 AR 4752 DI 10.1029/2003JD003712 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 760WM UT WOS:000187858300008 ER PT J AU Palmer, PI Jacob, DJ Mickley, LJ Blake, DR Sachse, GW Fuelberg, HE Kiley, CM AF Palmer, PI Jacob, DJ Mickley, LJ Blake, DR Sachse, GW Fuelberg, HE Kiley, CM TI Eastern Asian emissions of anthropogenic halocarbons deduced from aircraft concentration data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE anthropogenic; halocarbon emissions; troposphere; TRACE-P ID METHYL CHLOROFORM; ATMOSPHERIC HYDROXYL; TRANSPORT PATHWAYS; TROPOSPHERIC OH; PACIFIC; OUTFLOW; TRENDS AB The Montreal Protocol restricts production of ozone-depleting halocarbons worldwide. Enforcement of the protocol has relied mainly on annual government statistics of production and consumption of these compounds (bottom-up approach). We show here that aircraft observations of halocarbon: CO enhancement ratios on regional to continental scales can be used to infer halocarbon emissions, providing independent verification of the bottom-up approach. We apply this top-down approach to aircraft observations of Asian outflow from the TRACE-P mission over the western Pacific (March-April 2001) and derive emissions from eastern Asia (China, Japan, and Korea). We derive an eastern Asian carbon tetrachloride (CCl4) source of 21.5 Gg yr(-1), several-fold larger than previous estimates and amounting to similar or equal to30% of the global budget for this gas. Our emission estimate for CFC-11 from eastern Asia is 50% higher than inventories derived from manufacturing records. Our emission estimates for methyl chloroform (CH3CCl3) and CFC-12 are in agreement with existing inventories. For halon 1211 we find only a strong local source originating from the Shanghai area. Our emission estimates for the above gases result in a similar or equal to40% increase in the ozone depletion potential (ODP) of Asian emissions relative to previous estimates, corresponding to a similar or equal to10% global increase in ODP. C1 Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Univ Calif Irvine, Dept Earth & Syst Sci, Irvine, CA 92697 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA. RP Harvard Univ, Div Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02138 USA. EM pip@io.harvard.edu; djj@io.harvard.edu; ljm@io.harvard.edu; drblake@uci.edu; g.w.sachse@larc.nasa.gov; fuelberg@met.fsu.edu; ckiley@huey.met.fsu.edu RI Palmer, Paul/F-7008-2010; Mickley, Loretta/D-2021-2012; OI Mickley, Loretta/0000-0002-7859-3470; Martin, Randall/0000-0003-2632-8402 NR 24 TC 36 Z9 37 U1 3 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 17 PY 2003 VL 108 IS D24 AR 4753 DI 10.1029/2003JD003591 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 760WM UT WOS:000187858300005 ER PT J AU Beirle, S Platt, U Wenig, M Wagner, T AF Beirle, S Platt, U Wenig, M Wagner, T TI Weekly cycle of NO2 by GOME measurements: a signature of anthropogenic sources SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID TROPOSPHERIC NO2; AIR-POLLUTANTS; EMISSIONS AB Nitrogen oxides ( NO+ NO2 = NOx and reservoir species) are important trace gases in the troposphere with impact on human health, atmospheric chemistry and climate. Besides natural sources ( lightning, soil emissions) and biomass burning, fossil fuel combustion is estimated to be responsible for about 50% of the total production of NOx. Since human activity in industrialized countries largely follows a seven- day cycle, fossil fuel combustion is expected to be reduced during weekends. This " weekend effect" is well known from local, ground based measurements, but has never been analysed on a global scale before. The Global Ozone Monitoring Experiment ( GOME) on board the ESA- satellite ERS- 2 allows measurements of NO2 column densities. By estimating and subtracting the stratospheric column, and considering radiative transfer, vertical column densities ( VCD) of tropospheric NO2 can be determined ( e. g. Leue et al., 2001). We demonstrate the statistical analysis of weekly cycles of tropospheric NO2 VCDs for different regions of the world. In the cycles of the industrialized regions and cities in the US, Europe and Japan a clear Sunday minimum of tropospheric NO2 VCD can be seen. Sunday NO2 VCDs are about 25 - 50% lower than working day levels. Metropolitan areas with other religious and cultural backgrounds ( Jerusalem, Mecca) show different weekly patterns corresponding to different days of rest. In China, no weekly pattern can be found. The presence of a weekly cycle in the measured tropospheric NO2 VCD may help to identify the different anthropogenic source categories. Furthermore, we estimated the lifetime of tropospheric NO2 by analysing the mean weekly cycle exemplarily over Germany, obtaining a value of about 6 h in summer and 18 - 24 h in winter. C1 Heidelberg Univ, Inst Umweltphys, D-6900 Heidelberg, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Beirle, S (reprint author), Heidelberg Univ, Inst Umweltphys, D-6900 Heidelberg, Germany. EM beirle@iup.uni-heidelberg.de RI Wenig, Mark/K-7279-2012 NR 20 TC 158 Z9 171 U1 2 U2 23 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD DEC 16 PY 2003 VL 3 BP 2225 EP 2232 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 754PD UT WOS:000187324800001 ER PT J AU Cane, HV Richardson, IG AF Cane, HV Richardson, IG TI Reply to comment on "Coronal mass ejections, interplanetary ejecta and geomagnetic storms" by Gopalswamy et al. SO GEOPHYSICAL RESEARCH LETTERS LA English DT Editorial Material ID DECREASES C1 NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Cane, HV (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 661, Greenbelt, MD 20771 USA. NR 7 TC 5 Z9 5 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 16 PY 2003 VL 30 IS 24 AR 2233 DI 10.1029/2003GL017685 PG 2 WC Geosciences, Multidisciplinary SC Geology GA 760VX UT WOS:000187856900002 ER PT J AU Gopalswamy, N Manoharan, PK Yashiro, S AF Gopalswamy, N Manoharan, PK Yashiro, S TI Comment on "Coronal mass ejections, interplanetary ejecta and geomagnetic storms" by H.V. Cane, I.G. Richardson, and O.C.St. Cyr SO GEOPHYSICAL RESEARCH LETTERS LA English DT Editorial Material ID DISTURBANCES; 1-AU C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Catholic Univ Amer, Washington, DC 20064 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Code 695-0, Greenbelt, MD 20771 USA. RI Gopalswamy, Nat/D-3659-2012 NR 8 TC 5 Z9 5 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 16 PY 2003 VL 30 IS 24 AR 2232 DI 10.1029/2003GL017562 PG 2 WC Geosciences, Multidisciplinary SC Geology GA 760VX UT WOS:000187856900001 ER PT J AU Carr, ME AF Carr, ME TI Simulation of carbon pathways in the planktonic ecosystem off Peru during the 1997-1998 El Nino and La Nina SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE El Nino; La Nina; carbon flow; planktonic; upwelling ID CALIFORNIA CURRENT; UPWELLING REGION; NORTHERN CHILE; PHYTOPLANKTON; OCEAN; VARIABILITY; MODEL; FOOD; RESPIRATION; TRANSITION AB A numerical model is used to quantify the pathways of carbon flow through the planktonic ecosystem from 1996 through 1998 at 9.5degreesS off the coast of Peru. The objective was to evaluate the response of the planktonic ecosystem to the forcing associated with normal conditions in 1996, the 1997-1998 El Nino, and the La Nino a which began in June of 1998. During El Nino, the depth of the upper layer increased, temperature increased, and the nitrate concentration in the source water for upwelling was reduced. La Nino a forcing was the opposite. The simulated phytoplankton biomass, carbon uptake, vertical export, and food available for higher trophic levels were reduced during the El Nino period compared to normal conditions. Phytoplankton biomass and uptake were slightly less during La Nino than in 1996, though carbon export and advective loss were significantly enhanced. A series of numerical experiments were run to determine whether the upwelling rate, source water characteristics, depth of the upper layer, or phytoplankton size composition of the source water was the primary forcing factor for the planktonic community. Although all factors contributed to the magnitude of the simulated response, the primary determinant for El Nino conditions was the concentration of new nitrogen in the upwelling source water, followed by depth of the upper layer and upwelling rate. The depth of the upper layer was the dominant forcing term for La Nina, followed by upwelling rate and temperature of the source water. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91009 USA. RP Carr, ME (reprint author), CALTECH, Jet Prop Lab, MS 300-323,4800 Oak Grove Dr, Pasadena, CA 91009 USA. NR 45 TC 5 Z9 6 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC 16 PY 2003 VL 108 IS C12 AR 3380 DI 10.1029/1999JC000064 PG 15 WC Oceanography SC Oceanography GA 760WV UT WOS:000187859000001 ER PT J AU Holmes, BJ AF Holmes, BJ TI 21st century networking - Avionics will play a key role in enabling transformation of the US aviation system SO AVIATION WEEK & SPACE TECHNOLOGY LA English DT Article C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Holmes, BJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MCGRAW HILL INC PI NEW YORK PA 1221 AVENUE OF THE AMERICAS, NEW YORK, NY 10020 USA SN 0005-2175 J9 AVIAT WEEK SPACE TEC JI Aviat. Week Space Technol. PD DEC 15 PY 2003 VL 159 IS 24 BP 74 EP 75 PG 2 WC Engineering, Aerospace SC Engineering GA 756AA UT WOS:000187442600037 ER PT J AU Todorovski, L Weroski, S Langley, P Potter, C AF Todorovski, L Weroski, S Langley, P Potter, C TI Using equation discovery to revise an Earth ecosystem model of the carbon net production SO ECOLOGICAL MODELLING LA English DT Article; Proceedings Paper CT 3rd European Ecological Modelling Conference CY SEP 10-15, 2001 CL DUBROVNIK, CROATIA DE machine learning; equation discovery; model revision; carbon net production ID PREDICTION; FLUXES AB Equation discovery approaches to automated modeling from observed data usually derive equation-based models from scratch rather than from an initial model already established in the domain of use. In this paper, we present an approach that uses new or recent observational data to improve an existing equation-based model. The approach is used to reduce the error of the Earth,ecosystem model of the net production of carbon in the atmosphere. We revise the initial ecosystem model in two directions. First, we calibrate the values of the constant parameters in the model on new observational data. Second, we allow the use of alternative equation structures for some of the sub-models of the initial model and use our approach to choose among them. Experiments show that both revision of values of the constant parameters and revision of the structures of sub-models can considerably reduce the error of the initial model. (C) 2003 Elsevier B.V. All rights reserved. C1 Jozef Stefan Inst, Dept Intelligent Syst, Ljubljana 1000, Slovenia. Inst Study Learning & Expertise, Palo Alto, CA 94306 USA. NASA, Ames Res Ctr, Ecosyst Sci Branch, Moffett Field, CA 94035 USA. RP Todorovski, L (reprint author), Jozef Stefan Inst, Dept Intelligent Syst, Jamova 39, Ljubljana 1000, Slovenia. NR 18 TC 12 Z9 12 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3800 J9 ECOL MODEL JI Ecol. Model. PD DEC 15 PY 2003 VL 170 IS 2-3 BP 141 EP 154 DI 10.1016/S0304-3800(03)00222-9 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 756JB UT WOS:000187461000004 ER PT J AU ElAhl, AMS He, MQ Zhou, PZ Harris, GL Salamanca-Riba, L Felt, F Shaw, HC Sharma, A Jah, M Lakins, D Steiner, T Mohammad, SN AF ElAhl, AMS He, MQ Zhou, PZ Harris, GL Salamanca-Riba, L Felt, F Shaw, HC Sharma, A Jah, M Lakins, D Steiner, T Mohammad, SN TI Systematic study of effects of growth conditions on the (nano-, meso-, micro)size and (one-, two-, three-dimensional) shape of GaN single crystals grown by a direct reaction of Ga with ammonia SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID GALLIUM NITRIDE NANOWIRES; MOLECULAR-BEAM EPITAXY; CHEMICAL-VAPOR-DEPOSITION; BLUE; SEMICONDUCTORS; NANORODS; INP(001); SAPPHIRE; LAYERS; WIRES AB A series of experiments have been conducted to systematically study the effects of growth conditions (NH3 flow rate, growth temperature, chamber pressure, and growth location) on the size (nano, meso, or micro) and the shape (one, two, or three dimensional) of GaN single crystal products grown by a direct reaction of Ga with NH3. A growth map with a wider range of experimental parameters was developed; it has three distinct zones. The size and shape of the products in every zone were found to depend on both temperature and NH3 flow rate with other growth conditions fixed. An effective surface diffusion length consisting of the Ga atomic surface diffusion length and the GaN molecular surface diffusion length, and the anisotropy of the Ga surface diffusion length and the GaN growth rate in different growth directions were introduced into the growth model, in such a way that it allowed successful explanation of all observed results. The optimal growth parameters could thus be determined, which conclusively demonstrated that nanowires with uniform diameter, clear crystal structure, length larger than 1 mm, uniform location distribution, and high yield can be obtained. Such a growth map based on in-depth understanding of the growth mechanism provides a clear direction for growing various materials with desired size and shape. (C) 2003 American Institute of Physics. C1 Howard Univ, Dept Elect Engn, Washington, DC 20059 USA. Howard Univ, Mat Sci Res Ctr Excellence, Washington, DC 20059 USA. Univ Maryland, Dept Mat & Nucl Engn, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Component Technol & Radiat Effects Branch, Greenbelt, MD 20771 USA. AF Off Sci Res, AF Lab, Arlington, VA 22203 USA. RP Mohammad, SN (reprint author), Howard Univ, Dept Elect Engn, 2300 6th St NW, Washington, DC 20059 USA. RI Salamanca-Riba, Lourdes/B-3785-2009 OI Salamanca-Riba, Lourdes/0000-0001-8155-6403 NR 37 TC 33 Z9 33 U1 3 U2 15 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD DEC 15 PY 2003 VL 94 IS 12 BP 7749 EP 7756 DI 10.1063/1.1622992 PG 8 WC Physics, Applied SC Physics GA 750AV UT WOS:000186969900058 ER PT J AU Wang, DY AF Wang, DY TI Quantum dynamics scattering study of AB+CDE reactions: A seven-dimensional treatment for the H-2+C2H reaction SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID RATE-CONSTANT MEASUREMENTS; DIMENSIONALITY CALCULATIONS; REDUCED DIMENSIONALITY; TEMPERATURE-DEPENDENCE; C2H; H-2; PHOTOCHEMISTRY; ACETYLENE; D2; ATMOSPHERE AB A time-dependent wave packet approach is presented for the quantum dynamics study of the AB+CDE reaction system for zero total angular momentum. A seven-degree-of-freedom calculation is employed to study the chemical reaction of H-2+C2H-->H+C2H2 by treating C2H as a linear molecule. Initial state selected reaction probabilities are presented for various initial rovibrational states. This study shows that the vibrational excitation of H-2 enhances the reaction probability, whereas the excitation of C2H has only a small effect on the reactivity. An integral cross section is also reported for the initial ground states of H-2 and C2H. The theoretical and experimental results agree with each other very well when the calculated seven-dimensional results are adjusted to account for the lower transition state barrier heights found in recent ab initio calculations. (C) 2003 American Institute of Physics. C1 NASA, Eloret, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Wang, DY (reprint author), NASA, Eloret, Ames Res Ctr, MS T27B-1, Moffett Field, CA 94035 USA. NR 41 TC 16 Z9 16 U1 1 U2 9 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 15 PY 2003 VL 119 IS 23 BP 12057 EP 12062 DI 10.1063/1.1624831 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 750AW UT WOS:000186970000004 ER PT J AU Tao, WK Shie, CL Simpson, J Braun, S Johnson, RH Ciesielski, PE AF Tao, WK Shie, CL Simpson, J Braun, S Johnson, RH Ciesielski, PE TI Convective systems over the South China Sea: Cloud-resolving model simulations SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID TROPICAL SQUALL-LINE; MEASURING MISSION TRMM; TOGA-COARE; MOISTURE BUDGETS; NUMERICAL-SIMULATION; STRATIFORM PRECIPITATION; BULK PARAMETERIZATION; MESOSCALE PROCESSES; CUMULUS ENSEMBLES; SURFACE PROCESSES AB The two-dimensional version of the Goddard Cumulus Ensemble ( GCE) model is used to simulate two South China Sea Monsoon Experiment (SCSMEX) convective periods [18-26 May (prior to and during the monsoon onset) and 2-11 June ( after the onset of the monsoon) 1998]. Observed large-scale advective tendencies for potential temperature, water vapor mixing ratio, and horizontal momentum are used as the main forcing in governing the GCE model in a semiprognostic manner. The June SCSMEX case has stronger forcing in both temperature and water vapor, stronger low-level vertical shear of the horizontal wind, and larger convective available potential energy (CAPE). The temporal variation of the model-simulated rainfall, time- and domain-averaged heating, and moisture budgets compares well to those diagnostically determined from soundings. However, the model results have a higher temporal variability. The model underestimates the rainfall by 17% to 20% compared to that based on soundings. The GCE model-simulated rainfall for June is in very good agreement with the Tropical Rainfall Measuring Mission (TRMM), precipitation radar (PR), and the Global Precipitation Climatology Project (GPCP). Overall, the model agrees better with observations for the June case rather than the May case. The model-simulated energy budgets indicate that the two largest terms for both cases are net condensation (heating/drying) and imposed large-scale forcing (cooling/moistening). These two terms are opposite in sign, however. The model results also show that there are more latent heat fluxes for the May case. However, more rainfall is simulated for the June case. Net radiation (solar heating and longwave cooling) are about 34% and 25%, respectively, of the net condensation (condensation minus evaporation) for the May and June cases. Sensible heat fluxes do not contribute to rainfall in either of the SCSMEX cases. Two types of organized convective systems, unicell (May case) and multicell (June case), are simulated by the model. They are determined by the observed mean U wind shear (unidirectional versus reverse shear profiles above midlevels). Several sensitivity tests are performed to examine the impact of the radiation, microphysics, and large-scale mean horizontal wind on the organization and intensity of the SCSMEX convective systems. C1 NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Branch, Atmospheres Lab, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP Tao, WK (reprint author), NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Branch, Atmospheres Lab, Code 912, Greenbelt, MD 20771 USA. NR 59 TC 55 Z9 57 U1 0 U2 4 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD DEC 15 PY 2003 VL 60 IS 24 BP 2929 EP 2956 DI 10.1175/1520-0469(2003)060<2929:CSOTSC>2.0.CO;2 PG 28 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 750FY UT WOS:000186981700001 ER PT J AU Coy, L Stajner, I DaSilva, AM Joiner, J Rood, RB Pawson, S Lin, SJ AF Coy, L Stajner, I DaSilva, AM Joiner, J Rood, RB Pawson, S Lin, SJ TI High-frequency planetary waves in the polar middle atmosphere as seen in a data assimilation system SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID 4-DAY WAVE; BAROTROPIC INSTABILITY; STRATOSPHERE; MODEL; TRANSPORT; WINTER; MESOSPHERE; OZONE; JET AB The 4-day wave often dominates the large-scale wind, temperature, and constituent variability in the high-latitude Southern Hemisphere winter near the stratopause. This study examines the winter Southern Hemisphere vortex of 1998 using 4-times-daily output from a data assimilation system to focus on the polar 2-day, wave-number-2 component of the 4-day wave. The data assimilation system products are from a test version of the finite volume data assimilation system (fvDAS) being developed at the Goddard Space Flight Center (GSFC) and include an ozone assimilation system. Results show that the polar 2-day wave in temperature and ozone dominates over other planetary-scale disturbances during July 1998 at 70degreesS. The period of the quasi-2-day wave is somewhat shorter than 2 days (about 1.7 days) during July 1998 with an average perturbation temperature amplitude for the month of over 2.5 K. The 2-day wave propagates more slowly than the zonal mean zonal wind, consistent with Rossby wave theory, and has Eliassen-Palm (EP) flux divergence regions associated with regions of negative horizontal potential vorticity gradients, as expected from linear instability theory. Results for the assimilation-produced ozone mixing ratio show that the 2-day wave represents a major source of ozone variation in this region. The ozone wave in the assimilation system is in good agreement with the wave seen in the Polar Ozone and Aerosol Measurement (POAM) ozone observations for the same time period. Some differences from linear instability theory are noted, as well as spectral peaks in the ozone field, not seen in the temperature field, that may be a consequence of advection. C1 USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Coy, L (reprint author), USN, Res Lab, EO Hulburt Ctr Space Res, Code 7646,4555 Overlook Ave SW, Washington, DC 20375 USA. RI Joiner, Joanna/D-6264-2012; da Silva, Arlindo/D-6301-2012; Stajner, Ivanka/B-5228-2009; Rood, Richard/C-5611-2008; Pawson, Steven/I-1865-2014 OI da Silva, Arlindo/0000-0002-3381-4030; Stajner, Ivanka/0000-0001-6103-3939; Rood, Richard/0000-0002-2310-4262; Pawson, Steven/0000-0003-0200-717X NR 26 TC 6 Z9 6 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD DEC 15 PY 2003 VL 60 IS 24 BP 2975 EP 2992 DI 10.1175/1520-0469(2003)060<2975:HPWITP>2.0.CO;2 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 750FY UT WOS:000186981700003 ER PT J AU Cheng, Y Canuto, VM Howard, AM AF Cheng, Y Canuto, VM Howard, AM TI Comments on "On an improved model for the turbulent PBL" SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Editorial Material ID SHEAR-DRIVEN FLOWS; DYNAMICAL MODEL; 2-DIMENSIONAL HILLS; BOUNDARY-LAYER; NUMERICAL-SIMULATION; CLOSURE-MODEL; CONVECTION; REGIMES C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Canuto, VM (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. NR 30 TC 6 Z9 6 U1 1 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD DEC 15 PY 2003 VL 60 IS 24 BP 3043 EP 3046 DI 10.1175/1520-0469(2003)060<3043:COOAIM>2.0.CO;2 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 750FY UT WOS:000186981700008 ER PT J AU Knuth, KH AF Knuth, KH TI Intelligent machines in the twenty-first century: foundations of inference and inquiry SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE inference; probability; entropy; Bayesian methods; lattice theory; machine intelligence ID MATHEMATICAL-THEORY; INFORMATION; COMMUNICATION; PROBABILITIES; MECHANICS AB The last century saw the application of Boolean algebra to the construction of computing machines, which work by applying logical transformations to information contained in their memory. The development of information theory and the generalization of Boolean algebra to Bayesian inference have enabled these computing machines, in the last quarter of the twentieth century, to be endowed with the ability to learn by making inferences from data. This revolution is just beginning as new computational techniques continue to make difficult problems more accessible. Recent advances in our understanding of the foundations of probability theory have revealed implications for areas other than logic. Of relevance to intelligent machines, we recently identified the algebra of questions as the free distributive algebra, which will now allow us to work with questions in a way analogous to that which Boolean algebra enables us to work with logical statements. In this paper, we examine the foundations of inference and inquiry. We begin with a history of inferential reasoning, highlighting key concepts that have led to the automation of inference in modern machine-learning systems. We then discuss the foundations of inference in more detail using a modern viewpoint that relies on the mathematics of partially ordered sets and the scaffolding of lattice theory. This new viewpoint allows us to develop the logic of inquiry and introduce a measure describing the relevance of a proposed question to an unresolved issue. Last, we will demonstrate the automation of inference, and discuss how this new logic of inquiry will enable intelligent machines to ask questions. Automation of both inference and inquiry promises to allow robots to perform science in the far reaches of our solar system and in other star systems by enabling them not only to make inferences from data, but also to decide which question to ask, which experiment to perform, or which measurement to take given what they have learned and what they are designed to understand. C1 NASA, Ames Res Ctr, Computat Sci Div, Moffett Field, CA 94035 USA. RP Knuth, KH (reprint author), NASA, Ames Res Ctr, Computat Sci Div, Moffett Field, CA 94035 USA. NR 47 TC 8 Z9 8 U1 0 U2 1 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD DEC 15 PY 2003 VL 361 IS 1813 BP 2859 EP 2873 DI 10.1098/rsta.2003.1268 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 752ZA UT WOS:000187205000015 PM 14667302 ER PT J AU Hu, JN Tan, B Shabanov, N Crean, KA Martonchik, JV Diner, DJ Knyazikhin, Y Myneni, RB AF Hu, JN Tan, B Shabanov, N Crean, KA Martonchik, JV Diner, DJ Knyazikhin, Y Myneni, RB TI Performance of the MISR LAI and FPAR algorithm: a case study in Africa SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE MISR; FpAR; visible/near-infrared spectral bands ID LEAF-AREA INDEX; PHOTOSYNTHETICALLY ACTIVE RADIATION; MULTISCALE ANALYSIS; ABSORBED PAR; MODIS; VEGETATION; PRODUCT; LAND; VALIDATION; FRACTION AB The Multi-angle Imaging SpectroRadiometer (MISR) instrument is designed to provide global imagery at nine discrete viewing angles and four visible/near-infrared spectral bands. The MISR standard products include green leaf area index (LAI) of vegetation and fraction of photosynthetically active radiation absorbed by vegetation (FPAR). These parameters are being routinely processed from MISR data at the Langley Atmospheric Sciences Data Center (ASDC) since October 2002. This paper describes the research basis for transitioning the MISR LAI/FPAR product from beta to provisional status. The quality and spatial coverage of MISR land surface reflectances that are input to the algorithm determine the quality and spatial coverage of the LAI and FPAR products. Therefore, considerable efforts have been expended to analyze the performance of the algorithm as a function of uncertainties of MISR surface reflectances and to establish the convergence property of the MISR LAI/FPAR algorithm, namely, that the reliability and accuracy of the retrievals increase with increased input information content and accuracy. An additional objective of the MISR LAI/FPAR algorithm is classification of global vegetation into biome types-information that is usually an input to remote sensing algorithms that use single-angle observations. An upper limit of uncertainties of MISR surface reflectances that allows discrimination between biomes, minimizes the impact of biome misidentification on LAI retrievals, and maximizes the spatial coverage of retrievals was estimated. Algorithm performance evaluated on a limited set of MISR data from Africa suggests valid LAI retrievals and correct biome identification in about 20% of the pixels, on an average, given the current level of uncertainties in the MISR surface reflectance data. The other 80% of the LAI values are retrieved using incorrect information about the type of biome. However, the use of multi-angle data minimizes the impact of biome misidentification on LAI retrievals; that is, with a probability of about 70%, uncertainties in LAI retrievals due to biome misclassification do not exceed uncertainties in the observations. We also discuss in depth the parameters that characterize LAI/FPAR product quality-such as quality assessment (QA) that is available to the users along with the product. The analysis of the MISR LAI/FPAR product presented here demonstrates the physical basis of the radiative transfer algorithm used in the retrievals and, importantly, that the reliability and accuracy of the retrievals increase with increased input information content and accuracy. Further improvements in the quality of MISR surface reflectances are therefore expected to lead to LAI and FPAR retrievals of increasing quality. (C) 2003 Elsevier Inc. All rights reserved. C1 Boston Univ, Dept Geog, Boston, MA 02215 USA. Jet Prop Lab, Pasadena, CA 91109 USA. RP Hu, JN (reprint author), Boston Univ, Dept Geog, 675 Commonwealth Ave, Boston, MA 02215 USA. RI Tan, Bin/G-1331-2012; Myneni, Ranga/F-5129-2012 NR 25 TC 29 Z9 32 U1 4 U2 17 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC 15 PY 2003 VL 88 IS 3 BP 324 EP 340 DI 10.1016/j.rse.2003.05.002 PG 17 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 751QN UT WOS:000187078600008 ER PT J AU Zuffada, C Elfouhaily, T Lowe, S AF Zuffada, C Elfouhaily, T Lowe, S TI Sensitivity analysis of wind vector measurements from ocean reflected GPS signals SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE wind vector; GPS signals; scattered fields ID SCATTERING; SURFACE; ALTIMETRY; MODEL AB The power received by a GPS receiver located on an airplane flying over the ocean and collecting the GPS signal reflected off the surface is estimated for varying wind speed and wind direction, platform altitude, satellite elevation angle, and receiver integration time. By accounting for the wind-induced anisotropy on the surface, it is shown that the trailing edges of computed waveforms change with both wind speed and direction. When the receiver integration time is properly chosen, substantial differences in the waveforms at different wind directions are exhibited even at the beginning of the trailing edge, particularly for reflections from high-elevation satellites. These differences are associated with the extent and directional properties of the scattered fields as a function of reflection angle. An analysis of the interdependence of the observational (geometric) parameters, the coherence time, and the receiver integration time is presented to suggest a suitable arrangement for enhanced measurement sensitivity to the wind direction. (C) 2003 Elsevier Inc. All rights reserved. C1 CALTECH, Jet Prop Lab, Flight Sci Expt Sect 328, Pasadena, CA 91109 USA. IRPHE, CNRS, IOA, F-13288 Marseille 9, France. RP Zuffada, C (reprint author), CALTECH, Jet Prop Lab, Flight Sci Expt Sect 328, 4800 Oak Grove Dr,MS 183-601, Pasadena, CA 91109 USA. NR 19 TC 18 Z9 20 U1 0 U2 2 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC 15 PY 2003 VL 88 IS 3 BP 341 EP 350 DI 10.1016/S0034-4257(03)00175-5 PG 10 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 751QN UT WOS:000187078600009 ER PT J AU Cardellach, E Ruffini, G Pino, D Rius, A Komjathy, A Garrison, JL AF Cardellach, E Ruffini, G Pino, D Rius, A Komjathy, A Garrison, JL TI Mediterranean Balloon Experiment: ocean wind speed sensing from the stratosphere, using GPS reflections SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE global positioning system (GPS); scatterometry; oceanography; bistatic radar ID SEA-SURFACE; SIGNALS; MODEL; SCATTERING; ALTIMETRY; SPECTRUM; SYSTEM; PARIS AB The MEditerranean Balloon EXperiment (MEBEX), conducted in August 99 from the middle-up stratosphere, was designed to assess the wind retrieval sensitivity of Global Navigation Satellite Systems Reflections (GNSSR) technology from high altitudes. Global Positioning System reflected signals (GPSR) collected at altitudes around 37 km with a dedicated receiver have been inverted to mean square slopes (MSS) of the sea surface and wind speeds. The theoretical tool to interpret the geophysical parameters was a bistatic model, which also depends on geometrical parameters. The results have been analyzed in terms of internal consistency, repeatability and geometry-dependent performance. In addition, wind velocities have been compared to independent measurements by QuikSCAT, TOPEX, ERS/RA and a Radio Sonde, with an agreement better than 2 m/s. A Numerical Weather Prediction Model (NWPM, the MM5 mesoscale forecast model) has also been used for comparison with varying results during the experiment. The conclusion of-this study confirms the capability of high altitude GPSR/Delay-map receivers with low gain antennas to infer surface winds. (C) 2003 Elsevier Inc. All rights reserved. C1 CSIC, IEEC, ES-08034 Barcelona, Spain. Star Lab, Ed Observat Fabra, E-08035 Barcelona, Spain. Univ Colorado, CCAR, Boulder, CO 80309 USA. Purdue Univ, W Lafayette, IN 47907 USA. RP Cardellach, E (reprint author), NASA, Jet Propuls Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Cardellach, Estel/C-9418-2012; Pino, David/F-7940-2014; Antonio, Rius/A-4873-2012 OI Cardellach, Estel/0000-0001-8908-0972; Pino, David/0000-0002-4512-0175; Antonio, Rius/0000-0002-5947-2649 NR 24 TC 44 Z9 49 U1 0 U2 6 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC 15 PY 2003 VL 88 IS 3 BP 351 EP 362 DI 10.1016/S0034-4257(03)00176-7 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 751QN UT WOS:000187078600010 ER PT J AU Mayr, HG Mengel, JG Talaat, ER Porter, HS Chan, KL AF Mayr, HG Mengel, JG Talaat, ER Porter, HS Chan, KL TI Planetary-scale inertio gravity waves in the Mesosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID DOPPLER-SPREAD PARAMETERIZATION; MIDDLE ATMOSPHERE; MOMENTUM DEPOSITION; 12-HOUR OSCILLATION; SOUTH-POLE; MU-RADAR AB In the polar region of the upper mesosphere, horizontal wind oscillations have been observed with periods around 10 hours. Waves with such periods are generated in our Numerical Spectral Model (NSM), and they are identified as planetary-scale inertio gravity waves (IGW). These waves have periods between 9 and 11 hours and appear above 70 km in the zonal mean (m = 0), as well as in m = 1 to 4 propagating eastward and westward. They grow in magnitude to altitudes near 100 km and have vertical wavelengths of about 25 km. The m = 1 westward IGWs have the largest amplitudes, up to 30 m/s at the poles. The IGWs occur intermittently but reveal systematic seasonal variations. Their amplitudes generally are largest in late winter and spring. Numerical experiments show that the waves also appear without tidal excitation. Like the planetary waves in the model, the IGWs are produced by instabilities that arise in the mean zonal circulation. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Lanham, MD USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. Furman Univ, Greenville, SC 29613 USA. Hong Kong Univ Sci & Technol, Hong Kong, Hong Kong, Peoples R China. RP Mayr, HG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 21 TC 5 Z9 5 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 13 PY 2003 VL 30 IS 23 AR 2228 DI 10.1029/2003GL018376 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 756PG UT WOS:000187489800003 ER PT J AU Washenfelder, RA Wennberg, PO Toon, GC AF Washenfelder, RA Wennberg, PO Toon, GC TI Tropospheric methane retrieved from ground-based near-IR solar absorption spectra SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID HALOGEN OCCULTATION EXPERIMENT; ATMOSPHERIC METHANE; CM-1 AB High-resolution near-infrared solar absorption spectra recorded between 1977 and 1995 at the Kitt Peak National Solar Observatory are analyzed to retrieve column abundances of methane (CH4), hydrogen fluoride (HF), and oxygen (O-2). Employing a stratospheric "slope equilibrium" relationship between CH4 and HF, the varying contribution of stratospheric CH4 to the total column is inferred. Variations in the CH4 column due to changes in surface pressure are determined from the O-2 column abundances. By this technique, CH4 tropospheric volume mixing ratios are determined with a precision of similar to0.5%. These display behavior similar to Mauna Loa in situ surface measurements, with a seasonal peak-to-peak amplitude of approximately 30 ppbv and a nearly linear increase between 1977 and 1983 of 18.0 +/- 0.8 ppbv yr(-1), slowing significantly after 1990. C1 CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Washenfelder, RA (reprint author), CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. RI Washenfelder, Rebecca/E-7169-2010; Wennberg, Paul/A-5460-2012 OI Washenfelder, Rebecca/0000-0002-8106-3702; NR 14 TC 38 Z9 38 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 13 PY 2003 VL 30 IS 23 AR 2226 DI 10.1029/2003GL017969 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 756PG UT WOS:000187489800001 ER PT J AU Jenkins, GS Ryu, JH Thompson, AM Witte, JC AF Jenkins, GS Ryu, JH Thompson, AM Witte, JC TI Linking horizontal and vertical transports of biomass fire emissions to the Tropical Atlantic Ozone Paradox during the Northern Hemisphere winter season: 1999 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE biomass burning; West Africa; winter season ID TROPOSPHERIC OZONE; GLOBAL PRECIPITATION; SATELLITE; AEROSOL; MAXIMUM; AFRICA AB The horizontal and vertical transport of biomass fire emissions in West Africa for January 1999, are examined using all available data including wind, fire, aerosol, precipitation, lightning and outgoing longwave radiation. Ozonesonde data from the Aerosols99 Trans-Atlantic cruise are also included with rain and wind analyses. The results here support earlier studies that ozone and ozone precursors associated with biomass burning are confined to the lower troposphere primarily due to the lack of deep convection over land areas. Ozone and its precursors are horizontally transported equatorward or toward the west by winds in the 1000-700 hPa layers. However, rising adiabatic motions associated with the diurnal evolution of the West African planetary boundary layer can transport ozone and its precursors vertically into the free troposphere above the marine boundary layer. Moreover, lightning from South America, Central Africa and mesoscale convective systems in the Gulf of Guinea can lead to elevated ozone mixing ratios in the middle and upper troposphere of the tropical south Atlantic. The results presented here shed light of the proposed ozone paradox during Northern Hemisphere winter. C1 Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. RP Jenkins, GS (reprint author), Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA. EM osei@essc.psu.edu RI Thompson, Anne /C-3649-2014 OI Thompson, Anne /0000-0002-7829-0920 NR 19 TC 17 Z9 17 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 13 PY 2003 VL 108 IS D23 AR 4745 DI 10.1029/2002JD003297 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 756QL UT WOS:000187492400002 ER PT J AU Rakov, VA Crawford, DE Kodali, V Idone, VP Uman, MA Schnetzer, GH Rambo, KJ AF Rakov, VA Crawford, DE Kodali, V Idone, VP Uman, MA Schnetzer, GH Rambo, KJ TI Cutoff and reestablishment of current in rocket-triggered lightning SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE lightning; current cutoff; stepping ID COMMON PHYSICAL PROCESSES; TRANSMISSION-LINE MODEL; RETURN-STROKE MODELS; TIME DERIVATIVES; MAGNETIC-FIELDS; ELECTRIC-FIELDS; M-COMPONENT; LEADER; RADIATION; ARRESTERS AB A total of three negative rocket-triggered lightning flashes without return strokes (two from 1997 and one from 1993) are analyzed in this paper in order to study the processes associated with the disintegration of the triggering wire and its replacement by an air-plasma channel. It appears that the gap resulting from the vaporization of the triggering wire by the upward-positive leader current is bridged by a leader/return-stroke type process. Electric fields at distances of 50, 110, and 500 m, the corresponding magnetic fields at 500 m, and the currents to ground are examined for the two 1997 flashes. The electric field prior to the triggering wire's vaporization in these flashes exhibits a positive (atmospheric electricity sign convention) millisecond-scale ramp due to the upward-extending positive leader. The electric field changes observed at the three distances just prior to wire vaporization are consistent with an equivalent point charge of about 0.3 C at a height of 1.2 to 1.5 km, suggesting that the charge density distribution at that time is strongly skewed toward the upward positive leader tip. The length of the triggering wire at the time of its vaporization was estimated from still photographs to be about 210-220 m. Following the ramp, a microsecond-scale V-shaped negative pulse, which resembles the close electric field signature of a small dart-leader/return-stroke sequence, is observed. The corresponding magnetic field decreases abruptly, simultaneously with the onset of the leading edge of the V-shaped pulse, to values near zero and remains there for tens of microseconds, indicating the attempted interruption (cutoff) of the upward positive leader current flow to ground through the triggering wire as it is vaporized by this current. Following the abrupt decrease, the magnetic field exhibits a rapid increase at a time corresponding to the trailing edge of the V-shaped electric field pulse, suggesting that the vaporized triggering wire is replaced by an air-plasma channel that becomes part of the upward positive leader channel when electrical connection to ground is restored. For the third triggered lightning flash, from 1993, similar inferences regarding the processes involved in the replacement of the triggering wire by an air-plasma channel are made from high-speed (streak) photography and from measurements of the current to ground and electric field at 30 m. In this flash, the upward positive leader exhibited very pronounced stepping: step current pulses had peaks, as measured at the ground, that were up to a few kiloamperes, and step charges that were up to 100 mC. Characterization of the attempted interruption and the following reestablishment of current to ground in rocket-triggered lightning may have important implications for the understanding of channel current cutoff in natural lightning flashes and may provide new insights into the formation of strokes observed to occur in the same channel within a millisecond or less. C1 Univ Florida, Dept Elect & Comp Engn, Gainesville, FL 32611 USA. NASA, Kennedy Space Ctr, FL 32899 USA. SUNY Albany, Dept Earth & Atmospher Sci, Albany, NY 12222 USA. RP Rakov, VA (reprint author), Univ Florida, Dept Elect & Comp Engn, 216 Larsen Hall,POB 116200, Gainesville, FL 32611 USA. EM rakov@ece.ufl.edu RI Rakov, Vladimir/A-8775-2009 OI Rakov, Vladimir/0000-0002-4582-9483 NR 41 TC 26 Z9 26 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 13 PY 2003 VL 108 IS D23 AR 4747 DI 10.1029/2003JD003694 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 756QL UT WOS:000187492400006 ER PT J AU Chin, CS Samanta, MP AF Chin, CS Samanta, MP TI Global snapshot of a protein interaction network - a percolation based approach SO BIOINFORMATICS LA English DT Article ID SACCHAROMYCES-CEREVISIAE; INTERACTION GENERALITY; RELIABILITY; COMPLEXES AB Motivation: Biologically significant information can be revealed by modeling large-scale protein interaction data using graph theory based network analysis techniques. However, the methods that are currently being used draw conclusions about the global features of the network from local connectivity data. A more systematic approach would be to define global quantities that measure (1) how strongly a protein ties with the other parts of the network and (2) how significantly an interaction contributes to the integrity of the network, and connect them with phenotype data from other sources. In this paper, we introduce such global connectivity measures and develop a stochastic algorithm based upon percolation in random graphs to compute them. Results: We show that, in terms of global connectivities, the distribution of essential proteins is distinct from the background. This observation highlights a fundamental difference between the essential and the non-essential proteins in the network. We also find that the interaction data obtained from different experimental methods such as immunoprecipitation and two-hybrid techniques contribute differently to network integrities. Such difference between different experimental methods can provide insight into the systematic bias present among these techniques. C1 Univ Calif San Francisco, Dept Biochem & Biophys, San Francisco, CA 94143 USA. NASA, Ames Res Ctr, NASA Adv Supercomp Div, Moffett Field, CA 94035 USA. RP Chin, CS (reprint author), Univ Calif San Francisco, Dept Biochem & Biophys, San Francisco, CA 94143 USA. NR 21 TC 22 Z9 23 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1367-4803 J9 BIOINFORMATICS JI Bioinformatics PD DEC 12 PY 2003 VL 19 IS 18 BP 2413 EP 2419 DI 10.1093/bioinformatics/btg339 PG 7 WC Biochemical Research Methods; Biotechnology & Applied Microbiology; Computer Science, Interdisciplinary Applications; Mathematical & Computational Biology; Statistics & Probability SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Computer Science; Mathematical & Computational Biology; Mathematics GA 753DX UT WOS:000187217700010 PM 14668225 ER EF