FN Thomson Reuters Web of Science™ VR 1.0 PT J AU KOEKEMOER, AM HENKEL, C GREENHILL, LJ DEY, A VANBREUGEL, W ANTONUCCI, R CODELLA, C AF KOEKEMOER, AM HENKEL, C GREENHILL, LJ DEY, A VANBREUGEL, W ANTONUCCI, R CODELLA, C TI A WATER-VAPOR GIGA-MASER IN THE ACTIVE GALAXY TXFS2226-184 SO NATURE LA English DT Article ID STAR-FORMING REGIONS; GALACTIC NUCLEI; H2O MASERS; EMISSION; NGC-3079 AB ACTIVE galactic nuclei are thought to be powered by gas falling into a massive black hole; the different types of active galaxy mag arise because we view them through a thick torus of molecular gas at varying angles of inclination(1). One way to determine whether the black hole is surrounded by a torus, which would obscure the accretion disk around the black hole along certain lines of sight, is to search for water masers, as these exist only in regions with plentiful molecular gas. Since the first detection(2) of an extragalactic water maser in 1979, they have come to be associated primarily with active galaxies, and have even been used to probe the mass of the central engine(3). Here we report the detection of a water giga-maser in the radio galaxy TXFS2226-184. The strength of the emission supports a recently proposed theory of maser pumping(4) that allows for even more powerful masers, which might be detectable at cosmological distances. Water masers may accordingly provide a may to determine distances to galaxies outside the usual distance ladder, providing an independent calibration of the Hubble constant(3,5). C1 MAX PLANCK INST RADIOASTRON,D-53121 BONN,GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. LAWRENCE LIVERMORE NATL LAB,LIVERMORE,CA 94550. UNIV CALIF SANTA BARBARA,DEPT PHYS,SANTA BARBARA,CA 93106. RP KOEKEMOER, AM (reprint author), MT STROMLO & SIDING SPRING OBSERV,WESTON,ACT 2611,AUSTRALIA. OI Codella, Claudio/0000-0003-1514-3074; Koekemoer, Anton/0000-0002-6610-2048 NR 31 TC 40 Z9 42 U1 0 U2 0 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD DEC 14 PY 1995 VL 378 IS 6558 BP 697 EP 699 DI 10.1038/378697a0 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA TK379 UT WOS:A1995TK37900044 PM 7501016 ER PT J AU BABB, JF AF BABB, JF TI NUCLEAR SPIN-ROTATION INTERACTION IN THE HYDROGEN MOLECULAR ION SO PHYSICAL REVIEW LETTERS LA English DT Article ID DOUBLE-RESONANCE; HYPERFINE-STRUCTURE; SPECTROSCOPY; SPECTRUM; STATE; HD AB The nuclear spin-rotation interaction in the hyperfine structure of the hydrogen molecular ion is investigated. The interaction constants are determined and are found to differ in sign and magnitude compared to another theory, but they are in agreement with some values derived from experiment. RP BABB, JF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Babb, James/0000-0002-3883-9501 NR 41 TC 6 Z9 6 U1 0 U2 3 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 11 PY 1995 VL 75 IS 24 BP 4377 EP 4380 DI 10.1103/PhysRevLett.75.4377 PG 4 WC Physics, Multidisciplinary SC Physics GA TJ630 UT WOS:A1995TJ63000010 ER PT J AU YANG, J OHASHI, N FUKUI, Y AF YANG, J OHASHI, N FUKUI, Y TI INTERFEROMETRIC OBSERVATIONS OF THE CIRCUMSTELLAR MOLECULAR-STRUCTURE AROUND THE YOUNG STELLAR OBJECT IN L1287 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (L1287); ISM, JETS AND OUTFLOWS; ISM, MOLECULES; STARS, PRE-MAIN-SEQUENCE ID STAR FORMATION; OUTFLOWS; KINEMATICS; TAURUS; CLOUDS; SAMPLE; CORE; JET AB Results of high-resolution interferometric observations of CS (2-1) emission from the young stellar object IRAS 00338+6312 and its neighboring region in L1287 are presented. Strong and localized emission has been detected. The global CS distribution appears elongated and has a size of 0.14 pc x 0.08 pc. The CS emission shows drastically different structures at different radial velocities, including a high-velocity bipolar pattern extended over 16 km s(-1) and a flattened structure perpendicular to the outflow axis at lower velocities. The high-velocity lobes are clumpy and have been apparently accelerated. It is found that the IRAS source is located in the central part of the low-velocity CS structure, while three other optical features, including the two FU Orionis candidates RNO 1B and RNO 1C, are located gear or outside the edge of the low-velocity CS component. The possible driving source of the outflow in L1287 is discussed on the basis of the available data. C1 NOBEYAMA RADIO OBSERV, MINAMISA KU, NAGANO 38413, JAPAN. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NAGOYA UNIV, DEPT ASTROPHYS, CHIKUSA KU, NAGOYA, AICHI 46401, JAPAN. RP YANG, J (reprint author), ACAD SINICA, PURPLE MT OBSERV, NANJING 210008, PEOPLES R CHINA. NR 29 TC 17 Z9 17 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 1995 VL 455 IS 1 BP 175 EP 181 DI 10.1086/176565 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TG830 UT WOS:A1995TG83000017 ER PT J AU CASELLI, P MYERS, PC THADDEUS, P AF CASELLI, P MYERS, PC THADDEUS, P TI RADIO-ASTRONOMICAL SPECTROSCOPY OF THE HYPERFINE-STRUCTURE OF N2H+ SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, MOLECULES; MOLECULAR DATA ID ION; NITROGEN; U93.174; CLOUDS AB We present high spectral resolution and high-sensitivity observations of the J = 1 --> 0 transition of N2H+ at 93 GHz toward the quiescent low-mass cloud core L1512 in Taurus. The relative frequencies of the seven hyperfine components of this transition have been determined with precision similar to 1 kHz, and the absolute frequencies with precision similar to 7 kHz The hyperfine coupling constants have been determined with precision an order of magnitude higher than previously in the laboratory. Relative intensities of the hyperfine components of N2H+ in L1512 as well as in a sample of similar to 60 low-mass cloud cores are not consistent with a single excitation temperature model fit, indicating the presence of excitation anomalies. RP CASELLI, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 15 TC 141 Z9 141 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 1995 VL 455 IS 1 BP L77 EP L80 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TG831 UT WOS:A1995TG83100019 ER PT J AU GRINDLAY, JE COOL, AM CALLANAN, PJ BAILYN, CD COHN, HN LUGGER, PM AF GRINDLAY, JE COOL, AM CALLANAN, PJ BAILYN, CD COHN, HN LUGGER, PM TI SPECTROSCOPIC IDENTIFICATION OF PROBABLE CATACLYSMIC VARIABLES IN THE GLOBULAR-CLUSTER NGC-6397 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BINARIES, GENERAL; GALAXY, STELLAR CONTENT; GLOBULAR CLUSTERS, INDIVIDUAL (NGC 6397); NOVAE, CATACLYSMIC VARIABLES; STARS, STATISTICS; WHITE DWARFS; X-RAYS, STARS ID X-RAY SOURCES; DISCOVERY; BINARIES; 47-TUCANAE; PULSARS; MASS; CORE AB The existence of compact binaries in dense clusters is of considerable interest for testing theories of binary production and evolution, as well as the dynamical evolution and survival of the clusters in which they reside. Here, using the newly repaired Hubble Space Telescope to observe the collapsed core of the nearby globular cluster NGC 6397, we report the first spectra of stars well below the main-sequence turnoff near the center of a dense globular star cluster. The spectra confirm our WFPC1 photometry that these objects are almost certainly the long-sought population of cataclysmic variables (CVs) in globulars, and that they are the likely counterparts for the recently discovered (ROSAT) low-luminosity X-ray sources in this cluster. The spectra suggest the CVs are magnetic (DQ Her type), raising the intriguing possibility that magnetic white dwarfs are preferentially produced in globular cluster cores. C1 UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. YALE UNIV,DEPT ASTRON,NEW HAVEN,CT 06520. INDIANA UNIV,DEPT ASTRON,BLOOMINGTON,IN 47405. RP GRINDLAY, JE (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 35 TC 57 Z9 57 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 1995 VL 455 IS 1 BP L47 EP L50 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TG831 UT WOS:A1995TG83100012 ER PT J AU MATHUR, S ELVIS, M SINGH, KP AF MATHUR, S ELVIS, M SINGH, KP TI STRONG X-RAY-ABSORPTION IN A BROAD ABSORPTION-LINE QUASAR - PHL-5200 SO ASTROPHYSICAL JOURNAL LA English DT Article DE QUASARS, ABSORPTION LINES; QUASARS, INDIVIDUAL (PHL 5200); X-RAYS, GALAXIES ID EMISSION; QSOS AB We present ASCA observations of the z = 1.98 prototype broad absorption line quasar (BALQSO): PHL 5200. The source was detected in both SIS and GIS. A power-law spectrum(alpha(E) = 0.6(-0.6)(+0.9)) with large intrinsic absorption (N-H = 1.3(-1.1)(+2.3) x 10(23) cm(-2)) best describes the spectrum. Excess column density over the local Galactic value is required at the 99% confidence level. This detection suggests that, although BALQSOs are X-ray-quiet, it is strong absorption in the BAL region that makes them appear faint to low-energy X-ray experiments. The required intrinsic absorbing column density is 2-3 orders of magnitude larger than earlier estimates of column densities in BALQSOs. This implies that the BAL systems are much more highly ionized than was previously thought. C1 NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771. RP MATHUR, S (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 30 TC 50 Z9 50 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 1995 VL 455 IS 1 BP L9 EP L12 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TG831 UT WOS:A1995TG83100003 ER PT J AU WILKES, BJ SCHMIDT, GD SMITH, PS MATHUR, S MCLEOD, KK AF WILKES, BJ SCHMIDT, GD SMITH, PS MATHUR, S MCLEOD, KK TI OPTICAL-DETECTION OF THE HIDDEN NUCLEAR ENGINE IN NGC-4258 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, ACTIVE; GALAXIES, INDIVIDUAL (NGC 4258); GALAXIES, NUCLEI; POLARIZATION ID ACTIVE GALACTIC NUCLEI; NGC-4258; GALAXIES; SPECTROPOLARIMETRY; DWARF; ARMS AB The subparsec masing disk recently found to be orbiting a central mass of similar to 3.6 x 10(7) M. in the Seyfert/LINER galaxy NGC 4258 (Miyoshi and coworkers) provides the most compelling evidence to date for the existence of a massive black hole in the nucleus of a galaxy. The disk is oriented nearly edge-on, and the X-ray spectrum is heavily absorbed. Therefore, in this galaxy, the optical emission-line spectrum generally exhibited by an active galactic nucleus is perhaps best sought using polarized light: probing for light scattered off material surrounding the central source. New polarimetry of NGC 4258 has uncovered a compact polarized nucleus whose spectrum consists of a faint blue continuum similar to those of unobscured quasars (F-v proportional to v(-1.1)), plus broadened (similar to 1000 km s(-1)) emission lines. The lines are strongly linearly polarized (5%-10%) at a position angle (85 degrees +/- 2 degrees) coincident with the plane of the maser disk. This result provides substantiating evidence for a weakly active central engine in NGC 4258 and for the existence of obscuring, orbiting tori, which impart many of the perceived distinctions between various types of active galaxies. C1 UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. RP WILKES, BJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Wilkes, Belinda/0000-0003-1809-2364 NR 24 TC 45 Z9 45 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 1995 VL 455 IS 1 BP L13 EP L16 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TG831 UT WOS:A1995TG83100004 ER PT J AU BARTEL, N SORATHIA, B BIETENHOLZ, MF CARILLI, CL DIAMOND, P AF BARTEL, N SORATHIA, B BIETENHOLZ, MF CARILLI, CL DIAMOND, P TI THE NUCLEAR JET AND COUNTERJET REGION OF THE RADIO GALAXY CYGNUS-A SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article; Proceedings Paper CT Colloquium on Quasars and Active Galactic Nuclei - High Resolution Radio Imaging CY MAR 24-25, 1995 CL NATL ACD SCI, BECKMAN CTR, IRVINE, CA HO NATL ACD SCI, BECKMAN CTR ID VLBI-OBSERVATIONS; TELESCOPE AB Very-long-baseline interferometry images of the nuclear region of the radio galaxy Cygnus A reveal a pronounced ''core'' and a knotty jet and counterjet. The knots are moving away from the core at apparent speeds which are subluminal for h = 1 [h = H-0/100 km . s(-1). Mpc(-1); 1 parsec (pc) = 3.09 x 10(16)m] and about c for h = 0.5. The jet is aligned with the outer, kiloparsec-scale jet to within 2 degrees. The counterjet has a total flux density at 5 GHz of about one-fifth of that of the jet. In the context of the twin relativistic jet model for active galactic nuclei, the jet in Cygnus A is oriented at an angle to our line of sight of 35-80 degrees and 55-85 degrees, and the intrinsic velocity of the jet fluid is 0.4-0.6c and 0.6-1c for h = 1 and h = 0.5, respectively. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NATL RADIO ASTRON OBSERV,SOCORRO,NM 87801. RP BARTEL, N (reprint author), YORK UNIV,DEPT PHYS & ASTRON,N YORK,ON M3J 1P3,CANADA. NR 18 TC 6 Z9 6 U1 0 U2 0 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD DEC 5 PY 1995 VL 92 IS 25 BP 11371 EP 11373 DI 10.1073/pnas.92.25.11371 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA TJ222 UT WOS:A1995TJ22200011 PM 11607600 ER PT J AU MORAN, J GREENHILL, L HERRNSTEIN, J DIAMOND, P MIYOSHI, M NAKAI, N INOUE, M AF MORAN, J GREENHILL, L HERRNSTEIN, J DIAMOND, P MIYOSHI, M NAKAI, N INOUE, M TI PROBING ACTIVE GALACTIC NUCLEI WITH H2O MEGAMASERS SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article; Proceedings Paper CT Colloquium on Quasars and Active Galactic Nuclei - High Resolution Radio Imaging CY MAR 24-25, 1995 CL NATL ACD SCI, BECKMAN CTR, IRVINE, CA HO NATL ACD SCI, BECKMAN CTR ID WATER-VAPOR MASER; EMISSION; GALAXY; NGC-3079 AB We describe the characteristics of the rapidly rotating molecular disk in the nucleus of the mildly active galaxy NGC4258. The morphology and kinematics of the disk are delineated by the point-like water-vapor emission sources at 1.35-cm wavelength, High angular resolution [200 mu as where as is arcsec, corresponding to 0.006 parsec (pc) at 6.4 million pc] and high spectral resolution (0.2 km . s(-1) or nu/Delta nu = 1.4 x 10(6)) with the Very-Long-Baseline Array allow precise definition of the disk. The disk is very thin, but slightly warped, and is viewed nearly edge-on. The masers show that the disk is in nearly perfect Keplerian rotation within the observable range of radii of 0.13-0.26 pc. The approximately random deviations from the Keplerian rotation curve among the high-velocity masers are approximate to 3.5 km . s(-1) (rms), These deviations may be due to the masers lying off the midline by about +/-4 degrees or variations in the inclination of the disk by +/-4 degrees. Lack of systematic deviations indicates that the disk has a mass of <4 x 10(6) solar mass (Mo), The gravitational binding mass is 3.5 x 10(7) M., which must lie within the inner radius of the disk and requires that the mass density be >4 x 10(9) M.. pc(-3). If the central mass were in the form of a star cluster with a density distribution such as a Plummer model, then the central mass density would be 4 x 10(12) M.. pc(-3). The lifetime of such a cluster would be short with respect to the age of the galaxy [Maoz, E. (1995) Astrophys. J. Lett. 147, L91-L94]. Therefore, the central mass may be a black hole. The disk as traced by the systemic velocity features is unresolved in the vertical direction, indicating that its scale height is <0.0003 pc (hence the ratio of thickness to radius, H/R, is <0.0025). For a disk in hydrostatic equilibrium the quadrature sum of the sound speed and Alfven velocity is <2.5 km . s(-1), so that the temperature of the disk must be <1000 K and the toroidal magnetic field component must be <250 mG. If the molecular mass density in the disk is 10(10) cm(-3), then the disk mass is approximate to 10(4) M., and the disk is marginally stable as defined by the Toomre stability parameter Q (Q = 6 at the inner edge and 1 at the outer edge), The inward drift velocity is predicted to be <0.007 km . s(-1), for a viscosity parameter of 0.1, and the accretion rate is <7 x 10(-5) M.. yr(-1). At this value the accretion would be sufficient to power the nuclear x-ray source of 4 x 10(40) ergs(-I) (1 erg = 0.1 mu J). The volume of individual maser components may be as large as 10(46) cm(3), based on the velocity gradients, which is sufficient to supply the observed luminosity, The pump power undoubtedly comes from the nucleus, perhaps in the form of x-rays, The warp may allow the pump radiation to penetrate the disk obliquely [Neufeld, D. A. & Maloney, P. R. (1995) Astrophys. J. Lett. 447, L17-L19], A total of 15 H2O megamasers have been identified out of >250 galaxies searched, Galaxy NGC4258 may be the only case where conditions are optimal to reveal a well-defined nuclear disk Future measurement of proper motions and accelerations for NGC4258 will field an accurate distance and a more precise definition of the dynamics of the disk. C1 NATL RADIO ASTRON OBSERV,SOCORRO,NM 87801. NATL ASTRON OBSERV,MIZUSAWA ASTROGEODYNAM OBSERV,MIZUSAWA,IWATE 023,JAPAN. NATL ASTRON OBSERV,NOBEYAMA RADIO OBSERV,MINAMISA KU,NAGANO 38413,JAPAN. RP MORAN, J (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MAIL STOP 42,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 58 TC 44 Z9 44 U1 0 U2 1 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD DEC 5 PY 1995 VL 92 IS 25 BP 11427 EP 11433 DI 10.1073/pnas.92.25.11427 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA TJ222 UT WOS:A1995TJ22200023 PM 11607612 ER PT J AU SHARRER, GT AF SHARRER, GT TI THE GREAT GLANDERS EPIZOOTIC, 1861-1866 - A CIVIL-WAR LEGACY SO AGRICULTURAL HISTORY LA English DT Article RP SHARRER, GT (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 40 TC 17 Z9 17 U1 0 U2 1 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0002-1482 J9 AGR HIST JI Agric. Hist. PD WIN PY 1995 VL 69 IS 1 BP 79 EP 101 PG 23 WC Agriculture, Multidisciplinary; History; History & Philosophy Of Science SC Agriculture; History; History & Philosophy of Science GA QT126 UT WOS:A1995QT12600004 PM 11639801 ER PT J AU Hedlin, E AF Hedlin, E TI Expanding the foundation SO AMERICAN ARCHIVIST LA English DT Article AB The archival profession today is doubly challenged. Not only must we deal with dramatic increases in the volume and complexity of paper records, we must also develop programs and strategies for electronic records. The latter, in particular, will require years of research, analysis, testing, and development. However, the resources needed to support years of intensive work in multiple archival settings are not present. The author contends that the profession's most pressing need is the development of greater infrastructure to support research efforts, and she offers examples of the types of organizations that we need to foster. RP Hedlin, E (reprint author), OFF SMITHSONIAN INST ARCH,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU SOC AMER ARCHIVISTS PI CHICAGO PA SUITE 504, 600 S FEDERAL, CHICAGO, IL 60605 SN 0360-9081 J9 AM ARCHIVIST JI Am. Arch. PD WIN PY 1995 VL 58 IS 1 BP 10 EP 15 PG 6 WC History; Information Science & Library Science SC History; Information Science & Library Science GA UB744 UT WOS:A1995UB74400006 ER PT J AU Stine, JK AF Stine, JK TI Computer in the United States: From laboratory to market, 1930 to 1960 - Cortada,JW SO AMERICAN HISTORICAL REVIEW LA English DT Book Review RP Stine, JK (reprint author), SMITHSONIAN INST,AMER MUSEUM NAT HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER HISTORICAL REVIEW PI WASHINGTON PA 400 A ST SE, WASHINGTON, DC 20003 SN 0002-8762 J9 AM HIST REV JI Am. Hist. Rev. PD DEC PY 1995 VL 100 IS 5 BP 1726 EP 1726 DI 10.2307/2170153 PG 1 WC History SC History GA TM223 UT WOS:A1995TM22300294 ER PT J AU WILLIS, D AF WILLIS, D TI SLIGH,CLARISSA SO APERTURE LA English DT Article RP WILLIS, D (reprint author), SMITHSONIAN INST,NATL AFRICAN AMER MUSEUM PROJECT,WASHINGTON,DC 20560, USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU APERTURE PI NEW YORK PA 20 EAST 23RD ST, NEW YORK, NY 10010 SN 0003-6420 J9 APERTURE JI Aperture PD WIN PY 1995 IS 138 BP 4 EP 11 PG 8 WC Art SC Art GA QX033 UT WOS:A1995QX03300002 ER PT J AU JOENSEN, KD VOUTOV, P SZENTGYORGYI, A ROLL, J GORENSTEIN, P HOGHOJ, P CHRISTENSEN, FE AF JOENSEN, KD VOUTOV, P SZENTGYORGYI, A ROLL, J GORENSTEIN, P HOGHOJ, P CHRISTENSEN, FE TI DESIGN OF GRAZING-INCIDENCE MULTILAYER SUPERMIRRORS FOR HARD-X-RAY REFLECTORS SO APPLIED OPTICS LA English DT Article DE MULTILAYER; SUPERMIRROR; OPTIMIZATION; REFLECTIVITY; HARD-X-RAY OPTICS; X-RAY TELESCOPES; SYNCHROTRON OPTICS; PLASMA SPECTROSCOPY OPTICS ID SUPER-MIRRORS; OPTICS AB Extremely broadband grazing-incidence multilayers for hard-x-ray reflection can be obtained by a gradual change of the layer thicknesses down through the structure. Existing approaches for designing similar neutron optics, called supermirrors, are shown to provide respectable performance when applied to x-ray multilayers. However, none of these approaches consider the effects of imperfect layer interfaces and absorption in the overlying layers. Adaptations of neutron designs that take these effects into account are presented, and a thorough analysis of two specific applications (a single hard-x-ray reflector and a hard-x-ray telescope) shows that an improved performance can be obtained. A multilayer whose bilayer thicknesses are given by a power law expression is found to provide the best solution; however, it is only slightly better than some of the adapted neutron designs. (C) 1995 Optical Society of America C1 INST MAX VON LAUE PAUL LANGEVIN,F-38042 GRENOBLE,FRANCE. DANISH SPACE RES INST,DK-2800 LYNGBY,DENMARK. RP JOENSEN, KD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 34 TC 88 Z9 89 U1 0 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 SN 0003-6935 J9 APPL OPTICS JI Appl. Optics PD DEC 1 PY 1995 VL 34 IS 34 BP 7935 EP 7944 PG 10 WC Optics SC Optics GA TH295 UT WOS:A1995TH29500018 PM 21068887 ER PT J AU Loring, S AF Loring, S TI Untitled SO ARCTIC LA English DT Letter RP Loring, S (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,ARCTIC STUDIES CTR,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARCTIC INST N AMER PI CALGARY PA UNIV OF CALGARY 2500 UNIVERSITY DRIVE NW 11TH FLOOR LIBRARY TOWER, CALGARY AB T2N 1N4, CANADA SN 0004-0843 J9 ARCTIC JI Arctic PD DEC PY 1995 VL 48 IS 4 BP 400 EP 400 PG 1 WC Environmental Sciences; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA TP285 UT WOS:A1995TP28500013 ER PT J AU WEATHERFORD, E AF WEATHERFORD, E TI TO END AND BEGIN AGAIN + NATIVE-AMERICAN INDIAN VIDEO ART - THE WORK OF MASAYESVA,VICTOR SO ART JOURNAL LA English DT Article RP WEATHERFORD, E (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER INDIAN,FILM VIDEO CTR,WASHINGTON,DC 20560, USA. NR 7 TC 2 Z9 2 U1 0 U2 2 PU COLLEGE ART ASSOC PI NEW YORK PA 275 SEVENTH AVE, NEW YORK, NY 10001 SN 0004-3249 J9 ART J JI Art J. PD WIN PY 1995 VL 54 IS 4 BP 48 EP 52 DI 10.2307/777694 PG 5 WC Art SC Art GA TM507 UT WOS:A1995TM50700007 ER PT J AU Guirado, JC Marcaide, JM Alberdi, A Elosegui, P Ratner, MI Shapiro, II Kilger, R Mantovani, F Venturi, T Rius, A Ros, E Trigilio, C Whitney, AR AF Guirado, JC Marcaide, JM Alberdi, A Elosegui, P Ratner, MI Shapiro, II Kilger, R Mantovani, F Venturi, T Rius, A Ros, E Trigilio, C Whitney, AR TI Proper motion of components in 4C 39.25 SO ASTRONOMICAL JOURNAL LA English DT Article ID COMPACT RADIO-SOURCES; VLBI OBSERVATIONS; INTERFEROMETRY; 4C-39.25; GEODESY; 4C39.25; SYSTEM AB From a series of simultaneous 8.4 and 2.3 GHz VLBI observations of the quasar 4C 39.25 phase referenced to the radio source 0920 + 390, carried out in 1990-1992, we have measured the proper motion of component b in 4C 39.25: mu(alpha) = 90 +/- 43 mu as/yr, mu(delta) = 7 +/- 68 mu as/yr, where the quoted uncertainties account for the contribution of the statistical standard deviation and the errors assumed for the parameters related to the geometry of the interferometric array, the atmosphere, and the source structure. This proper motion is consistent with earlier interpretations of VLBI hybrid mapping results, which showed an internal motion of this component with respect to other structural components, Our differential astrometry analyses show component b to be the one in motion, Our results thus further constrain models of this quasar. (C) 1995 American Astronomical Society. C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. UNIV VALENCIA,DEPT ASTRON,E-46100 BURJASSOT,SPAIN. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. INTA,ASTRON ESPACIAL & FIS FUNDAMENTAL LAB,E-28080 MADRID,SPAIN. SATELLITENBEOBACHTUNGSSTN WETTZELL,D-93444 KOETZTING,GERMANY. CNR,IST RADIOASTRON,I-40129 BOLOGNA,ITALY. CSIC,CTR ESTUDIOS AVANZADOS,E-17300 BARCELONA,SPAIN. CNR,IST RADIOASTRON,I-96017 NOTO,ITALY. NEROC,HAYSTACK OBSERV,WESTFORD,MA 01886. RP Guirado, JC (reprint author), CSIC,INST ASTROFIS ANDALUCIA,E-18080 GRANADA,SPAIN. RI Antonio, Rius/A-4873-2012; OI Antonio, Rius/0000-0002-5947-2649; Venturi, Tiziana/0000-0002-8476-6307 NR 44 TC 27 Z9 28 U1 0 U2 2 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 1995 VL 110 IS 6 BP 2586 EP 2596 DI 10.1086/117715 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TL326 UT WOS:A1995TL32600007 ER PT J AU Huterer, D Sasselov, DD Schechter, PL AF Huterer, D Sasselov, DD Schechter, PL TI Distances to nearby galaxies: Combining fragmentary data using four different methods SO ASTRONOMICAL JOURNAL LA English DT Article ID RR LYRAE STARS; GLOBULAR-CLUSTER SYSTEM; BAADE-WESSELINK METHOD; LARGE MAGELLANIC CLOUD; PROPER MOTIONS; ABSOLUTE MAGNITUDES; GALACTIC-CENTER; BV PHOTOMETRY; SCALE; VARIABLES AB The primary distance indicators are established in our Galaxy and the Local Group. There are at least four different methods which give good distances: methods using proper motions, RR Lyraes, Cepheid variables, and Type II supernovae. However, the data on independent distances are very fragmentary, due partly to nature and partly to technological limits. As a result the data are rarely put together in a consistent way; instead, the discussion of distance scales is often focused on one or two methods or on individual objects. Hence the question: what is the current situation with our overall knowledge of distances to the nearby galaxies? We try to answer this question by combining the fragmentary data from all four methods for fifteen objects: the galactic center, the globular clusters M2, M3, M4, M13, M22, M92, and 47 Tuc, the galaxies IC 1613, M31, M33, M81, M100, and M101, and the Large Magellanic Cloud. We pay special attention to covariances among the different distance estimates. This most complete combination to date shows that all four methods are consistent within their random and systematic uncertainties. (C) 1995 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Huterer, D (reprint author), MIT,DEPT PHYS,CAMBRIDGE,MA 02139, USA. NR 67 TC 35 Z9 35 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 1995 VL 110 IS 6 BP 2705 EP 2714 DI 10.1086/117724 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TL326 UT WOS:A1995TL32600016 ER PT J AU Blanton, EL Schmidt, BP Kirshner, RP Ford, CH Chromey, FR Herbst, W AF Blanton, EL Schmidt, BP Kirshner, RP Ford, CH Chromey, FR Herbst, W TI Observations of the type II-P SN 1991G in NGC 4088 SO ASTRONOMICAL JOURNAL LA English DT Article ID EXTRAGALACTIC DISTANCE SCALE; BOLOMETRIC LIGHT-CURVE; LARGE MAGELLANIC CLOUD; NA-I; SUPERNOVAE; SN-1987A; MODEL; PHOTOMETRY; TELESCOPE AB We present VRI photometry and optical spectra of SN 1991G in NGC 4088. The strong Ha P-Cygni feature observed in the early spectrum coupled with the shape of the light curve demonstrate that SN 1991G is of type IT-P (plateau), SN 1991G's plateau, which lasts approximate to 120 days, is longer than that of other well-observed SNe, We combine our photometry and spectroscopy to estimate the time of the explosion to be JD 2448280+/-3 (1991 January 23 UT), 26 days before our first photometric observation. The expansion velocity of the material at the photosphere, derived from absorption lines in our spectra, of 5590+/-340 km/s at 22 days after the explosion is slower than that: observed for all the SNe II studied by Schmidt rt al. [ApJ, 395, 366 (1992)] other than SN 1987A. We find that the bolometric luminosity of SN 1991G is lower than that of typical SNe II-P during both its plateau phase and exponential tail and find that SN 1991G ejected less Ni-56 than most other type II-P SNe. Using the analytical models of SNe II-P by Popov [ApJ, 414, 712 (1993)], we compare the explosion properties of SN 1991G to SN 1969L and SN 1992am, This comparison suggests that the explosion energy of SN 1991G was likely smaller than that of the others, and that there may be a correlation of explosion energy with the mass of ejected Ni-56. (C) 1995 American Astronomical Society. C1 COLUMBIA UNIV,DEPT ASTRON,NEW YORK,NY 10027. MT STROMLO & SIDING SPRING OBSERV,WESTON PK,ACT 2611,AUSTRALIA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. SETI INST,MT VIEW,CA 94043. VASSAR COLL,DEPT PHYS & ASTRON,POUGHKEEPSIE,NY 12601. WESLEYAN UNIV,DEPT ASTRON,MIDDLETOWN,CT 06459. ASSOC UNIV RES ASTRON INC,NATL OPT OBSERV,KITT PEAK NATL OBSERV,TUCSON,AZ. RI Blanton, Elizabeth/H-4501-2014 NR 39 TC 18 Z9 18 U1 1 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 1995 VL 110 IS 6 BP 2868 EP 2875 DI 10.1086/117735 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TL326 UT WOS:A1995TL32600027 ER PT J AU MCLEOD, BA RIEKE, MJ AF MCLEOD, BA RIEKE, MJ TI THE EFFECTS OF STARBURSTS AND LOW SURFACE BRIGHTNESS GALAXIES ON FAINT GALAXY MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, PHOTOMETRY; GALAXIES, STARBURST; GALAXIES, STELLAR CONTENT ID NUMBER MAGNITUDE COUNTS; INITIAL MASS FUNCTION; REDSHIFT SURVEY; LUMINOSITY FUNCTION; FIELD GALAXIES; SPECTROSCOPIC SURVEY; EVOLUTION; CATALOG; SAMPLE; SCALES AB We present models predicting the magnitude, redshift, and color distributions of field galaxies. We explore whether a fading starburst scenario can account for the observations of faint blue galaxies. We marginally rule out a starburst scenario with a local initial mass function (IMF) because the models predict too many nearby faint galaxies that are not observed. A burst model with a truncated IMF reproduces the counts and redshift distributions well but produces too blue a population. We show that surface brightness selection has a significant effect on the distributions. In particular, adding a population of low-surface brightness galaxies, known to exist locally, can explain the counts for B-J < 23. They do not, however, account for the steepness of the counts at fainter magnitudes. Finally, we show that the colors of galaxies in a K-band-selected sample are too blue to be consistent with a constant star formation rate, passive-evolution model. C1 UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. RP MCLEOD, BA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MS-20,CAMBRIDGE,MA 02138, USA. NR 69 TC 17 Z9 17 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 1995 VL 454 IS 2 BP 611 EP 622 DI 10.1086/176515 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TF088 UT WOS:A1995TF08800009 ER PT J AU AVNI, Y WORRALL, DM MORGAN, WA AF AVNI, Y WORRALL, DM MORGAN, WA TI THE UNDERLYING DISTRIBUTION OF THE OPTICAL TO X-RAY SPECTRAL INDEX FOR QUASARS IN THE PRESENCE OF DETECTION THRESHOLDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE METHODS, STATISTICAL; QUASARS, GENERAL; X-RAYS, GALAXIES ID ASTRONOMICAL DATA; UPPER LIMITS; OBJECTS AB Statistical methods, applied in a standard way to find underlying distributions from data subject to large non-random threshold effects, often underestimate the uncertainties. We show through simulations that increasing the permissible range of the underlying distribution allows conservative estimates of the uncertainties to be derived. Our simulations are roughly matched to measurements of the optical to X-ray spectral index of optically selected quasars in the presence of thresholds similar to those of flux-limited surveys. For each configuration of thresholds, and several derived parameters of interest, we find the extent that it is necessary to increase the permissible range of the underlying distribution so that derived uncertainties are not underestimated. We apply these results to perform nonparametric fits to the most recent compilation of Einstein Observatory X-ray measurements of optically selected quasars. We verify that the mean optical to X-ray spectral index, alpha(ox), generally increases with 2500 Angstrom spectral luminosity, l(o), although the dependence is weaker, or possibly absent, for l(o) less than or similar to 10(31) ergs s(-1) Hz(-1). We derive the intrinsic distribution of alpha(ox) in bands of l(o), together with uncertainties. C1 DICKINSON COLL,DEPT PHYS & ASTRON,CARLISLE,PA 17013. RP AVNI, Y (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 18 TC 24 Z9 24 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 1995 VL 454 IS 2 BP 673 EP 682 DI 10.1086/176520 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TF088 UT WOS:A1995TF08800014 ER PT J AU FULLER, GA LADD, EF PADMAN, R MYERS, PC ADAMS, FC AF FULLER, GA LADD, EF PADMAN, R MYERS, PC ADAMS, FC TI THE CIRCUMSTELLAR MOLECULAR CORE AROUND L1551-IRS-5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; ISM, JETS AND OUTFLOWS; STARS, INDIVIDUAL (L1551 IRS 5); STAR, PRE-MAIN-SEQUENCE ID STAR-FORMING REGIONS; EMBEDDED YOUNG STARS; DENSE CORES; OPTICAL OBSERVATIONS; DARK CLOUDS; IMAGES; OBJECTS; MODELS; RADIO; MASS AB We present maps of (CO)-O-18 and (CO)-O-17 J = 2 --> 1 emission toward the embedded young star L1551 IRS 5. The (CO)-O-17 emission traces a compact region similar to 1900 AU in radius which is centered on the star which contains similar to 0.1 M. of material. The integrated (CO)-O-17 emission has a crosslike structure aligned in the cardinal directions which is very similar to the structure seen in the submillimeter continuum emission from this source. A spatially more extended component of material which contains an additional 0.1 M. of material within 20 '' of IRS 5, also contributes to the (CO)-O-17 emission. The cross gas is warmer and has a larger velocity dispersion than the more extended gas. The motions of the extended material imply a virial mass of 1-3 M., which is dominated by the mass of the central star plus disk. The (CO)-O-18 lines have considerable line wing emission and part of the cross is evident in this wing emission. Comparison with existing maps of the outflow near IRS 5 suggests that the cross material is part of the heated wall of the cavity evacuated by the outflow. The presence of such structures near embedded stars complicates the search for accreting material. However, the properties of the extended (CO)-O-17 emission constrain the mass accretion rate in L1551 IRS 5 to be less than 1.4 x 10(-5) M. yr(-1). Comparison with the observed mass outflow rate from IRS 5 at a similar size scale suggests that there is currently little or no net accretion of material from the larger scale dense core into the central 2000 AU radius region about IRS 5. C1 ASSOC UNIV INC,NATL RADIO ASTRON OBSERV,TUCSON,AZ 85721. UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822. UNIV CAMBRIDGE,CAVENDISH LAB,MULLARD RADIO ASTRON OBSERV,CAMBRIDGE CB3 0HE,ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV MICHIGAN,DEPT PHYS,ANN ARBOR,MI 48109. NR 58 TC 19 Z9 19 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 1995 VL 454 IS 2 BP 862 EP 871 DI 10.1086/176539 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TF088 UT WOS:A1995TF08800033 ER PT J AU STAUFFER, JR HARTMANN, LW NAVASCUES, DBY AF STAUFFER, JR HARTMANN, LW NAVASCUES, DBY TI AN AGE ESTIMATE FOR THE BETA-PICTORIS ANALOG HR-4796A SO ASTROPHYSICAL JOURNAL LA English DT Article DE BINARIES, VISUAL; CIRCUMSTELLAR MATTER; STARS, EVOLUTION; STARS, INDIVIDUAL (HR 4796) ID CIRCUMSTELLAR DISK; DUST DEBRIS; M-DWARFS; STARS; TEMPERATURE; EVOLUTION; HR-4796 AB We have obtained a high-resolution, moderate signal-to-noise spectrum for the M dwarf companion to HR 4796A, an A0 star with a beta Pictoris-type IR excess. The spectrum of the M star shows an extraordinarily strong lithium 6708 Angstrom absorption line with an equivalent width of similar to 550 m Angstrom. Age estimates derived from the lithium strength and from pre-main-sequence isochrone fitting indicate an age of about 8 +/- 2 Myr for HR 4796B. Assuming this age is also applicable to HR 4796A, we conclude that HR 4796A is a relatively normal A star seen at an unusual time (i.e., when it is very young) rather than an A star of ''average'' age which has somehow managed to retain or acquire a dense, circumstellar disk, in rough agreement with conclusions reached previously by Jura et al. C1 SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. UNIV COMPLUTENSE MADRID,FAC FIS,DEPT ASTROFIS,E-28040 MADRID,SPAIN. RI Barrado Navascues, David/C-1439-2017 OI Barrado Navascues, David/0000-0002-5971-9242 NR 36 TC 113 Z9 113 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 1995 VL 454 IS 2 BP 910 EP 916 DI 10.1086/176544 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TF088 UT WOS:A1995TF08800038 ER PT J AU MCLEOD, KK RIEKE, GH AF MCLEOD, KK RIEKE, GH TI LUMINOUS QUASARS IN LUMINOUS EARLY-TYPE HOST GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, PHOTOMETRY; INFRARED, GALAXIES; QUASARS, GENERAL ID ACTIVE GALACTIC NUCLEI; RADIO-LOUD; UNDERLYING GALAXIES; HOMOGENEOUS SAMPLE; QSOS; SPECTROSCOPY; DIFFERENCE AB Some recent observations of nearby quasars with Hubble Space Telescope (HST) have apparently failed to detect host galaxies. We review the HST observations as well as near-infrared ground-based observations of the same objects. We find that the quasar hosts can be detected in the HST data if they are smoothed sufficiently to reveal low surface brightness. The smooth hosts are very difficult to detect with HST but are more easily visible in the deeper, ground-based IR images. The V - H colors obtained by combining the HST and IR data are compatible with normal galaxy colors at the redshifts of the quasars. This behavior can be explained if the hosts are massive early-type galaxies. All together, HST images have been reported for 15 luminous quasars, similar to 13 of which have smooth early-type hosts. This kind of galaxy therefore appears to be the most common host for a luminous quasar. C1 UNIV ARIZONA, STEWARD OBSERV, TUCSON, AZ 85721 USA. RP SMITHSONIAN ASTROPHYS OBSERV, 60 GARDEN ST, MS12, CAMBRIDGE, MA 02138 USA. NR 33 TC 64 Z9 64 U1 0 U2 0 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 1 PY 1995 VL 454 IS 2 BP L77 EP + PN 2 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TF089 UT WOS:A1995TF08900002 ER PT J AU Mitrovica, JX Davis, JL AF Mitrovica, JX Davis, JL TI The influence of a finite glaciation phase on predictions of post-glacial isostatic adjustment SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article ID DEEP MANTLE VISCOSITY; GLOBAL SEA-LEVEL; PLEISTOCENE DEGLACIATION; GRAVITATIONAL-FIELD; EARTHS ROTATION; ZONAL HARMONICS; RHEOLOGY; FENNOSCANDIA; INFERENCE; HISTORY AB We predict relative sea level (RSL) variations, present day three-dimensional (3D) crustal deformation rates and baseline velocities, and a set of anomalies in the gravitational field of the planet, using a suite of models for the space-time geometry of the Pleistocene ice sheets. These models are distinguished on the basis of the details of the glaciation phase, and they include the cases of: an infinite glaciation phase (i.e., an assumption of isostatic equilibrium at the time of the last glacial maximum - LGM), a steady uniform glaciation, and a glaciation in which the bulk of the accumulation is limited to the final stages of the growth phase. Comparison of the observational records of postglacial RSL change with predictions based on the assumption of isostatic equilibrium at LGM have commonly been used to infer both the space-time geometry of the final deglaciation event and the mantle viscosity. We conclude that both these applications may be influenced significantly by the incorporation of a finite glacial cycle. As an example, RSL predictions, which assume isostatic equilibrium at LGM, and those which incorporate a relatively rapid glaciation phase, can differ by a factor of 2 or more at some sites within previously glaciated regions when an Earth model characterized by a lower mantle viscosity of 10(22) Pa s is adopted. We have also found that differences in the adopted model for the glaciation event are capable of explaining entirely the discrepancies (similar to 0.2 mm/yr) between previously published predictions of present day tangential velocities in North America. These discrepancies are characterized by a dominant long-wavelength signal and, hence, they do not necessarily influence (strongly) predictions of baseline velocities. Variations in the glaciation model can also have an important effect on predictions of peak gravity anomalies over previously glaciated regions, and secular variations in the zonal harmonics of the Earth's geoid. In both cases the effect may be sufficient to alter significantly the signal from other geophysical processes which may need to be invoked to reconcile the observational constraints. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP Mitrovica, JX (reprint author), UNIV TORONTO,DEPT PHYS,60 ST GEORGE ST,TORONTO,ON M5S 1A7,CANADA. RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 46 TC 11 Z9 11 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD DEC PY 1995 VL 136 IS 3-4 BP 343 EP 361 DI 10.1016/0012-821X(95)00160-E PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA TR076 UT WOS:A1995TR07600019 ER PT J AU STOUFFER, PC BIERREGAARD, RO AF STOUFFER, PC BIERREGAARD, RO TI USE OF AMAZONIAN FOREST FRAGMENTS BY UNDERSTORY INSECTIVOROUS BIRDS SO ECOLOGY LA English DT Review DE AMAZONIA; BIRD COMMUNITIES; BRAZIL; CECROPIA; COLONIZATION; DENDROCOLAPTIDAE; FORMICARIIDAE; FRAGMENTATION; FURNARIIDAE; INSECTIVORY; VISMIA ID BARRO-COLORADO ISLAND; TROPICAL DEFORESTATION; HABITAT FRAGMENTATION; SPECIES RICHNESS; NEST PREDATION; RAIN-FOREST; EXTINCTION; ABUNDANCE; DYNAMICS; PANAMA AB We sampled understory insectivorous birds in Amazonian forest fragments from before isolation through 9 yr after isolation. We accumulated 3658 mist net captures of 84 insectivorous species in five 1-ha fragments and four 10-ha fragments. Abundance and species richness declined dramatically after isolation, even though fragments were separated from continuous forest by only 70-650 m. Three species of obligate army ant followers disappeared within the first 2 yr after isolation. Mixed-species flocks containing 13 commonly netted species disintegrated within 2-3 yr after isolation, although three species that dropped out of flocks persisted in fragments. Among insectivores not associated with flocks or army ants, only two species of edge specialists were unaffected by fragmentation. Overall, loss of forest insectivores was not compensated for by an increase in nonforest or previously uncommon species. Secondary vegetation surrounding fragments strongly affected use of fragments after isolation. Fragments surrounded by Vismia, the dominant regrowth where felled forest was burned and temporarily used as cattle pasture, remained depauperate. In contrast, many species returned to fragments by moving through regenerating forest dominated by Cecropia, which occurred in areas where the felled forest was not burned. Both 1- and IO-ha fragments surrounded by Cecropia were used by ant followers by 5 yr after isolation. Mixed-species flocks reassembled in 10-ha fragments surrounded by Cecropia by 7-9 yr after isolation, and augmented their group territories by foraging in secondary forest outside fragments. Solitary species were more variable in their responses, although several species returned to 10-ha fragments surrounded by Cecropia. Terrestrial insectivores, such as Sclerurus leafscrapers and various antbirds, did not return to any fragments, and appear to be the group most vulnerable to fragmentation. Ordination of the insectivore community showed that I-ha fragments diverged from their pre-isolation communities more than did 10-ha fragments. Communities in 10-ha fragments surrounded by Cecropia were more closely associated with pre-isolation communities than those in fragments surrounded by Vismia. Over time, communities in 10-ha fragments surrounded by Cecropia became more like pre-isolation communities, although communities in other fragments generally continued to diverge. C1 SMITHSONIAN INST,BIODIVERS PROGRAMS,WASHINGTON,DC 20560. NR 98 TC 343 Z9 373 U1 9 U2 79 PU ECOLOGICAL SOC AMER PI TEMPE PA ARIZONA STATE UNIV CENTER ENVIRONMENTAL STUDIES, TEMPE, AZ 85287 SN 0012-9658 J9 ECOLOGY JI Ecology PD DEC PY 1995 VL 76 IS 8 BP 2429 EP 2445 DI 10.2307/2265818 PG 17 WC Ecology SC Environmental Sciences & Ecology GA TJ312 UT WOS:A1995TJ31200007 ER PT J AU SAKAI, AK WAGNER, WL FERGUSON, DM HERBST, DR AF SAKAI, AK WAGNER, WL FERGUSON, DM HERBST, DR TI ORIGINS OF DIOECY IN THE HAWAIIAN FLORA SO ECOLOGY LA English DT Article DE AUTOCHTHONOUS EVOLUTION; BREEDING SYSTEMS; COLONISTS; DIMORPHISM; DIOECY; ENDEMISM; EVOLUTION OF PLANT BREEDING SYSTEMS; GYNODIOECY; HAWAIIAN ISLANDS; ISLANDS; LONG-DISTANCE DISPERSAL OF PLANTS; SEXUAL DIMORPHISM OF FLOWERS ID NEW-ZEALAND; SEED PLANTS; EVOLUTION; COMPOSITAE; MADIINAE; ISLANDS; BIOLOGY AB Because of its presumed high levels of dioecy (separate male and female plants), study of the native Hawaiian angiosperm flora has been important in development of many hypotheses about conditions favoring the evolution of dioecy. The importance of ecological correlates with dioecy has proven difficult to assess, however, because of lack of data on the origins of dioecy in the Hawaiian Islands. Clearly, these correlations are of greater interest in taxa where dioecy evolved in the Hawaiian Islands (autochthonous evolution of dioecy) than in taxa that are the result of dioecious colonists with subsequent speciation in the Hawaiian Islands. Because the Hawaiian flora is small and extremely isolated, colonists can be identified and their breeding systems hypothesized, thus allowing inferences on the origins of dioecy. Using current taxonomic information, the incidence of dioecy in native Hawaiian angiosperm species is 14.7%, lower than previous estimates, but still the highest of any known flora worldwide. Ten percent of the colonists were sexually dimorphic (dioecious, gynodioecious, polygamodioecious, and subdioecious), and over half (55.2%) of current dimorphic species are in lineages arising from dimorphic colonists, showing that dimorphism is high in part because colonists were dimorphic. Autochthonous evolution of dimorphism occurred in at least 12 lineages (e.g., hermaphroditic colonists of Bidens (Asteraceae), the Hawaiian Alsinoideae (Caryophyllaceae), and Hedyotis (Rubiaceae) led to species-rich lineages that include many dimorphic species). One-third (31.8%) of current dimorphic species are in lineages arising from monomorphic colonists. Dioecy in the Hawaiian Islands is a result of both dimorphic colonists as well as evolution of dioecy in Hawaiian lineages from hermaphroditic colonists. The high incidence of dimorphism is not because dimorphic colonists evolved more species per colonist than monomorphic colonists. Detailed studies of individual lineages are critical to elucidate causal factors in the evolution of dioecy. C1 USA,CORPS ENGINEERS,FT SHAFTER,HI 96858. SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,WASHINGTON,DC 20560. RP SAKAI, AK (reprint author), UNIV CALIF IRVINE,DEPT ECOL & EVOLUTIONARY BIOL,IRVINE,CA 92717, USA. NR 48 TC 100 Z9 110 U1 3 U2 28 PU ECOLOGICAL SOC AMER PI TEMPE PA ARIZONA STATE UNIV CENTER ENVIRONMENTAL STUDIES, TEMPE, AZ 85287 SN 0012-9658 J9 ECOLOGY JI Ecology PD DEC PY 1995 VL 76 IS 8 BP 2517 EP 2529 DI 10.2307/2265825 PG 13 WC Ecology SC Environmental Sciences & Ecology GA TJ312 UT WOS:A1995TJ31200014 ER PT J AU SAKAI, AK WAGNER, WL FERGUSON, DM HERBST, DR AF SAKAI, AK WAGNER, WL FERGUSON, DM HERBST, DR TI BIOGEOGRAPHICAL AND ECOLOGICAL CORRELATES OF DIOECY IN THE HAWAIIAN FLORA SO ECOLOGY LA English DT Article DE ANGIOSPERMS; BIOGEOGRAPHY OF PLANT BREEDING SYSTEMS; BREEDING SYSTEMS; DIOECY; ECOLOGICAL CORRELATES OF DIOECY; ENDEMISM; EVOLUTION OF PLANT BREEDING SYSTEMS; GYNODIOECY; HAWAIIAN ISLANDS; ISLAND BIOGEOGRAPHY; ISLANDS; LONG-DISTANCE DISPERSAL OF PLANTS; SEXUAL DIMORPHISM OF FLOWERS ID SEXUAL SELECTION; SEED PLANTS; BREEDING SYSTEMS; FLOWERING PLANTS; NEW-ZEALAND; EVOLUTION; POLLINATION; ISLANDS; FOREST; CARYOPHYLLACEAE AB The angiosperm flora of the Hawaiian Islands, with its high incidence of dioecy, has been central in development of hypotheses about the evolution of dioecy. Based on a recent taxonomic treatment of the Hawaiian angiosperm flora, we analyzed biogeographic patterns of dioecy as well as the association of dioecy with ecological traits potentially important in the evolution of dioecy for native current species and genera. We also analyzed patterns for presumed colonists of the flora to control better for phylogenetic patterns in these traits. Dioecy is associated with woodiness, especially trees; however, this pattern does not hold for gynodioecy. Within woody species, dimorphism (dioecy, gynodioecy, subdioecy, polygamodioecy) is associated with mesic habitats and occurs more frequently in species with lowland and lowland-montane distributions. In contrast, in the endemic Hawaiian Alsinoideae (Schiedea and Alsinidendron) and in Bidens (two groups with autochthonous evolution of dimorphism), dimorphism is associated with more xeric habitats, and for the former group, with wind pollination. For the entire angiosperm flora, dimorphic species are associated with flowers that are small and green. Woody dioecious species and genera are disproportionately associated with wind pollination; hermaphroditic species are disproportionately bird pollinated primarily because of one species-rich lineage in the Campanulaceae. There was no association of dimorphism and pollinator type for colonists. Because of a few species-rich lineages, dimorphism is associated with dry fruits at the specific level, but at the generic level and for colonists, dimorphism is associated with fleshy fruits. Dioecious and gynodioecious species are found more often on older islands, a result of speciation of dimorphic colonists as well as autochthonous evolution of dimorphism. Single-island endemism is not associated with dioecy in the flora as a whole or with dimorphism within lineages evolving dimorphism autochthonously; thus Baker's law is not supported within the Hawaiian Islands. Because the Hawaiian angiosperm flora originated from a minimum of only 291 colonists, many of the associations of dimorphism with ecological traits occur because of the influence of only a few species-rich lineages. Better knowledge of phylogenetic patterns and further ecological studies, particularly within those groups evolving dioecy autochthonously, are needed to determine causality. C1 USA, CORPS ENGINEERS, FT SHAFTER, HI 96858 USA. SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT BOT, WASHINGTON, DC 20560 USA. RP SAKAI, AK (reprint author), UNIV CALIF IRVINE, DEPT ECOL & EVOLUTIONARY BIOL, IRVINE, CA 92717 USA. NR 64 TC 91 Z9 95 U1 6 U2 21 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD DEC PY 1995 VL 76 IS 8 BP 2530 EP 2543 DI 10.2307/2265826 PG 14 WC Ecology SC Environmental Sciences & Ecology GA TJ312 UT WOS:A1995TJ31200015 ER PT J AU STINE, JK AF STINE, JK TI GRAND-COULEE - HARNESSING A DREAM - PITZER,PC SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review RP STINE, JK (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGAN AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47401 SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD DEC PY 1995 VL 82 IS 3 BP 1266 EP 1267 DI 10.2307/2945240 PG 2 WC History SC History GA TK240 UT WOS:A1995TK24000133 ER PT J AU Wright, SJ Calderon, O AF Wright, SJ Calderon, O TI Phylogenetic patterns among tropical flowering phenologies SO JOURNAL OF ECOLOGY LA English DT Article DE Barro Colorado Island; comparative method; Panama; tropical forest ID COSTA-RICA; INDIVIDUAL FLOWERS; PLANT-COMMUNITIES; SEASONAL DROUGHT; MOIST FOREST; LIFE-HISTORY; DRY FORESTS; SEED SIZE; COMPETITION; UNDERSTORY AB 1 The ability of phylogenetic, water stress and 'shared-pollinator' hypotheses to explain flowering times was tested for the flora of Barro Colorado Island, Panama. Both quantitative (217 species) and qualitative (1173 species) flowering data were used. 2 Descriptive metrics calculated from quantitative flowering data indicated that mean flowering times fell in the final two months of the dry season and the first two months of the wet season for 56% of species and that flowering was concentrated in a short, predictable part of the year for the great majority of species. 3 The 'shared-pollinator' hypothesis predicted that congeners should have temporally segregated flowering times. This hypothesis was rejected for 57 of 59 genera. 4 The water stress hypothesis predicted that species from drier habitats and life forms with limited access to soil water should flower in the wet season. This hypothesis was also rejected. 5 There were, however, strong phylogenetic patterns. Both the mean and the variance of flowering times were similar among congeners. The variance of flowering times was also similar among confamilials, and mean flowering times were concentrated in the wet season for monocotyledons. C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 54 TC 116 Z9 127 U1 4 U2 23 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0022-0477 J9 J ECOL JI J. Ecol. PD DEC PY 1995 VL 83 IS 6 BP 937 EP 948 DI 10.2307/2261176 PG 12 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA TL883 UT WOS:A1995TL88300003 ER PT J AU GOMEZ, B GLASCOCK, MD BLACKMAN, MJ TODD, IA AF GOMEZ, B GLASCOCK, MD BLACKMAN, MJ TODD, IA TI NEUTRON-ACTIVATION ANALYSIS OF OBSIDIAN FROM KALAVASOS-TENTA SO JOURNAL OF FIELD ARCHAEOLOGY LA English DT Note ID FISSION AB The small quantity of obsidian used by the Aceramic Neolithic occupants of Cyprus was imported, there being no source on the island. The chemical composition, determined by neutron, activation analysis, of six samples of obsidian from Kalavasos-Tenta indicates that they were derived from the central Anatolian, Gollu Dag (Ciftlik: Group 2b) source. On the basis of chemical composition, obsidian from five Cypriot Aceramic Neolithic sites has the same provenance. Our data suggest that the fragments we analyzed were not derived from a single core and, because obsidian occurs throughout the Aceramic period of occupation of Kalavasos-Tenta, it appears unlikely that the 36 artifacts recovered from the site represent a one-time transfer of material. This suggests an enduring supply and implies to us that the inhabitants of Kalavasos-Tenta were never completely isolated from the mainland. C1 UNIV MISSOURI,RES REACTOR,ARCHACOMETRY LAB,COLUMBIA,MO. SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560. VASILIKOS VALLEY PROJECT,KALAVASOS,CYPRUS. RP GOMEZ, B (reprint author), INDIANA STATE UNIV,TERRE HAUTE,IN 47809, USA. NR 27 TC 8 Z9 8 U1 0 U2 0 PU JOURNAL FIELD ARCHAEOLOGY PI BOSTON PA BOSTON UNIV 675 COMMUNWEALTH AVE, BOSTON, MA 02215 SN 0093-4690 J9 J FIELD ARCHAEOL JI J. Field Archaeol. PD WIN PY 1995 VL 22 IS 4 BP 503 EP 508 DI 10.2307/530200 PG 6 WC Archaeology SC Archaeology GA TG237 UT WOS:A1995TG23700010 ER PT J AU SEUTIN, G LETZER, M AF SEUTIN, G LETZER, M TI THE SHORT-TAILED NIGHTHAWK IS A TREE NESTER SO JOURNAL OF FIELD ORNITHOLOGY LA English DT Article AB A nest of the Short-tailed Nighthawk, Lurocalis semitorquatus noctivagus, was found in Panama. It was located on a 15-cm diameter, horizontal branch in an Erythrina fusca tree, 6 to above ground. The tree was growing on the side of a pond in semi-open habitat, close to old second-growth, lowland forest. The nestling period was at least 24 d. The nest was similar to that recently described for L. s. nattereri, confirming that unlike any other Caprimulgidae, this nighthawk is an arboreal nester. The validity of previous accounts of ground nesting by the species is questioned, and the finding is discussed in the context of the uncertain taxonomy of the Short-tailed Nighthawk complex, and of the evolution of ground nesting in Caprimulgiformes. C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. NR 14 TC 2 Z9 2 U1 0 U2 0 PU ASSOC FIELD ORNITHOLOGISTS PI BELOIT PA BELOIT COLLEGE, DEPT BIOLOGY, 700 COLLEGE ST, BELOIT, WI 53511 SN 0273-8570 J9 J FIELD ORNITHOL JI J. Field Ornithol. PD WIN PY 1995 VL 66 IS 1 BP 30 EP 36 PG 7 WC Ornithology SC Zoology GA QH364 UT WOS:A1995QH36400004 ER PT J AU WASHBURN, WE AF WASHBURN, WE TI DESOTO,HERNANDO AND THE INDIANS OF FLORIDA - MILANICH,JT, HUDSON,C SO JOURNAL OF INTERDISCIPLINARY HISTORY LA English DT Book Review RP WASHBURN, WE (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU MIT PRESS PI CAMBRIDGE PA 55 HAYWARD ST JOURNALS DEPT, CAMBRIDGE, MA 02142 SN 0022-1953 J9 J INTERDISCIPL HIST JI J. Interdiscip. Hist. PD WIN PY 1995 VL 25 IS 3 BP 506 EP 507 DI 10.2307/205727 PG 2 WC History SC History GA PZ508 UT WOS:A1995PZ50800040 ER PT J AU Faust, MA AF Faust, MA TI Observation of sand-dwelling toxic dinoflagellates (Dinophyceae) from widely differing sites, including two new species SO JOURNAL OF PHYCOLOGY LA English DT Article DE Belize, Central America; benthic dinoflagellates; Carrie Bow Cay, Belize; Coolia tropicalis sp nov; coral rubble; Dinophyceae; epiphytic; Gambier-discus belizenus sp nov; morphology; peridiniales; sand-dwelling; scanning electron microscopy; South Water Cay, Belize; taxonomy ID SP-NOV; GAMBIERDISCUS; COOLIA AB Dinoflagellate associations, including toxic and potentially toxic benthic species, were examined in sand from South Water Cay and Carrie Bow Gay, Belize. The inshore sand habitat in localized areas of warm shallow lagoonal waters supported blooms of toxic assemblages of dinoflagellates. In the sand, the dominant microalgae were dinoflagellates; cyanobacteria were a minor component and diatoms were absent. Ciliates and nematodes were present. Assemblages of microorganisms in colored sand were examined for 4 consecutive days after which a storm washed away the parch. The sand-dwelling dinoflagellate assemblage included 16 species where densities ranged from as low as 1.3% to 15% of total cell densities. The dominant species was Scrippsiella subsalsa, having 1.8 x 10(5) to 2.6 x 10(5) cells . g(-1) sand. Toxic dinoflagellates identified in the sand were Gambierdiscus toxicus, Ostreopsis lenticularis, Prorocentrum lima, Prorocentrum mexicanum, and Amphidinium carteri. The potentially toxic Ostreopsis labens, Gambierdiscus belizeanus sp. nov., and Coolia tropicalis sp, nov. were also identified. Toxic and potentially toxic species represented 36% to 60% of total microalgal cell assemblage. The morphology of a new sand-dwelling species, Gambierdiscus belizeanus sp. nov., was examined with the scanning electron microscope. The plate formula was P-o, 3', 7 '', 6c, 8s?, 5''', 1p, and 2''''. Dimensions of G. belizeanus cells were 53-67 mu m long, 54-63 mu m wide, and 92-98 mu m in dorsoventral depth. Cells were deeply areolated, ellipsoid in apical view, and compressed anteroposteriorly. The cells of G. belizeanus were identified by the cell's long, narrow, pentagonal, posterior intercalary plate (1p) wedged between the wide postcingular plates 2''' and 4'''; 1p occupied 20% of the width of the hypotheca. The plate formula for Coolia tropicalis sp. nov. was P-o, 3', 7 '', 7c, 8s?, 5''' and 2''''. Cell size ranges were 23-40 mu m long, 25-39 mu m wide, and 35-65 mu m in dorsoventral diameter. Cells were spherical, smooth, and covered with scattered round pores. The epitheca was smaller than the hypotheca. Precingular plates 1 '' and 7 '' were small and narrow, and the first apical plate 1' and precingular plate 6 '' were the largest plates on the epitheca. The apical pore was straight and 7 mu m long, and was situated in the apical plate complex. Cells of C. tropicalis were distinguished from C. monotis by the wedge-shaped plate 1', a four-sided 3' plate, and a short apical pore. RP Faust, MA (reprint author), SMITHSONIAN INST,MUSEUM NATL HIST NAT,DEPT BOT,4201 SILVER HILL RD,SUITLAND,MD 20746, USA. NR 19 TC 98 Z9 110 U1 1 U2 19 PU PHYCOLOGICAL SOC AMER INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD DEC PY 1995 VL 31 IS 6 BP 996 EP 1003 DI 10.1111/j.0022-3646.1995.00996.x PG 8 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA TQ782 UT WOS:A1995TQ78200020 ER PT J AU Emry, RJ Lucas, SG Szalay, FS Tleuberdina, PA AF Emry, RJ Lucas, SG Szalay, FS Tleuberdina, PA TI A new herpetotheriine didelphid (marsupialia) from the Oligocene of central Asia SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article C1 NEW MEXICO MUSEUM NAT HIST & SCI,ALBUQUERQUE,NM 87104. CUNY HUNTER COLL,DEPT ANTHROPOL,NEW YORK,NY 10021. INST ZOOL,LAB PALEOZOOL,ALMA ATA 480032,KAZAKHSTAN. RP Emry, RJ (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL,WASHINGTON,DC 20560, USA. NR 14 TC 8 Z9 9 U1 0 U2 0 PU SOC VERTEBRATE PALEONTOLOGY PI CHICAGO PA 401 NORTH MICHIGAN AVE, CHICAGO, IL 60611-4267 SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD DEC PY 1995 VL 15 IS 4 BP 850 EP 854 PG 5 WC Paleontology SC Paleontology GA UH152 UT WOS:A1995UH15200013 ER PT J AU Hughes, NC Chapman, RE AF Hughes, NC Chapman, RE TI Growth and variation in the Silurian proetide trilobite Aulacopleura konincki and its implications for trilobite palaeobiology SO LETHAIA LA English DT Review DE morphometrics; trilobites; ontogeny; variability; segmentation; Silurian; Czech Republic ID CAMBRIAN TRILOBITES; CLASSIFICATION; EVOLUTION; ASSEMBLAGES; EXUVIATION; AUSTRALIA; ARTHROPOD; CRUSTACEA; ISOPODA; ORIGIN AB Morphometric analysis of growth in Aulacopleura konincki reveals several important features: (1) morphological variability is approximately constant throughout growth, increasing slightly in later ontogeny; (2) shape is more tightly constrained than the numbers of postcephalic segments, which can be quite variable; and (3) a major ontogenetic transition occurs at glabellar lengths of about 1.7 mm. This transition divides the ontogeny into two distinct growth phases, is smooth rather than abrupt, and is expressed as changes in growth trajectories, especially in the pygidium. The transition is not strictly correlated with the number of thoracic or pygidial segments. These results suggest a re-evaluation of the concepts of meraspid and holaspid growth stages in A. konincki using growth trajectories rather than thoracic segment number to define the stages. Developmental flexibility in holaspid segment numbers in this phylogenetically advanced trilobite suggests that environmental factors, rather than phylogenetic constraint, may explain variations in segment production patterns within some advanced Trilobita. C1 SMITHSONIAN INST,WASHINGTON,DC 20560. RP Hughes, NC (reprint author), CINCINNATI MUSEUM NAT HIST,GEIER COLLECT & RES CTR,1720 GILBERT AVE,CINCINNATI,OH 45202, USA. NR 119 TC 62 Z9 63 U1 0 U2 3 PU SCANDINAVIAN UNIVERSITY PRESS PI OSLO PA PO BOX 2959 TOYEN, JOURNAL DIVISION CUSTOMER SERVICE, N-0608 OSLO, NORWAY SN 0024-1164 J9 LETHAIA JI Lethaia PD DEC PY 1995 VL 28 IS 4 BP 333 EP 353 DI 10.1111/j.1502-3931.1995.tb01824.x PG 21 WC Paleontology SC Paleontology GA TP732 UT WOS:A1995TP73200008 ER PT J AU Riley, S AF Riley, S TI My soul to keep - Hawkes,J SO LIBRARY JOURNAL LA English DT Book Review RP Riley, S (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD DEC PY 1995 VL 120 IS 20 BP 154 EP 154 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA TK468 UT WOS:A1995TK46800260 ER PT J AU Wing, SL Dimichele, WA AF Wing, SL Dimichele, WA TI Conflict between local and global changes in plant diversity through geological time SO PALAIOS LA English DT Article ID COAL-SWAMP VEGETATION; DIVERSIFICATION; PALEOECOLOGY; PALEOBOTANY; EVOLUTION; PATTERNS; FOSSILS AB Reliable measurement of the original diversity of paleo-vegetation must account for many influences: the amount of time and space represented by the sample, the number of plant parts in the sample, the stature of the paleo-vegetation in, relation to sample area, and the preservational quality of the sample, as well as the number of species in the source community and their relative abundances. Plant compression fossil assemblages from river or delta floodplain environments generally have undergone minimal time and space averaging, which allows species richness to be measured and compared at a variety of temporal and spatial scales. Comparison of late Paleozoic and early Cenozoic wet floodplain. vegetation reveals little difference in species richness or diversity at the smallest measurable spatial scale, based on samples of a Jew square meters representing 0.1-0.5 hectares of source vegetation. Outcrop transects several hundred meters to several kilometers long that sample across minor variations in wet floodplain habitat also show similar levels of diversity in the Paleozoic and Cenozoic, with the exception of one Cenozoic transect with very high diversity. Diversity differences between Paleozoic and Cenozoic sites and transects are far less than would be expected based on global species richness curves for the Devonian through Pleistocene. The small differences in the diversity of wet floodplain vegetation probably relate to several factors, including the number of trees that can coexist in a small area, difficult edaphic conditions on wet floodplains, and perhaps the geologically early colonization and saturation of these habitats. The difficulty of making reliable measures of plant diversity in the fossil record, and the absence of change observed with relatively high quality data, suggest that biological explanations for changes in global species richness through geological time are premature. RP Wing, SL (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALAEONTOL,NHB 121,WASHINGTON,DC 20560, USA. RI DiMichele, William/K-4301-2012; OI Wing, Scott/0000-0002-2954-8905 NR 62 TC 62 Z9 63 U1 2 U2 6 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 1731 E 71ST STREET, TULSA, OK 74136-5108 SN 0883-1351 J9 PALAIOS JI Palaios PD DEC PY 1995 VL 10 IS 6 BP 551 EP 564 DI 10.2307/3515094 PG 14 WC Geology; Paleontology SC Geology; Paleontology GA TT452 UT WOS:A1995TT45200007 ER PT J AU CIRAC, JI LEWENSTEIN, M AF CIRAC, JI LEWENSTEIN, M TI COOLING OF ATOMS IN EXTERNAL FIELDS SO PHYSICAL REVIEW A LA English DT Article ID DOPPLER LIMIT; HYDROGEN; TRAP AB We present a cooling scheme based on interactions between atoms in different internal states and on energy shifts produced by external fields. The scheme predicts temperatures below the photon recoil limit without atomic losses. It can be considered as an alternative route to reach the conditions for Bose-Einstein condensation. C1 UNIV CASTILLA LA MANCHA,DEPT FIS APLICADA,E-13071 CIUDAD REAL,SPAIN. POLISH ACAD SCI,CENTRUM FIZ TEORET,PL-02668 WARSAW,POLAND. RP CIRAC, JI (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,MS 14,CAMBRIDGE,MA 02138, USA. RI Lewenstein, Maciej/I-1337-2014 OI Lewenstein, Maciej/0000-0002-0210-7800 NR 30 TC 6 Z9 6 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD DEC PY 1995 VL 52 IS 6 BP 4737 EP 4740 DI 10.1103/PhysRevA.52.4737 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA TK652 UT WOS:A1995TK65200055 ER PT J AU Canto, LF Donangelo, R Lotti, P Hussein, MS AF Canto, LF Donangelo, R Lotti, P Hussein, MS TI Effect of Coulomb dipole polarizability of halo nuclei on their near-barrier fusion with heavy targets SO PHYSICAL REVIEW C LA English DT Article ID LI-11 AB We show that the very strong Coulomb dipole polarizability and breakup of Li-11 reduces significantly its near-barrier fusion cross section with a heavy target nucleus. We suggest that the measurement of sigma(F) concomitantly with that bf;he elastic scattering would allow an unambiguous extraction of the dipole polarizability of halo nuclei. C1 MIT,CTR THEORET PHYS,NUCL SCI LAB,CAMBRIDGE,MA 02139. MIT,DEPT PHYS,CAMBRIDGE,MA 02139. HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. IST NAZL FIS NUCL,SEZ PADOVA,I-35131 PADUA,ITALY. UNIV SAO PAULO,INST FIS,BR-01498 SAO PAULO,BRAZIL. RP Canto, LF (reprint author), UNIV FED RIO DE JANEIRO,INST FIS,CAIXA POSTAL 68528,BR-21945970 RIO JANEIRO,BRAZIL. RI Canto, Luiz /I-3733-2012 NR 11 TC 53 Z9 53 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2813 J9 PHYS REV C JI Phys. Rev. C PD DEC PY 1995 VL 52 IS 6 BP R2848 EP R2850 PG 3 WC Physics, Nuclear SC Physics GA TL812 UT WOS:A1995TL81200007 ER PT J AU JAKUPOVIC, J ZDERO, C KING, RM AF JAKUPOVIC, J ZDERO, C KING, RM TI FURANOEREMOPHILANES FROM GYNOXY SPECIES SO PHYTOCHEMISTRY LA English DT Article DE GYNOXYS ACOSTAE; G-BUXIFOLIA; G-NITIDA; COMPOSITAE; FURANOEREMOPHILANES; SESQUITERPENES AB Five new furanoeremophilanes were isolated from three Gynoxys species. The structures of three 3 alpha,6 beta-diacyloxyfuranoeremophilanes previously isolated from G. sancto-antonii have to be revised to the corresponding 1 beta,6 beta derivatives. C1 SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560. RP JAKUPOVIC, J (reprint author), TECH UNIV BERLIN,INST ORGAN CHEM,STR 17 JUNI 135,D-10623 BERLIN,GERMANY. NR 7 TC 3 Z9 3 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0031-9422 J9 PHYTOCHEMISTRY JI Phytochemistry PD DEC PY 1995 VL 40 IS 6 BP 1677 EP 1679 DI 10.1016/0031-9422(95)00543-G PG 3 WC Biochemistry & Molecular Biology; Plant Sciences SC Biochemistry & Molecular Biology; Plant Sciences GA TK094 UT WOS:A1995TK09400015 ER PT J AU VANDERLINDEN, FR AF VANDERLINDEN, FR TI FOR THE GREATEST ACHIEVEMENT - A HISTORY OF THE AERO-CLUB-OF-AMERICA AND THE NATIONAL-AERONAUTIC-ASSOCIATION - ROBIE,B SO PUBLIC HISTORIAN LA English DT Book Review RP VANDERLINDEN, FR (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,DEPT AERONAUT,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD WIN PY 1995 VL 17 IS 1 BP 110 EP 111 PG 2 WC History SC History GA QH060 UT WOS:A1995QH06000024 ER PT J AU MARCAIDE, JM ALBERDI, A ROS, E DIAMOND, P SHAPIRO, II GUIRADO, JC JONES, DL KRICHBAUM, TP MANTOVANI, F PRESTON, RA RIUS, A SCHILIZZI, RT TRIGILIO, C WHITNEY, AR WITZEL, A AF MARCAIDE, JM ALBERDI, A ROS, E DIAMOND, P SHAPIRO, II GUIRADO, JC JONES, DL KRICHBAUM, TP MANTOVANI, F PRESTON, RA RIUS, A SCHILIZZI, RT TRIGILIO, C WHITNEY, AR WITZEL, A TI EXPANSION OF SN 1993J SO SCIENCE LA English DT Article ID RADIO; SUPERNOVA; MODEL; EMISSION; SYSTEM AB A sequence of images from very long baseline interferometry shows that the young radio supernova SN 1993J is expanding with circular symmetry. However, the circularly symmetric images show emission asymmetries. A scenario in which freely expanding supernova ejecta shock mostly isotropic circumstellar material is strongly favored. The sequence of images constitutes the first ''movie'' of a radio supernova. C1 INTA,ASTROFIS ESPACIAL & FIS FUNDAMENTAL,E-28080 MADRID,SPAIN. CSIC,INST ASTROFIS ANDALUCIA,E-18080 GRANADA,SPAIN. NATL RADIO ASTRON OBSERV,SOCORRO,NM 87801. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CALTECH,JET PROP LAB,PASADENA,CA 91109. MAX PLANCK INST RADIOASTRON,D-50131 BONN,GERMANY. CNR,IST RADIOASTRON,I-40129 BOLOGNA,ITALY. CSIC,CTR ESTUDIOS AVANCATS,E-17300 BLANES,SPAIN. JOINT INST VLBI EUROPE,7990 AA DWINGELOO,NETHERLANDS. LEIDEN OBSERV,2300 RA LEIDEN,NETHERLANDS. CNR,IST RADIOASTRON,NOTO,ITALY. MIT,HAYSTACK OBSERV,WESTFORD,MA 01886. RP MARCAIDE, JM (reprint author), UNIV VALENCIA,DEPT ASTRON,E-46100 BURJASSOT,SPAIN. OI Ros, Eduardo/0000-0001-9503-4892 NR 34 TC 46 Z9 46 U1 0 U2 4 PU AMER ASSOC ADVAN SCIENCE PI WASHINGTON PA 1333 H ST NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD DEC 1 PY 1995 VL 270 IS 5241 BP 1475 EP 1478 DI 10.1126/science.270.5241.1475 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA TH375 UT WOS:A1995TH37500032 ER PT J AU Kohl, JL Esser, R Gardner, LD Habbal, S Daigneau, PS Dennis, EF Nystrom, GU Panasyuk, A Raymond, JC Smith, PL Strachan, L VanBallegooijen, AA Noci, G Fineschi, S Romoli, M Ciaravella, A Modigliani, A Huber, MCE Antonucci, E Benna, C Giordano, S Tondello, G Nicolosi, P Naletto, G Pernechele, C Spadaro, D Poletto, G Livi, S VonderLuhe, O Geiss, J Timothy, JG Gloeckler, G Allegra, A Basile, G Brusa, R Wood, B Siegmund, OHW Fowler, W Fisher, R Jhabvala, M AF Kohl, JL Esser, R Gardner, LD Habbal, S Daigneau, PS Dennis, EF Nystrom, GU Panasyuk, A Raymond, JC Smith, PL Strachan, L VanBallegooijen, AA Noci, G Fineschi, S Romoli, M Ciaravella, A Modigliani, A Huber, MCE Antonucci, E Benna, C Giordano, S Tondello, G Nicolosi, P Naletto, G Pernechele, C Spadaro, D Poletto, G Livi, S VonderLuhe, O Geiss, J Timothy, JG Gloeckler, G Allegra, A Basile, G Brusa, R Wood, B Siegmund, OHW Fowler, W Fisher, R Jhabvala, M TI The ultraviolet coronagraph spectrometer for the solar and heliospheric observatory SO SOLAR PHYSICS LA English DT Article DE sun; solar; corona; solar wind; UV spectroscopy; UV coronagraph ID MICROCHANNEL PLATES; POLAR-REGION; TEMPERATURES; RADII; SUN AB The SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) is composed of three reflecting telescopes with external and internal occultation and a spectrometer assembly consisting of two toric grating spectrometers and a visible light polarimeter. The purpose of the UVCS instrument is to provide a body of data that can be used to address a broad range of scientific questions regarding the nature of the solar corona and the generation of the solar wind. The primary scientific goals are the following: to locate and characterize the coronal source regions of the solar wind, to identify and understand the dominant physical processes that accelerate the solar wind, to understand how the coronal plasma is heated in solar wind acceleration regions, and to increase the knowledge of coronal phenomena that control the physical properties of the solar wind as determined by in situ measurements. To progress toward these goals, the UVCS will perform ultraviolet spectroscopy and visible polarimetry to be combined with plasma diagnostic analysis techniques to provide detailed empirical descriptions of the extended solar corona from the coronal base to a heliocentric height of 12 solar radii. C1 UNIV FLORENCE,I-50125 FLORENCE,ITALY. EUROPEAN SPACE AGCY,ESTEC,DEPT SPACE SCI,2200 AG NOORDWIJK,NETHERLANDS. UNIV TURIN,I-10125 TURIN,ITALY. UNIV PADUA,I-35131 PADUA,ITALY. OSSERV ASTROFIS CATANIA,I-95125 CATANIA,ITALY. OSSERV ASTROFIS ARCETRI,I-50125 FLORENCE,ITALY. MAX PLANCK INST AERON,D-37189 KATLENBURG LINDAU,GERMANY. EUROPEAN SO OBSERV,D-85748 GARCHING,GERMANY. INT SPACE SCI INST,CH-3012 BERN,SWITZERLAND. UNIV NEW BRUNSWICK,NEW BRUNSWICK,NB E3B 5A3,CANADA. UNIV MARYLAND,COLLEGE PARK,MD 20742. ALENIA SPAZIO,I-10146 TURIN,ITALY. OFFICINE GALILEO,DIV OTT & SPAZIO,I-50013 FLORENCE,ITALY. BRUSAG,CH-8712 STAFA,SWITZERLAND. OERLIKON CONTRAVES,SPACE DIV,CH-8052 ZURICH,SWITZERLAND. UNIV CALIF BERKELEY,SPACE SCI LAB,BERKELEY,CA 94720. BALL CORP,ELECTROOPT & CRYOGEN DIV,BOULDER,CO 80306. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. OSSERVATORIO ASTRON PALERMO,PALERMO,ITALY. RP Kohl, JL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Romoli, Marco/H-6859-2012; Naletto, Giampiero/S-6329-2016; OI Naletto, Giampiero/0000-0003-2007-3138; Giordano, Silvio/0000-0002-3468-8566; pernechele, claudio/0000-0002-7752-6268 NR 31 TC 360 Z9 363 U1 1 U2 10 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD DEC PY 1995 VL 162 IS 1-2 BP 313 EP 356 DI 10.1007/BF00733433 PG 44 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TM503 UT WOS:A1995TM50300011 ER PT J AU Lewis, PO AF Lewis, PO TI MEGA: Molecular evolutionary genetics analysis, version 1.02. SO SYSTEMATIC BIOLOGY LA English DT Software Review ID NUCLEOTIDE SUBSTITUTIONS; SEQUENCES; NUMBER; DNA C1 DUKE UNIV,DEPT BOT,DURHAM,NC 27708. RP Lewis, PO (reprint author), SMITHSONIAN INST,LAB MOLEC SYSTEMAT,WASHINGTON,DC 20560, USA. NR 15 TC 1 Z9 1 U1 1 U2 1 PU SOC SYSTEMATIC BIOLOGISTS PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY NHB 163, WASHINGTON, DC 20560 SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD DEC PY 1995 VL 44 IS 4 BP 576 EP 577 DI 10.2307/2413665 PG 2 WC Evolutionary Biology SC Evolutionary Biology GA TQ871 UT WOS:A1995TQ87100012 ER PT J AU EBERHARD, WG CORDERO, C AF EBERHARD, WG CORDERO, C TI SEXUAL SELECTION BY CRYPTIC FEMALE CHOICE ON MALE SEMINAL PRODUCTS - A NEW BRIDGE BETWEEN SEXUAL SELECTION AND REPRODUCTIVE PHYSIOLOGY SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Article ID MALE ACCESSORY-GLANDS; INSECT REPRODUCTION; DROSOPHILA; SPERM; COMPETITION; HANDICAPS; PROTEINS; ECOLOGY; FITNESS; CRICKET AB Selection clearly focuses on differences in reproduction, but studies of reproductive physiology generally have been carried out in a near vacuum of modern evolutionary theory. This lack of contact between the two fields may be about to change. New ideas indicate that sexual selection by cryptic female choice has affected the evolution of products in male semen that influence female reproductive behavior and physiology. C1 UNIV COSTA RICA,ESCUELA BIOL,SAN JOSE,COSTA RICA. NATL AUTONOMOUS UNIV MEXICO,CTR ECOL,MEXICO CITY 04510,DF,MEXICO. RP EBERHARD, WG (reprint author), SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 51 TC 126 Z9 127 U1 3 U2 51 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, OXON, ENGLAND OX5 1GB SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD DEC PY 1995 VL 10 IS 12 BP 493 EP 496 DI 10.1016/S0169-5347(00)89205-8 PG 4 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA TF925 UT WOS:A1995TF92500016 PM 21237123 ER PT J AU Marshall, JT AF Marshall, JT TI Birds of coniferous forest on Mount Graham, Arizona SO WILSON BULLETIN LA English DT Article RP Marshall, JT (reprint author), NATL MUSEUM NAT HIST,SMITHSONIAN INST,DEPT VERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 11 TC 0 Z9 0 U1 0 U2 1 PU WILSON ORNITHOLOGICAL SOC PI ANN ARBOR PA MUSEUM OF ZOOLOGY UNIV MICHIGAN, ANN ARBOR, MI 48109 SN 0043-5643 J9 WILSON BULL JI Wilson Bull. PD DEC PY 1995 VL 107 IS 4 BP 719 EP 723 PG 5 WC Ornithology SC Zoology GA TN550 UT WOS:A1995TN55000015 ER PT J AU Juanes, F Smith, LD AF Juanes, F Smith, LD TI The ecological consequences of limb damage and loss in decapod crustaceans: A review and prospectus SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Review DE autotomy; decapod crustacean; functional and energetic costs; injury frequency; limb damage; limb loss; regeneration; survival benefits ID CALLINECTES-SAPIDUS RATHBUN; CRAYFISH ORCONECTES-RUSTICUS; NECORA-PUBER BRACHYURA; CRAB CARCINUS-MAENAS; VELVET SWIMMING CRAB; BLUE CRABS; FIDDLER CRABS; UCA-PUGILATOR; POPULATION REGULATION; AGONISTIC BEHAVIOR AB Autotomy, the reflex severance of an appendage, is considered an adaptation to avoid predators and limit wounds. While an autotomy response may provide immediate survival benefits, the loss of one or more appendages can result in long-term functional and energetic costs. In this paper, we present an overview of the incidence of limb damage and loss in decapod crustaceans;review the literature on the ecological consequences of such injury; and suggest areas for future research. A survey of limb damage and loss in field populations showed consistently high incidences of injury in 14 reviewed species. Typically, chelipeds were the limb type lost most often and injuries were distributed symmetrically. No consistent correlation existed between injury frequency and body size among species. In general, the frequency of injury was independent of sex and moult stage. Fishery practices were responsible for substantial limb loss in some commercial species. In terms of energetic costs, experiments demonstrated that limb injury could reduce growth increment and affect intermoult duration. Functionally, limb damage was capable of reducing foraging efficiency and mating success, and increasing vulnerability to intra- and interspecific attack. The magnitude of these effects depended on the type and number of limbs lost. Given the prevalence of injury in decapod crustacean populations, the costs involved, and the ecological importance of many crustacean species, nonlethal injury has the potential to affect population dynamics and community processes. Convincing evidence of autotomy's effects beyond the level of the individual, however, is, at present, lacking. Future work should redress this shortcoming. In addition, comparative studies are needed on decapod species from different habitats and with different lifestyles before generalizations can be made about the costs and benefits of autotomy. C1 SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. RP Juanes, F (reprint author), UNIV MASSACHUSETTS,DEPT FORESTRY & WILDLIFE MANAGEMENT,AMHERST,MA 01003, USA. NR 158 TC 170 Z9 177 U1 3 U2 41 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD NOV 29 PY 1995 VL 193 IS 1-2 BP 197 EP 223 DI 10.1016/0022-0981(95)00118-2 PG 27 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA TL477 UT WOS:A1995TL47700014 ER PT J AU RALLS, K AF RALLS, K TI ENCYCLOPEDIA OF ENVIRONMENTAL BIOLOGY - NIERENBERG,WA SO NATURE LA English DT Book Review RP RALLS, K (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 1 TC 0 Z9 0 U1 4 U2 23 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD NOV 23 PY 1995 VL 378 IS 6555 BP 347 EP 348 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA TF893 UT WOS:A1995TF89300044 ER PT J AU RALLS, K AF RALLS, K TI PRINCIPLES OF CONSERVATION BIOLOGY - MEFFE,GK, CARROLL,CR SO NATURE LA English DT Book Review RP RALLS, K (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 1 TC 0 Z9 0 U1 4 U2 23 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD NOV 23 PY 1995 VL 378 IS 6555 BP 347 EP 348 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA TF893 UT WOS:A1995TF89300042 ER PT J AU RALLS, K AF RALLS, K TI A PRIMER OF CONSERVATION BIOLOGY - PRIMACK,RB SO NATURE LA English DT Book Review RP RALLS, K (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 1 TC 0 Z9 0 U1 4 U2 23 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD NOV 23 PY 1995 VL 378 IS 6555 BP 347 EP 348 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA TF893 UT WOS:A1995TF89300041 ER PT J AU RALLS, K AF RALLS, K TI CONSERVATION BIOLOGY IN THEORY AND PRACTICE - CAUGHLEY,G, GUNN,A SO NATURE LA English DT Book Review RP RALLS, K (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 1 TC 0 Z9 0 U1 4 U2 23 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD NOV 23 PY 1995 VL 378 IS 6555 BP 347 EP 348 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA TF893 UT WOS:A1995TF89300043 ER PT J AU WERREN, JH WINDSOR, D GUO, LR AF WERREN, JH WINDSOR, D GUO, LR TI DISTRIBUTION OF WOLBACHIA AMONG NEOTROPICAL ARTHROPODS SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article ID CYTOPLASMIC INCOMPATIBILITY; DROSOPHILA-SIMULANS AB Wolbachia are a group of cytoplasmically inherited bacteria that cause reproduction alterations in arthropods, including parthenogenesis, reproductive incompatibility and feminization of genetic males. Two major subdivisions of Wolbachia (A and B) occur. Wolbachia are found in a number of well-studied insects, but their overall distribution in arthropods has not been well studied. A survey for Wolbachia in 157 Panamanian neotropical arthropod species was done using a polymerase chain reaction assay. detected in 26 of 154 insect species (16.9%) and zero of three arachnids (0%). Extrapolating to the estimated total number of insect species present globally (10-30 million), an estimated 1.69-5.07 million insect species are infected with these bacteria, making Wolbachia an extremely abundant bacterial group. Wolbachia were found in each of the major insect orders examined, including Coleoptera (6/57 infected), Diptera (5/14), Hemiptera/Homoptera (1/7), Hymenoptera (6/23) Lepidoptera (7/43) and Orthoptera (1/8). Of the 26 positives, eight species were found to be singly infected with A group Wolbachia, nine singly with B group Wolbachia and nine doubly infected with both A and B group Wolbachia. Double infections occur at significantly higher frequencies than expected by chance. The abundance of Wolbachia further supports their potential importance as a mechanism for rapid speciation in insects. C1 SMITHSONIAN TROP RES INST, PANAMA CITY, PANAMA. RP WERREN, JH (reprint author), UNIV ROCHESTER, DEPT BIOL, ROCHESTER, NY 14627 USA. NR 30 TC 379 Z9 430 U1 7 U2 61 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD NOV 22 PY 1995 VL 262 IS 1364 BP 197 EP 204 DI 10.1098/rspb.1995.0196 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA TH712 UT WOS:A1995TH71200013 ER PT J AU SIEMIGINOWSKA, A KUHN, O ELVIS, M FIORE, F MCDOWELL, J WILKES, BJ AF SIEMIGINOWSKA, A KUHN, O ELVIS, M FIORE, F MCDOWELL, J WILKES, BJ TI TESTING MODELS FOR THE QUASAR BIG BLUE BUMP VIA COLOR-COLOR DIAGRAMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; GALAXIES, PHOTOMETRY; QUASARS, GENERAL; RADIATION MECHANISMS, THERMAL ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRA; THIN ACCRETION DISKS; ENERGY-DISTRIBUTIONS; ULTRAVIOLET EXCESS; PG QUASARS; BLACK-HOLE; VARIABILITY; CONTINUUM; UV AB We discuss several models of quasar big blue bump emission in color-color and color-luminosity diagrams. We define several broad passbands: IR (0.8-1.6 mu m), VIS (4000-8000 Angstrom), UV (1000-2000 Angstrom), UV1 (1400-2000 Angstrom) and UV2 (1000-1400 Angstrom), and SX (0.2-0.4 keV). The colors have been chosen to investigate characteristics of the big blue bump: (1) IR/VIS color represents the importance of the IR component and shows the contribution around similar to 1 mu m; (2) UV/VIS color shows the slope of the big blue bump (in a region where it dominates, a higher value means the bump gets steeper); (3) the combination of IR/VIS/UV colors shows the relative strength of the big blue bump and the IR component; (4) UV1/UV2 color is important as an indicator of a flattening of the spectrum in this region and the presence of the far-UV turnover, (5) UV/SX tests the relationship between the big blue bump and the soft X-ray component. All colors are needed to investigate the range of model parameters. We describe the colors for several models: accretion disk models in Schwarzschild and Kerr geometries, single-temperature optically thin emission, combination of the main emission model and nonthermal power law or dust, and irradiation of the disk surface. We test models against the sample of 47 low-redshift quasars from Elvis et al. We and that (1) modified blackbody emission from an accretion disk in a Kerr geometry can successfully reproduce both the luminosities and colors of the quasars except for the soft X-ray emission; (2) no additional components (hot dust or power-law) are needed to fit the optical-UV colors when the irradiation of the surface of the disk is included in the model; (3) even modest (10%) irradiation of the surface of the disk modifies significantly the optical colors; (4) the simplest, single-temperature, free-free models need either an additional component or a range of temperatures to explain the observations. Tables of predicted colors for each model family are provided on the AAS CD-ROM. A part of the tables is listed in the Appendix. RP SIEMIGINOWSKA, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Wilkes, Belinda/0000-0003-1809-2364; Fiore, Fabrizio/0000-0002-4031-4157 NR 75 TC 34 Z9 34 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 1995 VL 454 IS 1 BP 77 EP 94 DI 10.1086/176467 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TD743 UT WOS:A1995TD74300009 ER PT J AU BALLY, J DEVINE, D FESEN, RA LANE, AP AF BALLY, J DEVINE, D FESEN, RA LANE, AP TI TWIN HERBIG-HARO JETS AND MOLECULAR OUTFLOWS IN L1228 SO ASTROPHYSICAL JOURNAL LA English DT Article DE INFRARED, ISM, LINES AND BANDS; ISM, INDIVIDUAL (L122S); ISM, JETS AND OUTFLOWS; STARS, PRE-MAIN-SEQUENCE ID CEPHEUS FLARE; CO OBSERVATIONS; STELLAR JET; CLOUDS; EMISSION; REGION; STARS; GAS AB We present new optical, near-infrared, and millimeter wavelength observations of the dark cloud L1228 located in the Cepheus Flare. There are at least two active young stellar objects within a 2' diameter region in the L1228 cloud core that drive two separate Herbig-Haro (HH) outflows, a molecular hydrogen jet, and associated CO outflows. The red nebulous object RNO 129 (HH 198), located 1 degrees north of the L1228 cloud core, is a Herbig-Haro flow from a T Tauri star located near the eastern end of the HH object. The Herbig-Haro object HH 199 is associated with a large molecular outflow (L1228A) centered on a low-luminosity (4 L.) young stellar object IRAS 20582+7724, the brightest infrared source in this cloud core. The brightest visual wavelength components, HH 199R1 and R2, lie about 8' to the southwest of the IRAS source, where the redshifted lobe of the CO outflow may be breaking out of the molecular cloud. A chain of faint blueshifted (V approximate to -40 to -150 km s(-1)) HH objects, HH 199B1 through HH 199B6, lies to the northeast of the IRAS source toward the blueshifted lobe of the L1228A CO outflow. The projected distance between HH 199R2 and HH 199B6 is about 20' or nearly 2 pc. Near the center of this outflow, a chain of knots bright in the 2.122 mu m wavelength S(1) line of molecular hydrogen extends for about 1' along a nearly east-west axis on both sides of IRAS 20582+7724. This axis differs from that of the L1228A/HH 199 outflow by about 40 degrees. We consider a model in which the jet from IRAS 20582+7724 varies in its ejection direction. At present, the outflow as traced by the H-2 jet appears to be impacting dense C3H2 emitting clumps east and west of the IRAS source. A redshifted CO ridge extends 10' to the west of the IRAS source at the same orientation as the H-2 jet, but a more prominent northeast-southwest ridge extends along the HH 199 optical axis from HH 199B6 in the northeast, through the IRAS source, to HH 199R2 in the southwest. A periodic blueshifted (V approximate to -40 to -150 km s(-1)) chain of Herbig-Haro objects, HH 200, is superimposed on the redshifted lobe of the L1228A outflow. It is associated with the low-velocity blueshifted CO lobe of a second outflow, L1228B. The source of this jet is an embedded T Tauri star located 1'.5 northwest of IRAS 20582+7724. There is a faint HH object 9' to the northeast of the source of the HH 200 jet, directly opposite the location of the bright bow shock at the end of the blueshifted lobe of the HH 200 jet. This lobe may mark the location of an invisible counterjet. HH 200 has a projected length of over 18' corresponding to 1.8 pc (assuming a distance of 300 pc to L1228), and it shows quasi-periodic knot spacing of roughly 1' corresponding to a projected spacing of 0.09 pc. At a flow velocity of 300 km s(-1), and an assumed outflow inclination angle of 45 degrees, this spacing may be a result of episodes of enhanced mass loss occurring roughly every 500 years. C1 DARTMOUTH COLL, DEPT PHYS & ASTRON, WILDER LAB 6127, HANOVER, NH 03755 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. KITT PEAK NATL OBSERV, TUCSON, AZ 85726 USA. RP BALLY, J (reprint author), UNIV COLORADO, CTR ASTROPHYS & SPACE ASTRON, DEPT ASTROPHYS PLANETARY & ATMOSPHER SCI, BOULDER, CO 80309 USA. OI BALLY, JOHN/0000-0001-8135-6612 NR 32 TC 50 Z9 51 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 1995 VL 454 IS 1 BP 345 EP + DI 10.1086/176486 PN 1 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TD743 UT WOS:A1995TD74300028 ER PT J AU LIU, WH DALGARNO, A AF LIU, WH DALGARNO, A TI THE OXYGEN TEMPERATURE OF SN 1987A SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC PROCESSES; CIRCUMSTELLAR MATTER; MOLECULAR PROCESSES STARS, INDIVIDUAL (SN 1987A); SUPERNOVAE, INDIVIDUAL (SN 1987A) ID SUPERNOVA 1987A; INFRARED PHOTOMETRY; CARBON-MONOXIDE; MU-M; SN-1987A; SPECTROPHOTOMETRY; EMISSION; SPECTROSCOPY; ABSORPTION; COBALT AB The temperature of the oxygen core of SN 1987A is calculated by analyzing the processes that heat and cool the gas and the processes that form and destroy carbon monoxide. The heating efficiency is calculated by including the processes by which the energetic electrons created by the radioactive decay of Co-56 lose energy in a mixed gas of O, C, and CO. The effects of nonuniform energy distribution in the supernova ejecta at early times due to the large optical depths of the gamma-rays are studied by reducing the energy input rate to match the observed emission of CO. The oxygen core contains a cold CO-emitting region which is effectively cooled by the vibrational emission of CO and heated by the O and C, and a hot O-emitting region which contains neither CO nor SiO and is cooled by the metastable transitions of O. The temperature in the CO-emitting region is constant at about 1800 K in the first year and drops to 700 K at 800 days, consistent with that derived from the observed spectral shapes of the CO emission. The temperature in the O-emitting region is relatively high. It ranges from 4800 K at 100 days to 2200 K at 800 days, in agreement with that derived from the observations of the [OI] lambda lambda 6300, 6364. The mass of CO predicted by the thermal-chemical model and the mass derived from the observations agree well provided no microscopic mixing of helium is permitted into the oxygen core. RP LIU, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 41 TC 55 Z9 56 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 1995 VL 454 IS 1 BP 472 EP 479 DI 10.1086/176498 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TD743 UT WOS:A1995TD74300040 ER PT J AU BLAIR, WP RAYMOND, JC LONG, KS KRISS, GA AF BLAIR, WP RAYMOND, JC LONG, KS KRISS, GA TI A FAR-ULTRAVIOLET SPECTRUM OF THE PUPPIS-A SUPERNOVA REMNANT USING THE HOPKINS-ULTRAVIOLET-TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (PUPPIS A); ISM, SUPERNOVA REMNANTS; SHOCK WAVES; ULTRAVIOLET, ISM ID CYGNUS LOOP; X-RAY; OPTICAL-EMISSION; DISCOVERY; FILAMENT; RADIO; CLOUD AB We report the first successful far-ultraviolet spectroscopic observation of a filament in the Puppis A supernova remnant. We observed a position on the eastern side of the remnant near the brightest X-ray region using the Hopkins Ultraviolet Telescope during the Astro-2 space shuttle mission in 1995 March. The spectrum covers the 820-1840 Angstrom spectral range with similar to 3 Angstrom resolution and shows numerous lines of C, N, O, Ne, He, and possibly Si. Comparison of this spectrum to solar abundance shock models indicates a shock velocity of approximately 160-180 km s(-1). A slight overabundance of N is possible for this position, consistent with a shocked interstellar medium picture for the observed filament. This is at odds with the much larger overabundance of N indicated by optical data from other regions of the outer shell in Puppis A. Comparison with optical CCD images obtained at Las Campanas Observatory and with Einstein HRI data indicates that the region observed corresponds to a very recent encounter between the blast wave and an interstellar cloud. The interaction of the shock wave with this cloud is responsible for the bright X-ray emission in this region. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. RP BLAIR, WP (reprint author), JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,34TH & CHARLES ST,BALTIMORE,MD 21218, USA. NR 36 TC 19 Z9 19 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 1995 VL 454 IS 1 BP L35 EP & PN 2 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TD744 UT WOS:A1995TD74400009 ER PT J AU LONG, KS BLAIR, WP RAYMOND, JC AF LONG, KS BLAIR, WP RAYMOND, JC TI HOPKINS-ULTRAVIOLET-TELESCOPE OBSERVATIONS OF U-GEMINORUM FAR FROM OUTBURST SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, BINARIES, CLOSE; STARS, INDIVIDUAL (U GEMINORUM); STARS, NOVAE, CATACLYSMIC VARIABLES; ULTRAVIOLET, STARS ID WHITE-DWARF; NOVAE AB The Hopkins Ultraviolet Telescope was used during the Astro-2 Space Shuttle mission to obtain a far-ultraviolet (820-1840 Angstrom) spectrum of the dwarf nova U Geminorum in its low state. At the time of the observation, U Gem had been at optical minimum for 185 days. The HUT spectrum is dominated by the white dwarf star, and shows (among other things) very strong, broad hydrogen Lyman absorption lines. A comparison with solar abundance white dwarf models indicates a temperature near similar to 30,000 K. Comparison to a similar spectrum obtained during the Astro-l mission in 1990, only 10 days after U Gem had returned to the low state following a normal outburst, confirms that the average temperature of the white dwarf in U Gem drops substantially between outbursts. Furthermore, differences between the models and the data at the shortest wavelengths in both spectra support the hypothesis that the surface temperature is nonuniform and that a decrease in the relative importance of a hot region, possibly a belt, on the surface of the white dwarf causes the observed 30% decline in flux at 1450 Angstrom far from outburst. C1 JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP LONG, KS (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. NR 18 TC 17 Z9 17 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 1995 VL 454 IS 1 BP L39 EP L42 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TD744 UT WOS:A1995TD74400010 ER PT J AU RAYMOND, JC BLAIR, WP LONG, KS AF RAYMOND, JC BLAIR, WP LONG, KS TI DETECTION OF ULTRAVIOLET EMISSION-LINES IN SN-1006 WITH THE HOPKINS-ULTRAVIOLET-TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (SN 1006); ISM, SUPERNOVA REMNANTS; SHOCK WAVES; ULTRAVIOLET, ISM ID FAST SHOCK-WAVE; CYGNUS LOOP; OPTICAL-EMISSION; SUPER-NOVA; REMNANTS; SN-1006; FILAMENT AB The Hopkins Ultraviolet Telescope (HUT) was used during the Astro-2 space shuttle mission in 1995 March to observe emission lines of H I, He II, C IV, N V, and O VI from the faint optical Balmer line filament at the northwest edge of the SN 1006 supernova remnant. This is the first successful far-ultraviolet observation of a nonradiative shock wave with velocity in excess of 300 km s(-1) and the first detection of ultraviolet emission lines from SN 1006. The observed line widths are consistent with the similar to 2300 km s(-1) width reported for H alpha, implying that the velocities of different ions are independently randomized in the shock and that ion-ion temperature equilibration is ineffective. A faint continuum in the spectrum is consistent with relatively strong dust-scattered starlight along this line of sight, visible because of the large HUT spectrograph aperture used for this observation. The relative line intensities are in reasonable agreement with existing model predictions for a 2300 km s(-1) shock. However, proton excitation rates may compete with electron excitation in producing the emission lines and need to be included in the model calculations before a comprehensive analysis can be attempted. C1 JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. RP RAYMOND, JC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 28 TC 43 Z9 43 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 1995 VL 454 IS 1 BP L31 EP & PN 2 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TD744 UT WOS:A1995TD74400008 ER PT J AU DALGARNO, A AF DALGARNO, A TI ION/MOLECULE REACTIONS IN ASTROPHYSICAL PLASMAS SO INTERNATIONAL JOURNAL OF MASS SPECTROMETRY LA English DT Article DE ASTROPHYSICAL PLASMAS; ION MOLECULE REACTIONS ID RADIATIVE ASSOCIATION; DISSOCIATIVE RECOMBINATION; CARBON-MONOXIDE; HEH+; HYDROGEN; SN-1987A; COLLISIONS; CHEMISTRY; MOLECULES; SPECTRUM AB A description is given of some molecular processes occurring in the recombination era of the early Universe and in the response of molecular gas to ultraviolet radiation, X-rays and gamma rays. RP DALGARNO, A (reprint author), HARVARD UNIV, HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NR 64 TC 10 Z9 10 U1 1 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1387-3806 J9 INT J MASS SPECTROM JI Int. J. Mass Spectrom. PD NOV 15 PY 1995 VL 149 BP 429 EP 437 DI 10.1016/0168-1176(95)04274-O PG 9 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA TG497 UT WOS:A1995TG49700039 ER PT J AU KALFATOVIC, MR AF KALFATOVIC, MR TI ART TODAY - LUCIESMITH,E SO LIBRARY JOURNAL LA English DT Book Review RP KALFATOVIC, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD NOV 15 PY 1995 VL 120 IS 19 BP 73 EP 73 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA TE126 UT WOS:A1995TE12600054 ER PT J AU RILEY, S AF RILEY, S TI THE 100 SECRET SENSES - TAN,A SO LIBRARY JOURNAL LA English DT Book Review RP RILEY, S (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD NOV 15 PY 1995 VL 120 IS 19 BP 101 EP 101 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA TE126 UT WOS:A1995TE12600230 ER PT J AU ALVAREZ, F HINES, AH REAKAKUDLA, ML AF ALVAREZ, F HINES, AH REAKAKUDLA, ML TI THE EFFECTS OF PARASITISM BY THE BARNACLE LOXOTHYLACUS-PANOPAEI (GISSLER) (CIRRIPEDIA, RHIZOCEPHALA) ON GROWTH AND SURVIVAL OF THE HOST CRAB RHITHROPANOPEUS-HARRISII (GOULD) (BRACHYURA, XANTHIDAE) SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE CHESAPEAKE BAY; CRAB; HOST-PARASITE INTERACTION; PARASITIC CASTRATION; RHIZOCEPHALAN BARNACLE ID BRIAROSACCUS-CALLOSUS BOSCHMA; SACCULINA-GRANIFERA BOSCHMA; COMMERCIAL SAND CRAB; PORTUNUS-PELAGICUS L; TEXANUS AB The crab Rhithropanopeus harrisii (Gould) (Brachyura: Xanthidae) was infected in the laboratory with the parasitic barnacle Loxothylacus panopaei (Gissler) (Cirripedia: Rhizocephala). Crabs and barnacles were collected in the Rhode River in the Chesapeake Bay, MD. Forty-three out of 153 R. harrisii, including stages from megalopa (<1 mm of carapace width) to crab 8 stage (+/-8 mm of carapace width), developed a mature parasite (external after exposure to rhizocephalan cypris larvae. The duration of the internal phase of the parasite (from infection to the emergence of the external averaged 33 days and was independent of host size. Recently emerged externae (virgin externae) exposed to male cypris larvae, matured after fertilization in an average of 15 days. Host molting frequency and molt increments did not differ significantly between parasitized and control crabs. Survival to the crab 9 stage (+/-9.5 mm of carapace width) was 6% for hosts parasitized during the megalopal stage (<1 mm of carapace width), while it was 50% for the controls. The results of this study are discussed relative to the prevalences of L. panopaei found in the Chesapeake Bay. C1 UNIV MARYLAND,DEPT ZOOL,COLLEGE PK,MD 20742. SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21307. NR 30 TC 30 Z9 31 U1 3 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD NOV 13 PY 1995 VL 192 IS 2 BP 221 EP 232 DI 10.1016/0022-0981(95)00068-3 PG 12 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA TF978 UT WOS:A1995TF97800005 ER PT J AU KOCHANEK, CS AF KOCHANEK, CS TI GRAVITATIONAL LENSING LIMITS ON COLD DARK-MATTER AND ITS VARIANTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, THEORY; DARK MATTER; GRAVITATIONAL LENSING; LARGE-SCALE STRUCTURE OF UNIVERSE ID LARGE-SCALE STRUCTURE; COSMOLOGICAL CONSTANT; ISOTHERMAL SPHERES; GALAXY CLUSTERS; REDSHIFT SURVEY; UNIVERSE; LENSES; STATISTICS; DISCOVERY; QUASARS AB Standard Omega(0) = 1 cold dark matter (CDM) needs 0.27 < sigma(8) < 0.63 (2 sigma) to fit the observed number of large separation lenses, and the constraint is nearly independent of H-0 = 100 h km s(-1) Mpc(-1). This range is strongly inconsistent with the COBE estimate of sigma(8) = (2.8 +/- 0:2)h. Tilting the primordial spectrum proportional to k(n) from n = 1 to 0.3 less than or similar to n less than or similar to 0.7, using an effective Hubble constant of 0.15 less than or similar to Gamma = h less than or similar to 0.30, or reducing the matter density to 0.15 less than or similar to Omega(0) h less than or similar to 0.3 either with no cosmological constant lambda(0) = 0) or in a flat universe with a cosmological constant (Omega(0) + lambda(0) = 1), can bring the lensing estimate of sigma(8) into agreement with the COBE estimates. The models and values for sigma(8) consistent with both lensing and COBE match the estimates from the local number density of clusters and correlation functions. The conclusions are insensitive to systematic errors except for the assumption that cluster core radii are singular. If clusters with rho proportional to (r(2) + s(2))(-1) have core radii exceeding s = 15h(-1)sigma(3)(2) kpc for a cluster with velocity dispersion sigma = 10(3) sigma(3) km s(-1), then the estimates are invalid. There is, however, a fine-tuning problem in making the cluster core radii large enough to invalidate the estimates of sigma(8) while producing several lenses that do not have central or ''odd images.'' The estimated completeness of the current samples of lenses larger than 5''.0 is 20%, because neither quasar surveys nor lens surveys are optimized to find this class of lenses. RP KOCHANEK, CS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 73 TC 78 Z9 79 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 1995 VL 453 IS 2 BP 545 EP 558 DI 10.1086/176417 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TC992 UT WOS:A1995TC99200003 ER PT J AU FULLER, GA LADA, EA MASSON, CR MYERS, PC AF FULLER, GA LADA, EA MASSON, CR MYERS, PC TI THE INFRARED NEBULA AND OUTFLOW IN LYNDS-483 SO ASTROPHYSICAL JOURNAL LA English DT Article DE INFRARED, ISM, CONTINUUM; ISM, INDIVIDUAL (L483); ISM, JETS AND OUTFLOWS; ISM, STRUCTURE; RADIO LINES, ISM ID SUBMILLIMETER-WAVELENGTH OBSERVATIONS; AURIGA MOLECULAR CLOUD; EMBEDDED YOUNG STARS; FORMING DENSE CORES; DARK CLOUDS; COLLAPSE; MODELS; IMAGES; JET AB Near-infrared and submillimeter observations of IRAS 18148-0440 in the Lynds 483 dark cloud are presented. The near-infrared images show nebulous emission extending up to similar to 60'' from the IRAS position. The IRAS source is not directly detected at any wavelength and is obscured by more than 70 mag of visual extinction, Submillimeter continuum measurements indicate the presence of similar to 0.3 M. of material within about 1900 AU of the central star. At 2.2 mu m the near-infrared nebula is bipolar with approximately cylindrical lobes which extend east and west of the IRAS source and coincide with the bipolar lobes of the CO outflow from the source. The western lobe of the nebula is significantly brighter than the eastern lobe and is spatially coincident with the blueshifted CO emission from the outflow. If the nebular lobes have equal intrinsic brightness, their apparent brightness implies that the outflow has an inclination angle of similar to 40 degrees to the plane of the sky and that the density distribution within the dense gas around IRAS 18148-0440 has a radial profile steeper than r(-1). There is a bright knot of molecular hydrogen emission close to the end of the blueshifted CO with a jet like feature extending from the knot back toward the location of the embedded star. The knot of emission is thought to be tracing the region where the stellar wind is impacting the surrounding dense gas. The observations suggest that IRAS 18148-0440 is very young and that its outflow is driven by a jet from the central star. C1 UNIV MARYLAND,DEPT ASTRON,COLLEGE PK,MD 20742. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP FULLER, GA (reprint author), NATL RADIO ASTRON OBSERV,EDGEMONT RD,CHARLOTTESVILLE,VA 22903, USA. NR 33 TC 36 Z9 36 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 1995 VL 453 IS 2 BP 754 EP 760 DI 10.1086/176437 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TC992 UT WOS:A1995TC99200023 ER PT J AU DAW, A DELUCA, EE GOLUB, L AF DAW, A DELUCA, EE GOLUB, L TI OBSERVATIONS AND INTERPRETATION OF SOFT-X-RAY LIMB ABSORPTION SEEN BY THE NORMAL INCIDENCE X-RAY TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE SUN, CHROMOSPHERE; SUN, X-RAYS ID TRANSITION REGION; QUIET SUN; SOLAR; MODELS AB The Normal Incidence X-Ray Telescope (NIXT) obtained a unique set of high-resolution full-disk solar images which were exposed simultaneousy by X-rays in a passband at 63.5 Angstrom and by visible light. The perfect alignment of a photospheric visible-light image with a coronal X-ray image enables us to present observations of X-ray intensity as a function of an accurately determined height above the visible limb. The height at which the observed X-ray intensity peaks varies from 4000 km in active regions to 9000 km in quiet regions of the Sun. The interpretation of the observations stems from the previously established fact that, for the coronal loops, emission in the NIXT bandpass peaks sharply just above the footpoints. Because there is not a sharp peak in the observed X-ray intensity as a function of off-limb height, we conclude that the loop footpoints, when viewed at the limb, are obscured by absorption in chromospheric material along the line of sight. We calculate the X-ray intensity as a function of height predicted by a number of different idealizations of the solar atmosphere, and we compare these calculations with the observed X-ray intensity as a function of height. The calculations use existing coronal and chromospheric models. In order for the calculations to reproduce the observed off-limb X-ray intensities, we are forced to assume an atmosphere in which the footpoints of coronal loops are interspersed along the line of sight with cooler chromospheric material extending to heights well above the loop footpoints. We argue that the absorption coefficient for NIXT X-rays by chromospheric material is roughly proportional to the neutral hydrogen density, and we estimate an average neutral hydrogen density and scale height implied by the data. C1 SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. RP HARVARD UNIV, DEPT PHYS, CAMBRIDGE, MA 02138 USA. RI daw, adrian/D-2297-2012; DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Golub, Leon/0000-0001-9638-3082 NR 23 TC 28 Z9 28 U1 0 U2 1 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 NOV 10 PY 1995 VL 453 IS 2 BP 929 EP + DI 10.1086/176453 PN 1 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TC992 UT WOS:A1995TC99200039 ER PT J AU WEST, MJ COTE, P JONES, C FORMAN, W MARZKE, RO AF WEST, MJ COTE, P JONES, C FORMAN, W MARZKE, RO TI INTRACLUSTER GLOBULAR-CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERS, GENERAL; GALAXIES, ELLIPTIC AND LENTICULAR, CD; GALAXIES, STAR CLUSTERS; X-RAYS, GALAXIES ID LOCAL GROUP; GALAXIES; SYSTEMS; ELLIPTICALS AB Globular cluster populations of supergiant elliptical galaxies are known to vary widely, from extremely populous systems like that of UGC 9799, the centrally dominant galaxy in Abell 2052, to globular-cluster-poor galaxies such as NGC 5629 in Abell 2666. Here we propose that these variations point strongly to the existence of a population of globular clusters that are not bound to individual galaxies but, rather, move freely throughout the cores of clusters of galaxies. Such intracluster globular clusters may have originated as tidally stripped debris from galaxy interactions and mergers, or, alternatively, they may have formed in situ in some scenarios of globular cluster formation. C1 NATL RES COUNCIL CANADA,HERZBERG INST ASTROPHYS,DOMINION ASTROPHYS OBSERV,VICTORIA,BC V8X 4M6,CANADA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP WEST, MJ (reprint author), ST MARYS UNIV,DEPT PHYS & ASTRON,HALIFAX,NS B3H 3C3,CANADA. OI Forman, William/0000-0002-9478-1682 NR 35 TC 89 Z9 90 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 1995 VL 453 IS 2 BP L77 EP L80 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TC993 UT WOS:A1995TC99300007 ER PT J AU WILNER, DJ ZHAO, JH HO, PTP AF WILNER, DJ ZHAO, JH HO, PTP TI THE MOLECULAR MEDIUM OF H1413+117 - BIMA CO(3-2) AND HCO+(4-3) OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, ISM; GRAVITATIONAL LENSING; ISM, MOLECULES ID GALAXY IRAS 10214+4724; GAS; QUASAR AB We report observations of the CO (3-2) and HCO+ (4-3) lines toward H1413+117, the z = 2.56 ''cloverleaf'' quasar, obtained simultaneously with the BIMA. These observations, with beam size 2.8 x 2.4, confirm the CO (3-2) emission redshifted to 3 mm wavelength observed at lower resolution by Barvainis and coworkers. We find an upper limit to the HCO+ (4-3)/CO (3-2) intensity ratio of 0.33. This suggests that the mean density of the molecular gas, averaged over the beam, is lower than the 10(7) cm(-3) ''critical density'' of the HCO+ (4-3) line for collisional excitation. The implications of this limit depend primarily on the size scale probed by the observations. The physical conditions appear generally consistent with an average over molecular complexes in the central kiloparsecs of nearby starburst galaxies but may differ from those in the inner 300 pc of NGC 1068, the active nucleus with the best studied molecular medium. The technique of simultaneous line observation at millimeter wavelengths, which minimizes relative calibration uncertainties, is especially valuable for the broad, weak lines from high-redshift objects far which accurate absolute calibration is troublesome. We note several diagnostic molecular line pairs, redshifted into the 3 mm band, accessible to simultaneous measurement with the present generation of millimeter interferometers. RP WILNER, DJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 17 TC 19 Z9 19 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 1995 VL 453 IS 2 BP L91 EP L94 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TC993 UT WOS:A1995TC99300010 ER PT J AU LITTLER, MM LITTLER, DS AF LITTLER, MM LITTLER, DS TI CLOD SPREADING IN THE SEA-SURFACE MICROLAYER - RESPONSE SO SCIENCE LA English DT Letter RP LITTLER, MM (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,WASHINGTON,DC 20560, USA. NR 4 TC 1 Z9 2 U1 0 U2 0 PU AMER ASSOC ADVAN SCIENCE PI WASHINGTON PA 1333 H ST NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD NOV 10 PY 1995 VL 270 IS 5238 BP 897 EP 898 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA TD878 UT WOS:A1995TD87800003 ER PT J AU BAILYN, CD OROSZ, JA MCCLINTOCK, JE REMILLARD, RA AF BAILYN, CD OROSZ, JA MCCLINTOCK, JE REMILLARD, RA TI DYNAMICAL EVIDENCE FOR A BLACK-HOLE IN THE ECLIPSING X-RAY NOVA GRO-J1655-40 SO NATURE LA English DT Article ID BINARY AB X-RAY novae are binary systems in which a compact object accretes gas from a companion star. In several cases there is good evidence that the compact object is a black hole(1-5). The best evidence for the presence of a black hole comes from measuring the orbital velocity of the companion star and thereby determining the minimum mass of the compact object; when this mass exceeds the maximum mass for a neutron star (less than or similar to 3 solar masses(6)), a black hole seems the only remaining possibility. The unusual X-ray nova GRO J1655 - 40 (refs 7-10) is unique because it emits superluminal radio jets, suggesting that it is a low-luminosity counterpart to active galactic nuclei(7,9), which are thought to be powered by accretion onto a massive black hole. Here we report observations of the optical counterpart(10) of GRO J1655 - 40, which show that the system undergoes periodic eclipses; the edge-on geometry thus implied allows a determination of the companion star's true velocity. The mass of the compact object derived from the velocity curve is at least 3.16+/-0.15 solar masses, which strongly supports its identification as a black hole. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. MIT,CTR SPACE RES,CAMBRIDGE,MA 02139. RP BAILYN, CD (reprint author), YALE UNIV,DEPT ASTRON,POB 208101,NEW HAVEN,CT 06520, USA. NR 22 TC 105 Z9 105 U1 0 U2 0 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD NOV 9 PY 1995 VL 378 IS 6553 BP 157 EP 159 DI 10.1038/378157a0 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA TD759 UT WOS:A1995TD75900044 ER PT J AU MCCARTHY, MC GOTTLIEB, CA COOKSY, AL THADDEUS, P AF MCCARTHY, MC GOTTLIEB, CA COOKSY, AL THADDEUS, P TI EVIDENCE FOR NONRIGID HCCN SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID MAGNETIC-RESONANCE SPECTROSCOPY; ROTATIONAL SPECTRUM; MICROWAVE SPECTROSCOPY; DOUBLING PARAMETERS; HYPERFINE-STRUCTURE; ELECTRONIC STATES; MOLECULES; TRIPLET; CARBENE AB Rotational transitions from seven low-lying vibrational states of HCCN and five low-lying vibrational states of DCCN have been detected in the frequency range from 100 to 400 GHz with (+/-1) a sensitive millimeter-wave spectrometer. The CCH bending states nu(5)(+/-1), 2 nu(5)(+/-2), and 3 nu(5)(+/-3), and the CCN bending state nu(4)(+/-1) have been assigned. In addition, transitions from three vibrational states in HCCN and one in DCCN with zero orbital angular momentum (l) were also detected. These states in all likelihood originate from the three lowest l=0 excited states, i.e., (nu(4)+nu(5)>(-0) (nu(4) + nu(5))(+0), and 2 nu(5)(0). Analysis of the high-accuracy millimeter-wave frequency data establishes that HCCN is not a near-rigid bent molecule and intensity measurements confirm that the CCH bending states are much lower in energy than in typical well-behaved linear molecules. The low barrier to linearity in HCCN and DCCN of similar to 235 cm(-1), estimated from intensity measurements and the ab initio calculations of Malmquist et al. [Theor. Chim. Acta 73, 155 (1988)], confirms that HCCN is quasilinear. (C) 1995 American Institute of Physics. C1 UNIV HARTFORD,DIV APPL SCI,CAMBRIDGE,MA 02138. UNIV MISSISSIPPI,DEPT CHEM,UNIVERSITY,MS 38677. RP MCCARTHY, MC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI McCarthy, Michael/0000-0001-9142-0008 NR 30 TC 53 Z9 54 U1 0 U2 2 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD NOV 8 PY 1995 VL 103 IS 18 BP 7779 EP 7787 DI 10.1063/1.470193 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA TC854 UT WOS:A1995TC85400011 ER PT J AU MCCARTHY, MC GOTTLIEB, CA THADDEUS, P HORN, M BOTSCHWINA, P AF MCCARTHY, MC GOTTLIEB, CA THADDEUS, P HORN, M BOTSCHWINA, P TI STRUCTURE OF THE CCCN AND CCCCH RADICALS - ISOTOPIC-SUBSTITUTION AND AB-INITIO THEORY SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID LABORATORY MICROWAVE SPECTROSCOPY; EQUILIBRIUM GEOMETRY; ELECTRON CORRELATION; HYPERFINE-STRUCTURE; WAVE-FUNCTIONS; IRC +10216; BASIS-SETS; C3N; C4H; IDENTIFICATION AB The millimeter-wave rotational spectra of the C-13 isotopic species of the CCCCH and CCCN radicals and (CCCN)-N-15 were measured and the rotational, centrifugal distortion, and spin-rotation constants determined, as previously done for the normal isotopic species [Gottlieb et al., Astrophys, J. 275, 916 (1983)]. Substitution (r(s)) structures were determined for both radicals. For CCCN, an equilibrium structure derived by converting the experimental rotational constants to equilibrium constants using vibration-rotation coupling constants calculated ab initio was compared with a large-scale coupled cluster RCCSD(T) calculation. The calculated vibration-rotation coupling constants and vibrational frequencies should aid future investigations of vibrationally excited CCCN. Less extensive RCCSD(T) calculations are reported here for CCCCH. The equilibrium geometries, excitation energies (T-e), and dipole moments of the A(2) Pi excited electronic state in CCCN and CCCCH were also calculated. We estimate that T-e=2400+/-50 cm(-1) in CCCN, but in CCCCH the excitation energy is very small (T-e=100+/-50 cm(-1)). Owing to a large Fermi contact interaction at the terminal carbon, hyperfine structure was resolved in (CCCCH)-C-13. Measurements of the fundamental N=0-->1 rotational transition of CCCCH with a Fourier transform spectrometer described in the accompanying paper by Chen et al., yielded precise values of the Fermi contact and dipole-dipole hyperfine coupling constants in all four C-13 species. The Fermi contact interaction is approximately two times larger in CCCN, allowing a preliminary estimation of hyperfine coupling constant b(F) in (CCCN)-C-13 and (CCCN)-C-13 from the millimeter-wave rotational spectra. (C) 1995 American Institute of Physics. C1 HARVARD UNIV,DIV APPL SCI,CAMBRIDGE,MA 02138. UNIV GOTTINGEN,INST PHYS CHEM,D-37077 GOTTINGEN,GERMANY. RP MCCARTHY, MC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI McCarthy, Michael/0000-0001-9142-0008 NR 43 TC 98 Z9 100 U1 2 U2 7 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD NOV 8 PY 1995 VL 103 IS 18 BP 7820 EP 7827 DI 10.1063/1.470198 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA TC854 UT WOS:A1995TC85400016 ER PT J AU CHEN, W NOVICK, SE MCCARTHY, MC GOTTLIEB, CA THADDEUS, P AF CHEN, W NOVICK, SE MCCARTHY, MC GOTTLIEB, CA THADDEUS, P TI C-13 HYPERFINE-STRUCTURE OF THE CCCCH RADICAL SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID TRANSFORM MICROWAVE SPECTROMETER; LABORATORY DETECTION; COUPLING-CONSTANTS; VIBRONIC STRUCTURE; ELECTRONIC STATES; C2H SPECTRUM; C6H AB The fundamental (N = 1 - 0) rotational transitions of the ground (2) Sigma(+) electronic state of the four singly substituted C-13 isotopomers of CCCCH have been measured by pulsed-jet Fourier transform microwave spectroscopy. In each isotopomer this transition is split into many well-resolved hyperfine components owing to interaction between the electron spin and the molecular rotation, the proton spin, and the C-13 nuclear spin. Here, the hyperfine transition frequencies are analyzed with the higher rotational millimeter-wave frequencies described in the previous paper of McCarthy et al. to produce a precise set of rotational, centrifugal distortion, spin-rotation, and hyperfine coupling constants. In particular, the Fermi-contact interaction of the C-13 nucleus has been measured at each substituted position, yielding information on the distribution of the unpaired electron spin density along the carbon chain. The Fermi-contact constants, b(F)(C-13), of 396.8(6), 57.49(5), -9.54(2), and 18.56(4) MHz, for successive C-13 substitutions starting furthest from hydrogen indicate that the electronic structure is essentially acetylenic with alternating triple and single bonds. (C) 1995 American Institute of Physics. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. HARVARD UNIV,DIV APPL SCI,CAMBRIDGE,MA 02138. RP CHEN, W (reprint author), WESLEYAN UNIV,DEPT CHEM,MIDDLETOWN,CT 06459, USA. NR 21 TC 33 Z9 33 U1 0 U2 2 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD NOV 8 PY 1995 VL 103 IS 18 BP 7828 EP 7833 DI 10.1063/1.470199 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA TC854 UT WOS:A1995TC85400017 ER PT J AU GURWELL, MA AF GURWELL, MA TI EVOLUTION OF DEUTERIUM ON VENUS SO NATURE LA English DT Letter ID WATER RP GURWELL, MA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 4 TC 9 Z9 9 U1 0 U2 1 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD NOV 2 PY 1995 VL 378 IS 6552 BP 22 EP 23 DI 10.1038/378022b0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA TC469 UT WOS:A1995TC46900036 PM 7477280 ER PT J AU MONTALI, RJ CONNOLLY, BM ARMSTRONG, DL SCANGA, CA HOLMES, KV AF MONTALI, RJ CONNOLLY, BM ARMSTRONG, DL SCANGA, CA HOLMES, KV TI PATHOLOGY AND IMMUNOHISTOCHEMISTRY OF CALLITRICHID HEPATITIS, AN EMERGING DISEASE OF CAPTIVE NEW-WORLD PRIMATES CAUSED BY LYMPHOCYTIC CHORIOMENINGITIS VIRUS SO AMERICAN JOURNAL OF PATHOLOGY LA English DT Article ID INFECTION; ARENAVIRUS; MARMOSETS; TAMARINS; PATHOGENESIS; FEVER AB Callitrichid hepatitis is an arenavirus infection that recently emerged as a highly fatal disease of New World primates in the Callitrichidae family. As we previously reported, these primates develop hepatitis after contact with mice that are infected with variants of LCMV (LCMV(CH)), recently determined to have 86% identity with GC-P gene of the Armstrong and Western strains of LCMV. Here, we describe the histopathological lesions and tissue localization of viral antigens in confirmed cases of callitrichid hepatitis from recent outbreaks in two U.S. zoos. The liver in marmosets and tamarins with fatal infections consistently showed degeneration, necrosis, and inflammation, with variable involvement of the spleen, lymph nodes, adrenal glands, intestine, pancreas, and central nervous system. Lymphocytic choriomeningitis virus antigens were identified immunohistochemically in necrotic foci in these organs as well as in nondegenerating areas in lungs, kidneys, urinary bladder, brain, and testes. The multi-organ tropism and histological pattern of LCMV infection in marmosets and tamarins are similar to those reported for the highly virulent arenavirus that causes lassa fever in humans. Comparative studies of callitrichid hepatitis and Lassa fever would therefore be mutually beneficial for human and nonhuman primate medicine. C1 GEORGETOWN UNIV,DEPT PATHOL,WASHINGTON,DC. HENRY DOORLY ZOO,OMAHA,NE. UNIFORMED SERV UNIV HLTH SCI,DEPT PATHOL,BETHESDA,MD 20814. RP MONTALI, RJ (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT PATHOL,3001 CONNECTICUT AVE NW,WASHINGTON,DC 20008, USA. FU NIAID NIH HHS [AI-27203] NR 28 TC 17 Z9 19 U1 1 U2 3 PU AMER SOC INVESTIGATIVE PATHOLOGY, INC PI BALTIMORE PA 428 EAST PRESTON ST, BALTIMORE, MD 21202-3993 SN 0002-9440 J9 AM J PATHOL JI Am. J. Pathol. PD NOV PY 1995 VL 147 IS 5 BP 1441 EP 1449 PG 9 WC Pathology SC Pathology GA TD741 UT WOS:A1995TD74100027 PM 7485406 ER PT J AU ABOUARAB, M THOMSEN, JL FROHLICH, B LYNNERUP, N AF ABOUARAB, M THOMSEN, JL FROHLICH, B LYNNERUP, N TI HISTOLOGICAL STAINING OF SECONDARY OSTEONS SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Note C1 ODENSE UNIV,INST FORENS MED,DK-5000 ODENSE C,DENMARK. SMITHSONIAN INST,DEPT ANTHROPOL,WASHINGTON,DC 20560. UNIV COPENHAGEN,BIOL ANTHROPOL LAB,DK-2200 COPENHAGEN,DENMARK. NR 6 TC 3 Z9 3 U1 0 U2 1 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD NOV PY 1995 VL 98 IS 3 BP 391 EP 394 DI 10.1002/ajpa.1330980311 PG 4 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA TD443 UT WOS:A1995TD44300010 PM 8572161 ER PT J AU SCHMIDT, PR CHILDS, ST AF SCHMIDT, PR CHILDS, ST TI ANCIENT AFRICAN IRON PRODUCTION SO AMERICAN SCIENTIST LA English DT Article C1 NATL PK SERV,WASHINGTON,DC 20240. SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560. RP SCHMIDT, PR (reprint author), UNIV FLORIDA,DEPT ANTHROPOL,GAINESVILLE,FL 32611, USA. NR 10 TC 8 Z9 8 U1 0 U2 0 PU SIGMA XI-SCI RES SOC PI RES TRIANGLE PK PA PO BOX 13975, RES TRIANGLE PK, NC 27709 SN 0003-0996 J9 AM SCI JI Am. Scientist PD NOV-DEC PY 1995 VL 83 IS 6 BP 524 EP 533 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RZ961 UT WOS:A1995RZ96100013 ER PT J AU SMITH, RW AF SMITH, RW TI THE FONTANA HISTORY OF ASTRONOMY AND COSMOLOGY - NORTH,J SO ANNALS OF SCIENCE LA English DT Book Review RP SMITH, RW (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,DEPT SPACE HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU TAYLOR & FRANCIS LTD LONDON PI LONDON PA ONE GUNDPOWDER SQUARE, LONDON, ENGLAND EC4A 3DE SN 0003-3790 J9 ANN SCI JI Ann. Sci. PD NOV PY 1995 VL 52 IS 6 BP 624 EP 625 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA TF876 UT WOS:A1995TF87600011 ER PT J AU BARRET, D MOTCH, C PIETSCH, W AF BARRET, D MOTCH, C PIETSCH, W TI ROSAT-PSPC X-RAY OBSERVATIONS AND FOLLOW-UP OPTICAL-IDENTIFICATION OF GS1826-24 - DISCOVERY OF A LOW-MASS X-RAY BINARY WITH A BLACK-HOLE PRIMARY SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE STARS, INDIVIDUAL, GS1826-24; X-RAYS, STARS; X-RAYS, BURSTS; STARS, NEUTRON ID ABSORPTION; CATALOG AB We report on the ROSAT-PSPC all sky survey and pointed observations of GS 1826-24, performed on September-October 1990 and October 1992, respectively. The source was detected by ROSAT on both occasions, as well as in the course of a June 1992 observation of the nearby globular cluster NGC 6642. The ROSAT spectrum can be adequately described by a power law with photon index in the range 1.5 - 1.8, consistent with earlier measurements. The unabsorbed 0.1 - 2.4 keV flux measured by ROSAT remained constant around 1.3 x 10(-10) ergs s(-1) cm(-2). The total column density towards GS 1826-24 is similar to 5 X 10(21) H atoms cm(-2). No X-ray bursts were detected during any of the ROSAT observations representing a total observing time of about 8 hours. Since its discovery in 1988 by GINGA, the source was detected in 1989 by TTM and from 1990 through 1992 by ROSAT at almost the same level of X-ray intensity. This rules out the hypothesis that the source is a soft X-ray transient. We also report on the follow-up optical study of the source which led to the identification of a V = 19 optical counterpart located at a = 18h 29mn 28.2s, delta = -23 degrees 47'49''.1 (equinox 2000.0; +/- 2''). The optical faintness of the companion indicates that GS1826-24 is a low-mass X-ray binary system. We estimate the distance to be larger than 10 kpc thus implying that its persistent X-ray luminosity exceeds 10(37) ergs s(-1). GS1826-24 could be an X-ray burst source because it lies inside the large error box of an unidentified X-ray burster, and its basic X-ray properties (i.e. strong flickering, and hard spectrum in X-rays) have been observed from low-luminosity X-ray bursters. However, its rather large X-ray luminosity together with the non-detection of X-ray bursts favor the black hole hypothesis for GS1826-24. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. OBSERV ASTRON, CNRS, UA 1280, F-67000 STRASBOURG, FRANCE. MAX PLANCK INST EXTRATERR PHYS, D-85740 GARCHING, GERMANY. RP BARRET, D (reprint author), UPS, CNRS, CTR ETUD SPATIALE RAYONNEMENTS, 9 AV COLONEL ROCHE, BP 4346, TOULOUSE, FRANCE. NR 33 TC 20 Z9 20 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1995 VL 303 IS 2 BP 526 EP 534 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TE384 UT WOS:A1995TE38400025 ER PT J AU BARTELMANN, M AF BARTELMANN, M TI CLUSTER MASS ESTIMATES FROM WEAK LENSING SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE GALAXIES, CLUSTERING; COSMOLOGY, DARK MATTER; COSMOLOGY, GRAVITATIONAL LENSING ID DEEP CCD SURVEY; DARK MATTER; GALAXIES AB The reliability of cluster lens reconstruction techniques based on weak lensing is studied in terms of the accuracy of their reproduction of the total cluster mass as a function of distance from the cluster center. To do so, a variety of reconstruction algorithms is applied to synthetic lensing data created using a sample of 60 numerically modeled clusters, and the mass reconstruction is compared to the known deflector mass. The results can be summarized as follows: (1) Reconstruction algorithms which require integrations extending over the entire real plane yield unreliable results, because they give rise to boundary effects which are hard to control; mass overestimates are more likely and more substantial in this case than underestimates. (2) Reconstruction techniques which avoid these boundary effects yield reliable lower bounds to the cluster mass. The tightness of such bounds depends on the size of the field, which can be extended synthetically to improve the results considerably. For the sample of numerical cluster models, the best lower bounds, achieved by combining synthetic field extension with non-linear, finite-field reconstruction, decline from 100% to 80% of the true cluster mass going from the cluster center to an angular distance of 2.'5. The 80% error bars of the lower mass bounds are +/-10% to 15%. C1 MAX PLANCK INST ASTROPHYS, D-85740 GARCHING, GERMANY. RP BARTELMANN, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Bartelmann, Matthias/A-5336-2014 NR 28 TC 43 Z9 43 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 1995 VL 303 IS 3 BP 643 EP 655 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TG523 UT WOS:A1995TG52300008 ER PT J AU SEWARD, FD SCHMIDT, B SLANE, P AF SEWARD, FD SCHMIDT, B SLANE, P TI X-RAY-EMISSION FROM THE SUPERNOVA REMNANT CTA-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, SEYFERT; ISM, INDIVIDUAL (CTA 1); SUPERNOVA REMNANTS; X-RAYS, ISM ID INTERSTELLAR-MEDIUM; CATALOG; CLOUDS AB Three pointings of the ROSAT PSPC have been used to map the X-ray emission of CTA 1. Emission is brightest at the center and extends in all directions to the boundaries of the remnant. The luminosity is model-dependent and (at 1.4 kpc), is, L(x)(0.1-2.4 keV) = 5-8 x 10(34) ergs s(-1). Emission from the center is harder and considerably brighter than that from the rim. Spectra from several parts of the remnant are fitted with two component models. Both a two-temperature thermal model and a model consisting of a power law and a soft thermal component produce good fits to all regions. The spectra do not allow us to distinguish between a remnant with hot evaporated material at the center, or an old Crab-like remnant. Both are plausible models for CTA 1. The ROSAT HRI was used to obtain an accurate location of a bright unresolved source within the remnant. This is identified as a background active galactic nucleus. Properties of eight weaker, unresolved X-ray sources within or nearby the remnant are tabulated RP SEWARD, FD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 23 TC 33 Z9 33 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 1995 VL 453 IS 1 BP 284 EP 292 DI 10.1086/176388 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TB033 UT WOS:A1995TB03300026 ER PT J AU CURIEL, S RAYMOND, JC WOLFIRE, M HARTIGAN, P MORSE, J SCHWARTZ, RD NISENSON, P AF CURIEL, S RAYMOND, JC WOLFIRE, M HARTIGAN, P MORSE, J SCHWARTZ, RD NISENSON, P TI MOLECULAR H-2 EMISSION IN HH 47A - HUBBLE-SPACE-TELESCOPE GHRS AND FOC OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (HH 47); ISM, JETS AND OUTFLOWS; MOLECULAR PROCESSES; SHOCK WAVES; STARS, PRE-MAIN-SEQUENCE ID HERBIG-HARO OBJECTS; ULTRAVIOLET CONTINUUM; INFRARED-EMISSION; HYDROGEN EMISSION; HIGH-RESOLUTION; LINE EMISSION; SHOCK-MODELS; H2 EMISSION; CLOUDS; JET AB We present Hubble Space Telescope ultraviolet observations of the bow shock at the end of the HH 47 stellar jet obtained with the Goddard High Resolution Spectrograph (GHRS) and the Faint Object Camera (FOG). The GHRS spectrum shows three prominent emission lines of H-2 which are produced by Ly alpha fluorescence and one line that we cannot identify. Fluorescence from Ly alpha generated in the bow shock and Mach disk of HH 47A can account for the observed H-2 line fluxes provided that the H, absorbs about one-third of these Ly alpha photons. We find that our FOC image of HH 47A is made up of about 70% hydrogen two-photon continuum and about 30% fluorescent H-2 emission. This image closely resembles optical [S II] and H alpha images of HH 47A but differs significantly from H, images of the region taken at near-infrared wavelengths. This is because the two-photon continuum and the Ly alpha photons which drive H-2 fluorescence both originate in the Hat-emitting gas, and the Ly alpha mean free path is small. The presence of molecular hydrogen in HH 47A is difficult to understand. If the H-2 forms in a dense region between the bow shock and the Mach disk, then the emission should be significantly more blueshifted than observed. Models that excite H-2 using C-shocks or magnetic precursors assume that molecular hydrogen exists in the preshock gas of HH 47A. However, this gas lies within the wake of a previous high-velocity ejection from the star and is exposed to ionizing radiation from the Gum Nebula, so we would not expect to find any H-2 in this region. Numerical calculations indicate that the UV H-2 line emission may be produced by either reformed H-2 molecules in the region between the bow shock and the Mach disk or from a C-shock or magnetic precursor, while the near-infrared H-2 emission observed in HH 47A arises mainly from C-shock or magnetic precursor along the wings of the bow shock. We propose that the scenario that best explains the current results is one in which the HH 47A bow shock is running into a clump of molecular gas which could be either comoving with the preshock gas or nearly stationary with respect to the ambient cloud, primary on its more distant face. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV CALIF BERKELEY, DEPT ASTRON, BERKELEY, CA USA. NASA, AMES RES CTR, MOFFETT FIELD, CA 94035 USA. RICE UNIV, HOUSTON, TX 77251 USA. SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. UNIV MISSOURI, DEPT PHYS & ASTRON, ST LOUIS, MO 63121 USA. NR 30 TC 32 Z9 32 U1 0 U2 0 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 NOV 1 PY 1995 VL 453 IS 1 BP 322 EP 331 DI 10.1086/176392 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TB033 UT WOS:A1995TB03300030 ER PT J AU KUMAR, P NARAYAN, R LOEB, A AF KUMAR, P NARAYAN, R LOEB, A TI ON THE INTERACTION OF CONVECTION AND ROTATION IN STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE CONVECTION; STARS, ROTATION; SUN, INTERIOR; SUN, ROTATION; TURBULENCE ID MIXING-LENGTH CONVECTION AB We use a recent formulation of turbulent convection to study rotation in convective media. The formalism is based on the Boltzmann equation for the distribution function of convective blobs and represents an extension of mixing-length theory. The details of the interactions between blobs are introduced through a model of the collision term. We obtain the stress tenser and other correlation functions of a rotating convective fluid from the second moments of the Boltzmann equation. In steady state, and in the absence of large-scale circulation, the Reynolds stress must vanish. We use this condition to determine the equilibrium rotation profile in the equatorial plane of convective stars. Even in the simple case of isotropic scattering of convective blobs, the equilibrium rotation profile is not necessarily solid body rotation; solid body rotation arises only when the scattering is perfectly elastic, whereas in the opposite limit of completely inelastic scattering, the equilibrium profile consists of a uniform distribution of specific angular momentum. If the scattering is allowed to be anisotropic, then we find an even wider range of equilibrium rotation profiles; in particular, we find that for certain choices of the parameters it is possible to have a rising rotation profile, similar to that observed in the equatorial plane of the Sun. In phenomenological models of the solar rotation, the Reynolds stress is written in a generalized form which includes anisotropic viscosity and Lambda-terms, the latter giving a nonzero shear stress even when there is no velocity shear. Our analysis gives rise to both anisotropic viscosity and Lambda-terms quite naturally and shows that both effects should be generically present. We provide analytical expressions for these effects in terms of the parameters of the interblob scattering function. We also consider the effect of rotation on the condition for convective instability. According to linear analysis, convection in the equatorial plane is suppressed if the epicyclic frequency exceeds the imaginary part of the Brunt-Vaisala frequency. However, when the scattering of blobs is included in the analysis, we show that the stability condition is modified, and there can be a new kind of instability even when linear theory predicts stability. This new instability has a zero growth rate when the scattering frequency goes to zero but has a growth time comparable to the convection time when the collision frequency is comparable to the Brunt-Vaisala frequency. Thus, this instability is a secular instability and possibly a finite amplitude instability, which arises primarily as a result of the scattering of eddies. We discuss the generalization of these results for regions away from the equatorial plane. Finally, we show that the direction of angular momentum flow can be very different in the linear limit compared to fully developed convection. When the convective perturbations are infinitesimally small, corresponding to the linear limit, we show that the angular momentum how is in such a direction as to drive the system toward a constant angular momentum configuration. This is in agreement with the result obtained by Ryu & Goodman through linear mode analysis of a Keplerian accretion disk. However, in saturated convection, when the perturbations are fully nonlinear, the angular momentum flow is such as to drive the system toward the equilibrium rotation profiles described above. Thus, the angular momentum flux is outward in the case of fully developed convection in a Keplerian disk. This means that convection is a viable mechanism to generate viscosity in accretion disks. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP KUMAR, P (reprint author), MIT,DEPT PHYS,CAMBRIDGE,MA 02139, USA. NR 24 TC 21 Z9 21 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 1995 VL 453 IS 1 BP 480 EP 494 DI 10.1086/176409 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TB033 UT WOS:A1995TB03300047 ER PT J AU KENYON, SJ HARTMANN, L AF KENYON, SJ HARTMANN, L TI PRE-MAIN-SEQUENCE EVOLUTION IN THE TAURUS-AURIGA MOLECULAR CLOUD SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE INFRARED, STARS; ISM, CLOUDS; STARS, EVOLUTION; STARS, LUMINOSITY FUNCTION, MASS FUNCTION; STARS, PRE-MAIN-SEQUENCE ID YOUNG STELLAR OBJECTS; ORION POPULATION STARS; OPHIUCHI DARK CLOUD; LOW-MASS STARS; SPECTRAL ENERGY-DISTRIBUTIONS; EMISSION-LINE STARS; X-RAY SOURCES; SUBMILLIMETER-WAVELENGTH OBSERVATIONS; MODEL SCATTERING ENVELOPES; FORMING DENSE CORES AB This paper analyzes optical and infrared photometry of pre-main-sequence stars in the Taurus-Auriga molecular cloud. More than half of the stars in our sample have excess near-infrared emission. The near-infrared excesses correlate very well with other measures of activity, such as Hot emission, ultraviolet excess emission, millimeter continuum emission, and the presence of reflection nebulae and molecular outflows. The infrared colors and the ratio of far-infrared to bolometric luminosity display a smooth progression from the most deeply embedded protostars to optically visible T Tauri stars. Infalling envelope models account for the colors of protostars; simple disk models similarly reproduce the colors of many T Tauri stars. Both the stellar birth line and a 10(5) yr isochrone provide a reasonable upper envelope to the luminosity distribution of optically visible stars in the H-R diagram. Only a few stars in the cloud have apparent ages exceeding 2-3 x 10(6) yr, as derived from detailed stellar evolution calculations. The distribution of stars in the H-R diagram indicates that the cloud has formed stars at a roughly constant rate for the past 1-2 x 10(6) yr. Analyses of the J- and K-luminosity functions support this conclusion. Within the uncertainties, the observed mass distribution for optically visible stars agrees with a Miller-Scale initial mass function. Source statistics imply a lifetime of 1-2 X 10(5) yr for the typical protostar in Taurus-Auriga. There is no evidence, however, that these sources lie on the stellar birth line. Indeed, the protostellar luminosity function is essentially identical to the luminosity function derived for optically visible T Tauri stars in the cloud. These results provide some support for the evolutionary sequence-embedded protostar --> T Tauri star with a circumstellar disk --> T Tauri star without a circumstellar disk-currently envisioned in standard models of low-mass star formation. Source statistics and infrared color-color diagrams demonstrate that pre-main-sequence stars develop bluer colors and display less evidence for circumstellar material with time. The data show little evidence, however, for the luminosity evolution expected along the proposed evolutionary sequence. Time-dependent accretion during the infall phase may account for the low luminosity of Taurus-Auriga protostars; this hypothesis requires more tests. RP KENYON, SJ (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 261 TC 1281 Z9 1284 U1 1 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 1995 VL 101 IS 1 BP 117 EP 171 DI 10.1086/192235 PG 55 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RZ600 UT WOS:A1995RZ60000005 ER PT J AU ROTH, TL MUNSON, L SWANSON, WF WILDT, DE AF ROTH, TL MUNSON, L SWANSON, WF WILDT, DE TI HISTOLOGICAL CHARACTERISTICS OF THE UTERINE ENDOMETRIUM AND CORPUS-LUTEUM DURING EARLY EMBRYOGENESIS AND THE RELATIONSHIP TO EMBRYONIC MORTALITY IN THE DOMESTIC CAT SO BIOLOGY OF REPRODUCTION LA English DT Article ID INTRAUTERINE ARTIFICIAL-INSEMINATION; CHEETAH ACINONYX-JUBATUS; FERTILIZATION INVITRO; ESTRADIOL RECEPTOR; OVARIAN ACTIVITY; PANTHERA-TIGRIS; LH-RELEASE; PROGESTERONE; PREGNANCY; OVIDUCT AB Pregnancy rates are low and litter sizes generally small when assisted reproduction techniques are used in gonadotropin-treated felid (cat) species. A prerequisite to determining whether or not abnormal morphological changes in the uterine lumen or corpus luteum (CL) are related to this reproductive failure is the documentation of normal histological kinetics during natural embryogenesis. This study characterized the histological changes of the endometrium and ovarian CL during the early stages of preimplantation embryonic development in the naturally estrous, mated queen. The purpose was to 1) develop a system for dating the cat endometrium and CL of early pregnancy; 2) document the frequency of abnormal uterine and CL histology under natural mating conditions; and 3) compare histological traits of queens producing good-vs. poor-quality embryos, Naturally estrous, mated queens were ovariohysterectomized at 64 h (n = 8), 76 h (n = 11), 100 h (n = 8), 124 h (n = 7), 148 h (n = 6), or 480 h (n = 8) after first copulation, Embryos collected from oviductal and uterine flushings were graded for quality, and uteri and ovaries were fixed in formalin. Fixed tissue sections were stained and multiple histological traits described for each uterine (endometrial height, endometrial vacuolation, percentage of glandular cells with subnuclear vacuoles, number of mitoses, nuclear-to-cytoplasmic ratio) and ovarian (presence of tertiary follicles, vacuolation of luteal cell cytoplasm, luteal cell shape) sample. Modest histological changes were observed at each time point, and these were documented in detail. The most prominent modifications occurred at 124 h after first copulation and included thickening of the endometrium, straightening of the glands, increased cytoplasmic vacuolation, and increased epithelial height. Of 15 queens failing to produce good-quality embryos, only 4 expressed unusual histological characteristics; and 3 of 25 queens producing only high-quality embryos exhibited abnormal uterine or CL cellular integrity. Therefore, aberrant histological changes are not primarily responsible for failure of the naturally estrous, mated queen to produce good-quality embryos, Furthermore, a normative database now is available to date the endometrium and CL of early pregnancy and to examine the impact of exogenous gonadotropins and assisted techniques on uterine/CL structure and function. C1 UNIV TENNESSEE,COLL VET MED,DEPT PATHOL,KNOXVILLE,TN. RP ROTH, TL (reprint author), NATL ZOOL PK,SMITHSONIAN INST,DEPT REPROD PHYSIOL,CONSERVAT & RES CTR,1500 REMOUNT RD,FRONT ROYAL,VA, USA. FU NICHD NIH HHS [R01 HD 23853] NR 37 TC 17 Z9 18 U1 1 U2 9 PU SOC STUDY REPRODUCTION PI MADISON PA 1526 JEFFERSON ST, MADISON, WI 53711-2106 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD NOV PY 1995 VL 53 IS 5 BP 1012 EP 1021 DI 10.1095/biolreprod53.5.1012 PG 10 WC Reproductive Biology SC Reproductive Biology GA TA200 UT WOS:A1995TA20000004 PM 8527503 ER PT J AU SWANSON, WF ROTH, TL BROWN, JL WILDT, DE AF SWANSON, WF ROTH, TL BROWN, JL WILDT, DE TI RELATIONSHIP OF CIRCULATING STEROID-HORMONES, LUTEAL LUTEINIZING-HORMONE RECEPTOR AND PROGESTERONE CONCENTRATION, AND EMBRYONIC MORTALITY DURING EARLY EMBRYOGENESIS IN THE DOMESTIC CAT SO BIOLOGY OF REPRODUCTION LA English DT Article ID SEXUAL-BEHAVIOR; OVARIAN ACTIVITY; ESTROUS-CYCLE; GONADOTROPIN RECEPTORS; INVITRO FERTILIZATION; EARLY-PREGNANCY; LH-RELEASE; BITCH; PLASMA; ESTRUS AB Serum hormones, corpus luteum (CL) progesterone, and CL LH receptors were characterized and interrelated to ovarian follicle and CL number and preimplantation embryo quality/survival in the cat, Blood samples were collected from queens ovariohysterectomized at 64 (n = 7), 76 (n = 11), 100 (n = 8), 124 (n = 7), 148 (n = 6), or 480 (n = 8) h after first copulation (3-times-daily matings on Days 2 and 3 of estrus). Ovarian CL were enucleated, weighed, and bisected; one hemi-CL was assayed for progesterone and the other for LH receptors, Serum was assessed for estradiol-17 beta and progesterone. Serum estradiol-17 beta concentrations did not return (p > 0.05) to baseline (similar to 20 pg/ml) until 124 h after first copulation, whereas serum progesterone began to increase (> 1 ng/ml) by 76 h, was elevated (p < 0.05) by 124 h, and continued to rise thereafter. Serum progesterone was highly correlated with CL mass and LH receptor and progesterone concentration (range, r = 0.69-0.82; p < 0.01). CL progesterone and LH receptor concentrations were similar (p > 0.05) at 64 and 76 h, and both increased (p < 0.05) at subsequent time intervals and were correlated closely (r = 0.65; p < 0.01), Although ovarian CL were distinct and well organized by 64 h, pronounced elevations in serum progesterone and CL LH receptors and progesterone did not occur until at least 36 h later. The rapid increase in serum progesterone concentrations between 100 and 148 h was related to accelerated LH receptor synthesis and CL progesterone production and not entirely to enhanced CL growth. There were few discernible differences in hormonal and luteal traits between queens with viable embryos or high implantation rates and females with degenerate embryos, unfertilized oocytes, or poor implantation, with one consistent exception, Queens with poor fertility in the 64-, 76-, and 100-h groups had higher (p < 0.05) CL progesterone concentrations than cats with viable embryos, suggesting that altered follicular dynamics (perhaps premature luteinization) adversely impacted oocyte/embryo quality. In summary, there is a direct and significant relationship between circulating progesterone, CL mass, and CL progesterone/LH receptors during preimplantation embryogenesis in the domestic cat, The temporal kinetics of these events are remarkably similar among mated females and, with the possible exception of CL progesterone, appear unrelated to embryonic viability. C1 NATL ZOOL PK,SMITHSONIAN INST,CONSERVAT & RES CTR,FRONT ROYALE,VA. FU NICHD NIH HHS [HD 23853] NR 47 TC 24 Z9 27 U1 1 U2 6 PU SOC STUDY REPRODUCTION PI MADISON PA 1526 JEFFERSON ST, MADISON, WI 53711-2106 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD NOV PY 1995 VL 53 IS 5 BP 1022 EP 1029 DI 10.1095/biolreprod53.5.1022 PG 8 WC Reproductive Biology SC Reproductive Biology GA TA200 UT WOS:A1995TA20000005 PM 8527504 ER PT J AU BROOKS, DR MCLENNAN, DA CARPENTER, JM WELLER, SG CODDINGTON, JA AF BROOKS, DR MCLENNAN, DA CARPENTER, JM WELLER, SG CODDINGTON, JA TI SYSTEMATICS, ECOLOGY, AND BEHAVIOR - INTEGRATING PHYLOGENETIC PATTERNS AND EVOLUTIONARY MECHANISMS SO BIOSCIENCE LA English DT Article ID DIMORPHIC NUPTIAL COLORATION; GASTEROSTEUS-ACULEATUS L; SEXUAL SELECTION; PHYSALAEMUS-PUSTULOSUS; PARENTAL CARE; SENSORY EXPLOITATION; TEMPORAL CHANGES; FISHES; COMMUNICATION; FROG C1 AMER MUSEUM NAT HIST,DEPT ENTOMOL,NEW YORK,NY 10024. UNIV CALIF IRVINE,DEPT ECOL & EVOLUTIONARY BIOL,IRVINE,CA 92717. SMITHSONIAN INST,DEPT ENTOMOL,WASHINGTON,DC 20560. RP BROOKS, DR (reprint author), UNIV TORONTO,DEPT ZOOL,25 HARBORD ST,TORONTO,ON M5S 1A1,CANADA. NR 49 TC 13 Z9 13 U1 1 U2 4 PU AMER INST BIOL SCI PI WASHINGTON PA 730 11TH STREET, NW, WASHINGTON, DC 20001-4521 SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD NOV PY 1995 VL 45 IS 10 BP 687 EP 695 DI 10.2307/1312674 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA TB495 UT WOS:A1995TB49500008 ER PT J AU Hines, AH Ruiz, GM AF Hines, AH Ruiz, GM TI Temporal variation in juvenile blue crab mortality: Nearshore shallows and cannibalism in Chesapeake Bay SO BULLETIN OF MARINE SCIENCE LA English DT Article; Proceedings Paper CT Symposium on Blue Crab Recruitment - Environmental Control and Population Regulation, at the Estuarine-Research-Federation Conference CY NOV 16, 1993 CL HILTON HEAD ISL, SC SP Estuarine Res Federat ID LOBSTER PANULIRUS-CYGNUS; CALLINECTES-SAPIDUS; HABITAT SELECTION; PREDATION RATES; STRUCTURED POPULATIONS; RECRUITMENT DYNAMICS; CANCER-MAGISTER; YORK RIVER; ABUNDANCE; SETTLEMENT AB Adult abundance is determined by both recruitment and survival of juveniles. Blue crabs exhibit a distinct population size-structure reflecting seasonal cycles of recruitment and growth in the Rhode River, a subestuary lacking submerged vegetation in central Chesapeake Bay. Seasonally shifting modes in the size-structure, corresponding to juvenile, prepubertal and mature crabs, allowed trawl catches to be partitioned into 0+ and 1+ year classes of the crabs' 2-3 year life span. Fluctuations in the annual abundance of the year classes during 1988-1993 indicated that abundance of 0+ juveniles was not a good predictor of 1+ year-class abundance. We used tethering techniques to assess sources of, and temporal variation in, juvenile blue crab mortality as a function of water depth in the nearshore shallows of the subestuary. Laboratory experiments and analysis of remains of crabs tethered in the field indicated that cannibalism by large blue crabs was the source of 75-97% of mortality of juveniles. Crabs 30-50 mm CW suffered significantly higher mortality than 50-70 mm crabs. Mortality of tethered juveniles was significantly lower in shallow (15 cm) than deep (>70 cm) water. Mortality rates did not differ between day and night periods. Mortality of tethered juvenile blue crabs was high (40-90% per day) and exhibited significant seasonal and annual variation from 1989-1993; and water depth showed significant interaction effects with these components of temporal variability. Multiple regression analysis indicated that water temperature, abundance of 1+ year-class crabs in deep-water trawls, and abundance of 0+ year-class crabs in nearshore seines accounted for 82% of the annual variation in mortality of juveniles tethered at medium (40 cm) depth. Together, these results emphasize the importance of the nearshore shallows and body size as a crucial refuges for juvenile blue crabs encountering intense, but temporally variable cannibalism by large crabs. Juvenile mortality may be an important variable regulating population dynamics of blue crabs. RP Hines, AH (reprint author), SMITHSONIAN ENVIRONM RES CTR,POB 28,EDGEWATER,MD 21037, USA. NR 56 TC 83 Z9 86 U1 1 U2 8 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD NOV PY 1995 VL 57 IS 3 BP 884 EP 901 PG 18 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA TN246 UT WOS:A1995TN24600026 ER PT J AU Dittel, AI Hines, AH Ruiz, GM Ruffin, KK AF Dittel, AI Hines, AH Ruiz, GM Ruffin, KK TI Effects of shallow water refuge on behavior and density-dependent mortality of juvenile blue crabs in Chesapeake Bay SO BULLETIN OF MARINE SCIENCE LA English DT Article; Proceedings Paper CT Symposium on Blue Crab Recruitment - Environmental Control and Population Regulation, at the Estuarine-Research-Federation Conference CY NOV 16, 1993 CL HILTON HEAD ISL, SC SP Estuarine Res Federat ID PREDATOR-PREY INTERACTIONS; CALLINECTES-SAPIDUS; SPECIES INTERACTIONS; POPULATION-DYNAMICS; FORAGING MINNOWS; MARINE PREDATOR; HABITAT USE; YORK RIVER; ABUNDANCE; RISK AB This study experimentally tested aspects of behavior and density-dependent mortality of juvenile blue crabs utilizing nearshore shallow water as a refuge from cannibalism by large blue crabs. In a large laboratory tank with a depth gradient, individual juvenile blue crabs shifted their depth utilization from deep and medium depths to shallow water in the presence of a large crab, but not in the absence of another crab or in the presence of another small crab. Survival of juvenile crabs preyed upon by large crabs was significantly higher in laboratory tanks with depth gradients providing a shallow refuge than in lab tanks without depth gradients. In the laboratory, proportional mortality of juvenile crabs was inversely density-dependent, indicating a type II functional response of large crabs irrespective of the presence or absence of a shallow water refuge. In a non-vegetated subestuary of Chesapeake Bay, survival of tethered juveniles was significantly higher in shallow (30 cm) than deep (70 cm) water of a nearshore zone, where cannibalistic large blue crabs were their major source of mortality. Proportional mortality in the field was also inversely density-dependent in both shallow and deep water. The persistence of a type II functional response of predators in our laboratory and field experiments indicates that shallow water provides a significant but partially effective refuge to juvenile blue crabs, although such inversely density-dependent mortality patterns indicate a potentially unstable predator-prey interaction. Under intense predation pressure from cannibalistic large crabs, this partially effective refuge in the nearshore shallows potentially grants juvenile crabs a crucial reduction in mortality during their first year of life until they grow to a size large enough to obtain an absolute refuge from predation. C1 SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. UNIV DELAWARE,COLL MARINE STUDIES,LEWES,DE 19958. NR 60 TC 64 Z9 65 U1 1 U2 9 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD NOV PY 1995 VL 57 IS 3 BP 902 EP 916 PG 15 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA TN246 UT WOS:A1995TN24600027 ER PT J AU SMITH, BJ AF SMITH, BJ TI UNTITLED SO COLLEGE & RESEARCH LIBRARIES LA English DT Letter RP SMITH, BJ (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ASSN COLL RES LIBR PI CHICAGO PA 50 E HURON ST, CHICAGO, IL 60611 SN 0010-0870 J9 COLL RES LIBR JI Coll. Res. Libr. PD NOV PY 1995 VL 56 IS 6 BP 555 EP 555 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA TF598 UT WOS:A1995TF59800009 ER PT J AU Barboza, PS AF Barboza, PS TI Nutrient balances and maintenance requirements for nitrogen and energy in desert tortoises (Xerobates agassizii) consuming forages SO COMPARATIVE BIOCHEMISTRY AND PHYSIOLOGY A-PHYSIOLOGY LA English DT Article DE reptile; protein; amino acid; mineral; calcium; phosphorus; sodium; potassium; magnesium ID SEASONAL ENVIRONMENT; METABOLISM; WOMBATS; FIBER AB The North American tortoise Xerobates agassizii (synonym: Gopherus agassizii) consumes herbage and grasses produced from low and variable desert rains, Utilization of Sphaeralcea ambigua foliage and the grass Schismus barbatus were studied in 8 adult tortoises (2.3 kg body mass), The herbage contained more N but less fiber than the grass, Tortoises ingested and digested more dry matter and energy from herbage than grass, intakes and retention of N were greater from the herbage than the grass, but amino acid proportions and true N digestibilities were similar between diets, Herbage contained more Ca than grass, especially in relation to P (Ca:P 14.5 vs. 1.9), but this was ameliorated by lower absorption of Ca from the herbage, K intakes were greater from the herbage than the grass and associated with the digestive loss of Mg from herbage. Low Na content of both forages resulted in net losses of Na, Maintenance requirements for dietary N (14.4 mg . kg-0.75 . d(-1)) and for digestible energy (19.9 kJ . kg-0.75 . d(-1)) were lower than estimates for other herbivorous reptiles and consistent with the utilization of desert pastures where quality and abundance may be low and erratic. Modest requirements for these and other nutrients may enable desert tortoises to tolerate temporal deficiencies, but these must ultimately be corrected by a wider dietary selection, Consequently, both diversity and abundance of pasture growth may be critical to long-term nutrient balances of this threatened species. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. NR 36 TC 13 Z9 14 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0300-9629 J9 COMP BIOCHEM PHYS A JI Comp. Biochem. Physiol. A-Physiol. PD NOV-DEC PY 1995 VL 112 IS 3-4 BP 537 EP 545 DI 10.1016/0300-9629(95)02023-3 PG 9 WC Biochemistry & Molecular Biology; Physiology; Zoology SC Biochemistry & Molecular Biology; Physiology; Zoology GA TP104 UT WOS:A1995TP10400022 ER PT J AU POULIN, B LEFEBVRE, G AF POULIN, B LEFEBVRE, G TI ADDITIONAL INFORMATION ON THE USE OF TARTAR EMETIC IN DETERMINING THE DIET OF TROPICAL BIRDS SO CONDOR LA English DT Article DE REGURGITATION; TARTAR EMETIC; DIET; TROPICAL LAND BIRDS; PANAMA AB We evaluated the effect and effectiveness of antimony potassium tartrate (tartar emetic) on 137 bird species from 29 families and subfamilies from one humid forest site and two mangrove sites in central Panama. Of the 2,656 birds forced to regurgitate, we obtained 1,942 diet samples comprising 12,608 taxonomically identified items. Seventy birds (2.6%) died after administration of the emetic, with some Trochilidae (Phaethornis) and Pipridae (Pipra, Manacus) being especially sensitive to the chemical. No significant differences were found between the number of items regurgitated and that found in stomach contents. However, regurgitations using tartar emetic appeared to be more efficient than analyses of feces to investigate food preference. We also provide details on how to process samples of hummingbirds to permit pollen (flower) identification. RP POULIN, B (reprint author), SMITHSONIAN TROP RES INST,POB 2072,BALBOA,PANAMA. NR 15 TC 22 Z9 22 U1 1 U2 4 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0010-5422 J9 CONDOR JI Condor PD NOV PY 1995 VL 97 IS 4 BP 897 EP 902 DI 10.2307/1369529 PG 6 WC Ornithology SC Zoology GA TJ719 UT WOS:A1995TJ71900003 ER PT J AU CONDIT, R HUBBELL, SP FOSTER, RB AF CONDIT, R HUBBELL, SP FOSTER, RB TI MORTALITY-RATES OF 205 NEOTROPICAL TREE AND SHRUB SPECIES AND THE IMPACT OF A SEVERE DROUGHT SO ECOLOGICAL MONOGRAPHS LA English DT Article DE DEMOGRAPHY; DROUGHT; EL NINO; FOREST; MORTALITY; NEOTROPICS; TREES; TROPICAL ID TROPICAL RAIN-FORESTS; SHORT-TERM DYNAMICS; POPULATION-DYNAMICS; ENGELMANN SPRUCE; LODGEPOLE PINE; GROWTH; CANOPY; RECRUITMENT; MALAYSIA; DIVERSITY AB Mortality rates of 205 tree and shrub species were estimated during two intervals, 1982-1985 and 1985-1990, in two size classes, 1-10 and greater than or equal to 10 cm in diameter, in a 50-ha census plot in tropical moist forest on Barro Colorado Island in Panama. The severe dry season of 1983 was the focus of the study, since prior observations had demonstrated that it caused mortality in the forest. Here we document that forest-wide mortality was approximate to 3%/yr during the drought interval but only 2%/yr during the period afterwards, and that excess mortality during the first interval amounted to 2% of stems in the larger size class and 1% in the smaller Overall, just under 70% of all species had higher mortality during the first census interval, but not all species were equally affected. Canopy trees had significantly higher mean mortality rates during 1982-1985 than during 1985-1990, but treelets and shrubs showed no or slight differences. This was counter to our prediction that species with short root systems would suffer more from a long drought. Shrubs did, however, have higher mortality rates than trees and treelets during both census intervals. We also evaluated mortality rates for subgroups of species that specialized on different microhabitats in the forest. As we predicted, colonist species (those associated with light gaps) had higher mortality rates than generalist species, 7-10%/yr compared to 2-4%/yr, but only in the smaller size class. Unexpectedly, colonizers had similar mortality rates as non-colonizers in the larger size class. Gap colonizers and generalist species were similarly affected by the drought-both had elevated mortality during 1982-1985. Species whose distributions were associated with moister soils (on the slopes around the island's plateau or in a swamp in the midst of the 50-ha plot) also had elevated mortality during the drought period, but no more so than generalist species. This was counter to our prediction that species from moist microhabitats would suffer more during an extended drought than generalists. Understory treelets that were slope specialists had higher mortality than generalists during both census intervals, but not large trees that were slope specialists. Our conclusions emphasize diversity as well as pattern. Every trend we illustrated had well-documented exceptions: large trees with lower mortality during the drought period, for example. Clearly, accurate predictions about how tropical forests will respond to climatic perturbations will require much detailed information from many species. C1 PRINCETON UNIV,DEPT ECOL EVOLUT & BEHAV,PRINCETON,NJ 08544. FIELD MUSEUM NAT HIST,DEPT BOT,CHICAGO,IL 60605. RP CONDIT, R (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO,AA 34002, USA. NR 64 TC 394 Z9 419 U1 8 U2 81 PU ECOLOGICAL SOC AMER PI TEMPE PA ARIZONA STATE UNIV CENTER ENVIRONMENTAL STUDIES, TEMPE, AZ 85287 SN 0012-9615 J9 ECOL MONOGR JI Ecol. Monogr. PD NOV PY 1995 VL 65 IS 4 BP 419 EP 439 DI 10.2307/2963497 PG 21 WC Ecology SC Environmental Sciences & Ecology GA TC858 UT WOS:A1995TC85800002 ER PT J AU THOMPSON, KV AF THOMPSON, KV TI ONTOGENY OF FLEHMEN IN SABLE ANTELOPE, HIPPOTRAGUS-NIGER SO ETHOLOGY LA English DT Article ID DOMINANCE AB Flehmen, a conspicuous posture characterized by eversion of the upper lip, facilitates the transfer of nonvolatile urinary chemicals to the vomeronasal organ and therefore has been implicated in the control of reproduction in ungulates. The ontogeny of urine sampling and flehmen was investigated in semi-free-ranging sable antelope, Hippotragus niger, at the National Zoological Park's Conservation and Research Center because behavioural evidence suggests that flehmen is a mechanism of reproductive synchronization among females. During the first year of life, flehmen rates increased with age in both sexes. Flehmen rates of female calves equalled those of adult females by 4 months of age. Male calves first exhibited flehmen at younger ages than did female calves and showed greater increases in flehmen rate during development. Both sexes exhibited flehmen primarily after sampling urine of female conspecifics as it was being voided. During the first 2 months of life, sable antelope preferred to sample urine of other calves, but by 1 year of age adult females were the preferred targets. Females approaching sexual maturity preferred to sample urine from postpartum females (presumably resuming oestrous cycling) rather than from pregnant females, as expected if they were attempting to synchronize oestrus with experienced females. Results are consistent with the hypothesis that flehmen serves to coordinate reproduction among females and further suggest that flehmen may affect reproductive maturation. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. RI Thompson, Katerina/B-6146-2009 NR 23 TC 0 Z9 0 U1 0 U2 1 PU BLACKWELL WISSENSCHAFTS VERLAG GMBH PI BERLIN PA KURFURSTENDAMM 57, D-10707 BERLIN, GERMANY SN 0179-1613 J9 ETHOLOGY JI Ethology PD NOV PY 1995 VL 101 IS 3 BP 213 EP 221 PG 9 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA TF875 UT WOS:A1995TF87500004 ER PT J AU MANDERNACK, KW POST, J TEBO, BM AF MANDERNACK, KW POST, J TEBO, BM TI MANGANESE MINERAL FORMATION BY BACTERIAL-SPORES OF THE MARINE BACILLUS, STRAIN SG-1 - EVIDENCE FOR THE DIRECT OXIDATION OF MN(II) TO MN(IV) SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID DEEP-SEA; FERROMANGANESE NODULES; MICROBIAL OXIDATION; HYDROTHERMAL VENTS; OXIDE DEPOSITION; STATE; SEDIMENTS; BUSERITE; ACCUMULATION; NUCLEATION AB The spores of a marine Bacillus bacterium, strain SG-1, are able to oxidize Mn(II) over a wide range of temperatures (0-80 degrees C) and Mn(II) concentrations (<1 nM to >25 mM), in both low ionic strength N-(2-hydroxyethyl)piperazine-N'-ethanesulfonic acid (HEPES) buffer (HB) and in HEPES-buffered seawater (SW). Using SG-1 spores as a catalyst for manganese mineral formation, and by varying the temperature and Mn(II) concentration at pH 7.4-8.0, a variety of manganese oxide and manganate minerals were formed under environmentally relevant conditions in HB and SW. In general, mixed phases of lower valence state minerals (hausmannite, Mn3O4; feitknechtite, beta MnOOH; and manganite, gamma MnOOH) formed in HB and SW at high Mn(II) concentrations (10 mM initial), or at high temperatures (70 degrees C), by two weeks. beta MnOOH was favored at low temperatures (3 degrees C) and Mn3O4 at higher temperatures (55-70 degrees C). After 1 year of aging, gamma MnOOH became the dominant or only mineral present at 25 and 55 degrees C. At lower Mn(II) concentrations (initial concentrations less than or equal to 100 mu M in HB and less than or equal to 1 mM in SW), Mn(IV) minerals precipitated. In HB the Mn(IV) minerals most often resembled sodium buserite, evidenced by collapse of a 10 to 7 Angstrom phase with air drying at room temperature. In SW both buserite and Mg-rich noncollapsible 10 Angstrom manganates were formed. The Mg-rich 10 Angstrom manganates did not collapse to 7 Angstrom even with baking at 100 degrees C. The oxidation state of the minerals were generally higher in SW (as high as 3.7) than in HB (3.2). Mn(IV) minerals also formed at higher Mn(II) concentrations in SW than in HB. These observed differences between SW and HB may have resulted from differences in the chemical milieu, or because of the marine adapted physiology of the bacterial spores. Under a variety of conditions (HB and SW, 3-55 degrees C) Mn(IV) mineral formation often occurred at pH and Mn(II) concentrations too high to be favorable for the disproportionation of Mn3O4, or beta MnOOH to Mn(IV). The results strongly suggest direct oxidation of Mn(II) to Mn(IV) by SG-1 spores without lower valence intermediates. Considering the environmental relevance of these experiments, direct oxidation of Mn(II) to Mn(IV) by microbes is probably a common process in natural environments. C1 UNIV CALIF SAN DIEGO,SCRIPPS INST OCEANOG,DIV MARINE BIOL RES,LA JOLLA,CA 92093. UNIV CALIF SAN DIEGO,SCRIPPS INST OCEANOG,CTR MARINE BIOTECHNOL & BIOMED,LA JOLLA,CA 92093. SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560. RI Tebo, Bradley/A-8432-2017 OI Tebo, Bradley/0000-0002-6301-4325 NR 59 TC 106 Z9 114 U1 2 U2 36 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV PY 1995 VL 59 IS 21 BP 4393 EP 4408 DI 10.1016/0016-7037(95)00298-E PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA TE485 UT WOS:A1995TE48500005 ER PT J AU GREENWOOD, DR WING, SL AF GREENWOOD, DR WING, SL TI EOCENE CONTINENTAL CLIMATES AND LATITUDINAL TEMPERATURE-GRADIENTS SO GEOLOGY LA English DT Article ID HISTORY; REGION; MODEL AB Global climate during the Mesozoic and early Cenozoic is thought to have been warmer than at present, but there is debate about winter temperatures. Paleontological data indicate mild temperatures even at high latitudes and in mid-latitude continental interiors, whereas computer simulations of continental paleoclimates produce winter temperatures closer to modern levels. Foliar physiognomy and floristic composition of 23 Eocene floras from the interior of North America and Australia indicate cold month means generally >2 degrees C, even where the mean annual temperature (MAT) was <15 degrees C. Reconstructed Eocene latitudinal gradients of MAT are curvilinear but are about 0.4 degrees C per 1 degrees of latitude in continental interiors at mid-latitudes, much less than the 0.8-1.0 degrees C per 1 degrees of latitude observed in eastern and central North America today, but similar to modern gradients in the Southern Hemisphere mid-latitudes and on the west coast of North America. Latitudinal temperature gradients reconstructed here are broadly representative of Eocene climates, showing that the discrepancy between proxy data and simulations will not be resolved by regional adjustments to paleogeography or reinterpretation of individual fossil assemblages. Similar discrepancies between proxy data and general circulation model simulations for other time periods suggest that there is a basic flaw with the way climate models simulate heat transport to, or loss from, continental surfaces. RP GREENWOOD, DR (reprint author), NATL MUSEUM NAT HIST,DEPT PALEOBIOL,SMITHSONIAN INST,MRC 121,WASHINGTON,DC 20560, USA. RI Greenwood, David/C-2758-2008; OI Greenwood, David/0000-0002-8569-9695; Wing, Scott/0000-0002-2954-8905 NR 55 TC 293 Z9 302 U1 6 U2 38 PU GEOLOGICAL SOC AMERICA PI BOULDER PA PO BOX 9140 3300 PENROSE PLACE, BOULDER, CO 80301 SN 0091-7613 J9 GEOLOGY JI Geology PD NOV PY 1995 VL 23 IS 11 BP 1044 EP 1048 DI 10.1130/0091-7613(1995)023<1044:ECCALT>2.3.CO;2 PG 5 WC Geology SC Geology GA TD518 UT WOS:A1995TD51800021 ER PT J AU MITCHELL, DL OSTRO, SJ ROSEMA, KD HUDSON, RS CAMPBELL, DB CHANDLER, JF SHAPIRO, II AF MITCHELL, DL OSTRO, SJ ROSEMA, KD HUDSON, RS CAMPBELL, DB CHANDLER, JF SHAPIRO, II TI RADAR OBSERVATIONS OF ASTEROIDS 7-IRIS, 9-METIS, 12-VICTORIA, 216-KLEOPATRA, AND 654-ZELINDA SO ICARUS LA English DT Article ID GALILEO PHYSICAL MODEL; IMPACT EXPERIMENTS; ROTATION AXES; SURFACE; OBJECTS; SHAPE; SPIN; FRAGMENTATION; VELOCITY; VENUS AB We report 13-cm wavelength radar observations of the main-belt asteroids 7 Iris, 9 Metis, 12 Victoria, 216 Kleopatra, and 654 Zelinda obtained at Arecibo between 1980 and 1989. The echoes are highly polarized yet broadly distributed in Doppler frequency, indicating that our targets are smooth on decimeter scales but very rough on some scale(s) larger than about 1 m. The echo spectra are generally consistent with existing size, shape, and spin information based on radiometric, lightcurve, and occultation data. All of our targets possess distinctive radar signatures that reveal large-scale topography. Reflectivity spikes within narrow ranges of rotation phase suggest large flat regions on Iris, Metis, and Zelinda, while bimodal spectra imply nonconvex, possibly bifurcated shapes for Kleopatra and Victoria. Kleopatra has the highest radar albedo yet measured for a main-belt asteroid, indicating a high metal concentration and making Kleopatra the best main-belt candidate for a core remnant of a differentiated and subsequently disrupted parent body. Upon completion of the Arecibo telescope upgrade, there will be several opportunities per year to resolve main-belt asteroids with hundreds of delay-Doppler cells, which can be inverted to provide estimates of both three-dimensional shape and radar scattering properties. (C) 1995 Academic Press, Inc. C1 WASHINGTON STATE UNIV,DEPT ELECT ENGN,PULLMAN,WA 99164. CORNELL UNIV,NATL ASTRON & IONOSPHERE CTR,ITHACA,NY 14853. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MITCHELL, DL (reprint author), CALTECH,JET PROP LAB,PASADENA,CA 91109, USA. NR 69 TC 43 Z9 43 U1 0 U2 0 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD NOV PY 1995 VL 118 IS 1 BP 105 EP 131 DI 10.1006/icar.1995.1180 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TK354 UT WOS:A1995TK35400007 ER PT J AU PEQUEGNAT, LH WILLIAMS, AB AF PEQUEGNAT, LH WILLIAMS, AB TI 2 NEW SPECIES OF MUNIDOPSIS (DECAPODA, ANOMURA, GALATHEIDAE) FROM THE WESTERN ATLANTIC OOCEAN SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article AB New galatheid squat lobsters, Munidopsis glabra, from the continental slope of the northwestern Gulf of Mexico, and M. penescabra, from continental slope areas of the northwestern Gulf of Mexico and the western North Atlantic off Georgia, are described and illustrated. Munidopsis glabra is closely related to western Atlantic M. abbreviata (A. Milne Edwards, 1880). Munidopsis penescabra has affinities with eastern Pacific M. scabra Faxon, 1893, and M. tanneri Faxon, 1893, and with closely related western Atlantic M. sharreri(A. Milne Edwards, 1880) and M. kucki Baba and Camp, 1988. C1 SMITHSONIAN INST,SYSTEMAT LAB,NATL MARINE FISHERIES SERV,WASHINGTON,DC 20560. NR 5 TC 8 Z9 9 U1 0 U2 0 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD NOV PY 1995 VL 15 IS 4 BP 786 EP 792 DI 10.2307/1548827 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA TD670 UT WOS:A1995TD67000018 ER PT J AU Haig, SM Ballou, JD Casna, NJ AF Haig, SM Ballou, JD Casna, NJ TI Genetic identification of kin in Micronesian kingfishers SO JOURNAL OF HEREDITY LA English DT Article ID DNA FINGERPRINTS; RELATEDNESS; PARENTAGE; KINSHIP; STRAINS; LIONS AB Micronesian kingfishers (Halcyon cinnamomina cinnamomina) are a critically endangered species (n = 50 living birds), endemic to Guam, and recently extirpated from the wild, When the remnant population on Guam was taken from the wild, little was known about the 29 birds that founded the new captive population or what potential these birds held for forming viable populations, We used pedigree analyses and multilocus minisatellite DNA profiles to examine potential genetic relationships among these founders so that appropriate captive breeding strategies could be implemented and the species may one day be returned to the wild, Assuming founders were unrelated resulted in a significant correlation between relatedness calculated from a subsequent pedigree and DNA profile similarity (R(2) = 0.91, 2 df, P < .05), UPGMA cluster analyses of genetic distances (1 - DNA similarity) of all birds indicated further agreement between the pedigree and DNA data, However, UPGMA clustering of founders indicated that three groups of founders had unusually high similarity for unrelated birds, Comparison of these similarities with known relationships (i.e., unrelated birds and birds related by r = 0.5) suggested they fell within one standard deviation of the mean for related birds, but were also at the highest end of the range for unrelated birds. Unable to assign relatedness based on this analysis, we further proposed a series of hypotheses to explain relatedness among founders and used correlation analyses to evaluate the best fit of the data, One assumption that linked two sets of founders as siblings best described the relationship between similarity and relatedness (R(2) = 0.92, 3 df, P < .01) and is suggested for consideration in Micronesian kingfisher conservation, Similar approaches should be helpful in understanding relationships among unknown individuals in other populations, These analyses are best carried out when at least some pedigree information is known. C1 SMITHSONIAN INST, NATL ZOOL PK, DEPT ZOOL RES, WASHINGTON, DC 20008 USA. CLEMSON UNIV, S CAROLINA COOPERAT FISH & WILDLIFE RES UNIT, CLEMSON, SC USA. THERION CORP, TROY, NY USA. NR 46 TC 20 Z9 21 U1 1 U2 6 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-1503 J9 J HERED JI J. Hered. PD NOV-DEC PY 1995 VL 86 IS 6 BP 423 EP 431 PG 9 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA TL747 UT WOS:A1995TL74700002 ER PT J AU STUDIER, EH SEVICK, SH WILSON, DE BROOKE, AP AF STUDIER, EH SEVICK, SH WILSON, DE BROOKE, AP TI CONCENTRATIONS OF MINERALS AND NITROGEN IN MILK OF CAROLLIA AND OTHER BATS SO JOURNAL OF MAMMALOGY LA English DT Article DE CAROLLIA; BAT; MILK; NITROGEN; MINERAL; COMPOSITION; NUTRITION ID NEOTROPICAL BATS AB Concentrations of nitrogen and minerals were measured in milk of Carollia and a few other tropical species of bats. Compared with other mammals, milk of Carollia is high in potassium and low in calcium. Compared with milk of the insectivorous Tadarida brasiliensis, milk of Carollia is low in nitrogen. High potassium and low nitrogen concentrations in milk of Carollia may reflect its frugivorous diet, while low milk-calcium levels may relate to slow postnatal growth in these bats. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,WASHINGTON,DC 20560. UNIV TENNESSEE,DEPT ZOOL,KNOXVILLE,TN 37996. RP STUDIER, EH (reprint author), UNIV MICHIGAN,DEPT BIOL,FLINT,MI 48502, USA. NR 17 TC 9 Z9 10 U1 2 U2 4 PU AMER SOC MAMMALOGISTS PI PROVO PA BRIGHAM YOUNG UNIV, DEPT OF ZOOLOGY, PROVO, UT 84602 SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD NOV PY 1995 VL 76 IS 4 BP 1186 EP 1189 DI 10.2307/1382610 PG 4 WC Zoology SC Zoology GA TJ248 UT WOS:A1995TJ24800019 ER PT J AU BEHLING, H AF BEHLING, H TI A HIGH-RESOLUTION HOLOCENE POLLEN RECORD FROM LAGO DO PIRES, SE BRAZIL - VEGETATION, CLIMATE AND FIRE HISTORY SO JOURNAL OF PALEOLIMNOLOGY LA English DT Article; Proceedings Paper CT 1994 Meeting of the American-Quaternary-Association CY JUN 19-22, 1994 CL UNIV MINNESOTA, MINNEAPOLIS, MN SP Amer Quaternary Assoc HO UNIV MINNESOTA DE SOUTHEAST BRAZIL; PALYNOLOGY; HOLOCENE; CERRADO; FIRE; SEMIDECIDUOUS FOREST; PALEOECOLOGY; PALEOCLIMATOLOGY ID AMAZON AB Lago do Pires (17 degrees 57' S, 42 degrees 13' W) is situated at 390 m a.s.l. in the foothills of the Serra do Espinhaco, 250 km from the Brazilian Atlantic coast. The original vegetation of the study area has been almost destroyed by pastoral activity. Relicts of a dense 20-30 m tall tropical semideciduous forest are present only on a few hill tops. The dry season of the Lago do Fires region lasts for 4 months and the annual precipitation is 1250 mm. A high resolution pollen record from a 16 m long sediment core, composed of 77 samples, subdivided in 7 zones and 4 subzones, allows a reconstruction of Holocene paleoenvironments. For the early Holocene (9720-8810 B.P.), the results indicate that the region surrounding the lake was dominated by a herb savanna (campo cerrado) with Curatella americana (cerrado tree) and high fire frequency. Species of Cecropia, Urticales and a few others, form small gallery forests along the water courses. This vegetation pattern is consistent with a long dry season (perhaps 6 months) and a low annual precipitation. Between 8810 and 7500 years B.P. gallery forests expanded in the valleys and suggest a period of higher rainfall with shortened dry season (perhaps 5 months). Fire was less frequent. Reduction of gallery forests followed (7500-5530 B.P.), probably related to a return of drier climatic conditions (5-6 months dry season, lower precipitation). Fires were more frequent. Between 5530 and 2780 years B.P. in the vallyes were forests and on the hills still an open cerrado. The dry season probably was about 5 months and the rainfall was higher than in the previous period. Later (2780-970 B.P.) the more open cerrado on the hills changed to more closed cerrado. A dense and closed semideciduous forest existed in the region only in the latest Holocene period (since 970 B.P.) under the current climatic conditions. The vegetation was no longer influenced by fire. A very strong human impact by deforestation and use of fire occurred in the last decades. Today cerrado vegetation is generally restricted to central Brazil and exists in several small isolated 'Islands' (Hueck, 1956) in the area of semideciduous forest in SE Brazil which were more widespread during the drier periods of the Holocene. The wettest period of Holocene occurs in the present millenium. RP BEHLING, H (reprint author), SMITHSONIAN TROP RES INST,POB 2072,BALBOA,PANAMA. NR 57 TC 82 Z9 85 U1 0 U2 7 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0921-2728 J9 J PALEOLIMNOL JI J. Paleolimn. PD NOV PY 1995 VL 14 IS 3 BP 253 EP 268 DI 10.1007/BF00682427 PG 16 WC Environmental Sciences; Geosciences, Multidisciplinary; Limnology SC Environmental Sciences & Ecology; Geology; Marine & Freshwater Biology GA TD951 UT WOS:A1995TD95100004 ER PT J AU GREENBERG, R FOSTER, MS MARQUEZVALDELAMAR, L AF GREENBERG, R FOSTER, MS MARQUEZVALDELAMAR, L TI THE ROLE OF THE WHITE-EYED VIREO IN THE DISPERSAL OF BURSERA FRUIT ON THE YUCATAN PENINSULA SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE AVIAN ENERGETICS; BURSERA SIMARUBA; FRUGIVORY; MIGRATORY BIRDS; MUTUALISM; SEED DISPERSAL; VIREO GRISEUS AB White-eyed vireos (Vireo griseus) winter in the forests and secondary growth of the Yucatan Peninsula where Bursera simaruba (Burseraceae) is an abundant tree. Twenty-five per cent of all white-eyed vireos observed foraging visited Bursera trees. In addition, presence and abundance of territorial white-eyed vireos in small forest patches were correlated with the size of the Bursera crop. Vireos were the most reliable dispersers of Bursera seeds. These birds visited 32 of 35 trees observed for at least three hours. They accounted for approximately half of all bird visits, and two-thirds of the seeds dispersed. Most of the other species rarely visited (<5% of visits) or failed to remove seeds from the tree. Peculiarities of phenology and fruit structure may contribute to the tendency of Bursera to be dispersed by relatively few species. The capsules of Bursera fruits do not open when the fruit ripens; birds apparently locate ripe fruit using visual cues, although these are few. In addition, only a small portion of the crop ripens daily over a 7- or 8-month period. The vireo-Bursera simaruba relationship, found regionally on the Yucatan Peninsula, may result from the prolonged fruit ripening period (October-March), the relatively depauperate frugivore community and the relatively high density of small Bursera trees in the hurricane-disturbed dry forests. Small trees at ail rimes, and ail trees from October to February, depend upon territorial vireos for continuous, highly efficient local dispersal of a small number of fruits. In March and April residual fruits ripen rapidly and synchronously, attracting a greater variety of visitors for broad spectrum dispersal during a period of food scarcity. Thus, Bursera has an unusual two-phase phenological pattern, perhaps alternately to take advantage of both specialized and opportunistic dispersers. RP GREENBERG, R (reprint author), SMITHSONIAN MIGRATORY BIRD CTR,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 0 TC 26 Z9 27 U1 0 U2 3 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH STREET, NEW YORK, NY 10011-4211 SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD NOV PY 1995 VL 11 BP 619 EP 639 PN 4 PG 21 WC Ecology SC Environmental Sciences & Ecology GA TJ899 UT WOS:A1995TJ89900011 ER PT J AU JORDAN, HL HOWARD, J TOMPKINS, WA KENNEDYSTOSKOPF, S AF JORDAN, HL HOWARD, J TOMPKINS, WA KENNEDYSTOSKOPF, S TI DETECTION OF FELINE IMMUNODEFICIENCY VIRUS IN SEMEN FROM SEROPOSITIVE DOMESTIC CATS (FELIS-CATUS) SO JOURNAL OF VIROLOGY LA English DT Note ID POLYMERASE CHAIN-REACTION; INFECTED CELL; TRANSMISSION; TYPE-1; AIDS; PREVALENCE; CHEETAH; STAGE; MODEL; MEN AB Electroejaculates from experimentally infected domestic cats were evaluated for the presence of feline immunodeficiency virus (PIV). Virus was isolated from cell-free seminal plasma and seminal cells by cocultivation with a feline interleukin-2-dependent CD4(+) T-cell line, in which productive infection was demonstrated by syncytium formation and FIV gag p26 antigen secretion. In addition, an 868-bp segment of the FN gag provirus gene was identified in cocultured cells by PCR and Southern analysis. A 582-bp fragment of the FIV gag provirus genome was detected by nested PCR and Southern analysis in nonfractionated seminal cells and in sperm purified by a swim-up procedure. This is the first report describing the detection of replication-competent FIV in cell-free acid cell-associated forms in domestic cat semen. C1 N CAROLINA STATE UNIV, COLL VET MED, DEPT MICROBIOL PATHOL & PARASITOL, RALEIGH, NC 27606 USA. SMITHSONIAN INST, NATL ZOOL PK, WASHINGTON, DC 20008 USA. FU PHS HHS [1 R01 A132310-02] NR 51 TC 33 Z9 33 U1 0 U2 3 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0022-538X J9 J VIROL JI J. Virol. PD NOV PY 1995 VL 69 IS 11 BP 7328 EP 7333 PG 6 WC Virology SC Virology GA RZ100 UT WOS:A1995RZ10000096 PM 7474164 ER PT J AU MECKLENBURG, VM AF MECKLENBURG, VM TI NEW-YORK-CITY AND THE ASHCAN-SCHOOL + TURN-OF-THE-CENTURY AMERICAN PAINTING SO MAGAZINE ANTIQUES LA English DT Article RP MECKLENBURG, VM (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER ART,WASHINGTON,DC 20560, USA. NR 21 TC 0 Z9 0 U1 0 U2 0 PU BRANT PUBL, INC PI NEW YORK PA 575 BROADWAY, NEW YORK, NY 10012 SN 0161-9284 J9 MAG ANTIQUES JI Mag. Antiq. PD NOV PY 1995 VL 148 IS 5 BP 685 EP & PG 0 WC Art SC Art GA TC159 UT WOS:A1995TC15900009 ER PT J AU HOFFMANN, RS AF HOFFMANN, RS TI CONFLICT-RESOLUTION + THE SMITHSONIANS EXHIBITION ON THE ENOLA-GAY SO MUSEUM NEWS LA English DT Letter RP HOFFMANN, RS (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSN MUSEUMS PI WASHINGTON PA 1225 EYE ST NW SUITE 200, WASHINGTON, DC 20005 SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD NOV-DEC PY 1995 VL 74 IS 6 BP 7 EP & PG 0 WC Art SC Art GA TD477 UT WOS:A1995TD47700002 ER PT J AU ZORICH, D ANDERSON, M ANDREWS, R BROUN, E GATES, J ROSS, D SACHS, S AF ZORICH, D ANDERSON, M ANDREWS, R BROUN, E GATES, J ROSS, D SACHS, S TI ART-MUSEUMS IN A NEW MEDIUM + ROUND-TABLE ON THE ROLE OF THE NEWLY DEVELOPING TELECOMMUNICATIONS NETWORKS IN CULTURAL INSTITUTIONS SO MUSEUM NEWS LA English DT Discussion C1 EMORY UNIV,MICHAEL C CARLOS MUSEUM,ATLANTA,GA 30322. UNIV WASHINGTON,HENRY ART GALLERY,SEATTLE,WA 98195. SMITHSONIAN INST,NATL MUSEUM AMER ART,WASHINGTON,DC 20560. DALLAS MUSEUM ART,DALLAS,TX. WHITNEY MUSEUM AMER ART,NEW YORK,NY. DETROIT INST ARTS,DETROIT,MI. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSN MUSEUMS PI WASHINGTON PA 1225 EYE ST NW SUITE 200, WASHINGTON, DC 20005 SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD NOV-DEC PY 1995 VL 74 IS 6 BP 44 EP & PG 0 WC Art SC Art GA TD477 UT WOS:A1995TD47700013 ER PT J AU KONIGER, M HARRIS, GC VIRGO, A WINTER, K AF KONIGER, M HARRIS, GC VIRGO, A WINTER, K TI XANTHOPHYLL-CYCLE PIGMENTS AND PHOTOSYNTHETIC CAPACITY IN TROPICAL FOREST SPECIES - A COMPARATIVE FIELD-STUDY ON CANOPY, GAP AND UNDERSTORY PLANTS SO OECOLOGIA LA English DT Article DE PHOTOINHIBITION; PHOTOSYNTHESIS; TROPICAL FOREST; XANTHOPHYLL-CYCLE PIGMENTS ID CRASSULACEAN ACID METABOLISM; EXCESS LIGHT ENERGY; CHLOROPHYLL FLUORESCENCE; CAROTENOID COMPOSITION; PROTEIN COMPLEXES; HAWAIIAN FOREST; LEAVES; ZEAXANTHIN; SHADE; DISSIPATION AB Xanthophyll-cycle pigments and photosynthetic capacity (PSmax) were analyzed in 25 species from different light environments (canopy, gap, understory) within a Panamanian tropical forest. (1) Sun-exposed leaves of canopy tree species showed the highest photosynthetic capacities and largest xanthophyll-cycle pools (violaxanthin, antheraxanthin, zeaxanthin) of about 87 mmol mol(-1) chlorophyll with only small amounts of alpha-carotene [about 7 mmol mol(-1) chlorophyll = 8% of total (alpha+beta) carotene pool]. Under high natural photon flux densities (PFDs) canopy leaves rapidly converted up to 96% of the xanthophyll-cycle pool into zeaxanthin. The back reaction to violaxanthin occurred much faster in low light than in complete darkness. At the end of the night, zeaxanthin still accounted for, on average, 14% of the total xanthophyll-cycle pigments. (2) Leaves of gap plants had intermediate values of PSmax and a 43% lower total carotenoid content than canopy leaves. The average size of the xanthophyll-cycle pool was 35 mmol mol(-1) chlorophyll, and alpha-carotene accounted for up to 66% of the total (alpha+beta) carotene pool. Under high light conditions gap plants converted, on average, 86% of the xanthophyll-cycle pigments into zeaxanthin. The back reaction, following a decrease in ambient PFD, was slower than the forward reaction. At the end of the night, zeaxanthin accounted for, on average, 7% of the xanthophyll-cycle pigments in gap plants. (3) Understory plants showed the lowest values of PSmax and the smallest xanthophyll-cycle pool of about 22 mmol mol(-1) chlorophyll. alpha-Carotene accounted for up to 70% of total carotene. The conversion of xanthophyll-cycle pigments into zeaxanthin was negligible during short sunflecks of 1-2 min duration and PFDs up to about 400 mu mol m(-2) s(-1). At predawn, leaves of understory plants rarely contained any detectable zeaxanthin. Aechmea magdalenae, an understory CAM plant, showed exceptionally high rates of PSmax per unit leaf area compared to sympatric C-3 understory species. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 44 TC 61 Z9 65 U1 1 U2 9 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0029-8549 J9 OECOLOGIA JI Oecologia PD NOV PY 1995 VL 104 IS 3 BP 280 EP 290 DI 10.1007/BF00328362 PG 11 WC Ecology SC Environmental Sciences & Ecology GA TE433 UT WOS:A1995TE43300003 PM 28307583 ER PT J AU GAVRAS, P PINDZOLA, MS SCHULTZ, DR WELLS, JC AF GAVRAS, P PINDZOLA, MS SCHULTZ, DR WELLS, JC TI DIRECT SOLUTION OF THE TIME-DEPENDENT SCHRODINGER-EQUATION FOR PROTON-HYDROGEN COLLISIONS IN 2-DIMENSIONAL CARTESIAN SPACE SO PHYSICAL REVIEW A LA English DT Article ID ION-ATOM COLLISIONS; TRIPLE-CENTER TREATMENT; HARTREE-FOCK THEORY; CHARGE-TRANSFER; CROSS-SECTIONS; INTERMEDIATE ENERGIES; IONIZING COLLISIONS; ELECTRON-EMISSION; PROJECTILE-CHARGE; IONIZATION AB The wave function for the collision of a proton with a hydrogen atom is obtained by direct solution of the time-dependent Schrodinger equation in a model two-dimensional Cartesian space using lattice techniques. The dimensional reduction from the full three-dimensional (3D) space allows the consideration of huge collision ''volumes'' with minimal computational expense, while still preserving the idea of an impact parameter. The probabilities for charge exchange and ionization are estimated for different projectile energies ranging from 10 to 100 keV/amu. Comparisons with full 3D,calculations in smaller collision volumes show that the time-dependent behavior of the probability densities is quite similar for the 2D soft-core model interaction chosen here. The ionization dynamics are further analyzed in regard to the fate of that fraction of the probability density located near the saddle point between projectile and target potentials. C1 OAK RIDGE NATL LAB,DIV PHYS,OAK RIDGE,TN 37831. HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. RP GAVRAS, P (reprint author), AUBURN UNIV,DEPT PHYS,AUBURN,AL 36849, USA. RI Wells, Jack/D-3675-2016 OI Wells, Jack/0000-0002-5083-3030 NR 46 TC 9 Z9 9 U1 1 U2 2 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD NOV PY 1995 VL 52 IS 5 BP 3868 EP 3876 DI 10.1103/PhysRevA.52.3868 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA TE173 UT WOS:A1995TE17300070 ER PT J AU MATHEWS, PM SHAPIRO, II AF MATHEWS, PM SHAPIRO, II TI CONSTRAINTS ON DEEP-EARTH PROPERTIES FROM SPACE-GEODETIC DATA SO PHYSICS OF THE EARTH AND PLANETARY INTERIORS LA English DT Article; Proceedings Paper CT IASPEI/SEDI 27th General Assembly on Structure, Compositions and Evolution of the Earths Interior CY JAN 10-21, 1994 CL WELLINGTON, NEW ZEALAND SP IASPEI, SEDI ID INNER CORE DYNAMICS; FORCED NUTATIONS; INTERFEROMETRY; MODEL AB The amplitude of the Earth's nutation driven by a given component of the tidal potential is governed primarily by three parameters pi which are composites of a larger number of 'basic' Earth parameters (ellipticities, compliances, moments of inertia, etc., of the Earth and its core regions). We obtain estimates of the pi by least-squares fitting of nutation amplitudes estimated from very long baseline interferometry (VLBI) data to theoretical expressions based on an analytical formulation of nutation theory which incorporates the role of the solid inner core. We show how the estimates obtained, as well as the overall fit, vary with the ellipticity assumed for the inner core, and examine how the results are affected when otherwise unmodelled effects of ocean tides and mantle anelasticity are taken into account. Considering two anelasticity models, we find that the fit obtained with the use of one of them is noticeably worse than if the other is used or if no anelasticity correction is made. Independent of the corrections applied, the X(2) Of the fit is found to be smallest if the ellipticity e(s) of the solid inner core is taken as about half that of the Preliminary Reference Earth Model (PREM). Independent estimates of the ellipticity ef of the fluid core and other basic parameters on which the pi depend cannot be obtained from the estimates of the pi alone. Nevertheless, with certain assumptions that are less restrictive than those hitherto employed in the literature, we find ef to be 5.0% higher than the PREM value if the best-fit value is assigned to e,, and 4.7% higher if e(s) = e(s(PREM)); these values for ep are in accord with the estimate of Gwinn et al. (J. Geophys. Res., 91: 4755-4765, 1986), and correspond to a nonhydrostatic flattening of about 465 m and 435 m, respectively, of the core-mantle boundary. Our parameter estimates have implications for the value of the static part k(0) of the second-degree Love number k which seem to be hard to reconcile with information from other sources. Observational estimates of the amplitudes of the 18.6 year nutations are also found to be not satisfactorily matched with theoretical expectations. A careful re-examination of data analysis and theory is needed to resolve these problems. RP MATHEWS, PM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 14 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-9201 J9 PHYS EARTH PLANET IN JI Phys. Earth Planet. Inter. PD NOV PY 1995 VL 92 IS 1-2 BP 99 EP 107 DI 10.1016/0031-9201(95)03064-4 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA TE093 UT WOS:A1995TE09300011 ER PT J AU HILL, MG HOLLIDAY, VT STANFORD, DJ AF HILL, MG HOLLIDAY, VT STANFORD, DJ TI A FURTHER EVALUATION OF THE SAN-JON SITE, NEW-MEXICO SO PLAINS ANTHROPOLOGIST LA English DT Article DE PALEOINDIAN; ARCHAIC; BISON; SOUTHERN HIGH PLAINS; PLAYA ID SOUTHERN HIGH-PLAINS; TEXAS; DATES AB The San Jon site (LA 6437) is a well-known, but only briefly documented multicomponent archaeological locality situated on the northern rim of the Southern High Plains in Quay County, New Mexico. The site is in a small (360 m wide), dry lake basin or ''playa.'' Archaeological materials buried by basin fill are now being exposed along deep arroyo tributaries of a canyon that cut into the High Plains escarpment Excavations in 1941 provided evidence that Paleoindian and late Archaic hunters may have used the site to procure and process bison. A ceramic habitation also was documented. Fieldwork in 1993, 1994, and 1995, and reanalysis of the extant San Jon collection yielded additional data on the cultural chronology of the site and the complexity of the site's formational history. Two unfluted, lanceolate points were found in 1941, one of which is the type ''San Jon'' point recovered in association with an extinct species of bison (MNI = 5). The other Late Paleoindian point was found in association with modern bison in a redeposited context Both artifacts are now considered to be Firstview points. The ''San Jon'' level is dated to greater than or equal to 8400 yrs BP. In 1993, a latest Paleoindian or Early Archaic feature, very rare for the region, was found in situ directly above the ''San Jon'' bonebed and yielded the base of a lanceolate point, two small side-notched points, considerable lithic debitage, and bone. The feature dates between 8400 and 7600 yrs BP. The Late Archaic bonebed (MNI = 7) dates to < 3600 yrs BP. San Jon is one of the few sites in the region with a documented record of multiple in situ occupations spanning the Paleoindian, Archaic, and Late Prehistoric Traditions. C1 UNIV WISCONSIN,DEPT GEOG,MADISON,WI 53706. SMITHSONIAN INST,MUSEUM NATL HIST NAT,DEPT ANTHROPOL,WASHINGTON,DC 20560. RP HILL, MG (reprint author), UNIV WISCONSIN,DEPT ANTHROPOL,MADISON,WI 53706, USA. NR 76 TC 13 Z9 13 U1 0 U2 1 PU PLAINS ANTHROPOLOGICAL SOC PI LINCOLN PA 410 WEDGEWOOD DRIVE, LINCOLN, NE 68510 SN 0032-0447 J9 PLAINS ANTHROPOL JI Plains Anthropol. PD NOV PY 1995 VL 40 IS 154 BP 369 EP 390 PG 22 WC Anthropology SC Anthropology GA TH792 UT WOS:A1995TH79200003 ER PT J AU KRAUSE, GH VIRGO, A WINTER, K AF KRAUSE, GH VIRGO, A WINTER, K TI HIGH SUSCEPTIBILITY TO PHOTOINHIBITION OF YOUNG LEAVES OF TROPICAL FOREST TREES SO PLANTA LA English DT Article DE CHLOROPHYLL FLUORESCENCE; PHOTOINHIBITION (PHOTOSYNTHESIS); PHOTOSYNTHETIC GAS EXCHANGE; PHOTOSYSTEM II; TROPICAL FOREST SPECIES; XANTHOPHYLL CYCLE ID PHOTOSYSTEM-II; CHLOROPHYLL FLUORESCENCE; O-2 EVOLUTION; PHOTON YIELD; ELECTRON-TRANSPORT; QUANTUM YIELD; CO2 FIXATION; PHOTOSYNTHESIS; PLANTS; LIGHT AB Photoinhibition of photosynthesis was studied in young (but almost fully expanded) and mature canopy sun leaves of several tropical forest tree species, both under controlled conditions (exposure of detached leaves to about 1.8 mmol photons m(-2) s(-1)) and in the field. The degree of photoinhibition was determined by means of the ratio of variable to maximum chlorophyll (Ch1) fluorescence emission (F-V/F-M) and also by gas-exchange measurements. For investigations in situ, young and mature leaves with similar exposure to sunlight were compared. The results show a consistently higher degree of photoinhibition in the young leaves. In low light, fast recovery was observed in both types of leaves in situ, as well as in the laboratory. The fluorescence parameter 1-F-S/F'(M) (where F-S = stationary fluorescence and F'(M) = maximum fluorescence during illumination) was followed in situ during the course of the day in order to test its suitability as a measure of the photosynthetic yield of photosystem II (PSII). Electron-transport rates were calculated from these fluorescence signals and compared with rates of net CO2 assimilation. Measurements of diurnal changes in PSII 'yield' confirmed the increased susceptibility of young leaves to photoinhibition. Calculated electron transport qualitatively reflected net CO2 uptake in situ during the course of the day. Photosynthetic pigments were analyzed in darkened and illuminated leaves. Young and mature leaves showed the same Ch1 a/b ratio, but young leaves contained about 50% less Chi a + b per unit leaf area. The capacity of photosynthetic O-2 evolution per unit leaf area was decreased to a similar extent in young leaves. On a Ch1 basis, young leaves contained more a-carotene, more xanthophyll cycle pigments and, under strong illumination, more zeaxanthin than mature leaves. The high degree of reversible photoinhibition observed in these young sun leaves probably represents a dynamic regulatory process protecting the photosynthetic apparatus from severe damage by excess light. C1 UNIV DUSSELDORF,INST PLANT BIOCHEM,D-40225 DUSSELDORF,GERMANY. RP KRAUSE, GH (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. NR 41 TC 134 Z9 146 U1 2 U2 15 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0032-0935 J9 PLANTA JI Planta PD NOV PY 1995 VL 197 IS 4 BP 583 EP 591 PG 9 WC Plant Sciences SC Plant Sciences GA TJ713 UT WOS:A1995TJ71300004 ER PT J AU REVEAL, JL AF REVEAL, JL TI SUBFAMILY NAMES IN AN 1832 PREPRINT OF AN ARTICLE ON BOTANY FOR THE 7TH EDITION OF THE ENCYCLOPEDIA-BRITANNICA SO TAXON LA English DT Article AB An article on botany, written by George A. W. Arnott and ultimately published in the seventh edition of the Encyclopaedia britannica in 1842, first appeared as a preprint a decade earlier, being effectively published on 9 Mar 1832. Arnott validly published numerous subfamily names, many of which are presently attributed to later authors. C1 UNIV MARYLAND,DEPT PLANT BIOL,COLLEGE PK,MD 20742. RP REVEAL, JL (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT MRC166,WASHINGTON,DC 20560, USA. NR 16 TC 3 Z9 4 U1 0 U2 0 PU INT ASSN PLANT TAXONOMY PI BERLIN PA BOTANISCHER GARTEN & MUSEUM KONIGIN-LUISSE-STRASSE 6-8, W-1000 BERLIN, GERMANY SN 0040-0262 J9 TAXON JI Taxon PD NOV PY 1995 VL 44 IS 4 BP 589 EP 596 DI 10.2307/1223501 PG 8 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA TH337 UT WOS:A1995TH33700007 ER PT J AU OOSTERBROEK, P COURTNEY, G AF OOSTERBROEK, P COURTNEY, G TI PHYLOGENY OF THE NEMATOCEROUS FAMILIES OF DIPTERA (INSECTA) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE DIPTERA; NEMATOCERA; CLASSIFICATION; LARVA; PUPA; ADULT ID MOUNTAIN MIDGES DIPTERA; LOWER BRACHYCERA DIPTERA; DEUTEROPHLEBIIDAE; LARVAE; HOMOLOGIES; MORPHOLOGY; CLASSIFICATION; CHIRONOMIDAE; TAXONOMY; ORIGIN AB The relationships of the nematocerous families of Diptera are cladistically analysed using the parsimony programs PAUP and Hennig86. An extensive review, as well as a data matrix, is presented for 98 almost exclusively morphological characters (larva, 56; pupa, 6; adult, 36). Four infraorders are recognized, viz Ptychopteromorpha, Culicomorpha, Blephariceromorpha, Bibionomorpha, and a clade containing the 'higher Nematocera' and Brachycera. Traditionally the family Nymphomyiidae or the infraorder Tipulomorpha (=Tipulidae, with or without Trichoceridae) are considered the most basal clade of the extant Diptera On the basis of our cladistic analysis it is suggested that the Ptychopteromolpha-Culicomorpha clade is the sister-group of all other extant Diptera We provide evidence that the Axymyiidae are part of a monophyletic Bibionomorpha. The latter infraorder is proposed as the sister-group of the higher Nematocera and Brachycera. We transfer the Tipulidae (Tipulomorpha) to the higher Nematocera, at a position next to Trichoceridae and near the Anisopodidae-Brachycera lineage. Previous hypotheses concerning nematocerous relationships are reviewed. (C) 1995 The Linnean Society of London C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT ENTOMOL,WASHINGTON,DC. RP OOSTERBROEK, P (reprint author), UNIV AMSTERDAM,INST SYSTEMAT & POPULAT BIOL,DEPT ENTOMOL,PLANTAGE MIDDENLAAN 64,1018 DH AMSTERDAM,NETHERLANDS. NR 233 TC 121 Z9 130 U1 0 U2 14 PU ACADEMIC PRESS (LONDON) LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD NOV PY 1995 VL 115 IS 3 BP 267 EP 311 DI 10.1111/j.1096-3642.1995.tb02462.x PG 45 WC Zoology SC Zoology GA TJ760 UT WOS:A1995TJ76000002 ER PT J AU PATO, MP HUSSEIN, MS AF PATO, MP HUSSEIN, MS TI TIME-DELAY IN SEMICLASSICAL SCATTERING-THEORY SO MODERN PHYSICS LETTERS A LA English DT Article AB An asymptotic evaluation of the time delay in the context of the semiclassical approximation is performed. It is shown that it is related to Stokes's discontinuities of the asymptotic series caused by singularities determined by the turning points and points of equilibrium of the effective potential in the complex tau-plane. The theory is applied to the repulsive potentials inversely proportional to the fourth and the sixth power of the distance. The case of complex potentials, usually considered in nuclear scattering is also discussed. C1 MIT,CTR THEORET PHYS,NUCL SCI LAB,CAMBRIDGE,MA 02139. MIT,DEPT PHYS,CAMBRIDGE,MA 02139. HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. RP PATO, MP (reprint author), UNIV SAO PAULO,FINPE,INST FIS,CAIXA POSTAL 66318,BR-05389971 SAO PAULO,BRAZIL. NR 8 TC 0 Z9 0 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA JOURNAL DEPT PO BOX 128 FARRER ROAD, SINGAPORE 9128, SINGAPORE SN 0217-7323 J9 MOD PHYS LETT A JI Mod. Phys. Lett. A PD OCT 30 PY 1995 VL 10 IS 33 BP 2509 EP 2517 DI 10.1142/S0217732395002659 PG 9 WC Physics, Nuclear; Physics, Particles & Fields; Physics, Mathematical SC Physics GA TF043 UT WOS:A1995TF04300004 ER PT J AU BAUER, J IVANOV, M RZAZEWSKI, K REISS, HR AF BAUER, J IVANOV, M RZAZEWSKI, K REISS, HR TI SFA APPLIED TO THE ONE-DIMENSIONAL 2-ELECTRON MODEL ATOM SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID IONIZATION AB We calculate the total direct double photoionization rates in the strong-field approximation for a one-dimensional model. We study the role of the electron-electron repulsion in the final state for different frequencies and intensities of the applied laser field. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP BAUER, J (reprint author), CENTRUM FIZYKI TEORETYCZNEJ PAN,AL LOTNIKOW 32-46,PL-02668 WARSAW,POLAND. RI Rzazewski, Kazimierz/G-4854-2011; Bauer, Jaroslaw/J-8259-2013; Reiss, Howard/B-6538-2014 OI Rzazewski, Kazimierz/0000-0002-6082-3565; Reiss, Howard/0000-0003-1023-1462 NR 15 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TECHNO HOUSE, REDCLIFFE WAY, BRISTOL, ENGLAND BS1 6NX SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD OCT 28 PY 1995 VL 28 IS 20 BP 4413 EP 4419 DI 10.1088/0953-4075/28/20/006 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA TC056 UT WOS:A1995TC05600006 ER PT J AU CHAI, P DUDLEY, R AF CHAI, P DUDLEY, R TI LIMITS TO VERTEBRATE LOCOMOTOR ENERGETICS SUGGESTED BY HUMMINGBIRDS HOVERING IN HELIOX SO NATURE LA English DT Article ID POWER OUTPUT; INSECT FLIGHT; MUSCLE AB OXYGEN consumption(1) and muscle power output(2) of hovering hummingbirds are among the highest recorded for vertebrates. Maximum performance of hummingbirds thus approaches the upper limits of vertebrate aerobic locomotion(3). Because air density is a major determinant of aerodynamic power requirements(4), hovering flight performances(5) can be manipulated non-invasively using normoxic gas mixtures of variable density(6). Here we show that limits to the locomotor capacity of hovering ruby-throated hummingbirds are unequivocally indicated by aerodynamic failure at low densities less than half that of sea-level air. Hummingbirds demonstrate considerable power reserves, with muscle mass-specific power (assuming perfect elastic energy storage) averaging from 98 W kg(-1) in normal air to a maximum value of 133 W kg(-1) before aerodynamic failure, in contrast to such variable power expenditure, however, muscle efficiency remains approximately constant at 10%. Modulation of power output is attained primarily through variation in wing-stroke amplitude, with aerodynamic failure occurring near 180 degrees. C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. RP CHAI, P (reprint author), UNIV TEXAS, DEPT ZOOL, AUSTIN, TX 78712 USA. NR 18 TC 101 Z9 102 U1 1 U2 33 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD OCT 26 PY 1995 VL 377 IS 6551 BP 722 EP 725 DI 10.1038/377722a0 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA TB469 UT WOS:A1995TB46900053 ER PT J AU KERRICK, AD AKERLOF, CW BILLER, S BUCKLEY, J CARTERLEWIS, DA CAWLEY, MF CHANTELL, M CONNAUGHTON, V FEGAN, DJ FENNELL, S GAIDOS, J HILLAS, AM KWOK, PW LAMB, RC LAPPIN, T LESSARD, R MCENERY, J MEYER, DI MOHANTY, G QUINN, J ROSE, HJ ROVERO, AC SEMBROSKI, G SCHUBNELL, MS PUNCH, M WEEKES, TC WEST, M WILSON, C ZWEERINK, J AF KERRICK, AD AKERLOF, CW BILLER, S BUCKLEY, J CARTERLEWIS, DA CAWLEY, MF CHANTELL, M CONNAUGHTON, V FEGAN, DJ FENNELL, S GAIDOS, J HILLAS, AM KWOK, PW LAMB, RC LAPPIN, T LESSARD, R MCENERY, J MEYER, DI MOHANTY, G QUINN, J ROSE, HJ ROVERO, AC SEMBROSKI, G SCHUBNELL, MS PUNCH, M WEEKES, TC WEST, M WILSON, C ZWEERINK, J TI UPPER LIMITS ON TEV GAMMA-RAY EMISSION FROM ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, ACTIVE; GALAXIES, NUCLEI; GAMMA RAYS, OBSERVATIONS ID RADIATION; ENERGIES; GREATER; SEARCH AB The results of a search for TeV gamma-ray emission from 35 active galactic nuclei (AGNs) using the Whipple Observatory High Resolution Atmospheric Cerenkov Camera are reported. Fifteen of these objects have been detected at GeV energies by the EGRET experiment on the Compton Gamma Ray Observatory. None of the 35 objects gave a signal at the 3 sigma level; Mrk 421 remains the only AGN detected at TeV energies. The absence of a TeV signal may imply a change in the primary source spectrum and/or the effect of absorption by pair production on intergalactic infrared photons. C1 IOWA STATE UNIV SCI & TECHNOL,DEPT PHYS & ASTRON,AMES,IA 50011. UNIV MICHIGAN,RANDALL LAB PHYS,ANN ARBOR,MI 48109. UNIV LEEDS,DEPT PHYS,LEEDS LS2 9JT,W YORKSHIRE,ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,FRED LAWRENCE WHIPPLE OBSERV,AMADO,AZ 85645. ST PATRICKS COLL,DEPT PHYS,MAYNOOTH,KILDARE,IRELAND. UNIV DUBLIN TRINITY COLL,DEPT PHYS,DUBLIN 2,IRELAND. PURDUE UNIV,DEPT PHYS,W LAFAYETTE,IN 47907. RP KERRICK, AD (reprint author), NO KENTUCKY UNIV,DEPT PHYS & GEOL,HIGHLAND HTS,KY 41099, USA. RI McEnery, Julie/D-6612-2012; OI Punch, Michael/0000-0002-4710-2165 NR 37 TC 51 Z9 51 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1995 VL 452 IS 2 BP 588 EP 598 DI 10.1086/176331 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RY932 UT WOS:A1995RY93200011 ER PT J AU NARAYAN, R YI, I AF NARAYAN, R YI, I TI ADVECTION-DOMINATED ACCRETION - UNDERFED BLACK-HOLES AND NEUTRON-STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; BLACK HOLE PHYSICS; RADIATION MECHANISMS, NONTHERMAL; STARS, NEUTRON ID RELATIVISTIC THERMAL PLASMAS; X-RAY SOURCES; DISK ACCRETION; SPHERICAL ACCRETION; BOUNDARY-LAYERS; BINARY-SYSTEMS; CYGNUS X-1; MODEL; COMPTONIZATION; INSTABILITY AB We describe new optically thin solutions for rotating accretion flows around black holes and neutron stars. These solutions are advection dominated, so that most of the viscously dissipated energy is advected radially with the flow. We model the accreting gas as a two-temperature plasma and include cooling by bremsstrahlung, synchrotron, and Comptonization. We obtain electron temperatures T-e similar to 10(8.5)-10(10) K. The new solutions are present only for mass accretion rates M less than a critical rate M(crit) which we calculate as a function of radius R and viscosity parameter alpha. For M < M(crit) we show that there are three equilibrium branches of solutions. One of the branches corresponds to a cool optically thick flow which is the well-known thin disk solution of Shakura & Sunyaev. Another branch corresponds to a hot optically thin flow, discovered originally by Shapiro, Lightman, & Eardley (SLE). This solution is thermally unstable. The third branch corresponds to our new advection-dominated solution. This solution is hotter and more optically thin than the SLE solution but is viscously and thermally stable. It is related to the ion torus model of Rees et al. and may potentially explain the hard X-ray and gamma-ray emission from X-ray binaries and active galactic nuclei. For M < M(crit), our work suggests that an accretion flow can choose between two distinct states, namely, the thin disk solution and the new advection-dominated solution, both of which are apparently stable. We argue that, in certain circumstances, it is only the latter solution that is truly stable, and that a thin disk will spontaneously evaporate and convert itself into an advection-dominated flow. Even for M > M(crit) we suggest that a thin disk may evaporate partially so that a fraction of the accretion occurs via an advection-dominated hot corona. If these ideas are correct, then optically thin advection-dominated flows must be very widespread, possibly the most common form of sub-Eddington accretion in black holes. Our calculations indicate that advection-dominated accretion on black holes differs considerably from similar flows around neutron stars. The crucial physical difference, which has been mentioned previously in the literature, is that in the former the advected energy is lost into the hole, whereas in the latter it is thermalized and reradiated at the stellar surface, thereby providing soft photons which can Compton-cool the accreting gas. We obtain M(crit)similar to alpha(2)M(Edd) for accreting black holes, independent of the black hole mass, whereas it is similar to 0.1 alpha(2)M(Edd) for neutron stars. Advection-dominated accretion is therefore more likely to occur in accreting black holes, and these systems will be underluminous for their M because the bulk of the energy is advected into the hole rather than being radiated. We find that T-e in accreting black hole flows rises up to similar to 10(9)-10(10) K, compared to T-e similar to 10(8.5)-10(9) K in neutron star systems. Spectra of accreting black holes are therefore expected to be harder than those of accreting neutron stars. Pair effects are aso more likely in black hole systems, though only at higher M than those we consider. RP NARAYAN, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 66 TC 885 Z9 893 U1 5 U2 14 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1995 VL 452 IS 2 BP 710 EP 735 DI 10.1086/176343 PN 1 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RY932 UT WOS:A1995RY93200023 ER PT J AU CHENG, FH VRTILEK, SD RAYMOND, JC AF CHENG, FH VRTILEK, SD RAYMOND, JC TI AN ARCHIVAL STUDY OF HUBBLE-SPACE-TELESCOPE OBSERVATIONS OF HERCULES X-1/HZ HERCULIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; BINARIES, ECLIPSING; PULSARS, INDIVIDUAL (HERCULES X-L)-STARS,; INDIVIDUAL (HERCULES X-1); X-RAYS, STARS ID X-RAY SOURCE; MULTIWAVELENGTH CAMPAIGN; IUE AB We present an archival study of observations of Her X-1/HZ Her obtained by the Faint Object Spectrograph (FOS) on the Hubble Space Telescope (HST). The optical light curve of HZ Her has previously been modeled as an X-ray heated star (e.g., Bahcall & Bahcall 1972) or an X-ray heated star plus disk (e.g., Gerend & Boynton 1976; Howarth & Wilson 1983a, b). We have utilized the system geometry as modeled by Howarth & Wilson (1983a) and have added blackbody components to our X-ray heating code to allow us to match better the observed slope of the HST/FOS spectrum and the strength of the Balmer jump. By fitting our model to the HST/FOS spectrum obtained at total eclipse (binary phase 0.0), we determine the mean temperature of the unheated star surface to be 8100+/-240 K, consistent with an A7 star. From the best-fit model to the HST/FOS spectrum near the binary phase 0.5, we determine a mass transfer rate M = (6.5+/-0.9) x 10(-9) M(circle dot) yr(-1). C1 SHANGHAI JIAO TONG UNIV,INST SPACE SCI,SHANGHAI 200030,PEOPLES R CHINA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP CHENG, FH (reprint author), UNIV MARYLAND,DEPT ASTRON,COLLEGE PK,MD 20742, USA. NR 22 TC 32 Z9 32 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1995 VL 452 IS 2 BP 825 EP 832 DI 10.1086/176351 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RY932 UT WOS:A1995RY93200031 ER PT J AU ZUCKER, S TORRES, G MAZEH, T AF ZUCKER, S TORRES, G MAZEH, T TI STUDY OF SPECTROSCOPIC BINARIES WITH TODCOR .3. APPLICATION TO TRIPLE-LINED SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE BINARIES, SPECTROSCOPIC; STARS, INDIVIDUAL (HD 100018); TECHNIQUES, SPECTROSCOPIC ID MULTIPLE STELLAR-SYSTEMS; STARS; SEPARATION; SPECTRA; ORBITS AB In a previous paper we introduced TODCOR, a new two-dimensional correlation technique, to analyze spectra of binary stars and derive the Doppler shifts of the two components. We propose here a generalization of TODCOR to analyze spectra of triple-lined stellar systems and derive the Doppler shifts of the three components. The algorithm computes the correlation of the observed spectrum against combinations of three template spectra, with all possible shifts. Thus, the correlation is a three-dimensional function in velocity space. The location of the maximum of this function corresponds to the actual shifts of the three components. We demonstrate the difficulties of the one-dimensional cross-correlation and the advantages of the new algorithm with a simulated example. We also analyze with the algorithm a real test case, HD 100018, and we show that the velocities derived with the new extension of TODCOR solve a long-standing discrepancy between the old orbital elements and the mass estimate for the system. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP ZUCKER, S (reprint author), TEL AVIV UNIV, SCH PHYS & ASTRON, RAYMOND & BEVERLY SACKLER FAC EXACT SCI, IL-69978 TEL AVIV, ISRAEL. NR 33 TC 32 Z9 32 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1995 VL 452 IS 2 BP 863 EP 869 DI 10.1086/176354 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RY932 UT WOS:A1995RY93200034 ER PT J AU TORRES, G STEFANIK, RP LATHAM, DW MAZEH, T AF TORRES, G STEFANIK, RP LATHAM, DW MAZEH, T TI STUDY OF SPECTROSCOPIC BINARIES WITH TODCOR .4. THE MULTIPLICITY OF THE YOUNG NEARBY STAR HD-98800 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BINARIES, SPECTROSCOPIC; BINARIES, VISUAL; CIRCUMSTELLAR MATTER; STARS, INDIVIDUAL (HD 98800) ID HD-98800 AB We report extensive radial velocity observations of this unsual K-type ''Vega-excess'' star and show that each component of the well-known close visual pair is itself a spectroscopic binary. The primary is a single-lined binary with a period of 262 days, and the companion is a double-lined binary with a 315 day period. The difference in the center-of-mass velocities of HD 98800 A and B combined with astrometric information allow us to place tight constraints on the orbit of the wide pair. We show that if the pair is bound, the stars must now be approaching perisystem in an extremely eccentric, long-period orbit which does not leave enough room for a circumstellar dust disk around either of the spectroscopic binaries. However, there is no proof yet that the two visual components are physically connected, and it seems rather unlikely that we happen to be observing a system like this so close to maximum approach. We discuss alternative scenarios that seem just as unlikely and conclude that the stability of the disk is not yet understood. C1 SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560. TEL AVIV UNIV,SCH PHYS & ASTRON,RAYMOND & BEVERLY SACKLER FAC EXACT SCI,IL-69978 TEL AVIV,ISRAEL. RP TORRES, G (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 32 TC 49 Z9 49 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1995 VL 452 IS 2 BP 870 EP 878 DI 10.1086/176355 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RY932 UT WOS:A1995RY93200035 ER PT J AU NEFF, JE ONEAL, D SAAR, SH AF NEFF, JE ONEAL, D SAAR, SH TI ABSOLUTE MEASUREMENTS OF STARSPOT AREA AND TEMPERATURE - II-PEGASI IN 1989 OCTOBER SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, ACTIVITY; STARS, INDIVIDUAL (II PEGASI); STARS, LATE-TYPE; TECHNIQUES, SPECTROSCOPIC ID RS-CANUM-VENATICORUM; ROTATIONAL MODULATION; PHYSICAL PARAMETERS; DYNAMIC PHENOMENA; DRACONIS STARS; BINARY-SYSTEMS; AUGUST 1989; DRA STARS; M-DWARFS; X-RAY AB We are developing an empirical spectrum synthesis technique that yields independent measurements of starspot filling factor, f(S), and starspot temperature, T-S, by fitting TiO bands of differing temperature sensitivity. The absolute depth of the TiO bands constrains f(S), while the ratio of their depths is a function only of T-S. One strength of this technique is its ability to determine the spot parameters in traditionally difficult cases: slowly rotating stars, uniformly spotted stars, and stars that always have spots. For this initial study, we have used a simpler procedure of measuring the band depths in the most spotted star in our survey (the single-lined RS CVn binary system II Pegasi) and for a full grid of comparison stars (inactive G, K, and M dwarfs and giants). This yields T-S and f(S) for a given assumed temperature of the nonspotted photosphere, T-Q. The latter was further constrained by the use of simultaneous photometry. We have analyzed a series of spectra of II Peg obtained throughout a single 6.7 day rotational cycle in 1989 October. We find that starspots on II Peg are better modeled by comparison spectra of giants than by dwarfs. Combining TiO analysis with contemporaneous photometry, we find that cool starspots (T-S approximate to 3500 K) are always visible, with a fractional projected coverage of the visible hemisphere varying from 54% to 64% as the star rotates. The nonspotted photosphere has a temperature T-Q approximate to 4800 K. Our results imply that even at the historical light maximum of V = 7.2, at least 34% of II Peg was covered by starspots. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP NEFF, JE (reprint author), PENN STATE UNIV,DEPT ASTRON & ASTROPHYS,525 DAVEY LAB,UNIVERSITY PK,PA 16802, USA. NR 57 TC 68 Z9 68 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1995 VL 452 IS 2 BP 879 EP 893 DI 10.1086/176356 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RY932 UT WOS:A1995RY93200036 ER PT J AU SLANE, P LLOYD, N AF SLANE, P LLOYD, N TI SOFT-X-RAY EMISSION FROM SELECTED ISOLATED PULSARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE PULSARS, GENERAL; RADIATION MECHANISMS, NONTHERMAL; RADIATION MECHANISMS, THERMAL; X-RAYS, STARS ID MODEL ATMOSPHERES; NEUTRON-STARS AB The soft X-ray emission from isolated neutron stars (NSs) may originate from a number of processes, each of which probes a unique characteristic of the interior or magnetospheric structure. In order to characterize this emission in the context of current models, we have begun an archival investigation of such emission using data from the ROSAT Observatory. Here we report on analysis for seven pulsars based upon data taken with the ROSAT Position Sensitive Proportional Counter (PSPC). For each pulsar, we derive upper limits for the NS surface temperature as well as luminosity values or upper limits associated with a Crab-like power-law interpretation. Several of the pulsars were detected, and for these we have investigated scenarios for emission associated with the cooling of the hot NS interior as well as with the pulsar spin down. The emission from PSR 2334+61 and PSR 0114+58 appears consistent with a spin-down origin, although we cannot rule out emission associated with cooling of the NS interior. For PSR 1822-09, we find that the surface temperature upper limit implied by the nondetection falls below the predictions of several cooling models, potentially providing constraints on interpretations of the interior equation of state. Emission from the vicinity of PSR 1642-03 may be produced by an extended synchrotron nebula associated with the pulsar, but such models appear problematic. Alternatively, the observed flux may be produced by a background object in the field of the pulsar position. RP SLANE, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 23 TC 8 Z9 8 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1995 VL 452 IS 2 BP L115 EP L119 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RY935 UT WOS:A1995RY93500009 ER PT J AU KURUCZ, RL AF KURUCZ, RL TI THE PRIMORDIAL LITHIUM ABUNDANCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, THEORY; STARS, ABUNDANCES; STARS, ATMOSPHERES; STARS, POPULATION II AB The D lines of Li I in extreme Population II stars better than 5500 K are highly temperature sensitive because lithium is nearly all ionized. A one-dimensional model atmosphere represents a space and time average over the actual three-dimensional, moving, hot and cold convective structure. Neutral Li does not have the average behavior represented by the one-dimensional model. Lithium is overionized by a factor of 10 so that the Li abundance computed from a one-dimensional model is too small by this same factor. Consequently, log (N-Li/N-total + 12 > 3.0. This higher Li abundance resolves the only discrepancy in the radiatively driven cosmological model of the universe previously discussed by Kurucz. Because the baryon density is high enough to produce a flat, or nearly flat, universe, the number of stars can increase by a factor of 10, and the amount of radiation given off by those stars in the first billion years can increase by a factor of 10 over what is possible with a low baryon density. This model can explain the formation of Population III stars, globular clusters, galaxies, quasars, voids, galaxy clusters, streaming, and large-scale structure. It can explain isolated galactic evolution and morphology including bulges, disks, and abundances. RP KURUCZ, RL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 27 TC 38 Z9 38 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 1995 VL 452 IS 1 BP 102 EP 108 DI 10.1086/176283 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RX157 UT WOS:A1995RX15700009 ER PT J AU KOCHANEK, CS FALCO, EE SCHILD, R AF KOCHANEK, CS FALCO, EE SCHILD, R TI THE FKS GRAVITATIONAL LENS SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE GRAVITATIONAL LENSING; QUASARS, GENERAL ID HUBBLE-SPACE-TELESCOPE; QUASI-STELLAR OBJECTS; SNAPSHOT SURVEY; LUMINOSITY FUNCTION; GALAXY LUMINOSITY; TRIPLE QUASAR; STAR COUNTS; STATISTICS; CATALOG; SEARCH AB We describe the first part of a survey for lensed quasars. The first sample includes 142 images of 121 quasars. All images are analyzed using empirical point-spread functions and Monte Carlo simulations of the observations. We use Monte Carlo simulations to study the expected distribution of the properties of single stellar images, image pairs, symmetric image quads, known gravitational lenses, and statistical samples from the best-fitting statistical lens models. The Monte Carlo simulations reproduce the essential features of the observational data. We accidentally rediscovered the lensed pair LBQS 1009-0252; we found two strong lens candidates Q0010+023 and Q0011-002 that turned out to be low-redshift galaxies, one weaker candidate Q0456+025 that is probably a false positive, and one false positive Q0847+100; and we had two cosmic-ray hits on the quasar image, Q1318-050 and Q1038+311. With our candidate selection criteria we expect to find three statistical false positives in our sample based on the Monte CarIo simulations. Other than these seven objects we found five images within 6 ''.0 of the quasars, and we have identified two as a stars and one as the lower redshift quasar in LBQS 1009-0252. We found a total of 22 objects within 12 ''.0 of the quasars, seven of which are brighter than the quasar. Of these 22, we have identified eight as stars and one as a quasar. The spatial and magnitude distributions of these objects match the predicted distribution of stars and galaxies. Depending on the cosmological model and the mass normalization for E/SO galaxies, we expected to find between 0.8 and 2.5 lenses in this sample. RP KOCHANEK, CS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 54 TC 29 Z9 29 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 1995 VL 452 IS 1 BP 109 EP 139 DI 10.1086/176284 PN 1 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RX157 UT WOS:A1995RX15700010 ER PT J AU MATHUR, S ELVIS, M WILKES, B AF MATHUR, S ELVIS, M WILKES, B TI TESTING UNIFIED X-RAY ULTRAVIOLET ABSORBER MODELS WITH NGC-5548 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (NGC 5548); GALAXIES, ACTIVE; GALAXIES, SEYFERT; ULTRAVIOLET GALAXIES; X-RAYS, GALAXIES ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; TYPE-1 SEYFERT-GALAXIES; NGC-5548; ABSORPTION; SPECTRUM; STEPS; SIZE AB The bright Seyfert galaxy NGC 5548 shows absorption features in its X-ray and UV spectra. The large amount of optical/UV and X-ray monitoring data available for this object makes it an ideal candidate to test our model of a common X-ray/UV absorber. We show that the X-ray/UV absorption is caused by a highly ionized (2.2 < U < 2.8), high column density (N-H = 3.8 x 10(21) cm(-2)) gas situated outside the C IV emitting region (2 x 10(16) cm < r(abs) < 2 x 10(18) cm). The gas is outflowing with a mean velocity of 1200 +/- 260 km s(-1) and corresponding kinetic luminosity of similar to 10(43) ergs s(-1). The gas is more highly ionized and has a much larger column density than earlier estimates based on UV data alone. This third example of an X-ray/UV absorber reinforces our earlier conclusion that outflowing, highly ionized gas is common in the inner regions of quasars. RP MATHUR, S (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. OI Wilkes, Belinda/0000-0003-1809-2364 NR 33 TC 122 Z9 122 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 1995 VL 452 IS 1 BP 230 EP 237 DI 10.1086/176294 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RX157 UT WOS:A1995RX15700020 ER PT J AU HJORTH, J VESTERGAARD, M SORENSEN, AN GRUNDAHL, F AF HJORTH, J VESTERGAARD, M SORENSEN, AN GRUNDAHL, F TI DETECTION OF A FAINT OPTICAL JET IN 3C-120 SO ASTROPHYSICAL JOURNAL LA English DT Article ID PKS 0521-36; 3C-120; POLARIZATION; MORPHOLOGY; PHOTOMETRY; GALAXIES; SCALES; 3C120; M87 AB We report the detection of an optical jet in the nearby Seyfert 1 radio galaxy 3C 120. The optical jet coincides with the well-known radio jet and emits continuum radiation (B, V', I) with a radio-to-optical spectral index of 0.65. There are no clear optical counterparts to the radio knots, although the optical condensation A of the galaxy, which includes the bright 4'' radio knot, is found to be 12% polarized with the electric field vectors perpendicular to the jet. These findings indicate that 3C 120 contains the sixth known extragalactic optical synchrotron jet, quite similar in its properties to the jet of PKS 0521-36. The outer part of the jet is the faintest known optical jet and was discovered as the result of a dedicated effort to detect it. It is therefore possible that more optical jets can be discovered in systematic searches by combining deep imaging in the optical or near-infrared with careful galaxy subtraction methods. C1 AARHUS UNIV,INST PHYS & ASTRON,DK-8000 AARHUS C,DENMARK. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. COPENHAGEN UNIV OBSERV,DK-1350 COPENHAGEN,DENMARK. NORDIC OPT TELESCOPE,OBSERV ROQUE MUCHACHOS,E-38700 SANTA CRUZ PALMA,SPAIN. RP HJORTH, J (reprint author), UNIV CAMBRIDGE,INST ASTRON,MADINGLEY RD,CAMBRIDGE CB3 0HA,ENGLAND. RI Vestergaard, Marianne/M-5247-2014 OI Vestergaard, Marianne/0000-0001-9191-9837 NR 28 TC 21 Z9 21 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 1995 VL 452 IS 1 BP L17 EP & PN 2 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RX158 UT WOS:A1995RX15800005 ER PT J AU HIRAI, K HELLER, EJ GASPARD, P AF HIRAI, K HELLER, EJ GASPARD, P TI SPECTROSCOPY AND INTRAMOLECULAR DYNAMICS VIA MOLECULAR VIBROGRAM ANALYSIS SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SEMICLASSICAL DYNAMICS; QUANTUM-MECHANICS; FOURIER-TRANSFORM; BOUND SPECTRUM; CLOSED ORBITS; CS2 MOLECULE; CHAOS; PHOTOFRAGMENTATION AB Molecular spectra have traditionally been interpreted in the frequency domain and more recently in the time domain. For simple absorption and emission spectra these are the Fourier transform of one another. In this paper we illustrate that it can be useful to examine spectra in a compromise representation which balances uncertainties in time and energy. In this paper we give the basic ideas and several examples which reveal dynamical effects hidden in either energy or time representations. The resulting ''vibrogram'' is available from experimental spectra or theoretical calculations. (C) 1995 American Institute of Physics. C1 HARVARD UNIV,DEPT CHEM,CAMBRIDGE,MA 02138. HARVARD UNIV,HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. FREE UNIV BRUSSELS,SERV CHIM PHYS,BRUSSELS,BELGIUM. FREE UNIV BRUSSELS,CTR NONLINEAR PHENOMENA & COMPLEX SYST,BRUSSELS,BELGIUM. RP HIRAI, K (reprint author), UNIV WASHINGTON,DEPT CHEM,CAMBRIDGE,MA 02138, USA. NR 39 TC 21 Z9 21 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD OCT 8 PY 1995 VL 103 IS 14 BP 5970 EP 5978 DI 10.1063/1.470426 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA RY168 UT WOS:A1995RY16800011 ER PT J AU WALLER, TR AF WALLER, TR TI THE MISIDENTIFIED HOLOTYPE OF ARGOPECTEN CIRCULARIS (BIVALVIA, PECTINIDAE) SO VELIGER LA English DT Article AB The holotype of the common Eastern Pacific scallop Argopecten circularis (G. B. Sowerby I, 1835) was misidentified as a new species by Sowerby. Rather, it is a specimen of the Western Atlantic Bay Scallop, Argopecten irradians concentricus (Say, 1822), accompanied by erroneous data saying that it came from the Gulf of California at Guaymas, Mexico. The holotype of Pecten circularis is illustrated herein for the first time and its tangled background discussed. The valid name of this common species should become Argopecten ventricosus (G. B. Sowerby II, 1842), a lectotype for which is designated and figured. RP WALLER, TR (reprint author), SMITHSONIAN INST,MUSEUM NATL HIST NAT,DEPT PALEOBIOL,WASHINGTON,DC 20560, USA. NR 28 TC 2 Z9 6 U1 0 U2 0 PU CALIF MALACOZOOLOGICAL SOC INC PI SANTA BARBARA PA SANTA BARBARA MUSEUM NATURAL HISTORY, 2559 PUESTA DEL SOL RD, SANTA BARBARA, CA 93105 SN 0042-3211 J9 VELIGER JI Veliger PD OCT 2 PY 1995 VL 38 IS 4 BP 298 EP 303 PG 6 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA TC898 UT WOS:A1995TC89800003 ER PT J AU HERSHLER, R AF HERSHLER, R TI NEW FRESH-WATER SNAILS OF THE GENUS PYRGULOPSIS (RISSOOIDEA, HYDROBIIDAE) FROM CALIFORNIA SO VELIGER LA English DT Article ID GASTROPODA; SYSTEM AB Seven new species of Recent springsnails belonging to the large genus Pyrgulopsis are described from California. Pyrgulopsis diablensis sp. nov., known from a single site in the San Joaquin Valley, P. longae sp. nov., known from a single site in the Great Basin (Lahontan system), and P. taylori sp. nov., narrowly endemic in one south-central coastal drainage, are related to a group of previously known western species also having terminal and penial glands on the penis. Pyrgulopsis eremica sp. nov., from the Great Basin and other interior drainages in northeast California, and P. greggi sp. nov., narrowly endemic in the Upper Kern River basin, differ from all other described congeners in lacking penial glands, and are considered to be derived from a group of western species having a small distal lobe and weakly developed terminal gland. Pyrgulopsis gibba sp. nov., known from a few sites in extreme northeastern California (Great Basin), has a unique complement of penial ornament consisting of terminal gland, Dg3, and ventral gland. Pyrpulopsis ventricosa sp. nov., narrowly endemic in the Clear Lake basin, is related to two previously described California species also having a full complement of glands on the penis (Pg, Tg, Dg1-3) and an enlarged bursa copulatrix. RP HERSHLER, R (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 16 TC 10 Z9 10 U1 0 U2 0 PU CALIF MALACOZOOLOGICAL SOC INC PI SANTA BARBARA PA SANTA BARBARA MUSEUM NATURAL HISTORY, 2559 PUESTA DEL SOL RD, SANTA BARBARA, CA 93105 SN 0042-3211 J9 VELIGER JI Veliger PD OCT 2 PY 1995 VL 38 IS 4 BP 343 EP 373 PG 31 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA TC898 UT WOS:A1995TC89800008 ER PT J AU Chatters, JC Campbell, SK Smith, GD Minthorn, PE AF Chatters, JC Campbell, SK Smith, GD Minthorn, PE TI Bison procurement in the Far West: A 2,100-year-old kill site on the Columbia Plateau SO AMERICAN ANTIQUITY LA English DT Article AB Bison bones are found in Columbia Plateau archaeological sites from throughout the Holocene, yet no information on people tactics for procuring them has yet been reported. The discovery of the Tsulim Site, a 2,100-year-old bison kill near the Columbia River in central Washington, has provided the opportunity to investigate those tactics. Despite the deteriorated state of the evidence, analysis of stone artifacts, faunal remains, and site geology revealed that at least eight animals were killed in the apex of a parabolic dune during the early to mid-winter by hunters using both atlatl and bow. Local topography and meteorology make it most likely that the herd was encountered in a low paleochannel, driven northward between the limbs of the dune, up the steep channel wall, and into the kill area, a sort of inverted buffalo jump. Results not only illuminate the large-game hunting practices of the Plateau peoples, but also point out how much can be learned from disturbed, low-density scatters of debris that are often dismissed as insignificant. C1 WESTERN WASHINGTON UNIV,DEPT ANTHROPOL,BELLINGHAM,WA 98225. LARAMIE SOIL SYST,LARAMIE,WY 82070. SMITHSONIAN INST,NATL MUSEUM NAT HIST,REPATRIAT OFF,WASHINGTON,DC 20560. RP Chatters, JC (reprint author), APPL PALEOSCI,648 ST ST,RICHLAND,WA 99352, USA. NR 40 TC 10 Z9 11 U1 0 U2 8 PU SOC AMER ARCHAEOLOGY AMERICAN ANTIQUITY PI WASHINGTON PA 900 SECOND ST., NE #12 ATTN: BRIGHID BRADY-DE LAMBERT, WASHINGTON, DC 20002-3557 SN 0002-7316 J9 AM ANTIQUITY JI Am. Antiq. PD OCT PY 1995 VL 60 IS 4 BP 751 EP 763 DI 10.2307/282056 PG 13 WC Anthropology; Archaeology SC Anthropology; Archaeology GA TM862 UT WOS:A1995TM86200013 ER PT J AU HERKEN, G AF HERKEN, G TI OPERATION CROSSROADS - THE ATOMIC TESTS AT BIKINI ATOLL - WEISGALL,JM SO AMERICAN HISTORICAL REVIEW LA English DT Book Review RP HERKEN, G (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER HISTORICAL REVIEW PI WASHINGTON PA 400 A ST SE, WASHINGTON, DC 20003 SN 0002-8762 J9 AM HIST REV JI Am. Hist. Rev. PD OCT PY 1995 VL 100 IS 4 BP 1330 EP 1331 DI 10.2307/2168360 PG 2 WC History SC History GA TA731 UT WOS:A1995TA73100146 ER PT J AU WASHBURN, WE AF WASHBURN, WE TI AMERICA IN EUROPEAN CONSCIOUSNESS, 1493-1750 - KUPPERMAN,KO SO AMERICAN STUDIES INTERNATIONAL LA English DT Book Review RP WASHBURN, WE (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU GEORGE WASHINGTON UNIV PI WASHINGTON PA AMERICAN STUDIES PROGRAM, WASHINGTON, DC 20052 SN 0003-1321 J9 AM STUD INT JI Am. Stud. Int. PD OCT PY 1995 VL 33 IS 2 BP 85 EP 85 PG 1 WC History SC History GA TD116 UT WOS:A1995TD11600025 ER PT J AU WASHBURN, WE AF WASHBURN, WE TI UN-AMERICAN ACTIVITIES - THE TRIALS OF REMINGTON,WILLIAM - MAY,G SO AMERICAN STUDIES INTERNATIONAL LA English DT Book Review RP WASHBURN, WE (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU GEORGE WASHINGTON UNIV PI WASHINGTON PA AMERICAN STUDIES PROGRAM, WASHINGTON, DC 20052 SN 0003-1321 J9 AM STUD INT JI Am. Stud. Int. PD OCT PY 1995 VL 33 IS 2 BP 114 EP 115 PG 2 WC History SC History GA TD116 UT WOS:A1995TD11600059 ER PT J AU WASHBURN, WE AF WASHBURN, WE TI AN AMERICAN IN JAPAN, 1945-1948 - A CIVILIAN VIEW OF THE OCCUPATION - VANSTAAVEREN,J SO AMERICAN STUDIES INTERNATIONAL LA English DT Book Review RP WASHBURN, WE (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU GEORGE WASHINGTON UNIV PI WASHINGTON PA AMERICAN STUDIES PROGRAM, WASHINGTON, DC 20052 SN 0003-1321 J9 AM STUD INT JI Am. Stud. Int. PD OCT PY 1995 VL 33 IS 2 BP 115 EP 116 PG 2 WC History SC History GA TD116 UT WOS:A1995TD11600060 ER PT J AU WASHBURN, WE AF WASHBURN, WE TI THE QUOTABLE JOHNSON,PAUL - A TOPICAL COMPILATION OF HIS WIT, WISDOM AND SATIRE - MARLIN,GJ, RABATIN,RP SO AMERICAN STUDIES INTERNATIONAL LA English DT Book Review RP WASHBURN, WE (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU GEORGE WASHINGTON UNIV PI WASHINGTON PA AMERICAN STUDIES PROGRAM, WASHINGTON, DC 20052 SN 0003-1321 J9 AM STUD INT JI Am. Stud. Int. PD OCT PY 1995 VL 33 IS 2 BP 116 EP 116 PG 1 WC History SC History GA TD116 UT WOS:A1995TD11600061 ER PT J AU CREEL, S MONFORT, SL CREEL, NM WILDT, DE WASER, PM AF CREEL, S MONFORT, SL CREEL, NM WILDT, DE WASER, PM TI PREGNANCY, ESTROGENS AND FUTURE REPRODUCTIVE SUCCESS IN SERENGETI DWARF MONGOOSES SO ANIMAL BEHAVIOUR LA English DT Note ID SUPPRESSION; BEHAVIOR C1 ROCKEFELLER UNIV,FIELD RES CTR ECOL & ETHOL,NEW YORK,NY 10021. NATL ZOOL PK,CONSERVAT & RES CTR,FRONT ROYAL,VA. PURDUE UNIV,DEPT BIOL SCI,W LAFAYETTE,IN 47907. RP CREEL, S (reprint author), SELOUS CONSERVAT PROGRAMME,FRANKFURT ZOOL SOC,SELOUS WILD DOG PROJECT,BOX 1519,DAR ES SALAAM,TANZANIA. NR 15 TC 5 Z9 5 U1 2 U2 4 PU ACADEMIC PRESS (LONDON) LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD OCT PY 1995 VL 50 BP 1132 EP 1135 DI 10.1016/0003-3472(95)80113-8 PN 4 PG 4 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA TA687 UT WOS:A1995TA68700024 ER PT J AU WATSON, R AF WATSON, R TI RIGAUD PORTRAIT IDENTIFICATION SO APOLLO-THE INTERNATIONAL MAGAZINE OF THE ARTS LA English DT Letter RP WATSON, R (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU APOLLO MAGAZINE LTD PI LONDON PA 29 CHESHAM PLACE, LONDON, ENGLAND SW1X 8HB SN 0003-6536 J9 APOLLO JI Apollo-Int. Mag. Arts PD OCT PY 1995 VL 142 IS 404 BP 61 EP 61 PG 1 WC Art SC Art GA RZ265 UT WOS:A1995RZ26500022 ER PT J AU MATHUR, S ELVIS, M AF MATHUR, S ELVIS, M TI GB-1508+5714, THE FIRST Z-GREATER-THAN-4 RADIO-SELECTED QUASAR IN X-RAYS SO ASTRONOMICAL JOURNAL LA English DT Article ID MEDIUM-SENSITIVITY SURVEY; SPECTRA; OBJECTS AB We report the detection in x ray of a high redshift (z=4.30) radio-loud quasar, GB 1508 +/- 5714, the first radio-selected z>4 quasar seen in x rays. The quasar was observed serendipitously with the Einstein observatory IPC at 0.02 +/- 0.003 counts s(-1). It is ten times brighter than the other two z>4 x-ray detected quasars. The x-ray source is unusually hard, implying either alpha(E)<-0.2, or N-H>10(22) atoms cm(-2) (1 sigma limits) for a simple power-law plus intrinsic (z=4.3) absorption. Intrinsic absorption would make GB 1508 + 5714 similar to a large fraction of z similar to 3 radio-loud quasars. (C) 1995 American Astronomical Society. RP MATHUR, S (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 30 TC 11 Z9 11 U1 3 U2 3 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 1995 VL 110 IS 4 BP 1551 EP 1553 DI 10.1086/117627 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RZ271 UT WOS:A1995RZ27100008 ER PT J AU FRANKLIN, FA AF FRANKLIN, FA TI CHAOTIC ORBITS WITHIN THE 3/2-JOVIAN MEAN MOTION RESONANCE SO ASTRONOMICAL JOURNAL LA English DT Article ID RESTRICTED 3-BODY PROBLEM; HILDA-TYPE ASTEROIDS; ORIGINAL DISTRIBUTION; SECULAR RESONANCE; STABILITY; DYNAMICS; JUPITER; SATURN; SYSTEM AB Since the minor planet population as a whole shows a mean proper eccentricity, e(p), near 0.1, this paper starts by asking why the Hilda group, some sixty objects whose mean motions lie very close to 3/2 times that of Jupiter, all have e(p)>0.1. The Hildas execute small oscillations, usually called librations, about this 3/2 ratio and these oscillations have a well defined frequency v, which can, for example, be determined from periodic variations in a minor planet's semimajor axis or eccentricity. Another basic frequency, omega, is given by the apsidal motion. We show that orbits for which the two frequencies differ by small integral or half integral multiples [i.e., v=(n/2)omega, n=3,4,5....] are clearly chaotic, with Lyapunov times short enough to suggest instability. Such orbits lie within the 3:2 mean motion resonance and all have e(p)<0.1. Although the low e(p) region is streaked with chaotic zones, they are generally narrow, hence generating many chaotic orbits, and possibly depopulating the entire e(p)<0.1 region, would seem to require an added process that would slightly alter the loci of the resonances over time. At higher multiples of the two frequencies, particularly v=6 omega, orbits are remarkably regular, even when the amplitude of libration of successive conjunctions of Jupiter and a minor planet about the latter's pericenter is even as large as 90 deg. In fact, numerical results show that all of the real Hildas having large librations lie at or very close to such commensurabilities, while hypothetical bodies that do not are markedly chaotic. (C) 1995 American Astronomical Society. RP FRANKLIN, FA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 19 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 1995 VL 110 IS 4 BP 1879 EP 1893 DI 10.1086/117659 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RZ271 UT WOS:A1995RZ27100040 ER PT J AU PERIVOLAROPOULOS, L AF PERIVOLAROPOULOS, L TI SPECTRAL-ANALYSIS OF MICROWAVE BACKGROUND PERTURBATIONS INDUCED BY COSMIC STRINGS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMIC MICROWAVE BACKGROUND; COSMIC STRINGS; COSMOLOGY, THEORY; LARGE-SCALE STRUCTURE OF UNIVERSE ID DEGREE ANGULAR SCALES; INFLATIONARY UNIVERSE; PECULIAR VELOCITIES; DOMAIN-WALLS; ANISOTROPY; RADIATION; WAKES; COBE; FLUCTUATIONS; EVOLUTION AB Using a simple analytic model based on seed superposition we obtain an approximation to the spectrum of microwave background perturbations induced by cosmic strings on all angular scales larger than about 2 arcmin. We assume standard recombination in an Einstein-de Sitter universe with h=1/2 and study the fluctuation spectrum along a great circle in the sky. Doppler and potential perturbations on the last scattering surface (Sachs-Wolfe effect) are shown to dominate over post-recombination perturbations on scales smaller than about 2 degrees. Using a filter function corresponding to the COBE experiment we obtain a lower bound to the power spectrum index n greater than or similar to 1.35 in good agreement with the recently announced second year COBE data showing n similar or equal to 1.5. The only free parameter (G mu) of the string model is tired by normalizing on the COBE detection leading to G mu=1.6x10(-6). Other parameters (e.g., the rms string velocity) are fixed by comparing with string simulations. Using these parameter values we compare the rms temperature fluctuations (Delta T/T)(rms) predicted for ongoing experiments (Tenerife, SP91, MAX, OVRO, etc.) with detections and with the corresponding predictions of inflationary models. C1 BROWN UNIV,DEPT PHYS,PROVIDENCE,RI 02912. RP PERIVOLAROPOULOS, L (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,DIV THEORET ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Perivolaropoulos, Leandros/0000-0001-9330-2371 NR 62 TC 26 Z9 26 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 1995 VL 451 IS 2 BP 429 EP 435 DI 10.1086/176231 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RV626 UT WOS:A1995RV62600002 ER PT J AU VIKHLININ, A FORMAN, W JONES, C MURRAY, S AF VIKHLININ, A FORMAN, W JONES, C MURRAY, S TI MATCHED-FILTER SOURCE DETECTION APPLIED TO THE ROAST PSPC AND THE DETERMINATION OF THE NUMBER-FLUX RELATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, STATISTICS; METHODS, STATISTICAL; X-RAYS, GALAXIES ID X-RAY SURVEY; N-LOG S; NOISE AB We investigate the application, for X-ray astronomy, of a source detection algorithm similar to the so-called matched filter (MF) technique. From the instrument point-spread function (PSF) we construct filters which are much closer to optimal for point-source detection than are the square functions used in the traditional sliding box (SE) method and at the same time ensure local background subtraction. We develop the technique primarily for use with the ROSAT PSPC images. Through intensive Monte Carlo simulations we calibrate the method for the real PSPC PSF and the values of background intensity typically found for medium and deep exposure (>10,000 s) ROSAT fields. From the simulations, all those functions necessary to correct the measured source intensities and the number-flux relation (log N-log S) are derived. It is shown that, indeed, we are able to obtain unbiased estimates of source intensities and the log N-log S function down to S/N similar to 2, as long as the PSPC PSF approximation we use is valid. We compare our method with the SE technique, as it is traditionally used, and find that the MF algorithm always works significantly better than the SE method. In particular, the latter overestimates the source fluxes and the log N-log S function near the detection threshold and therefore requires additional calibrations to correct for these biases. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP VIKHLININ, A (reprint author), MOSCOW SPACE RES INST,PROFSOUZNAYA 84-32,MOSCOW 117810,RUSSIA. NR 13 TC 43 Z9 43 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 1995 VL 451 IS 2 BP 542 EP 552 DI 10.1086/176242 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RV626 UT WOS:A1995RV62600013 ER PT J AU VIKHLININ, A FORMAN, W JONES, C MURRAY, S AF VIKHLININ, A FORMAN, W JONES, C MURRAY, S TI ROSAT EXTENDED MEDIUM-DEEP SENSITIVITY SURVEY - SOURCE COUNTS FOR 130 FIELDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE SURVEYS; X-RAYS, GALAXIES ID X-RAY SURVEY; BACKGROUND SPECTRUM AB We present an analysis of serendipitous sources detected in 130 high Galactic latitude, long-exposure ROSAT PSPC observations. By application of an efficient source detection technique and analyzing a larger number of fields compared to previous studies, we have sufficiently increased the sky coverage of the survey and are able to investigate the X-ray source population over almost three decades of intensity, from approximately 1.2 x 10(-15) to approximately 7.0 x 10(-13) ergs s(-1) cm(-2) in the 0.5-2.0 keV energy band. Using the 2678 detected sources, we refine the extragalactic log N-log S and find that the differential number-flux relation is well described by a broken power law which flattens from alpha = 2.55 +/- 0.08 above a flux of 2.2 +/- 0.2 x 10(-14) ergs s(-1) cm(-2) to 1.86 +/- 0.06 at fainter fluxes, which is in a good agreement with previous studies. At our limiting flux of 1.2 x 10(-15) ergs s(-1) cm(-2), the detected (point) sources comprise 66 +/- 7% (68% confidence limits) of the X-ray background in the 1-2 keV band. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP VIKHLININ, A (reprint author), MOSCOW SPACE RES INST,PROFSOYUZNAYA 84-32,MOSCOW 117810,RUSSIA. NR 22 TC 25 Z9 25 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 1995 VL 451 IS 2 BP 553 EP 563 DI 10.1086/176243 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RV626 UT WOS:A1995RV62600014 ER PT J AU VIKHLININ, A FORMAN, W JONES, C MURRAY, S AF VIKHLININ, A FORMAN, W JONES, C MURRAY, S TI ROSAT EXTENDED MEDIUM-DEEP SENSITIVITY SURVEY - AVERAGE SOURCE SPECTRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE SURVEYS; X-RAYS, GENERAL ID X-RAY-SPECTRA; ACTIVE GALACTIC NUCLEI; GALAXIES; QUASARS; ABSORPTION AB We present a spectral analysis of the serendipitous sources detected in 130 high Galactic latitude, long-exposure ROSAT PSPC observations. By application of an efficient source detection technique and analyzing a large number of fields, we have detected 2678 sources above our limiting flux of 1.2 x 10(-15) ergs s(-1) cm(-2) (see Papers I and II). In this paper, we investigate the spectral properties of the detected sources. Analysis of hardness ratios as a function of flux confirms the suggestion in the recent work of Hasinger et al. that the source spectra show a hardening as the source fluxes decrease. Quantitatively, the hardness ratios are equivalent to a power-law energy index of 0.7 at a flux of 6 x 10(-15) ergs s(-1) cm(-2). In addition to analyzing mean hardness ratios, we performed detailed spectral fits to the average pulse-height data of the sources as a function of flux. We find that at fluxes above 2 x 10(-14) ergs s(-1) cm(-2), the average spectrum has a best-fit power-law energy index of 1.4 (after accounting for a Galactic stellar component). The best-fit power-law exponent decreases smoothly to 0.4 below a flux of 10(-14) ergs s(-1) cm(-2). This average spectrum of the faintest sources approaches that observed for the 2-10 keV X-ray background. We discuss the implications of measurements of the source counts and average spectra for models of the origin of the X-ray background. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP VIKHLININ, A (reprint author), MOSCOW SPACE RES INST,PROFSOYUZNAYA 84-32,MOSCOW 117810,RUSSIA. OI Forman, William/0000-0002-9478-1682 NR 33 TC 29 Z9 29 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 1995 VL 451 IS 2 BP 564 EP 574 DI 10.1086/176244 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RV626 UT WOS:A1995RV62600015 ER PT J AU ROBINSON, RD CARPENTER, KG PERCIVAL, JW BOOKBINDER, JA AF ROBINSON, RD CARPENTER, KG PERCIVAL, JW BOOKBINDER, JA TI A SEARCH FOR MICROFLARING ACTIVITY ON DME FLARE STARS .1. OBSERVATIONS OF THE DM8E STAR CN LEONIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, ACTIVITY; STARS, FLARE; STARS, INDIVIDUAL (CN LEONIS); ULTRAVIOLET, STARS ID X-RAY-EMISSION; SOLAR-FLARES; ENERGY-RELEASE; VARIABILITY; EXOSAT; AVALANCHES; DYNAMICS; CORONAE; FIELDS; REGION AB Microflares are frequent, short-duration, energetically weak disturbances occurring in the nonradiatively heated regions of the Sun and other magnetically active stars. They are thought to be the low-energy extension of hares commonly seen on active dMe stars and may be a major source of heating the chromosphere and corona of cool stars in general. In this paper we describe rapid time sequence UV photometry of the dMe star CN Leo taken with the High Speed Photometer (HSP) aboard the Hubble Space Telescope (HST). The filter was centered at 240 nm, near wavelengths at which flares are expected to have maximum intensity and the stellar background is small. During 2 hr of on-source observing, a total of 32 flarelike events were detected, with integrated counts ranging from 12 to more than 14,000. In most cases the events had integrated energy ranging between 10(27) and 10(28) ergs and can be classified as microflares. A considerable fine structure was seen in these events, with substantial variations sometimes occurring on timescales of less than 1 s. The occurrence rates for the smaller events showed a power-law distribution, with a slope comparable to that seen for larger events observed from the ground. Extrapolating the occurrence rate relation to nanoflare energies indicates a predicted count rate that is significantly smaller than that observed, suggesting that the nanoflares have a different energy distribution than the larger events. C1 NASA, GODDARD SPACE FLIGHT CTR, ASTRON & SOLAR PHYS LAB, GREENBELT, MD 20771 USA. SMITHSONIAN ASTROPHYS OBSERV, CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV WISCONSIN, SPACE ASTRON LAB, MADISON, WI 53706 USA. RP GODDARD SPACE FLIGHT CTR, COMP SCI CORP, ASTRON PROGRAM, CODE 681, GREENBELT, MD 20771 USA. RI Carpenter, Kenneth/D-4740-2012 NR 38 TC 30 Z9 30 U1 0 U2 0 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 OCT 1 PY 1995 VL 451 IS 2 BP 795 EP 805 DI 10.1086/176266 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RV626 UT WOS:A1995RV62600037 ER PT J AU ZHANG, Q HO, PTP WRIGHT, MCH WILNER, DJ AF ZHANG, Q HO, PTP WRIGHT, MCH WILNER, DJ TI SIO EMISSION IN A JET-LIKE MOLECULAR OUTFLOW TOWARD L1157 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, CLOUDS; ISM, INDIVIDUAL (L1157); ISM, JETS AND OUTFLOWS; STARS, FORMATION ID BIPOLAR OUTFLOWS; DARK CLOUD; JET; GAS; OBJECTS AB We report interferometric observations of the SiO (2-1) and CO (1-0) lines toward the blueshifted lobe of the L1157 bipolar outflow. These observations reveal clumpy SiO emission aligned with highly collimated CO emission. The SiO emission is enhanced in two prominent condensations, similar to those seen in VLA images of the NH3(3, 3) line. The SiO condensation closer to the outflow source peaks within 10 '' of a bright knot of the 2.1 mu m H-2 line emission and shows blueshifted emission extending more than 17 km s(-1) from the cloud velocity. The close association between the SiO and H-2 emission suggests that the SiO emission is excited in the accelerated postshock regions near the head of an underlying jet. The SiO condensation farther downstream shows a smaller velocity extent and no apparent associated H-2 emission. We suggest that the two condensations result from separate interactions of an episodic jet with the surrounding cloud core. In this scenario, the emission region farther downstream results from an older event. Both SiO condensations appear to lead the high-velocity CO emission, consistent with the idea that SiO emission is excited close to the head of the jet and the CO accelerated in the oblique outer wings of the bow shock. C1 UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. UNIV CALIF BERKELEY,RADIO ASTRON LAB,BERKELEY,CA 94720. RP ZHANG, Q (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 23 TC 67 Z9 67 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 1995 VL 451 IS 2 BP L71 EP & PN 2 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RV627 UT WOS:A1995RV62700008 ER PT J AU Larimer, JL Dudley, R AF Larimer, JL Dudley, R TI Accelerational implications of hummingbird display dives SO AUK LA English DT Article ID BEHAVIOR C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP Larimer, JL (reprint author), UNIV TEXAS,DEPT ZOOL,AUSTIN,TX 78712, USA. NR 18 TC 4 Z9 4 U1 0 U2 3 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0004-8038 J9 AUK JI AUK PD OCT PY 1995 VL 112 IS 4 BP 1064 EP 1066 PG 3 WC Ornithology SC Zoology GA UF267 UT WOS:A1995UF26700030 ER PT J AU Winker, K AF Winker, K TI Xiphorhynchus striatigularis (Dendrocolaptidae): Nomen monstrositatum SO AUK LA English DT Article RP Winker, K (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DIV BIRDS,WASHINGTON,DC 20560, USA. RI Winker, Kevin/M-2042-2014 OI Winker, Kevin/0000-0002-8985-8104 NR 23 TC 1 Z9 1 U1 0 U2 0 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0004-8038 J9 AUK JI AUK PD OCT PY 1995 VL 112 IS 4 BP 1066 EP 1070 PG 5 WC Ornithology SC Zoology GA UF267 UT WOS:A1995UF26700031 ER PT J AU TRAINER, JM MCDONALD, DB AF TRAINER, JM MCDONALD, DB TI SINGING PERFORMANCE, FREQUENCY MATCHING AND COURTSHIP SUCCESS OF LONG-TAILED MANAKINS (CHIROXIPHIA-LINEARIS) SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE SONG; MANAKIN; MATE CHOICE; COOPERATION; LEK ID MALE-MALE COOPERATION; MALE MATING SUCCESS; SEXUAL SELECTION; LEKKING BIRD; SONG; REPERTOIRE; EVOLUTION; CHOICE AB We examined the relationship between song performance and courtship success in the lek-mating long-tailed manakin (Chiroxiphia linearis) of Costa Rica. Teams of male manakins form cooperative partnerships consisting of a dominant alpha male and a beta male partner with a variable number of subordinate affiliates. Each alpha and beta partnership performs a joint song virtually in unison, which attracts females to their lek arena. We quantified four aspects of song performance, including synchrony, degree of consistency in the alpha male's singing, degree of consistency in the beta male's singing, and degree of sound frequency matching between partners. When all four variables were included in a discriminant function analysis, average frequency matching alone was useful in discriminating between teams with high rates of visitation by females and those with low visitation rates. Only frequency matching was correlated with the rate at which females visited display lek arenas. We propose that the degree of frequency matching provides an unambiguous ideal against which dual-male courtship performance can be assessed. This aspect of song performance may provide information useful to females in assessing a potential mate's ability to form a cooperative, long-term partnership. C1 SMITHSONIAN INST,MOLEC SYSTEMAT LAB,WASHINGTON,DC 20560. RP TRAINER, JM (reprint author), UNIV NO IOWA,DEPT BIOL,CEDAR FALLS,IA 50614, USA. RI McDonald, David/C-3195-2008 OI McDonald, David/0000-0001-8582-3775 NR 20 TC 36 Z9 36 U1 2 U2 8 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD OCT PY 1995 VL 37 IS 4 BP 249 EP 254 DI 10.1007/BF00177404 PG 6 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA TC816 UT WOS:A1995TC81600005 ER PT J AU JAECKLE, WB AF JAECKLE, WB TI TRANSPORT AND METABOLISM OF ALANINE AND PALMITIC ACID BY FIELD-COLLECTED LARVAE OF TEDANIA-IGNIS (PORIFERA, DEMOSPONGIAE) - ESTIMATED CONSEQUENCES OF LIMITED LABEL TRANSLOCATION SO BIOLOGICAL BULLETIN LA English DT Article ID DISSOLVED AMINO-ACIDS; MARINE INVERTEBRATE LARVAE; CRASSOSTREA-GIGAS THUNBERG; HALIOTIS-RUFESCENS; SWIMMING BEHAVIOR; BIVALVE LARVAE; SEAWATER; ECHINODERMATA; FERTILIZATION; EMBRYOS AB The epidermis of larvae of Tedania ignis (Porifera, Demospongiae) is uniformly ciliated except for the posterior pole. The epidermal cells are long, columnar, and monociliate; each cilium arises from an epidermal crypt; symbiotic bacteria were not observed in larval cells. These lecithotrophic (''nonfeeding'') larvae can feed by assimilating dissolved organic materials (DOM) from seawater. Larvae transported both the amino acid alanine (mean = 2.73 pmol larva(-1) h(-1); [S] = 1 mu M) and the fatty acid palmitic acid (mean = 16.27 pmol larva(-1) h(-1); [S] = 1 mu M) from seawater. Following assimilation, the label from alanine was recovered primarily in small molecular weight compounds; the label from palmitic acid was localized chiefly in the lipid fraction. Estimates of the contribution of transport to metabolism (mean respiration rate = 940.7 pmol O-2 larva(-1) h(-1)) reveal that alanine transport is energetically insignificant. Palmitic acid transport, in contrast, could account for 21%-55% of larval metabolism, Autoradiographic analysis of the distribution of the label in larvae suggests that epidermal cells are the chief recipients of the assimilated materials. Thus, the contribution of transport to whole-larva metabolism may underestimate the tissue-specific value, At palmitic acid concentrations of 1 and 0.25 mu M, the contribution of transport to the estimated metabolism of the epidermis would be 131% and 33% of energy requirements. Thus, the potential benefits of DOM to larvae are dependent not only on the nature of the epidermal transporters and the solute concentration, but also the degree to which materials are distributed among tissues. C1 SMITHSONIAN MARINE STN,FT PIERCE,FL 34946. NR 48 TC 33 Z9 33 U1 2 U2 8 PU MARINE BIOL LAB PI WOODS HOLE PA BIOLOGICAL BULL MBL STREET, WOODS HOLE, MA 02543 SN 0006-3185 J9 BIOL BULL JI Biol. Bull. PD OCT-NOV PY 1995 VL 189 IS 2 BP 159 EP 167 DI 10.2307/1542466 PG 9 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA TA771 UT WOS:A1995TA77100011 PM 27768480 ER PT J AU Wasshausen, DC AF Wasshausen, DC TI A new species, new combinations, and a new name in acanthaceae from northern South America SO BRITTONIA LA English DT Article DE Ruellia; Justicia; French Guiana; Guianas; Trinidad & Tobago; Acanthaceae AB A new species of Acanthaceae (Ruellia saulensis) is described and illustrated from French Guiana, and three new combinations (Justicia potarensis, J, flaviflora, and J. tobagensis) and one new name (Justicia coppenamensis) are proposed. The new species is compared to its closest relative (Ruellia rubra), and a justification of the transfers is provided. RP Wasshausen, DC (reprint author), SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560, USA. NR 10 TC 1 Z9 2 U1 0 U2 0 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 SN 0007-196X J9 BRITTONIA JI Brittonia PD OCT-DEC PY 1995 VL 47 IS 4 BP 422 EP 425 DI 10.2307/2807572 PG 4 WC Plant Sciences SC Plant Sciences GA TM230 UT WOS:A1995TM23000010 ER PT J AU POLCARI, S AF POLCARI, S TI GORKY,ARSHILE AND THE GENESIS OF ABSTRACTION SO BURLINGTON MAGAZINE LA English DT Art Exhibit Review RP POLCARI, S (reprint author), SMITHSONIAN INST,ARCHIVES AMER ART,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BURLINGTON MAG PUBL LTD PI LONDON PA 14-16 DUKES RD, LONDON, ENGLAND WC1H 9AD SN 0007-6287 J9 BURLINGTON MAG JI Burlingt. Mag. PD OCT PY 1995 VL 137 IS 1111 BP 709 EP 711 PG 3 WC Art SC Art GA TE137 UT WOS:A1995TE13700026 ER PT J AU POLCARI, S AF POLCARI, S TI GORKY,ARSHILE - THE 'BREAKTHROUGH YEARS' SO BURLINGTON MAGAZINE LA English DT Art Exhibit Review RP POLCARI, S (reprint author), SMITHSONIAN INST,ARCHIVES AMER ART,WASHINGTON,DC 20560, USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU BURLINGTON MAG PUBL LTD PI LONDON PA 14-16 DUKES RD, LONDON, ENGLAND WC1H 9AD SN 0007-6287 J9 BURLINGTON MAG JI Burlingt. Mag. PD OCT PY 1995 VL 137 IS 1111 BP 710 EP 711 PG 2 WC Art SC Art GA TE137 UT WOS:A1995TE13700027 ER PT J AU RALLS, K AF RALLS, K TI BUT IS IT SCIENCE SO CONSERVATION BIOLOGY LA English DT Letter RP RALLS, K (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 1 TC 1 Z9 1 U1 0 U2 1 PU BLACKWELL SCIENCE PUBL INC CAMBRIDGE PI CAMBRIDGE PA 238 MAIN ST, CAMBRIDGE, MA 02142 SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD OCT PY 1995 VL 9 IS 5 BP 983 EP 984 PG 2 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA TB449 UT WOS:A1995TB44900010 ER PT J AU STOUFFER, PC BIERREGAARD, RO AF STOUFFER, PC BIERREGAARD, RO TI EFFECTS OF FOREST FRAGMENTATION ON UNDERSTORY HUMMINGBIRDS IN AMAZONIAN BRAZIL SO CONSERVATION BIOLOGY LA English DT Article ID TROPICAL RAIN-FOREST; NECTAR-FEEDING BIRDS; TEMPORAL VARIATION; ABUNDANCE; COMMUNITY; PATTERNS; ORGANIZATION; DYNAMICS; ISLANDS; DISTURBANCE AB We sampled understory hummingbirds in Amazonian forest fragments from before isolation through nine yeats after isolation We recorded 377 captures of eight species in five I-ha fragments and four 10-ha fragments. The three species netted before isolation Phaethornis superciliosus, Phaethornis bourcieri, and Thalurania furcata, were nearly equally abundant at that time. After isolation abundance of P. bourcieri and T. furcata did not change, but P. superciliosus became nearly twice as common. Five additional species that were netted only after isolation represented about 10% of the post-isolation sample. The species recorded only after isolation were forest species usually found above the levels of nets;fragments were not colonized by nonforest species. Use of fragments did not differ between 1- and 10-ha fragments. The landscape surrounding the fragments included active cattle pasture, abandoned pasture, and Cecropia-dominated second growth, but this variation had little effect on use of fragments by hummingbirds. The results suggest that these understory hummingbirds can persist in a matric of fragments, secondary growth, and large forest patches. This response is much different than that of the insectivorous birds that dominate the understory bird community at the site, which are much more vulnerable to fragmentation. C1 SMITHSONIAN INST,BIODIVERS PROGRAM,NHB-106,WASHINGTON,DC 20560. NR 57 TC 112 Z9 123 U1 2 U2 33 PU BLACKWELL SCIENCE PUBL INC CAMBRIDGE PI CAMBRIDGE PA 238 MAIN ST, CAMBRIDGE, MA 02142 SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD OCT PY 1995 VL 9 IS 5 BP 1085 EP 1094 DI 10.1046/j.1523-1739.1995.9051085.x PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA TB449 UT WOS:A1995TB44900021 ER PT J AU WARKENTIN, IG GREENBERG, R ORTIZ, JS AF WARKENTIN, IG GREENBERG, R ORTIZ, JS TI SONGBIRD USE OF GALLERY WOODLANDS IN RECENTLY CLEARED AND OLDER SETTLED LANDSCAPES OF THE SELVA-LACANDONA, CHIAPAS, MEXICO SO CONSERVATION BIOLOGY LA English DT Article AB Many regions of Central America have undergone wide-scale habitat change as land has been converted for cultivation or grazing. Clearing for agriculture often leaves a variety of regenerating and remnant patches of wooded vegetation. Of particular importance is arroyo vegetation, or strips of trees or tall shrubs growing along streams. Although it is widely, acknowledged that tropical arroyo vegetation supports high densities of birds as avian habitat it remains poorly studied. We used point counts to study populations of migrant and resident songbirds in the arroyo vegetation of settled areas of the Selva Lacandona adjacent to the Montes Azules Biosphere Reserve of southeastern Mexico. Two study areas were established on lands that had been cleared and settled 20-35 and 10 years previously. Our objectives were to assess the value of arroyo vegetation to the conservation of avian species diversity and abundance in agricultural landscapes and to compare the composition and abundance of songbirds in cleared areas settled at different times over a 35-year period. Arroyo vegetation had a wide diversity of songbird species that, in overall terms differed little between those landscapes cleared recently and those cleared up to 35 years previously. In both areas we found a high abundance of habitat generalists and a smaller number of forest-dependent species, particularly migrants. Loss of forest specialists occurs rapidly, with little further loss as the arroyos become increasingly isolated. Our data also suggest that birds do not crowd into limited habitat as the surrounding vegetation is eliminated implying that the overall carrying capacity of the agricultural landscape is greatly enhanced as larger areas of arroyo vegetation are protected. Protection of arroyo vegetation will increase the diversity of birds living in agricultural areas and can be achieved simply by expanding upon land-use practices currently in use. C1 NATL ZOOL PK,SMITHSONIAN MIGRATORY BIRD CTR,WASHINGTON,DC 20008. UNIV MICHOACANA SAN NICOLAS DE HIDALGO,MORELIA,MICHOACAN,MEXICO. NR 22 TC 37 Z9 39 U1 0 U2 9 PU BLACKWELL SCIENCE PUBL INC CAMBRIDGE PI CAMBRIDGE PA 238 MAIN ST, CAMBRIDGE, MA 02142 SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD OCT PY 1995 VL 9 IS 5 BP 1095 EP 1106 PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA TB449 UT WOS:A1995TB44900022 ER PT J AU FLEISCHER, RC FULLER, G LEDIG, DB AF FLEISCHER, RC FULLER, G LEDIG, DB TI GENETIC-STRUCTURE OF ENDANGERED CLAPPER RAIL (RALLUS-LONGIROSTRIS) POPULATIONS IN SOUTHERN CALIFORNIA SO CONSERVATION BIOLOGY LA English DT Article ID COMPUTER-SIMULATION; DNA FINGERPRINTS; ALLELES; BOTTLENECK; HABITAT; DIFFERENTIATION; HETEROZYGOSITY; VARIABILITY; PARENTAGE; BEHAVIOR AB We assessed the genetic structure of two subspecies of endangered Clapper Rails (Rallus longirostris) in Southern California using DNA fingerprinting to uncover variation in minisatellite DNA. Minisatellite DNA variation in the Salton Sen population of the R. l. yumanensis subspecies was at a level typical of outbred avian species (average proportion of fragments shared, or S, was 0.33). Variation was extremely low (S from 0.63 to 0.77), however, within four coastal, salt-marsh populations of the subspecies R. l. levipes located along a transect extending about 260 km northwest from the Mexican border. Between-population similarity (S-ij) was also high for the four levipes populations, although individuals of the small, isolated population at Mugu Lagoon consistently clustered separately in phenograms constructed using neighbor-joining or other algorithms. Individuals of yumanensis always clustered as a sister group to all levipes individuals. The minisatellite data were contrasted with the extremely low mtDNA and RAPD variation we found in both subspecies. We propose that variation in these less-mutable markers was lost in a bottleneck that occurred at least 1000 years ago, thus allowing sufficient time for recovery of variation in the rapidly mutating (mu similar to 0.001/gamete/generation) minisatellites (t = 1/mu, or 1000 generations). A second more-recent bottleneck or series of bottlenecks within a metapopulation structure, likely resulted in the depauparate variation seen in levipes today. We suggest that translocations from large to small levipes populations could restore important genetic variation to the small populations and would not compromise genetic boundaries. C1 UNIV CALIF SANTA BARBARA,DEPT BIOL SCI,SANTA BARBARA,CA 93106. RP FLEISCHER, RC (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,GENET MOLEC LAB,WASHINGTON,DC 20008, USA. NR 68 TC 14 Z9 15 U1 0 U2 15 PU BLACKWELL SCIENCE PUBL INC CAMBRIDGE PI CAMBRIDGE PA 238 MAIN ST, CAMBRIDGE, MA 02142 SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD OCT PY 1995 VL 9 IS 5 BP 1234 EP 1243 DI 10.1046/j.1523-1739.1995.9051234.x PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA TB449 UT WOS:A1995TB44900036 ER PT J AU SHULMAN, MJ BERMINGHAM, E AF SHULMAN, MJ BERMINGHAM, E TI EARLY-LIFE HISTORIES, OCEAN CURRENTS, AND THE POPULATION-GENETICS OF CARIBBEAN REEF FISHES SO EVOLUTION LA English DT Article DE CORAL-REEF FISHES; DISPERSAL; GENE FLOW; HISTORICAL BIOGEOGRAPHY; LIFE HISTORY; MITOCHONDRIAL DNA; OCEAN CURRENTS ID MITOCHONDRIAL-DNA EVOLUTION; SEA-URCHINS; CORAL-REEF; RESTRICTION DATA; STRONGYLOCENTROTUS-PURPURATUS; DAMSELFISHES POMACENTRIDAE; NUCLEOTIDE SUBSTITUTIONS; PACIFIC; DIFFERENTIATION; PATTERNS AB Tropical reef fishes, along with many benthic invertebrates, have a life cycle that includes a sedentary, bottom-dwelling reproductive phase and a planktonic stage that occurs early in development. The adult benthic populations occupy disjunct, patchy habitats; the extent of gene flow due to dispersal of the planktonic life stage is generally unknown. We investigated dispersal, gene flow, and endemism in eight species of Caribbean reef fishes that varied in two life-history traits that may affect dispersal ability: egg type (pelagic and nonpelagic) and length of planktonic (usually larval) life. Using restriction endonuclease analyses of mitochondrial DNA (mtDNA), we estimated the degree of genetic differentiation among six populations of each of the eight species; these populations came from widely separated locales, occupying both the northern and southern current tracks within the Caribbean. In addition, we calculated mtDNA divergence between two of the study species and their sister taxa in the eastern Pacific. The transisthmian taxa have been isolated from one another for approximately 3 million yr and thus provide a divergence measure against which to assess intra-Caribbean mtDNA distances. Mean sequence divergence observed among conspecific Caribbean mtDNA haplotypes in each of the eight fish species was small, less than 0.7% for all but one species. This level of divergence is roughly one order of magnitude less than mtDNA divergence between Caribbean/eastern Pacific sister taxa. For each of the eight species of fishes, the predominant mtDNA haplotype was widespread in the Caribbean. Populations located in different major surface currents were no more differentiated from one another than populations occupying the same current track. These results suggest that there is considerable gene flow throughout the Caribbean, and that this gene flow has not been constrained by present-day ocean currents. We found statistically significant population subdivision for three Caribbean fish species, though between-population variance accounted for only 8%-17% of the total. Fishes showing population structure were: Stegastes leucostictus (nonpelagic eggs; short planktonic life); Gnatholepis thompsoni (nonpelagic eggs; long planktonic life); and Halichoeres bivittatus (pelagic eggs; short planktonic life). These results suggest that neither egg type nor length of larval life is a simple predictor of geographic structure in reef fish populations. C1 UNIV CALIF LOS ANGELES,DEPT BIOL,LOS ANGELES,CA 90024. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 91 TC 259 Z9 267 U1 4 U2 34 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 SN 0014-3820 J9 EVOLUTION JI Evolution PD OCT PY 1995 VL 49 IS 5 BP 897 EP 910 DI 10.2307/2410412 PG 14 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA TE990 UT WOS:A1995TE99000011 ER PT J AU PALMER, MA ARENSBURGER, P BOTTS, PS HAKENKAMP, CC REID, JW AF PALMER, MA ARENSBURGER, P BOTTS, PS HAKENKAMP, CC REID, JW TI DISTURBANCE AND THE COMMUNITY STRUCTURE OF STREAM INVERTEBRATES - PATCH-SPECIFIC EFFECTS AND THE ROLE OF REFUGIA SO FRESHWATER BIOLOGY LA English DT Article ID CHIRONOMIDAE LARVAE; MOUNTAIN STREAM; LOTIC SYSTEMS; DEBRIS DAMS; DIEL DRIFT; DYNAMICS; ECOLOGY; MACROINVERTEBRATES; RECOLONIZATION; MICROCRUSTACEA AB 1. We have previously shown that the impact of spates on stream invertebrates may differ among patches separated by distances of metres or less. Here we analyse the species-specific flood responses of larval chironomids and adult and near mature copepods living in different patch types. Four patch types (with eight replicates of each) were compared: the sandy mid-channel, fine sediments around darns, coarse sediments around dams, and dam debris. Additionally, since some fine sediment patches had been shown previously to act as flow refugia while others did not, we also examined species specific responses in refugium vs. non-refugium fine sediment patches. Detrended correspondence analysis was used to test for changes in assemblage structure (species composition and relative abundance). 2. Species richness was not altered in a predictable manner by floods; the least stable patch types (mid-channel and coarse patches) did not necessarily show reduced species richness during the spate. 3. As indicated by the spread of DCA ordination scores, there was generally a high degree of overlap in the species composition among the four patch types. Nevertheless, copepod species composition and relative abundance were more similar among patch types during the spate than pre-spate. Spates may induce a re-distribution of copepod species among the patch types. Chironomid species composition and relative abundance were no more similar among patch types during the spate than pre- or post-spate. 4. For both chironomids and copepods, species composition and relative abundance (as assessed by DCA ordination scores) in refugium patches changed more in response to the spate than in the non-refugium patches. An influx of individuals from just a few species for each group was responsible for the change in assemblage structure. Thus, despite the fact that our past work has shown that refugia may confer enhanced resistance and resilience of copepod and chironomid assemblages in terms of total faunal abundances, the present work suggests that resistance and resilience of the species composition of the community apparently are no greater in refugium patches than in non-refugium patches. C1 PENN STATE UNIV,DIV SCI,ERIE,PA 16563. SMITHSONIAN INST,MUSEUM NATL HIST NAT,DEPT INVERTEBRATE ZOOL MRC163,WASHINGTON,DC 20560. RP PALMER, MA (reprint author), UNIV MARYLAND,DEPT ZOOL,COLLEGE PK,MD 20742, USA. NR 53 TC 69 Z9 73 U1 0 U2 12 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0046-5070 J9 FRESHWATER BIOL JI Freshw. Biol. PD OCT PY 1995 VL 34 IS 2 BP 343 EP 356 DI 10.1111/j.1365-2427.1995.tb00893.x PG 14 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA TA714 UT WOS:A1995TA71400013 ER PT J AU HUBER, BT HODELL, DA HAMILTON, CP AF HUBER, BT HODELL, DA HAMILTON, CP TI MIDDLE-LATE CRETACEOUS CLIMATE OF THE SOUTHERN HIGH-LATITUDES - STABLE ISOTOPIC EVIDENCE FOR MINIMAL EQUATOR-TO-POLE THERMAL-GRADIENTS SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Review ID SEA DRILLING PROJECT; SOUTHWEST ATLANTIC-OCEAN; PLANKTONIC-FORAMINIFERA; VERTICAL-DISTRIBUTION; MODEL SIMULATIONS; FALKLAND PLATEAU; CARBON ISOTOPE; OXYGEN ISOTOPE; INDIAN-OCEAN; SEDIMENTS AB A detailed delta(18)O and delta(13)C stratigraphy has been generated from analysis of well-preserved Albian-early Maastrichtian foraminifera from Deep Sea Drilling Project (DSDP) Sites 511 and 327 (Falkland Plateau; approximate to 58 degrees S-62 degrees S paleolatitude) in the southern South Atlantic, and Cenomanian and Coniacian-Santonian foraminifera from DSDP Site 258 (Naturaliste Plateau; approximate to 58 degrees S paleolatitude) in the southern Indian Ocean. These results, when combined with previously published Maastrichtian stable isotope data from Ocean Drilling Program (ODP) Site 690 (Weddell Sea, approximate to 65 degrees S paleolatitude), pro,ide new insight into the climatic and oceanographic history of the southern high latitudes during middle-late Cretaceous time. The planktonic foraminifer delta(18)O curves reveal a gradual warming of surface waters from the Albian through the Cenomanian follow-ed by extremely warm surface waters from the Turonian through the early Campanian. Long-term cooling of surface waters began in the late early Campanian and continued through the end of the Maastrichtian. The benthic foraminifer delta(18)O record generally parallels changes in the oxygen isotopic curves defined by shallow-dwelling planktonic foraminifera. The vertical oxygen and carbon isotopic gradients were relatively low during the Albian-Cenomanian, high from the Turonian-early Campanian, and then low during the late Campanian and Maastrichtian. Foraminiferal oxygen isotopic data from published sources and this study are averaged for each site, corrected for latitudinal changes in salinity based on modern-day surface-water values, and plotted versus paleolatitude for the late Albian, Coniacian-Santonian, and late Maastrichtian. Differences between low- and high-latitude surface-water paleotemperatures are estimated at approximate to 14 degrees C during the late Albian and late Maastrichtian, but the Coniacian-Santonian reconstruction reveals only a 0-4 degrees C latitudinal temperature gradient. Uncertainty regarding Cretaceous salinity gradients and possible diagenetic alteration of delta(18)O values introduce error into our estimates of paleolatitudinal thermal gradients; however, apparent low equator-to-pole temperature differences could indicate much higher poleward heat transport than at present. C1 UNIV FLORIDA,DEPT GEOL,GAINESVILLE,FL 32611. RP HUBER, BT (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL,MRC-121,WASHINGTON,DC 20560, USA. NR 124 TC 326 Z9 348 U1 4 U2 45 PU GEOLOGICAL SOC AMERICA PI BOULDER PA PO BOX 9140 3300 PENROSE PLACE, BOULDER, CO 80301 SN 0016-7606 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD OCT PY 1995 VL 107 IS 10 BP 1164 EP 1191 DI 10.1130/0016-7606(1995)107<1164:MLCCOT>2.3.CO;2 PG 28 WC Geosciences, Multidisciplinary SC Geology GA RZ453 UT WOS:A1995RZ45300004 ER PT J AU ESSER, R HABBAL, SR AF ESSER, R HABBAL, SR TI CORONAL HEATING AND PLASMA PARAMETERS AT 1-AU SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SOLAR-WIND; TRANSITION REGION; STELLAR CORONAE; ENERGY-BALANCE; HOLES AB A three-fluid description of the solar wind is used to investigate the mass flux, helium abundance and flow speeds at 1 AU as a function of heat input in the inner corona. The solar wind model includes continuity, momentum and energy equations for each of the three species, electrons, protons, and alpha particles. The energy equations contain parameterized heat sources for any of the three species. The energy equation for the electrons also includes radiation losses in the transition region. We study the effect of heating different particle species. We show that for a given set of plasma parameters at the coronal base, heating the electrons, protons and alpha particles, or all three species, can result in the same mass flux, helium abundance and proton flow speed at 1 AU, yet very different plasma properties in the inner corona. The plasma parameters we consider are characteristic of the high speed solar wind. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, MS-15, CAMBRIDGE, MA 02138 USA. NR 18 TC 21 Z9 21 U1 0 U2 1 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 OCT 1 PY 1995 VL 22 IS 19 BP 2661 EP 2664 DI 10.1029/95GL02339 PG 4 WC Geosciences, Multidisciplinary SC Geology GA RX918 UT WOS:A1995RX91800028 ER PT J AU JETT, JA AF JETT, JA TI RECENT LITERATURE ON FORAMINIFERA SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Bibliography RP JETT, JA (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL,MRC-121,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD OCT PY 1995 VL 25 IS 4 BP 369 EP 371 PG 3 WC Paleontology SC Paleontology GA TF571 UT WOS:A1995TF57100007 ER PT J AU ESSER, R BRICKHOUSE, NS HABBAL, SR ALTROCK, RC HUDSON, HS AF ESSER, R BRICKHOUSE, NS HABBAL, SR ALTROCK, RC HUDSON, HS TI USING FE-X 6374-ANGSTROM AND FE-XIV 5303-ANGSTROM SPECTRAL-LINE INTENSITIES TO STUDY THE EFFECT OF LINE-OF-SIGHT INTEGRATION ON CORONAL TEMPERATURE INFERENCES SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND; EXCITATION; PROTON; RATES; MODEL; IRON; HOLE AB Polar coronal holes are relatively stable structures persisting over many solar rotations. The appearance of coronal holes in remote observations, however, can change on a daily basis due to variations of the denser and hotter plasma surrounding them. We explore the effect of these denser and hotter surrounding regions on coronal hole observations, using daily intensity measurements at 1.15 R(S) of the green Fe XIV 5303 Angstrom and red Fe X 6374 Angstrom spectral lines. The observations, which were carried out at the National Solar Observatory at Sacramento Peak, New Mexico, cover a time period of about four solar rotations. We show that the ''coronal hole'' temperatures derived using the line ratio technique, vary by more than 0.8 x 10(6) K over the time interval considered here. We also provide a short discussion of the expected accuracy of the atomic data for these two iron spectral lines. Using intensity measurements as a function of distance from the Sun, we briefly discuss how the regions surrounding the coronal holes might influence the inference of the temperature gradient in the coronal holes. The line of sight effect on the temperature gradient should be explored in more detail in the future using daily observations of the line intensities as a function of distance. These observations could be provided by ground-based coronagraphs and by instruments on board SOHO. C1 GEOPHYS DIRECTORATE, PHILLIPS LAB, SUNSPOT, NM 88349 USA. UNIV HAWAII, INST ASTRON, HONOLULU, HI 96822 USA. RP ESSER, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 32 TC 19 Z9 19 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-SPACE JI J. Geophys. Res-Space Phys. PD OCT 1 PY 1995 VL 100 IS A10 BP 19829 EP 19838 DI 10.1029/95JA00594 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RY274 UT WOS:A1995RY27400067 ER PT J AU YOU, L COOPER, J ZOLLER, P AF YOU, L COOPER, J ZOLLER, P TI QUANTUM-CLASSICAL CORRESPONDENCES FOR ATOMIC OPERATORS - A POSITIVE-P REPRESENTATION APPROACH SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS LA English DT Article ID OPTICAL BISTABILITY; SUPERFLUORESCENCE; PROPAGATION; SYSTEMS; LASER AB We demonstrate the successful simulation of classical stochastic differential equations obtained from the positive P phase-space technique for two-level atoms pumped by a near-resonant laser. Numerical results for both the resonance fluorescence spectrum and the absorption spectrum are compared with the exact results. (C) 1995 Optical Society of America C1 UNIV COLORADO,NATL INST STAND & TECHNOL,JOINT INST LAB ASTROPHYS,BOULDER,CO 80309. RP YOU, L (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,MS 14,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Zoller, Peter/O-1639-2014 OI Zoller, Peter/0000-0003-4014-1505 NR 26 TC 0 Z9 0 U1 0 U2 2 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 SN 0740-3224 J9 J OPT SOC AM B JI J. Opt. Soc. Am. B-Opt. Phys. PD OCT PY 1995 VL 12 IS 10 BP 1774 EP 1782 DI 10.1364/JOSAB.12.001774 PG 9 WC Optics SC Optics GA RZ091 UT WOS:A1995RZ09100003 ER PT J AU WASSER, SK VELLOSO, AD RODDEN, MD AF WASSER, SK VELLOSO, AD RODDEN, MD TI USING FECAL STEROIDS TO EVALUATE REPRODUCTIVE FUNCTION IN FEMALE MANED WOLVES SO JOURNAL OF WILDLIFE MANAGEMENT LA English DT Article DE CHRYSOCYON BRACHYURUS; ENDANGERED SPECIES; ESTROGEN; FECAL STEROID; MANED WOLF; PROGESTIN; RADIOIMMUNOASSAY; REPRODUCTION ID PAPIO-CYNOCEPHALUS-CYNOCEPHALUS; EXCRETED STEROIDS; PREGNANCY; URINARY; WOMEN AB This study represents the first attempt to apply fecal steroid measures to canids and suggests that these noninvasive measures can provide an important management tool for the endangered maned wolf (Chrysocyon brachyurus). We measured estrogen and progestin concentrations temporally in feces of 9 female maned wolves to determine whether these measures could be used to assess their reproductive function. Subjects were housed at 5 zoological parks in the United States. We collected 2-3 weekly samples for 3-5 months, beginning just prior to expected time of estrus (based on previous years). Fecal steroid measures indicated occurrence of ovulation and pregnancy in 8 of 9 wolves. Cycling females showed an estrogen surge (($) over bar x = 231.8 +/- 68.2 [SE] ng/g) coincident with the onset of the luteal phase progesterone rise. The estrogen surge was followed by a sustained rise in progestin levels of 27.2 +/- 2.65 mu g/g in conceptive cycles over the subsequent 63 days (1 gestation period), which was higher (P < 0.001) than the 7.6 +/- 0.73 mu g/g progestins in nonconceptive cycles. Estrogen concentrations in a young acyclic female never rose above 50 ng/g, whereas her progestin values remained below 3.0 mu g/g. Fecal steroid measures may provide a useful means of characterizing fertility, including ovulation and pregnancy, in female maned wolves. C1 UNIV WASHINGTON,DEPT OBSTET & GYNECOL,DIV REPROD ENDOCRINOL,SEATTLE,WA 98195. UNIV MARYLAND,DEPT ZOOL,COLLEGE PK,MD 20742. SMITHSONIAN INST,CTR CONSERVAT & RES,FRONT ROYAL,VA 22630. RP WASSER, SK (reprint author), CTR WILDLIFE CONSERVAT,5500 PHINNEY AVE N,SEATTLE,WA 98103, USA. NR 19 TC 27 Z9 28 U1 0 U2 10 PU WILDLIFE SOC PI BETHESDA PA 5410 GROSVENOR LANE, BETHESDA, MD 20814-2197 SN 0022-541X J9 J WILDLIFE MANAGE JI J. Wildl. Manage. PD OCT PY 1995 VL 59 IS 4 BP 889 EP 894 DI 10.2307/3801971 PG 6 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA RY589 UT WOS:A1995RY58900034 ER PT J AU KALFATOVIC, MR AF KALFATOVIC, MR TI GOING ONCE - A MEMOIR OF ART, SOCIETY, AND CHARITY - WOOLLEY,R SO LIBRARY JOURNAL LA English DT Book Review RP KALFATOVIC, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD OCT 1 PY 1995 VL 120 IS 16 BP 82 EP 82 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA RW889 UT WOS:A1995RW88900113 ER PT J AU FORREY, RC HILL, RN SHARMA, RD AF FORREY, RC HILL, RN SHARMA, RD TI CONVERGENCE ACCELERATION FOR THE KOHN VARIATIONAL METHOD IN THE PRESENCE OF A LONG-RANGE INTERACTION SO PHYSICAL REVIEW A LA English DT Article ID S-MATRIX VERSION; QUANTUM SCATTERING; PRINCIPLES AB This paper presents a distorted-wave generalization of the S-matrix version of the Kohn variational principle developed by Zhang, Chu, and Miller [J. Chem. Phys. 88, 10 (1988)]. For scattering in the presence of a long-range interaction, the large-r asymptotic solution to the Schrodinger equation is built into the Kohn variational principle order by order in an effort to accelerate the convergence of the short-range square integrable part of the basis-set expansion. The improvement in the rate of convergence is demonstrated by applying the method to a long-range model potential. Multichannel scattering is discussed. C1 UNIV DELAWARE,DEPT PHYS & ASTRON,NEWARK,DE 19716. PHILLIPS LAB,GPOS,BEDFORD,MA 01731. RP FORREY, RC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 21 TC 0 Z9 0 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD OCT PY 1995 VL 52 IS 4 BP 2948 EP 2954 DI 10.1103/PhysRevA.52.2948 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA TA424 UT WOS:A1995TA42400062 ER PT J AU EPSTEIN, ME AF EPSTEIN, ME TI FALSE-PARASITIZED COCOONS AND THE BIOLOGY OF AIDIDAE (LEPIDOPTERA, ZYGAENOIDEA) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE LEPIDOPTERA; AIDIDAE; COCOON CONSTRUCTION; PREDATOR AVOIDANCE; FALSE-PARASITIZED COCOONS AB Two or four holes in the outer mesh of cocoons in Aididae appear to mimic exit holes of parasitic Hymenoptera. Cocoon construction in Aides amanda (Stoll) from Venezuela is described and documented with photographs, along with notes on its biology. Annona punicifolia is reported as a larval hostplant of A. amanda. Literature on the cocoons and biology of Aididae are reviewed. Citations of Guyaba as a larval hostplant of A. amanda are considered to be erroneous based on misidentified larvae. Scenarios for the evolution of cocoon construction in Aididae are discussed, as are possible functions of the false exit holes in their cocoons. RP EPSTEIN, ME (reprint author), SMITHSONIAN INST,DEPT ENTOMOL,NHB 105,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 1995 VL 97 IS 4 BP 750 EP 756 PG 7 WC Entomology SC Entomology GA TD709 UT WOS:A1995TD70900003 ER PT J AU Molella, AP AF Molella, AP TI Tilting at windmills SO TECHNOLOGY AND CULTURE LA English DT Article C1 SMITHSONIAN INST,NATL MUSEUM AMER HIST,LEMELSON CTR STUDY INVENT & INNOVAT,WASHINGTON,DC 20560. RP Molella, AP (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,DEPT HIST,WASHINGTON,DC 20560, USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD OCT PY 1995 VL 36 IS 4 BP 1000 EP 1006 DI 10.2307/3106922 PG 7 WC History & Philosophy Of Science SC History & Philosophy of Science GA UV826 UT WOS:A1995UV82600010 ER PT J AU Worthington, W AF Worthington, W TI A century in the works: Freese and Nichols consulting engineers, 1894-1994 - Freese,SW, Sizemore,DL SO TECHNOLOGY AND CULTURE LA English DT Book Review RP Worthington, W (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD OCT PY 1995 VL 36 IS 4 BP 1031 EP 1033 DI 10.2307/3106931 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA UV826 UT WOS:A1995UV82600019 ER PT J AU Reingold, N AF Reingold, N TI Information and secrecy: Vannevar Bush, ultra, and the other Memex - Burke,C SO TECHNOLOGY AND CULTURE LA English DT Book Review RP Reingold, N (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD OCT PY 1995 VL 36 IS 4 BP 1051 EP 1053 DI 10.2307/3106942 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA UV826 UT WOS:A1995UV82600032 ER PT J AU Multhauf, RP AF Multhauf, RP TI Science has no national borders: Harry C. Kelly and the reconstruction of science and technology in postwar Japan - Yoshikawa,H, Kauffman,J SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD OCT PY 1995 VL 36 IS 4 BP 1055 EP 1057 DI 10.2307/3106944 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA UV826 UT WOS:A1995UV82600034 ER PT J AU CHRISTY, JH BACKWELL, PRY AF CHRISTY, JH BACKWELL, PRY TI THE SENSORY EXPLOITATION HYPOTHESIS SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Letter ID EVOLUTION RP CHRISTY, JH (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO,AA 34002, USA. RI Backwell, Patricia/C-8883-2009 NR 10 TC 11 Z9 11 U1 0 U2 9 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, OXON, ENGLAND OX5 1GB SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD OCT PY 1995 VL 10 IS 10 BP 417 EP 417 DI 10.1016/S0169-5347(00)89161-2 PG 1 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA RV502 UT WOS:A1995RV50200012 PM 21237089 ER PT J AU GREEN, R AF GREEN, R TI INDIN HUMOR, BICULTURAL PLAY IN NATIVE AMERICA - LINCOLN,K SO WESTERN FOLKLORE LA English DT Book Review RP GREEN, R (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CALIF FOLKLORE SOC PI POMONA PA WESTERN FOLKLORE DEPT OF ENGL/FOREIGN LANGUAGES 3801 W.TEMPLE AVENUE, POMONA, CA 91768-4010 SN 0043-373X J9 WESTERN FOLKLORE JI West. Folk. PD OCT PY 1995 VL 54 IS 4 BP 340 EP 341 DI 10.2307/1500314 PG 2 WC Folklore SC Arts & Humanities - Other Topics GA TV585 UT WOS:A1995TV58500011 ER PT J AU Rouse, GW Fauchald, K AF Rouse, GW Fauchald, K TI The articulation of annelids SO ZOOLOGICA SCRIPTA LA English DT Review ID MYZOSTOMA-CIRRIFERUM MYZOSTOMIDA; RIFTIA-PACHYPTILA JONES; PHYLOGENETIC RELATIONSHIP; COMPARATIVE ULTRASTRUCTURE; BACTERIAL SYMBIONTS; CLADISTIC-ANALYSIS; TUBE WORMS; POGONOPHORA; VESTIMENTIFERAN; EVOLUTION AB The aim of this paper is to assess the monophyly of the Annelida. Also, recent cladistic analyses of metazoan taxa, using a variety of data, have shown incongruities with regards to annelids and associated taxa that should be resolved. The Platyhelminthes is selected as the taxon to root our minimal length trees and polarise our characters in a parsimony analysis; ingroup taxa being Mollusca, Nemertea, Sipuncula, Echiura, Pogonophora, Vestimentifera, Euarthropoda, Onychophora, and the groups most commonly regarded as true 'annelids', the Clitellata and Polychaeta. We use 13 characters and a total of 33 states. This results in 18 minimal length trees of 23 steps. The consensus tree has the topology (Platyhelminthes (Nemertea (Sipuncula Mollusca (Echiura (Polychaeta (Vestimentifera Pogonophora) Clitellata (Euarthropoda Onychophora)))))). The name Articulata is applied to the Clitellata, Euarthropoda, Onychophora, Pogonophora, Polychaeta, and Vestimentifera. The Vestimentifera is the sister group to, or more likely a clade within, the frenulate pogonophores, and the name Pogonophora is retained for this group. In half of the 18 minimal length trees, the traditionally formulated Annelida, i.e. Polychaeta and Clitellata, is paraphyletic if the Pogonophora are excluded. In the remaining minimal length trees, a monophyletic Annelida cannot be formulated. The name Annelida should not be used unless relationships within the Articulata are resolved to show it is a monophyletic taxon. The taxon name Articulata, originally formulated to include the Annelida and Arthropoda by Cuvier, is defined as the clade stemming from the first ancestor to show repetition of homologous body structures derived by teloblastic growth with a pygidial growth zone (segmentation) and longitudinal muscles broken into bands. The Articulata is considered, on current evidence, to consist of four monophyletic groups; the Arthropoda, Clitellata, Polychaeta, and Pogonophora, though the latter group may be a clade of polychaetes. If this is shown, the Pogonophora should revert to the original family name Lamellisabellidae Uschakov, 1933. An indented classification reflective of the cladistic pattern is provided. Other recent hypotheses about metazoan systematics are analysed. C1 SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT INVERTEBRATE ZOOL, WASHINGTON, DC 20560 USA. RP Rouse, GW (reprint author), UNIV SYDNEY, SCH BIOL SCI A08, SYDNEY, NSW 2006, AUSTRALIA. RI Rouse, Greg/F-2611-2010 OI Rouse, Greg/0000-0001-9036-9263 NR 308 TC 128 Z9 133 U1 3 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0300-3256 EI 1463-6409 J9 ZOOL SCR JI Zool. Scr. PD OCT PY 1995 VL 24 IS 4 BP 269 EP 301 DI 10.1111/j.1463-6409.1995.tb00476.x PG 33 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA TQ891 UT WOS:A1995TQ89100001 ER PT J AU Schneider, JA AF Schneider, JA TI Phylogeny of the Cardiidae (Mollusca, Bivalvia): Protocardiinae, Laevicardiinae, Lahilliinae, Tulongocardiinae subfam n and Pleuriocardiinae subfam n SO ZOOLOGICA SCRIPTA LA English DT Review ID FOSSIL RECORD; CONSISTENCY INDEX; MORPHOLOGY; EVOLUTION; SHELLS; CLASSIFICATION; MORPHOGENESIS; EXTINCTION; CONSENSUS; PARSIMONY AB In a preliminary cladistic analysis of the bivalve family Cardiidae (Schneider 1992), members of the subfamilies Protocardiinae, Lahilliinae, and Laevicardiinae, plus the genus Nemocardium, were found to be the least derived taxa of cardiids. A cladistic analysis is undertaken of the genera and subgenera of these cardiid taxa, plus several Mesozoic taxa which have never been assigned to any subfamily. The Late Triassic Tulongocardium, which is placed in Tulongocardiinae subfam. n., is the sister taxon to all other cardiids. Protocardiinae is restricted to the genus Protocardia. Most other Mesozoic taxa which have been placed in the Protocardiinae are found to be members of the Lahilliinae. Nemocardium is placed in the Laevicardiinae. Incacardium, Pleuriocardia, and Dochmocardia form a monophyletic group, Pleuriocardiinae subfam. n. Pleuriocardiinae, Laevicardiinae, and the remaining members of the Cardiidae (herein informally termed ''eucardiids'') form a monophyletic group. C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. RP Schneider, JA (reprint author), YOUNGSTOWN STATE UNIV, DEPT GEOL, YOUNGSTOWN, OH 44555 USA. NR 159 TC 30 Z9 37 U1 0 U2 7 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0300-3256 J9 ZOOL SCR JI Zool. Scr. PD OCT PY 1995 VL 24 IS 4 BP 321 EP 346 DI 10.1111/j.1463-6409.1995.tb00478.x PG 26 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA TQ891 UT WOS:A1995TQ89100003 ER PT J AU COOPER, A COOPER, RA AF COOPER, A COOPER, RA TI THE OLIGOCENE BOTTLENECK AND NEW-ZEALAND BIOTA - GENETIC RECORD OF A PAST ENVIRONMENTAL CRISIS SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article ID MITOCHONDRIAL GENOME; EVOLUTION; ORGANIZATION; PERSPECTIVES; GLACIATION; AUSTRALIA; SEQUENCES; POSITIONS; ORIGINS; AMERICA AB Mitochondrial DNA (mtDNA) 12S sequences from the two New Zealand ratite orders, the kiwi and moa, indicate that each group represents a separate colonization event. However, the amount of mtDNA genetic diversity observed within each of the New Zealand groups is similar, and limited, which is not consistent with the ratite phylogenetic tree. We examine the Cenozoic (65-0 million years ago) geological history of New Zealand for possible causes and summarize evidence for land area and climatic changes. A genetic bottleneck is hypothesized and tested, by using molecular data from a second mitochondrial locus (ND6) and a further taxon, the New Zealand acanthisittid wrens. The data support the existence of a widespread genetic bottleneck during the mid-Cenozoic in New Zealand and demonstrate the benefits of synthesizing traditional research with new molecular techniques. C1 INST GEOL & NUCL SCI, LOWER HUTT, NEW ZEALAND. RP COOPER, A (reprint author), SMITHSONIAN INST, NATL ZOOL PK, WASHINGTON, DC 20008 USA. RI Cooper, Alan/E-8171-2012 OI Cooper, Alan/0000-0002-7738-7851 NR 63 TC 125 Z9 128 U1 0 U2 19 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD SEP 22 PY 1995 VL 261 IS 1362 BP 293 EP 302 DI 10.1098/rspb.1995.0150 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA RY772 UT WOS:A1995RY77200004 PM 8587872 ER PT J AU BARTELMANN, MF NARAYAN, R AF BARTELMANN, MF NARAYAN, R TI THE LENS PARALLAX METHOD - DETERMINING REDSHIFTS OF FAINT BLUE GALAXIES THROUGH GRAVITATIONAL LENSING SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, OBSERVATIONS; GALAXIES, CLUSTERS, GENERAL; GALAXIES, DISTANCES AND REDSHIFTS; GRAVITATIONAL LENSING ID DEEP CCD SURVEY; LUMINOSITY FUNCTION; DARK MATTER; EVOLUTION; CLUSTERS; IMAGES; MODELS; DISKS AB We propose a new technique, which we call the lens parallax method, to determine simultaneously the redshift distribution of the faint blue galaxies and the mass distributions of foreground clusters of galaxies. The method is based on gravitational lensing and makes use of the following: (1) the amplitude of lensing-induced distortions of background galaxies increases with redshift; (2) the surface brightnesses of galaxies decrease steeply with redshift. The distortions of galaxy images due to lensing are thus expected to be inversely correlated with surface brightness, allowing us to obtain relative distances to galaxies as a function of surface brightness. If the redshifts of the brightest galaxies are measured, then the relative distance scale can be converted to mean galaxy redshifts as a function of surface brightness. Further, by comparing the angular sizes of lensed galaxies with those of similar galaxies in empty control fields, it is possible to break the so-called mass sheet degeneracy inherent to cluster mass reconstruction techniques that are based purely on image ellipticities. This allows an unambiguous determination of the surface density of a lensing cluster. We describe an iterative algorithm based on these ideas and present numerical simulations which show that the proposed techniques are feasible with a sample of approximate to 10 rich clusters at moderate redshifts similar to 0.3-0.4 and an equal number of control fields. The numerical tests show that the method can be used to determine the redshifts of galaxies with an accuracy of Delta z approximate to 0.1-0.2 at z similar to 1-1.7, and to measure the masses of lensing clusters to about 5% accuracy. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RI Bartelmann, Matthias/A-5336-2014 NR 57 TC 35 Z9 35 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 1995 VL 451 IS 1 BP 60 EP 75 DI 10.1086/176200 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RU168 UT WOS:A1995RU16800006 ER PT J AU KROCKENBERGER, M GRINDLAY, JE AF KROCKENBERGER, M GRINDLAY, JE TI DISCOVERY OF DIFFUSE-X-RAY EMISSION IN 47-TUCANAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE DIFFUSE RADIATION; GLOBULAR CLUSTERS, INDIVIDUAL (47 TUCANAE); SHOCK WAVES; WHITE DWARFS; X-RAYS, ISM ID GLOBULAR-CLUSTER 47-TUCANAE; GAS; ULTRAVIOLET; PULSARS; WINDS; STARS; MASS AB We present the results of a search for diffuse X-ray sources in a 61,000 s ROSAT PSPC exposure of 47 Tuc. There is faint, soft emission on the northeast side of the cluster at a distance of 6' from the core. The location of this emission along the direction of proper motion of the cluster suggests that it might be due to a bow shock. We show that a simple shock model fits the observed luminosity and temperature. However, a bow shock can form only if the rotation of the halo gas at the height of 47 Tuc (z = 3.3 kpc) is small compared to the rotation of the Galactic plane. Therefore this observation provides not only the first X-ray detection of hot gas in a globular cluster, but also constrains the dynamics of the halo gas. We also find two sources of diffuse X-ray emission to the northeast of the cluster which are brighter and harder. We consider a variety of models for this emission, including thermal emission from a high-velocity wind from a hot white dwarf, and propose that it is due to inverse Compton emission from acceleration in the bow shock of low-energy cosmic-ray electrons from the population of millisecond pulsars in the cluster. RP KROCKENBERGER, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 41 TC 20 Z9 20 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 1995 VL 451 IS 1 BP 200 EP 209 DI 10.1086/176211 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RU168 UT WOS:A1995RU16800017 ER PT J AU RYUTOVA, MP HABBAL, SR AF RYUTOVA, MP HABBAL, SR TI THE EFFECTS OF MASS FLOWS ON THE DISSIPATION OF ALFVEN WAVES IN THE UPPER LAYERS OF THE SOLAR ATMOSPHERE SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; PLASMAS; SUN, ATMOSPHERE; WAVES AB The influence of parallel plasma flows on the propagation of shear Alfven waves along magnetic structures is considered. It is shown that even in a simple case of regular mass flows directed along the magnetic field, their presence considerably modifies the dissipation of shear Alfven waves, affecting both the magnitude and the height of maximum dissipation. The strongest effect occurs in the case of downflows when the flow velocity at a certain height becomes equal to the Alfven velocity. Near that point, the wave comes to extinction and gives off its energy completely. The axial extent of the absorption region is evaluated. This effect can be directly associated with observed high-velocity downflows in the transition region, and, in particular, can serve as a qualitative explanation for the high variability of the emission observed near 10(5) K. In the presence of upward mass flows and moderate downflows, the dissipation of phase-mixed Alfven waves is accompanied by the radial redistribution of the energy input across the magnetic structure, thus creating a mosaic pattern in the emitting regions. The flow velocities are assumed to be below the thresholds which correspond to the onset of hydrodynamic and dissipative instabilities. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP RYUTOVA, MP (reprint author), LAWRENCE LIVERMORE NATL LAB,INST GEOPHYS & PLANETARY PHYS,L-413,LIVERMORE,CA 94550, USA. NR 22 TC 22 Z9 22 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 1995 VL 451 IS 1 BP 381 EP 390 DI 10.1086/176227 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RU168 UT WOS:A1995RU16800033 ER PT J AU HEISE, C SMITH, PL CALAMAI, AG AF HEISE, C SMITH, PL CALAMAI, AG TI TRANSITION-PROBABILITIES FOR THE 3S(2)3P(2)-P-3(2,1)-3S3P(3)-S-5(2)0 INTERSYSTEM LINES OF S-III SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC DATA ID ISOELECTRONIC SEQUENCE; RADIATIVE LIFETIME; METASTABLE LEVEL; ENERGY-LEVELS; IDENTIFICATION; SULFUR; XVI AB Intensity ratios involving the spin-changing ''intercombination'' lines between the 3s3p(3) S-5(2)o metastable level of S III and its 3s(2)3p(2) P-3(2,1) ground term at about 172 nm could be useful astrophysical diagnostic tools if accurate atomic data were available. We report the first laboratory measurement of the radiative lifetime of the S-5(2)o metastable level of S III. The measurement was carried out by observing the decay radiation of a metastable S2+ population stored in a radio-frequency ion trap. Our result for the lifetime of the S-5(2)o level of S III is 48 +/- 5 mu s. This value is in good agreement with recent calculations for the low-Z members of the Si I isoelectronic sequence. Using calculated branching ratios, we estimate that A (171.312 nm) = 5400 +/- 900 s(-1) and A (172.894 nm) = 15400 +/- 2500 s(-1). C1 PHILADELPHIA COLL PHARM & SCI,DEPT MATH & PHYS,PHILADELPHIA,PA 19104. RP HEISE, C (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MAIL STOP 50,CAMBRIDGE,MA 02138, USA. NR 25 TC 8 Z9 8 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 1995 VL 451 IS 1 BP L41 EP L44 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RU169 UT WOS:A1995RU16900011 ER PT J AU WEST, MJ JONES, C FORMAN, W AF WEST, MJ JONES, C FORMAN, W TI SUBSTRUCTURE - CLUES TO THE FORMATION OF CLUSTERS OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, OBSERVATIONS; GALAXIES, CLUSTERS, GENERAL; LARGE-SCALE STRUCTURE OF UNIVERSE; X-RAYS, GALAXIES ID RICH CLUSTERS; COMA CLUSTER; ABELL CLUSTERS; POOR CLUSTERS; CD GALAXIES; DARK MATTER; EVOLUTION; CLASSIFICATION; SUPERCLUSTERS; UNIVERSE AB We have examined the spatial distribution of substructure in clusters of galaxies using Einstein X-ray observations. Subclusters are found to have a markedly anisotropic distribution that reflects the surrounding matter distribution on supercluster scales. Our results suggest a picture in which cluster formation proceeds by mergers of subclusters along large-scale filaments. The implications of such an anisotropic formation process for the shapes, orientations, and kinematics of clusters are discussed briefly. C1 STERREWACHT LEIDEN,2300 RA LEIDEN,NETHERLANDS. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OI Forman, William/0000-0002-9478-1682 NR 46 TC 90 Z9 90 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 1995 VL 451 IS 1 BP L5 EP L8 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RU169 UT WOS:A1995RU16900002 ER PT J AU OLSON, SL JAMES, HF AF OLSON, SL JAMES, HF TI NOMENCLATURE OF THE HAWAIIAN AKIALOAS AND NUKUPUUS (AVES, DREPANIDINI) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB The generic names Hemignathus Lichtenstein, 1839, and Heterorhynchus Lafresnaye, 1839, often used for the akialoas and the nukupuus, respectively, have the same type species (Hemignathus lucidus) so if the akialoas are given the status of a separate genus or subgenus, there is no generic-level name available for them. From a review of evidence concerning dates of publication we conclude that for nomenclatural purposes Hemignathus and Heterorhynchus were published simultaneously and Hemignathus has precedence according to the first reviser principle. The correct citation for the Oahu Akialoa is shown to be Drepanis ellisiana G. R. Gray (1859) rather than Hemignathus lichtensteini Wilson (1889). The name Hemignathus stejnegeri Wilson (1889) has priority over H. procerus Cabanis (1890) and is restored for the Kauai Akialoa. As no other name is available for akialoas, the new generic name Akialoa is proposed here (type species Certhia obscura Gmelin). The new names resulting from these nomenclatural changes are listed. RP OLSON, SL (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT VERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 56 TC 8 Z9 8 U1 2 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD SEP 19 PY 1995 VL 108 IS 3 BP 373 EP 387 PG 15 WC Biology SC Life Sciences & Biomedicine - Other Topics GA RW567 UT WOS:A1995RW56700001 ER PT J AU FELDER, DL MANNING, RB AF FELDER, DL MANNING, RB TI NEOCALLICHIRUS-CACAHUATE, A NEW SPECIES OF GHOST SHRIMP FROM THE ATLANTIC COAST OF FLORIDA, WITH REEXAMINATION OF NEOCALLICHIRUS-GRANDIMANA AND NEOCALLICHIRUS-LEMAITREI (CRUSTACEA, DECAPODA, CALLIANASSIDAE) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID THALASSINIDEA AB Diversity of infaunal crustaceans remains poorly known, even for macrofaunal forms from accessible shorelines that have been urbanized for decades and studied extensively. Neocallichirus cacahuate, new species, is described from sparsely vegetated intertidal flats of Peanut Island just inside Lake Worth Inlet on the Atlantic coast of Florida, where it occurs as a minor constituent of a thalassinid fauna dominated by the callianassids Neocallichirus rathbunae(Schmitt), Sergio mericeae Manning & Felder, and Callichirus major (Say). This new species, at first confused with Neocallichirus grandimana (Gibbes) which also occurs occasionly in this habitat, bears a general resemblance to the young of that larger congener in carapacial features, chelae, telson, and uropods. However, in addition to the much larger body size attained by N. grandimana, this species and N. cacahuate can be distinguished on the basis of differences in body coloration, eyes, proportions of cheliped articles, shape of the uropodal endopods, and sculpture of the first and second male pleopods. At present known from only four small specimens, all from the type locality, N. cacahuate appears to mature at a much smaller size than does N. grandimana. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560. RP FELDER, DL (reprint author), UNIV SW LOUISIANA,DEPT BIOL,BOX 42451,LAFAYETTE,LA 70504, USA. NR 19 TC 8 Z9 11 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD SEP 19 PY 1995 VL 108 IS 3 BP 477 EP 490 PG 14 WC Biology SC Life Sciences & Biomedicine - Other Topics GA RW567 UT WOS:A1995RW56700010 ER PT J AU CAIRNS, SD AF CAIRNS, SD TI NEW RECORDS OF AZOOXANTHELLATE STONY CORALS (CNIDARIA, SCLERACTINIA AND STYLASTERIDAE) FROM THE NEOGENE OF PANAMA AND COSTA-RICA SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Five new species of azooxanthellate Scleractinia are described from the Panamanian-Costa Rican Neogene: Septastraea altispina, Antillocyathus gracilis, Paracyathus adetos, Oxysmilia pliocenica, and Asterosmilia irregularis. Three additional species of azooxanthellate stony corals are also reported for the first time in the fossil record: Gardineria minor; Schizocyathus fissilis, and Stylaster roseus. The records of S. roseus are the first fossil occurrence of a stylasterid in the western Atlantic. RP CAIRNS, SD (reprint author), SMITHSONIAN INST,DEPT INVERTEBRATE ZOOL,NHB-163,W-329,WASHINGTON,DC 20560, USA. NR 43 TC 1 Z9 1 U1 1 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD SEP 19 PY 1995 VL 108 IS 3 BP 533 EP 550 PG 18 WC Biology SC Life Sciences & Biomedicine - Other Topics GA RW567 UT WOS:A1995RW56700016 ER PT J AU MITROVICA, JX DAVIS, JL AF MITROVICA, JX DAVIS, JL TI PRESENT-DAY POSTGLACIAL SEA-LEVEL CHANGE FAR FROM THE LATE PLEISTOCENE ICE SHEETS - IMPLICATIONS FOR RECENT ANALYSES OF TIDE-GAUGE RECORDS SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB We examine the sensitivity of predictions of the present-day rate of sea level change due to glacial isostatic adjustment (GIA) in two regions located within the 'far-field' of the Late Pleistocene ice sheets (Europe/north Africa and the western Pacific/Caribbean) to variations in the mantle viscosity profile. The regions considered here encompass the location of II (of 21) sites used in a recent determination, based on GIA-corrected tide gauge records, of the global rate of secular sea level change. Our analysis suggests that the mean GIA correction at the 11 far-field sites may vary by as much as 0.5 mm/yr, depending on the adopted Earth model, and we derive a bound on the (residual) secular sea level rise of 1.1 to 1.6 mm/yr. This bound is consistent with our analysis of the tide gauge record from the U.S. east coast, and it suggests that previous estimates of the residual sea level rise represent an upper bound. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MITROVICA, JX (reprint author), UNIV TORONTO,DEPT PHYS,60 ST GEORGE ST,TORONTO,ON M5S 1A7,CANADA. RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 6 TC 38 Z9 38 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 15 PY 1995 VL 22 IS 18 BP 2529 EP 2532 DI 10.1029/95GL02240 PG 4 WC Geosciences, Multidisciplinary SC Geology GA RW251 UT WOS:A1995RW25100023 ER PT J AU GINGERICH, O AF GINGERICH, O TI COSMOLOGY IN ANTIQUITY - WRIGHT,MR SO NATURE LA English DT Book Review RP GINGERICH, O (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD SEP 14 PY 1995 VL 377 IS 6545 BP 114 EP 114 DI 10.1038/377114a0 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RU754 UT WOS:A1995RU75400037 ER PT J AU DISTEFANO, R PAERELS, F RAPPAPORT, S AF DISTEFANO, R PAERELS, F RAPPAPORT, S TI LUMINOUS SUPERSOFT X-RAY SOURCES AND THE PLANETARY-NEBULA LUMINOSITY FUNCTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE BINARIES, CLOSE; PLANETARY NEBULAE, GENERAL; X-RAYS, ISM; X-RAYS, STARS ID STANDARD CANDLES; MAGELLANIC CLOUD; MODELS; DISTANCE; CAL-87; BINARY; LMC AB Theory suggests that luminous supersoft X-ray sources can be associated with ionization nebulae that have distinctive properties. In this work we point out that such supersoft nebulae can have luminosities in the [O III] lambda 5007 line similar to those associated with the most [O III]-luminous planetary nebulae. The implications of this connection between the well-studied class of planetary nebulae and the nebulae associated with supersoft sources are explored. Of particular interest to this investigation are ways in which the study of each of these classes of nebula may provide insights useful to the study of the other class. For example, we find that it is possible that some of the ''overluminous'' nebulae discovered in surveys for planetary nebulae may be supersoft nebulae. We propose specific observational strategies to test this hypothesis. Should it be verified, then we would have an example of how a search for planetary nebulae may lead to the discovery of supersoft nebulae, and of how the ''contamination'' of the planetary nebula luminosity function (PNLF) by supersoft nebulae may help us to resolve an outstanding puzzle about the PNLF. We also address the possible influence that such ''contamination'' may have on the use of the PNLF to determine distances. Although any such effect (if present at all) would be small, it is likely to be systematic, and is therefore susceptible to elimination, to help further refine the PNLF method of distance determination. Possibly even more interesting than this connection with a particular type of well-studied nebula is the potential importance of the study of supersoft nebulae to the overall study of supersoft sources, especially in extending the distances out to which systematic searches for individual sources can be performed. Our derivation of the supersoft nebulae luminosity function (SNLF, in [O III]) is a result that is independent of the comparison with the PNLF. The comparison with planetary nebulae, which can be studied in distant galaxies, suggests, however, that should a significant fraction of supersoft sources be associated with nebulae, then we may be able to conduct systematic studies of such sources out to distances at least as great as those to the Virgo cluster. Furthermore, for all sources, including those in the Local Group (where X-ray surveys have provided the complete census to date), we find that the selection effects for discovery via a nebula are different from those for discovery in an X-ray survey, in that surveys of nebulae may favor lower temperature sources than X-ray surveys. C1 UNIV CALIF BERKELEY, DEPT PHYS, BERKELEY, CA 94720 USA. MIT, DEPT PHYS, CAMBRIDGE, MA 02139 USA. MIT, CTR SPACE RES, CAMBRIDGE, MA 02139 USA. RP DISTEFANO, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 38 TC 12 Z9 12 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 1995 VL 450 IS 2 BP 705 EP 711 DI 10.1086/176176 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RT244 UT WOS:A1995RT24400019 ER PT J AU BALIUNAS, S SOON, W AF BALIUNAS, S SOON, W TI ARE VARIATIONS IN THE LENGTH OF THE ACTIVITY CYCLE-RELATED TO CHANGES IN BRIGHTNESS IN SOLAR-TYPE STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, ACTIVITY; STARS, CHROMOSPHERES; STARS, LATE-TYPE; STARS, MAGNETIC FIELDS; SUN, ACTIVITY; SUNSPOTS ID MAIN-SEQUENCE STARS; IRRADIANCE VARIATIONS; LINEAR-REGRESSION; MAGNETIC ACTIVITY; SUNSPOT CYCLE; TIME-SERIES; COOL STARS; K-EMISSION; LUMINOSITY; SUN AB We compare the average level of chromospheric activity and cycle length for solar-type stars as determined from 25 yr records of Ca II fluxes and from the sunspot record from 1750 to 1990. Both sets of data show an inverse relation between the cycle length and average activity level, with only a minor difference in the slopes. In turn, the amplitude of Ca II variability is positively correlated with the photometric brightness change during an activity cycle. The relationship between those observables provides a physical basis for the close correlation between the length of the sunspot cycle and mean terrestrial temperature over the last few centuries as shown by Friis-Christensen & Lassen. Solar brightness variations over the last several centuries can be estimated from this relationship by including stars with low Ca II fluxes which, we assume, are in states resembling the phase of solar activity known as the Maunder minimum (circa 1645-1715). Although the value of the slope connecting the mean level of Ca II activity and the cycle length is sensitive to the statistical treatment of the data, a lower limit to the slope can be determined reliably. This lower limit yields an increase of 0.4% of solar brightness from the solar Maunder minimum to the cyclic phase of sunspot activity which immediately followed the Maunder minimum. RP BALIUNAS, S (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 60 TC 51 Z9 52 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 1995 VL 450 IS 2 BP 896 EP 901 DI 10.1086/176193 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RT244 UT WOS:A1995RT24400036 ER PT J AU BROADHURST, T LEHAR, J AF BROADHURST, T LEHAR, J TI A GRAVITATIONAL LENS SOLUTION FOR THE IRAS GALAXY FSC-10214+4724 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (FSC 10214+4724); GRAVITATIONAL LENSING ID ACTIVE GALACTIC NUCLEI; CROSS-SECTIONS; LUMINOSITY AB We show that the z = 2.3 IRAS source FSC 10214 + 4724 is gravitationally lensed by an intervening elliptical galaxy. Its many anomalous properties can be explained if the active galactic nucleus (AGN) region of the source is much more magnified than its outer regions. We uncover a small counterimage to the are adjacent to the lensing galaxy, as predicted by our lens model. A redshift of unity for the lens is suggested by a red component in the observed spectrum, yielding a lensing mass interior to the critical radius of M(r < 3 kpc) approximate to 10(11) M., consistent with an ordinary massive galaxy. We present new high-resolution optical images which show a thin are of emission, implying that the optical source is compact (less than 0.5 kpc) and highly magnified (more than 20 times). Since the optical emission is known to be strongly polarized and Seyfert 2, we propose that the optical are is a highly magnified image of the inner ''mirror'' region of an obscured AGN. The central obscuring ''torus'' will be similarly magnified, naturally accounting for the large IR flux. We propose that cases like F10214 represent the obscured AGN counterparts to the lensed QSO population, and find that the probability of finding objects like F10214 in IRAS redshift surveys is reasonably large. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP BROADHURST, T (reprint author), JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218, USA. NR 28 TC 63 Z9 63 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 1995 VL 450 IS 2 BP L41 EP L44 DI 10.1086/316774 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RT246 UT WOS:A1995RT24600001 ER PT J AU CHEN, H ZHAO, JH OHASHI, N AF CHEN, H ZHAO, JH OHASHI, N TI DUST EMISSION FROM L1641N - AN OPTICALLY THICK CIRCUMSTELLAR DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; DUST, EXTINCTION; STARS, INDIVIDUAL (L1641N, 05338-0624) ID YOUNG STELLAR OBJECTS; STAR FORMATION; IRAS SOURCES; OUTFLOWS; LINE AB We have obtained high angular resolution (1 ''-3 '') continuum maps of the young stellar object L1641N (IRAS 05338-0624) at 2.0 mm, 7.0 mm, and 1.3 cm. The source positions at the three wavelengths coincide with a very red near-IR source detectable only at lambda > 4 mu m. The source is unresolved at 1.3 cm with a 1 '' beam (or 250 AU in radius). When combined with flux densities at other wavelengths, we find that the spectral energy distribution at mm wavelengths can be well fit by a power law with a spectral index of 2.1 +/- 0.2, and that the distribution between 2.0 mm and 6 cm can be well fit by a combination of the dust emission and optically thin free-free emission. Among several possible interpretations of the observed continuum spectrum, we favor optically thick dust emission from within 250 AU of L1641N, and the most probable origin of such emission is a circumstellar disk around the young star. We also discuss the physical properties of the optically thick disk. C1 HARVARD UNIV,SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 20 TC 17 Z9 17 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 1995 VL 450 IS 2 BP L71 EP L74 DI 10.1086/316773 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RT246 UT WOS:A1995RT24600008 ER PT J AU MENTEN, KM YOUNG, K AF MENTEN, KM YOUNG, K TI DISCOVERY OF STRONG VIBRATIONALLY EXCITED WATER MASERS AT 658 GHZ TOWARD EVOLVED STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; MASERS; STARS, AGE AND POST-AGE; STARS, MASS LOSS; STARS, VARIABLES, OTHER ID EMISSION; INTERSTELLAR; SPECTROSCOPY AB We report the astronomical discovery of the 1(10) --> 1(01) rotational transition within the v(2) = 1 vibrationally excited state of water vapor (H2O). Using the 10.4 m telescope of the Caltech Submillimeter Observatory, we detect strong maser emission in this line, which has a frequency near 658 GHz, toward a diverse sample of oxygen-rich red giant and supergiant stars. In circumstellar envelopes these 658 GHz H2O masers appear to be as common as SiO masers and H2O masers in other transitions, while we fail to detect 658 GHz H2O emission toward the W49 N and W51 N star-forming regions. For all of the 11 stars detected, the luminosity in the 658 GHz H(2)0 transition is comparable to or higher than the luminosity of any other known SiO or H2O maser line. C1 CALTECH SUBMILLIMETER OBSERV,HILO,HI 96720. RP MENTEN, KM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 31 TC 34 Z9 34 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 1995 VL 450 IS 2 BP L67 EP L70 DI 10.1086/316776 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RT246 UT WOS:A1995RT24600007 ER PT J AU ZHANG, Q HO, PTP AF ZHANG, Q HO, PTP TI AMMONIA MASER IN A MOLECULAR OUTFLOW TOWARD W51 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, CLOUDS; ISM, INDIVIDUAL (W51); MASERS; STARS, FORMATION ID INTERSTELLAR AMMONIA; STAR-FORMATION; THERMOMETER; EMISSION; REGIONS; LINE AB We report the discovery of a (NH3)-N-14 maser in the (J, K) = (3, 3) transition toward the W51-North H II complex. The maser line has a FWHM of 1.7 km s(-1) and an asymmetric profile, which suggests multiple features in the velocity range. Measured with the VLA, the maser emission has a peak flux of 230 mJy and a maximum deconvolved size of 0 ''.2. These values set a lower limit to the brightness temperature of 1.3 x 10(4) K. Thermal emission of ammonia was also detected toward this region. The elongated structure, velocity, and temperature gradients, and high excitation of the thermal ammonia indicate that the (3, 3) maser is excited in an expanding shell of a molecular outflow, powered possibly by the massive OB star D2. Molecular hydrogen densities and kinetic temperatures in the maser region are consistent with models of collisional pumping of the (3, 3) maser. RP ZHANG, Q (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Zhang, Qizhou/0000-0003-2384-6589 NR 20 TC 29 Z9 29 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 1995 VL 450 IS 2 BP L63 EP L66 DI 10.1086/316772 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RT246 UT WOS:A1995RT24600006 ER PT J AU KRISCHKE, M LORENZINI, EC SABATH, D AF KRISCHKE, M LORENZINI, EC SABATH, D TI A HYPERSONIC PARACHUTE FOR LOW-TEMPERATURE REENTRY SO ACTA ASTRONAUTICA LA English DT Article AB Atmospheric re-entry, even when initiated from a circular low-Earth orbit, requires heavy heat shields, ablative materials or radiative dissipation techniques. Semi-analytical and numerical simulations of the atmospheric re-entry from low-Earth orbits of a capsule with a 20-km, attached, heat resistant tether have shown that the thermal input flux on the capsule is reduced by more than one order of magnitude with respect to a comparable re-entry without tether. Long tethers have low ballistic coefficients and a large surface for heat dissipation. Moreover, a long tether is stabilized by gravity gradient and consequently tends to maintain a high angle of attack with respect to the wind velocity. The exposed surface of a 20-km-long l-mm diameter tether is 20 m(2), which is much larger than the cross section of a re-entry capsule. The resulting strong drag decelerates the capsule during re-entry like a conceivable hypersonic parachute would do. This paper describes the methods and results of the simulation of the SEDS endmass re-entry with different tethers. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 0 TC 5 Z9 6 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD SEP PY 1995 VL 36 IS 5 BP 271 EP 278 DI 10.1016/0094-5765(95)00108-C PG 8 WC Engineering, Aerospace SC Engineering GA TH068 UT WOS:A1995TH06800004 ER PT J AU LAUGHLIN, RM AF LAUGHLIN, RM TI FROM ALL FOR ALL - A TZOTZIL-TZELTAL TRAGICOMEDY SO AMERICAN ANTHROPOLOGIST LA English DT Article AB The script of a Highland Mayan play is introduced by an account of the founding and evolution of a Mayan performance group known as the Monkey Business Theatre. The play From All for All dramatizes the economic, social, and political forces that caused the Zapatistas to rise up and the Chiapas rain forests to fall. The role of the anthropologist as dramaturge and impresario, accompanying but not directing Maya colleagues, is explored. RP LAUGHLIN, RM (reprint author), SMITHSONIAN INST,NATL MUSEUM MAN,NATL MUSEUM NAT HIST,DEPT ANTHROPOL,WASHINGTON,DC 20560, USA. NR 0 TC 4 Z9 4 U1 0 U2 2 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 SN 0002-7294 J9 AM ANTHROPOL JI Am. Anthropol. PD SEP PY 1995 VL 97 IS 3 BP 528 EP 542 DI 10.1525/aa.1995.97.3.02a00110 PG 15 WC Anthropology SC Anthropology GA RR888 UT WOS:A1995RR88800010 ER PT J AU MATHIS, WN AF MATHIS, WN TI SHORE FLIES OF THE GALAPAGOS-ISLANDS (DIPTERA, EPHYDRIDAE) SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE DIPTERA; EPHYDRIDAE; SHORE FLIES; GALAPAGOS ISLANDS AB Fifteen species of shore flies, nearly doubling the number of known fauna, are reported from the Galapagos Islands. Of the 15 species, all but 2 are widespread in the Neotropics and apparently arrived on the Galapagos as introductions, which were probably independent events. The 2 apparent endemics, Philygria galapagensis Wirth and Scatella galapagensis Curran, may have speciated on these islands. The shore-fly fauna is disharmonic biogeographically, with only 11 of 20 tribes being represented. Ephydra, gilvipes Coquillett (new synonym) is conspecific with E. chilensis Macquart, the senior synonym. A lectotype for Paralimna decipiens Loew is designated. RP MATHIS, WN (reprint author), SMITHSONIAN INST, DEPT ENTOMOL, NHB 169, WASHINGTON, DC 20560 USA. NR 50 TC 6 Z9 7 U1 1 U2 3 PU ENTOMOLOGICAL SOC AMER PI LANHAM PA 10001 DEREKWOOD LANE, STE 100, LANHAM, MD 20706-4876 USA SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD SEP PY 1995 VL 88 IS 5 BP 627 EP 640 PG 14 WC Entomology SC Entomology GA RX492 UT WOS:A1995RX49200002 ER PT J AU GOLDBERG, S AF GOLDBERG, S TI GROVES AND OPPENHEIMER, THE STORY OF A PARTNERSHIP SO ANTIOCH REVIEW LA English DT Article RP GOLDBERG, S (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ANTIOCH REVIEW PI YELLOW SPRINGS PA BOX 148, YELLOW SPRINGS, OH 45387 SN 0003-5769 J9 ANTIOCH REV JI Antioch Rev. PD FAL PY 1995 VL 53 IS 4 BP 482 EP 493 PG 12 WC Literary Reviews SC Literature GA TF819 UT WOS:A1995TF81900021 ER PT J AU PIPERNO, DR AF PIPERNO, DR TI TROPICAL ARCHAEOBOTANY - APPLICATIONS AND NEW DEVELOPMENTS - HATHER,JG SO ANTIQUITY LA English DT Book Review RP PIPERNO, DR (reprint author), SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ANTIQUITY PUBL LTD PI CAMBRIDGE PA KINGS HEDGES ROAD, CAMBRIDGE, ENGLAND C83 2PQ SN 0003-598X J9 ANTIQUITY JI Antiquity PD SEP PY 1995 VL 69 IS 264 BP 641 EP 642 PG 2 WC Anthropology; Archaeology SC Anthropology; Archaeology GA RW151 UT WOS:A1995RW15100035 ER PT J AU PROSSER, CF STAUFFER, JR CAILLAULT, JP BALACHANDRAN, S STERN, RA RANDICH, S AF PROSSER, CF STAUFFER, JR CAILLAULT, JP BALACHANDRAN, S STERN, RA RANDICH, S TI AN X-RAY SURVEY OF THE OPEN CLUSTER NGC-6475 (M7) WITH ROSAT SO ASTRONOMICAL JOURNAL LA English DT Article ID MAIN-SEQUENCE; PHOTOMETRY; STARS; SKY AB A ROSAT x-ray survey, with complimentary optical photometry, of the open cluster NGC 6475 has enabled the detection of similar to 50 late-F to KO and similar to 70 K/M dwarf new candidate members, providing the first reliable detection of low-mass stars in this low galactic latitude, 220 Myr old cluster. The x-ray observations reported here have a typical limiting sensitivity of L(X) similar or equal to 10(29) erg/s. The detection frequency of early type cluster members is consistent with the hypothesis that the x-ray emitting early type stars are binary systems with an unseen, low-mass secondary producing the x rays. The ratio between x-ray and bolometric luminosity among NGC 6475 members saturates at a spectral-type/color which is intermediate between that in much younger and in much older clusters, consistent with rotational spindown of solar-type stars upon their arrival on the ZAMS. The upper envelope of x-ray luminosity as a function of spectral type is comparable to that of the Pleiades, with the observed spread in x-ray luminosity among low-mass members being likely due to the presence of binaries and relatively rapid rotators. However, the list of x-ray selected candidate members is likely biased against low-mass, slowly rotating single stars. While some preliminary spectroscopic information is given in an appendix, further spectroscopic observations of the new candidate members will aid in interpreting the coronal activity among solar-type NGC 6475 members and their relation to similar stars in older and younger open clusters. (C) 1995 American Astronomical Society. C1 UNIV GEORGIA,DEPT PHYS & ASTRON,ATHENS,GA 30602. OHIO STATE UNIV,DEPT ASTRON,COLUMBUS,OH 43210. LOCKHEED PALO ALTO RES LABS,PALO ALTO,CA 94304. MAX PLANCK INST EXTRATERR PHYS,D-85740 GARCHING,GERMANY. RP PROSSER, CF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MS-66,CAMBRIDGE,MA 02138, USA. OI Randich, Sofia/0000-0003-2438-0899 NR 42 TC 34 Z9 35 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 1995 VL 110 IS 3 BP 1229 EP 1247 DI 10.1086/117599 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RR927 UT WOS:A1995RR92700024 ER PT J AU DYCK, HM BENSON, JA SCHLOERB, FP AF DYCK, HM BENSON, JA SCHLOERB, FP TI IMAGING A BINARY STAR WITH A 2-TELESCOPE MICHELSON STELLAR INTERFEROMETER SO ASTRONOMICAL JOURNAL LA English DT Article ID LINE AB Using a two-telescope Michelson stellar interferometer we observed the well known visual binary star zeta Her. By rapidly driving the optical delay line of the interferometer we were able to obtain temporally distinct interferograms from each component of the binary, preserving the image position information. This observation is presented as an illustration of a technique for imaging with two telescopes which we have named ''delay-referenced interferometry.'' We discuss the implications our measurements for zeta Her and predict resolution Limits for other binary systems. With the aid of a simple illustration, we argue that delay referencing is a useful technique for more complex systems when the object is contained entirely within the detector field of view and within the isoplanatic patch. We show how ''snapshot'' observations at a variety of interferometer orientations may be used in tomographic backprojection of delay-referenced fringes to generate an image of such sources. (C) 1995 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV MASSACHUSETTS,DEPT PHYS & ASTRON,AMHERST,MA 01003. RP DYCK, HM (reprint author), UNIV WYOMING,DEPT PHYS & ASTRON,LARAMIE,WY 82071, USA. NR 28 TC 13 Z9 13 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 1995 VL 110 IS 3 BP 1433 EP 1439 DI 10.1086/117617 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RR927 UT WOS:A1995RR92700042 ER PT J AU LOINARD, L ALLEN, RJ LEQUEUX, J AF LOINARD, L ALLEN, RJ LEQUEUX, J TI AN UNBIASED SURVEY FOR CO EMISSION IN THE INNER DISK OF THE ANDROMEDA GALAXY SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE GALAXIES, INDIVIDUAL(M 31); GALAXIES, ISM; ISM, MOLECULES; RADIO LINES, GALAXIES ID IONIZED-GAS; M31; KINEMATICS; BULGE; M-31 AB Recently, Alien and Lequeux (1993) have detected faint CO emission from two massive molecular clouds in the inner disk of M 31. These clouds were first located optically by their dust content. In order to determine the validity of this selection criterion, we have carried out an ''unbiased'' survey at 26 positions regularly spaced every 3.6' along the major axis of M 31. Faint CO emission was detected for 16 of them. Dark clouds are seen optically at many of the positions where CO is detected, confirming a posteriori the proposition that there is a close correlation between the presence of dust and the presence of faint CO emission. However, we also find detectable CO emission at positions for which there are no catalogued dust clouds; the survey therefore points to a significantly larger area covering factor for the molecular gas in the inner disk of M 31 than previously thought. Our observations suggest that the mass surface density of gas perpendicular to the plane of the disk is as high as 10 M.pc(-2) in the inner regions of M 31, which exhibits no central ''gas hole'' contrary to the common belief. The velocities of the CO(1-0) lines trace a rotation curve which is in general agreement with that of the H I obtained earlier by Brinks and Shane (1984), although the component of the H I attributed by those authors to a warp of the outer disk of M 31 seen in projection on the inner disk does not appear to have a counterpart in CO at the present level of detection. The ratios of the integrated CO(2-1) to CO(1-0) line intensities, when both can be measured, are generally very low (similar to 0.4), consistent with models of cold (T-K < 5 K) molecular clouds at low density (similar to 100 cm(-3)). C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. OBSERV PARIS, DEMIRM, F-75014 PARIS, FRANCE. ECOLE NORMALE SUPER, F-75231 PARIS 05, FRANCE. RP LOINARD, L (reprint author), UNIV GRENOBLE 1, OBSERV GRENOBLE, ASTROPHYS LAB, BP 53X, F-38041 GRENOBLE, FRANCE. NR 28 TC 28 Z9 29 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 1995 VL 301 IS 1 BP 68 EP 74 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RU138 UT WOS:A1995RU13800010 ER PT J AU GREEN, PJ SCHARTEL, N ANDERSON, SF HEWETT, PC FOLTZ, CB BRINKMANN, W FINK, H TRUMPER, J MARGON, B AF GREEN, PJ SCHARTEL, N ANDERSON, SF HEWETT, PC FOLTZ, CB BRINKMANN, W FINK, H TRUMPER, J MARGON, B TI THE SOFT-X-RAY PROPERTIES OF A LARGE OPTICAL QSO SAMPLE - ROSAT OBSERVATIONS OF THE LARGE BRIGHT QUASAR SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, ACTIVE; QUASARS, GENERAL; SURVEYS; X-RAYS, GALAXIES ID ACTIVE GALACTIC NUCLEI; RADIO-QUIET QUASARS; ASTRONOMICAL DATA; LUMINOSITY FUNCTION; STATISTICAL-METHODS; EQUATORIAL FIELDS; GALAXY COUNTS; UPPER LIMITS; SPECTRA; EMISSION AB Of the more than 1000 QSOs in the Large Bright Quasar Survey (LBQS), we study the X-ray properties of 908 that were covered by the ROSAT All-Sky Survey (RASS). These data constitute among the largest, most homogeneous X-ray surveys of QSOs to date, and as such are well suited to the study of the multiwavelength properties of QSOs. Due to the approximate to 600 s RASS exposure times, only 10% of the QSOs are detected in X-rays. However, by stacking X-ray counts, we obtain effectively much more sensitive observations for an average QSO in bins of redshift or luminosity, and for several classes of QSOs. We confirm a correlation of alpha(ox) with luminosity for the overall sample. For higher redshifts and optical luminosities, radio-loud QSOs appear to become progressively more luminous in X-rays than radio-quiet QSOs. The X-ray properties of a subsample of 36 broad absorption line QSOs suggest that they are strongly absorbed or underluminous in the X-rays, while a subsample of 22 Fe II-strong QSOs is anomalously X-ray bright. C1 MAX PLANCK INST EXTRATERR PHYS, D-85740 GARCHING, GERMANY. UNIV WASHINGTON, DEPT ASTRON, SEATTLE, WA 98195 USA. UNIV CAMBRIDGE, INST ASTRON, CAMBRIDGE CB3 0HA, ENGLAND. UNIV ARIZONA, MULTIPLE MIRROR TELESCOPE OBSERV, TUCSON, AZ 85721 USA. RP GREEN, PJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Margon, Bruce/B-5913-2012 NR 69 TC 133 Z9 134 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1995 VL 450 IS 1 BP 51 EP 63 DI 10.1086/176118 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RQ577 UT WOS:A1995RQ57700007 ER PT J AU ZHAO, JH GOSS, WM HO, PTP AF ZHAO, JH GOSS, WM HO, PTP TI VLA OH OBSERVATIONS OF HIGH NEGATIVE VELOCITY GAS TOWARD SAGITTARIUS-A WEST - A HIGH-VELOCITY CLOUD INTERACTING WITH THE GALACTIC-CENTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXY, CENTER; ISM, CLOUDS; ISM, KINEMATICS AND DYNAMICS; RADIO LINES, ISM ID IONIZED-GAS; MOLECULAR GAS; CENTER REGION; GALAXY; KINEMATICS; RESOLUTION; RADIO; KILOMETERS; COMPLEX; PARSECS AB The high negative velocity cloud in the direction of Sgr A* at -180 km s(-1) was discussed by Glisten and Downes (1981) more than a decade ago. Since then, numerous observations have been carried out to determine the properties of this component; however, the nature of this feature was uncertain due to the lack of high angular resolution observations. Recently, we have carried out VLA observations of this feature in the H I and OH lines at V-LSR = -180 km s(-1) with an angular resolution of several arcseconds. The OH 1667 MHz absorption is the best tracer of the gas in front of the continuum sources in the Galactic center. Both the structure and the kinematics have been determined, and we show that the high negative velocity absorbing gas is well mixed with the ionized gas in the center of the Galaxy. The mass of neutral gas seen in absorption at -180 km s(-1) is about 5 x 10(3) M., only a small fraction of the entire cloud observed in CO emission. The observed kinematics are not consistent with ejection; outflow, or a possible association with the expanding molecular ring at V = -135 km s(-1). The location and morphology suggest that this high-velocity cloud may be tidally disrupted. Based on a numerical model, we demonstrate that the disrupted high-velocity gas can flow toward the Galactic center and interact with the central gravitational potential, thereby distorting the kinematics of the high-velocity gas projected in front of Sgr A West, This model also suggests that the mini-cavity 3'' southeast of Sgr A* could have resulted from the impact of a high negative velocity streamer. Both the morphology and the kinematics calculated in this model are consistent with the H92 alpha observations of the central 10'' of the Galaxy as published by Roberts, Yusef-Zadeh, and Goss (1995). C1 NATL RADIO ASTRON OBSERV, SOCORRO, NM 87801 USA. RP ZHAO, JH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 35 TC 14 Z9 15 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1995 VL 450 IS 1 BP 122 EP 136 DI 10.1086/176124 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RQ577 UT WOS:A1995RQ57700013 ER PT J AU SCOWEN, P HESTER, J CODE, A MACKIE, G LYNDS, CR ONEIL, EJ AF SCOWEN, P HESTER, J CODE, A MACKIE, G LYNDS, CR ONEIL, EJ TI HUBBLE-SPACE-TELESCOPE IMAGING OF THE WIND-BLOWN LOBE NGC-165 SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II REGIONS; ISM, INDIVIDUAL (NGC 6165); ISM, KINEMATICS AND DYNAMICS; STARS, INDIVIDUAL (HD 148937); STARS, MASS LOSS ID O-STARS; STELLAR WINDS; SUPER-GIANTS; SUPERGIANTS; VELOCITIES; HD-148937; NEARBY AB We have used the Hubble Space Telescope wide field/planetary camera to study the structure of the bipolar nebular NGC 6164/6165. Our study concentrates on the structure of a number of small clumps of material embedded within the southern lobe of the system (NGC 6165). These knots have a cometary appearance, with bright surfaces facing the central star, and streamers of material pointing away from the star, We present a simple model in which a bow shock forms between the stellar wind and clump material which has been photoionized by the UV radiation from HD 148937. The observed streamers are clump material which has been driven out of the region of high pressure between the clump and the bow shock. This model is able to account for most observed properties of the system quantitatively and leads to an estimated mass-loss rate for the star of 2.2 x 10(-5) M. yr(-1). C1 UNIV WISCONSIN,DEPT ASTRON,WASHBURN OBSERV,MADISON,WI 53706. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. KITT PEAK NATL OBSERV,NATL OPT ASTRON OBSERV,TUCSON,AZ 85726. RP SCOWEN, P (reprint author), ARIZONA STATE UNIV,DEPT PHYS & ASTRON,TEMPE,AZ 85287, USA. NR 22 TC 3 Z9 3 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1995 VL 450 IS 1 BP 196 EP 200 DI 10.1086/176131 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RQ577 UT WOS:A1995RQ57700020 ER PT J AU GAGNE, M CAILLAULT, JP STAUFFER, JR AF GAGNE, M CAILLAULT, JP STAUFFER, JR TI SPECTRAL AND TEMPORAL CHARACTERISTICS OF X-RAY-BRIGHT STARS IN THE PLEIADES SO ASTROPHYSICAL JOURNAL LA English DT Article DE OPEN CLUSTERS AND ASSOCIATIONS, INDIVIDUAL (PLEIADES); STARS, CORONAE; STARS, LATE-TYPE; STARS, ROTATION; X-RAYS, STARS ID CORONAL TEMPERATURES; EMISSION; FLARE; CLUSTER; EXOSAT; SOLAR; ROSAT; SKY AB We follow up our deep ROSAT imaging survey of the Pleiades (Stauffer et al. 1994) with an analysis of the spectral and temporal characteristics of the X-ray-bright stars in the Pleiades. Raymond and Smith (1977) one-and two-temperature models have been used to fit the position-sensitive proportional counter (PSPC) pulse height spectra of the dozen or so brightest sources associated with late-type Pleiades members. The best-fit temperatures suggest hot coronal temperatures for K, M, and rapidly rotating G stars, and cooler temperatures for F and slowly rotating G stars. In order to probe the many less X-ray-luminous stars, we have generated composite spectra by combining net counts from all Pleiades members according to spectral type and rotational velocity. Model fits to the composite spectra confirm the trend seen in the individual spectral fits, Particularly interesting is the apparent dependence of coronal temperature on L(X)/L(bol). A hardness-ratio analysis also confirms some of these trends. The PSPC data have also revealed a dozen or so strong X-ray flares with peak X-ray luminosities in excess of similar to 10(30) ergs s(-1). We have modeled the brightest of these flares with a simple quasi-static cooling loop model. The peak temperature and emission measure and the inferred electron density and plasma volume suggest a very large scale flaring event. The PSPC data were collected over a period of similar to 18 months, allowing us to search for source variability on timescales ranging from less than a day (in the case of dares) to more than a year between individual exposures. On approximately year-long timescales, roughly 25% of the late-type stars are variable. Since the Pleiades was also intensively monitored by the imaging instruments on the Einstein Observatory, we have examined X-ray luminosity variations on the 10 yr timescale between Einstein and ROSAT and find that up to 40% of the late-type stars are X-ray variable. Since there is only marginal evidence for increased variability on decade-long timescales, the variability observed on long and short timescales may have a common physical origin. C1 UNIV COLORADO,JOINT INST LAB ASTROPHYS,BOULDER,CO 80309. NATL INST STAND & TECHNOL,BOULDER,CO 80309. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP GAGNE, M (reprint author), UNIV GEORGIA,DEPT PHYS & ASTRON,ATHENS,GA 30602, USA. RI Gagne, Marc/C-1130-2013 NR 31 TC 69 Z9 69 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1995 VL 450 IS 1 BP 217 EP 232 DI 10.1086/176133 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RQ577 UT WOS:A1995RQ57700022 ER PT J AU NEUFELD, DA LEPP, S MELNICK, GJ AF NEUFELD, DA LEPP, S MELNICK, GJ TI THERMAL BALANCE IN DENSE MOLECULAR CLOUDS - RADIATIVE COOLING RATES AND EMISSION-LINE LUMINOSITIES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM, CLOUDS; ISM, MOLECULES; MOLECULAR PROCESSES; RADIATIVE TRANSFER; RADIO LINES, ISM ID FINE-STRUCTURE TRANSITIONS; INTERSTELLAR CLOUDS; RATE COEFFICIENTS; EXCITATION; SEARCH; OXYGEN; GAS; ABUNDANCES; OMC-1; CORES AB We consider the radiative cooling of fully shielded molecular astrophysical gas over a wide range of temperatures (10 K less than or equal to T less than or equal to 2500 K) and Ha densities (10(3) cm(-3) less than or equal to n(H-2) less than or equal to 10(10) cm(-3)). Our model for the radiative cooling of molecular gas includes a detailed treatment of the interstellar chemistry that determines the abundances of important coolant molecules, and a detailed treatment of the excitation of the species H-2, CO, H2O, HCl, O-2 C, O, and their isotopic variants where important. We present results for the total radiative cooling rate and for the cooling rate due to individual coolant species, as a function of the gas temperature, density, and optical depth. We have also computed the individual millimeter, submillimeter, and far-infrared line strengths that contribute to the total radiative cooling rate, and we have obtained example spectra for the submillimeter emission expected from molecular cloud cores. Many of the important cooling lines will be detectable using the Infrared Space Observatory and the Submillimeter Wave Astronomy Satellite. C1 UNIV NEVADA,DEPT PHYS,LAS VEGAS,NV 89154. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP NEUFELD, DA (reprint author), JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,3400 N CHARLES ST,BALTIMORE,MD 21218, USA. NR 40 TC 201 Z9 202 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 1995 VL 100 IS 1 BP 132 EP 147 DI 10.1086/192211 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RQ010 UT WOS:A1995RQ01000006 ER PT J AU PIPER, WH PARKER, PG RABENOLD, KN AF PIPER, WH PARKER, PG RABENOLD, KN TI FACULTATIVE DISPERSAL BY JUVENILE MALES IN THE COOPERATIVE STRIPE-BACKED WREN SO BEHAVIORAL ECOLOGY LA English DT Article DE CAMPYORHYNCHUS; COOPERATIVE BREEDING; DEMOGRAPHIC DATA; DNA FINGERPRINTING; HELPING BEHAVIOR; JUVENILE DISPERSAL; NATAL DISPERSAL AB present genetic and demographic data documenting juvenile dispersal in the cooperatively breeding stripe-backed wren (Campylorhynchus nuchalis) of Venezuela. Parentage and DNA fragment-sharing analyses revealed 12 cases in which juveniles were unrelated to other group members. Of these 12 foreign juveniles, (1) all were males, (2) eight of 12 had been found with breeding pairs lacking helpers rather than with groups containing helpers, and (3) four out of seven of those observed as adults courted or sired offspring with the dominant females in their new groups despite the strong incest avoidance of this species. Furthermore, juvenile males had a significant tendency to disappear from natal groups in their first year, and singleton juveniles observed with pairs after the breeding season were mostly males. These data support the hypothesis that foreign juveniles were dispersers from intact groups and not products of conspecific brood parasitism or adoption following group dissolution. We suggest that unassisted pairs might accept juvenile males into their groups as helpers to increase their future reproductive success and that dispersers themselves might leave large natal groups in which their helping is superfluous to join small groups of nonrelatives in which they might soon reproduce. RP PIPER, WH (reprint author), SMITHSONIAN INST,NATL ZOOL PK,MOLEC GENET LAB,WASHINGTON,DC 20008, USA. NR 0 TC 11 Z9 11 U1 3 U2 16 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 SN 1045-2249 J9 BEHAV ECOL JI Behav. Ecol. PD FAL PY 1995 VL 6 IS 3 BP 337 EP 342 DI 10.1093/beheco/6.3.337 PG 6 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA RK733 UT WOS:A1995RK73300014 ER PT J AU MONFORT, SL HARVEY, E GEURTS, L PADILLA, L SIMMONS, HA WILLIAMSON, LR AF MONFORT, SL HARVEY, E GEURTS, L PADILLA, L SIMMONS, HA WILLIAMSON, LR TI URINARY 3-ALPHA,17-BETA-ANDROSTANEDIOL GLUCURONIDE IS A MEASURE OF ANDROGENIC STATUS IN ELD DEER STAGS (CERVUS-ELDI-THAMIN) SO BIOLOGY OF REPRODUCTION LA English DT Article ID MONITORING OVARIAN-FUNCTION; PAPIO-CYNOCEPHALUS-CYNOCEPHALUS; MALE FALLOW DEER; SERUM TESTOSTERONE; PROGESTERONE METABOLITES; MACACA-FASCICULARIS; STEROID METABOLITES; LUTEINIZING-HORMONE; SEASONAL-CHANGES; FECAL STEROIDS AB To determine the primary excretory by-products of testosterone (T), 85 mu Ci [H-3]T was administered i,v, to two adult Eld's deer stags, Blood (10 mi) was collected by jugular venipuncture at 0, 5, 10, 15, 30, 45, 60, 90, 120, 150, 180, 240, and 480 min after isotope infusion, and all urine and feces were collected for 96 h after injection. Seventy percent of labeled circulating steroid was conjugated by 30 min postinfusion. The majority (80.4 +/- 3.2%) of T metabolites were excreted into urine, and 95.0 i: 0.9% of these were conjugated, 95.8 +/- 0.2% being hydrolyzable with glucuronidase. Seven urinary androgen metabolites, including androstanediol (5 alpha-androstan-3 alpha-17 beta-diol and 5 beta-androstan-3 alpha-17 beta-diol), were identified in glucuronidase-hydrolyzed, ether-extracted Eld's deer urine pools after gas chromatography/ mass spectrometry, A double-antibody I-125 RIA for 5 alpha-androstanediol-3 alpha,17 beta-diol, 17-glucuronide (3 alpha-diol-G) was validated for unprocessed urine, Longitudinal assessments of urine samples collected from 13 stags for 3 yr revealed biological concordance between fluctuations in urinary 3 alpha-diol-G and serum T,as well as seasonal changes in secondary sexual characteristics. Overall correlation between ''same-day'' matched serum T and urinary 3 alpha-diol-G was 0.58, (n = 6; p < 0.001). Thus, monitoring urinary 3 alpha-diol-G provides a noninvasive, alternative method for characterizing male endocrine interrelationships in an endangered ungulate species. RP MONFORT, SL (reprint author), SMITHSONIAN INST,NATL ZOOL PK,CONSERVAT & RES CTR,1500 REMT RD,FRONT ROYAL,VA 22630, USA. FU NICHD NIH HHS [HD 00903] NR 46 TC 6 Z9 6 U1 0 U2 2 PU SOC STUDY REPRODUCTION PI MADISON PA 1526 JEFFERSON ST, MADISON, WI 53711-2106 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD SEP PY 1995 VL 53 IS 3 BP 700 EP 706 DI 10.1095/biolreprod53.3.700 PG 7 WC Reproductive Biology SC Reproductive Biology GA RQ677 UT WOS:A1995RQ67700028 PM 7578696 ER PT J AU HARMON, ME WHIGHAM, DF SEXTON, J OLMSTED, I AF HARMON, ME WHIGHAM, DF SEXTON, J OLMSTED, I TI DECOMPOSITION AND MASS OF WOODY DETRITUS IN THE DRY TROPICAL FORESTS OF THE NORTHEASTERN YUCATAN PENINSULA, MEXICO SO BIOTROPICA LA English DT Article DE COARSE WOODY DEBRIS; DECAY; DECOMPOSITION; FINE WOODY DEBRIS; FIRE; HURRICANE; ORGANIC MATTER; TROPICAL FORESTS ID PICEA-TSUGA FORESTS; DECIDUOUS FOREST; WESTERN OREGON; LEAF-LITTER; FIR FOREST; DEBRIS; ECOSYSTEMS; BIOMASS; WASHINGTON; DYNAMICS AB The decomposition rates and mass of fine ( < 10-cm-diameter) and coarse ( > 10-cm-diameter) woody detritus were measured in the dry tropical forests of the northeastern Yucatan Peninsula. The smallest mass of woody detritus was found in undisturbed stands: fine fractions averaged 4.7 Mg ha(-1) and coarse fractions ranged between 13 and 38 Mg ha(-1). The largest mass of fine woody detritus (32.2 Mg ha(-1)) was found in a hurricane-disturbed forest; whereas, the largest mass of coarse woody detritus (99.5 Mg ha(-1)) was found in stands disturbed by catastrophic fires. A decomposition time-series study installed in 1989 indicated that decomposition rates varied greatly among species and diameters of branch segments. Over a 4-year period, the decomposition rate constant for fine woody detritus ranged from 0.151 to 1.019 year(-1) and that for coarse woody detritus ranged from 0.008 to 0.615 year(-1). The half-life of woody detritus increased 33-fold (among pieces ranging from 1 to 30 cm in diameter) for the most decay-resistant species (Manilkara zapota) but was relatively constant for the least decay-resistant species (Bursera simaruba). The wide range in decomposition rates observed in these forests indicates that the poor substrate quality of some species may override climatic (e.g., warm temperatures) and biotic (e.g., termites) factors favorable to rapid decomposition, leading to a substantial accumulation of woody detritus. C1 SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. CTR INVEST CIENT YUCATAN,MERIDA 97310,MEXICO. RP HARMON, ME (reprint author), OREGON STATE UNIV,DEPT FOREST SCI,PEAVY HALL 154,CORVALLIS,OR 97331, USA. OI Whigham, Dennis/0000-0003-1488-820X NR 40 TC 96 Z9 107 U1 2 U2 21 PU ASSN TROP BIOL PI ST LOUIS PA MISSOURI BOTANICAL GARDEN 2345 TOWER GROVE AVE, ST LOUIS, MO 63110 SN 0006-3606 J9 BIOTROPICA JI Biotropica PD SEP PY 1995 VL 27 IS 3 BP 305 EP 316 DI 10.2307/2388916 PG 12 WC Ecology SC Environmental Sciences & Ecology GA RX536 UT WOS:A1995RX53600003 ER PT J AU HOGAN, KP SMITH, AP SAMANIEGO, M AF HOGAN, KP SMITH, AP SAMANIEGO, M TI GAS-EXCHANGE IN 6 TROPICAL SEMI-DECIDUOUS FOREST CANOPY TREE SPECIES DURING THE WET AND DRY SEASONS SO BIOTROPICA LA English DT Article DE CANOPY TREES; GAS EXCHANGE; PANAMA; PHOTOSYNTHETIC RATE; SOMATAL CONDUCTANCE; TROPICAL SEASONALITY ID AUSTRALIAN RAINFOREST TREE; RAIN-FOREST; STOMATAL CONDUCTANCE; WATER RELATIONS; LIGHT; SEEDLINGS; PHOTOSYNTHESIS; TRANSPIRATION; INTERCEPTION; ENVIRONMENT AB Wet and dry season rates of photosynthesis and stomatal conductance were compared for upper canopy leaves of six species of tropical semi-deciduous forest trees. Photosynthetic rates showed no dear relationship to leaf form (simple/compound), specific leaf area, or seasonality (evergreen/deciduous). Photosynthetic rates for three of five evergreen species were similar in wet and dry seasons. The rates (in mu mol m(-2) sec(-1)) were 14.5 (wet season) and 15.5 (dry season) for Didymopanax morototoni, 13.8 (wet season) and 12.2 (dry season) for Ficus obtusifolia, and 10.4 (wet season) and 10.2 (dry season) for Luebea seemannii. In the dry season, stomatal conductance for all five evergreen species was half or less than in the wee season, except in Didymopanax, for which conductance was high in both seasons. For Anacardium excelsum and Cecropia longipes, photosynthetic rates in the dry season (4.71 and 6.38 pmol m(-2) sec(-1), respectively) were lower than in the wet season (8.62 and 12.4 mu mol m(-2) sec(-1)). For these species, the lower photosynthetic rates in the dry season were observed at internal CO2 concentrations (C-i) as high or higher than wet season C-i, suggesting: that photosynthetic activity was reduced by water stress. Pseudobombax septenatum, a dry season deciduous species, sometimes showed low levels of photosynthesis and stomatal conductance as well as low C-i levels, suggesting chat stomatal closure restricted photosynthetic activity. Higher stomatal conductance was associated with higher rates of photosynthesis among species and between seasons. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 36 TC 29 Z9 32 U1 0 U2 2 PU ASSN TROP BIOL PI ST LOUIS PA MISSOURI BOTANICAL GARDEN 2345 TOWER GROVE AVE, ST LOUIS, MO 63110 SN 0006-3606 J9 BIOTROPICA JI Biotropica PD SEP PY 1995 VL 27 IS 3 BP 324 EP 333 DI 10.2307/2388918 PG 10 WC Ecology SC Environmental Sciences & Ecology GA RX536 UT WOS:A1995RX53600005 ER PT J AU ROSENBERG, G LITTLER, DS LITTLER, MM OLIVEIRA, EC AF ROSENBERG, G LITTLER, DS LITTLER, MM OLIVEIRA, EC TI PRIMARY PRODUCTION AND PHOTOSYNTHETIC QUOTIENTS OF SEAWEEDS FROM SAO-PAULO STATE, BRAZIL SO BOTANICA MARINA LA English DT Article ID MARINE MACROALGAE; DARK RESPIRATION; RHODOPHYTA; OXYGEN; STRATEGIES; GROWTH; ALGAE; LIGHT; FORM AB Primary production was measured under natural conditions for five common species of seaweeds from the coast of the State of Sao Paulo, Brazil, using oxygen electrode and pH single-endpoint techniques. Productivity ranged from over 500 mu mol O-2 g dw(-1) h(-1) (about 6 mg C g dw(-1) h(-1)) for Ulva fasciata Delile (Chlorophyta), a sheet-like form, to 30 mu mol O-2 g dw(-1) h(-1) (about 0.36 mg C g dw(-1) h(-1)) in Laurencia papillosa (C. Agardh) Greville (Rhodophyta), a coarsely-branched form. Intermediate productivities were measured in two other coarsely-branched forms, Hypnea musciformis (Wulfen) Lamouroux (Rhodophyta) and Pterocladia capillacea (Gmelin) Bornet et Thuret (Rhodophyta) and in the thick-leathery species, Sargassum cymosum C. Agardh (Phaeophyta). Specific growth rates measured in the field or in continuous-flow seawater systems for commercially-valuable red algae range from 1% day(-1) in II capillacea to 14% day(-1) in H. musciformis. Primary production and growth rates are in agreement with the functional-form model of Littler and Littler. Available biomass information showed that the maximum standing stocks did not correspond to the growth potential determined from measurements of primary productivity and growth rates, suggesting that levels of standing stocks are determined more by physical factors (wave action) and biological interactions (grazing) than by intrinsic growth rate potentials. The measured ratios of net photosynthetic O-2 release to CO2 uptake (photosynthetic quotient, PQ), were consistently less than the theoretically expected values of 1.0 to 1.3 (mean measured values: 0.42 to 1.01). The PQ values did not vary according to taxonomic division or functional-form group and were unaffected by experimental nutrient (nitrate + phosphate) enrichment. The continued use of PQ = 1.00 is recommended to facilitate interconvertibility in comparisons between studies of primary production by seaweeds. C1 UNIV SAO PAULO,INST BIOCIENCIAS,DEPT BOT,BR-05422970 SAO PAULO,BRAZIL. RP ROSENBERG, G (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT MRC166,WASHINGTON,DC 20560, USA. RI Departamento de Botanica, IBUSP, Botany/J-1685-2012 NR 52 TC 31 Z9 32 U1 0 U2 9 PU WALTER DE GRUYTER & CO PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 0006-8055 J9 BOT MAR JI Bot. Marina PD SEP PY 1995 VL 38 IS 5 BP 369 EP 377 DI 10.1515/botm.1995.38.1-6.369 PG 9 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA TF243 UT WOS:A1995TF24300002 ER PT J AU BAYER, FM AF BAYER, FM TI 2 NEW SPECIES OF THE ALCYONACEAN GENUS PROTODENDRON (OCTOCORALLIA, ALCYONIIDAE) FROM THE INDIAN-OCEAN OFF NATAL SO BULLETIN OF MARINE SCIENCE LA English DT Article AB Two new species of the alcyoniid genus Protodendron obtained off the southeastern coast of Africa by the IIOE vessel ANTON BRUNN is described and compared with the type species, Protodendron repens (Thomson and Henderson, 1906). Taxonomic characters of all three species are illustrated by scanning electron micrographs. RP BAYER, FM (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20506, USA. NR 8 TC 1 Z9 1 U1 0 U2 0 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD SEP PY 1995 VL 57 IS 2 BP 301 EP 312 PG 12 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA RQ864 UT WOS:A1995RQ86400001 ER PT J AU BOUCAUDCAMOU, E ROPER, CFE AF BOUCAUDCAMOU, E ROPER, CFE TI DIGESTIVE ENZYMES IN PARALARVAL CEPHALOPODS SO BULLETIN OF MARINE SCIENCE LA English DT Article ID SQUID; HEXOSAMINIDASE; PURIFICATION; LOLIGINIDAE; GLAND; TRACT AB Fourteen enzymes involved in digestion (esterases, glycosidases and peptidases) were localized by histochemical methods in planktonic paralarvae belonging to four families of cephalopods: Octopodidae, Bolitaenidae (Octopods), Ommastrephidae and Enoploteuthidae (Oegopsid squids). The high protease activity and very low or histochemically undetectable amylasic activity indicate a carnivorous diet suggesting that the diet of paralarvae resembles that of adults. The digestive gland displays the highest enzyme activities which agrees with the key role of the gland in the digestive processes of cephalopods. In particular, the gland appears to be the main source of the proteolytic enzymes found in the posterior digestive tract. The high acid phosphatase activity, DAP II and acetyl-glycosaminidase activities, typically lysosomal, point to intracellular digestive processes in the gland. The posterior salivary glands are as well developed in squids as in octopods and they display several enzyme activities, most notably a high proteolytic activity. This could indicate that the salivary glands would be more involved in the digestive processes in paralarval squids than in adults where they are mostly poison glands. In all of the specimens studied, the whole digestive system appears to be already developed and able to digest prey. The high level of alkaline phosphatase activity of the skin suggests active exchanges with the external medium. It seems possible therefore that nutrients could be absorbed through the skin and provide a part of the energy necessary to the young cephalopods. C1 SMITHSONIAN MARINE STN LINK PORT,FT PIERCE,FL 34946. NR 64 TC 32 Z9 34 U1 0 U2 2 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD SEP PY 1995 VL 57 IS 2 BP 313 EP 327 PG 15 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA RQ864 UT WOS:A1995RQ86400002 ER PT J AU WARNER, DJ AF WARNER, DJ TI THE CAMPAIGN FOR MEDICAL MICROSCOPY IN ANTEBELLUM AMERICA SO BULLETIN OF THE HISTORY OF MEDICINE LA English DT Article ID 19TH-CENTURY RP WARNER, DJ (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 143 TC 6 Z9 6 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION 2715 NORTH CHARLES ST, BALTIMORE, MD 21218 SN 0007-5140 J9 B HIST MED JI Bull. Hist. Med. PD FAL PY 1995 VL 69 IS 3 BP 367 EP 386 PG 20 WC Health Care Sciences & Services; History & Philosophy Of Science SC Health Care Sciences & Services; History & Philosophy of Science GA RU880 UT WOS:A1995RU88000002 PM 7549408 ER PT J AU MONFORT, SL BROWN, JL WOOD, TC BUSH, M WILLIAMSON, LR WILDT, DE AF MONFORT, SL BROWN, JL WOOD, TC BUSH, M WILLIAMSON, LR WILDT, DE TI EFFECTS OF LONG-TERM CONTINUOUS GNRH ADMINISTRATION ON THE PITUITARY-GONADAL AXIS IN EIDS DEER STAGS (CERVUS-ELDI-THAMIN) SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article ID LHRH AGONIST; TESTOSTERONE SECRETION; TESTICULAR FUNCTION; HORMONE AGONIST; RHESUS-MONKEYS; LUTEINIZING-HORMONE; CONTINUOUS INFUSION; CONSTANT INFUSION; FALLOW DEER; DAMA-DAMA AB Eld's deer stags (Cervus eldi thamin) (in groups of three) were continuously administered gonadotropin-releasing hormone (GnRH) in control, low, medium, or high doses (0, 20.1 +/- 0.7, 83.3 +/- 2.6, and 292.9 +/- 4.9 ng . kg(-1) . d(-1), respectively) via osmotic minipumps for similar to 80 d to investigate the potential for precociously reactivating the pituitary-testicular axis during the nonbreeding season. Secretory patterns of LH, FSH, and testosterone concentrations were qualitatively similar among treatments. However, in the low-dose group, basal LH and FSH concentrations were both increased (p < 0.05) and pituitary responsiveness to a superimposed GnRH challenge was augmented (p < 0.05) after 12 weeks of treatment compared with all other groups. Despite these endocrine changes, continuous low-dose GnRH administration was not effective for precociously inducing testicular activity in this seasonally breeding species. High-dose GnRH administration initially induced a transient increase in LH, FSH, and testosterone secretion and delayed but did not prevent, the seasonal decline in spermatogenesis. After 6-12 weeks of high-dose GnRH administration, however, attenuated pituitary responsiveness appeared to delay the normal seasonal reactivation of the pituitary-gonadal axis. In conclusion, prolonged, continuous low-dose GnRH administration did not effectively translate into a precocious onset of testicular activity; therefore, this specific approach is unlikely to be useful for prolonging the fertile period in this seasonally breeding species. RP MONFORT, SL (reprint author), NATL ZOOL PK,CTR CONSERVAT & RES,1500 REMOUNT RD,FRONT ROYAL,VA 22630, USA. NR 30 TC 0 Z9 0 U1 2 U2 2 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA ON K1A 0R6, CANADA SN 0008-4301 J9 CAN J ZOOL JI Can. J. Zool.-Rev. Can. Zool. PD SEP PY 1995 VL 73 IS 9 BP 1609 EP 1619 DI 10.1139/z95-191 PG 11 WC Zoology SC Zoology GA TF324 UT WOS:A1995TF32400004 ER PT J AU LITTLER, DM LITTLER, DS AF LITTLER, DM LITTLER, DS TI A COLONIAL TUNICATE SMOTHERS CORALS AND CORALLINE ALGAE ON THE GREAT-ASTROLABE-REEF, FIJI SO CORAL REEFS LA English DT Note RP LITTLER, DM (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,WASHINGTON,DC 20560, USA. NR 6 TC 5 Z9 6 U1 0 U2 3 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD SEP PY 1995 VL 14 IS 3 BP 148 EP 149 PG 2 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA RY338 UT WOS:A1995RY33800004 ER PT J AU BEEHLER, BM SENGO, JB FILARDI, C MERG, K AF BEEHLER, BM SENGO, JB FILARDI, C MERG, K TI DOCUMENTING THE LOWLAND RAIN-FOREST AVIFAUNA IN PAPUA-NEW-GUINEA - EFFECTS OF PATCHY DISTRIBUTIONS, SURVEY EFFORT AND METHODOLOGY SO EMU LA English DT Article ID BIRD COMMUNITY AB Between 1979 and 1993 we conducted five ornithological field surveys of varying duration in the Lakekamu Basin, a large tract of alluvial rainforest in southern Papua New Guinea. 184 species were recorded, 143 classified as forest-dwelling, 76 as obligate forest-dwellers, and 16 as obligate nonforest species. The Lakekamu list is comparable in size to one produced for Brown River (Bell 1982) but differs in composition (70 species confined to one or the other list). The Brown River list included more upland species whereas the Lakekamu list more aquatic and nonforest species. A comparison of censuses from three survey sires within the Lakekamu Basin indicate that a number of forest species are patchily distributed on the local scale, and that replication of forest censuses is difficult to achieve at high resolution. Analysis of mist-netting data from the Basin, when weighed against the effort required, indicates that it is not an efficient survey tool for short-term field surveys of Papuan forest birds. In contrast, the importance of audial censusing is stressed. C1 YALE UNIV,SCH FORESTRY & ENVIRONM STUDIES,NEW HAVEN,CT 06511. UNIV FLORIDA,DEPT ZOOL,GAINESVILLE,FL 32611. UNIV PAPUA NEW GUINEA,DEPT BIOL,PORT MORESBY,PAPUA N GUINEA. RP BEEHLER, BM (reprint author), SMITHSONIAN INST,DIV BIRDS,CONSERVAT INT & WILDLIFE CONSERVAT SOC,MNH MRC 116,WASHINGTON,DC 20560, USA. NR 24 TC 14 Z9 15 U1 1 U2 6 PU ROYAL AUSTRALASIAN ORNITHOL UN PI MOONEE PONDS PA 21 GLADSTONE ST, MOONEE PONDS VICTORIA 3039, AUSTRALIA SN 0158-4197 J9 EMU JI Emu PD SEP PY 1995 VL 95 BP 149 EP 161 PN 3 PG 13 WC Ornithology SC Zoology GA TE642 UT WOS:A1995TE64200001 ER PT J AU ADLER, GH AUSTIN, CC DUDLEY, R AF ADLER, GH AUSTIN, CC DUDLEY, R TI DISPERSAL AND SPECIATION OF SKINKS AMONG ARCHIPELAGOS IN THE TROPICAL PACIFIC-OCEAN SO EVOLUTIONARY ECOLOGY LA English DT Article DE ARCHIPELAGOS; ENDEMISM; ISLANDS; SKINKS; SPECIATION; SPECIES DIVERSITY; PACIFIC OCEAN ID SCINCIDAE; LACERTILIA; LIZARDS AB We examined the potential effects of geography on the distribution and speciation of skinks on tropical Pacific archipelagos. The entire tropical Pacific skink fauna was divided into continental (found also in continental areas), Pacific (endemic to the study area but found within more than one archipelago) and endemic (found within only one archipelago) species categories. The number and proportion of skinks within each species category were determined for each of the 27 archipelagos in the study area. Nine geographic variables reflecting archipelago size, isolation and elevation were estimated for each archipelago. Principal components analysis was used to reduce the nine variables to three uncorrelated composite variables that were interpreted as representing archipelago size, isolation and elevation. Numbers and proportions of skinks in each category within an archipelago were related to the composite geographic variables using multiple linear regression analysis. Archipelago size and isolation were important predictors of both skink diversity and endemism. Results were then compared to diversity and endemism of birds within the study area. Skinks showed an archipelago-wide level of endemism similar to that of birds. On an archipelago by archipelago basis, however, large differences between birds and skinks were evident. In particular, the New Caledonia skink fauna was much more endemic than that of birds. The bird faunas of Hawaii and the Marquesas were nearly completely endemic, while no endemic skinks occurred in these two archipelagos. These differences presumably reflect the relative dispersal powers of skinks and birds and, consequently, rates of colonization and speciation. Differences may also be due partly to morphological conservatism among isolated skink populations and the occurrence of cryptic species that have not yet been identified as separate species. The discovery of such cryptic species, however, is unlikely to increase the endemic skink fauna of Hawaii and other distant archipelagos to a level commensurate with that of birds. Differences in endemism between skinks and birds may also be due to unknown local ecological interactions. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. UNIV TEXAS,DEPT ZOOL,AUSTIN,TX 78712. RP ADLER, GH (reprint author), UNIV WISCONSIN,DEPT BIOL & MICROBIOL,OSHKOSH,WI 54901, USA. NR 43 TC 29 Z9 31 U1 0 U2 4 PU CHAPMAN HALL LTD PI LONDON PA 2-6 BOUNDARY ROW, LONDON, ENGLAND SE1 8HN SN 0269-7653 J9 EVOL ECOL JI Evol. Ecol. PD SEP PY 1995 VL 9 IS 5 BP 529 EP 541 DI 10.1007/BF01237834 PG 13 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA RU027 UT WOS:A1995RU02700006 ER PT J AU HAYNES, JT MELSON, WG KUNK, MJ AF HAYNES, JT MELSON, WG KUNK, MJ TI COMPOSITION OF BIOTITE PHENOCRYSTS IN ORDOVICIAN TEPHRAS CASTS DOUBT ON THE PROPOSED TRANS-ATLANTIC CORRELATION OF THE MILLBRIG K-BENTONITE (UNITED-STATES) AND THE KINNEKULLE K-BENTONITE (SWEDEN) SO GEOLOGY LA English DT Article ID NORTH-AMERICA AB Biotite phenocryst compositions in three thick, widespread Ordovician K-bentonites, the Deicke and Millbrig from Big Ridge, Alabama, and the Kinnekulle from Mossen, Vastergotland, Sweden, fall into three distinct groups, and so the proposed intercontinental correlation of the Millbrig and the Kinnekulle is suspect. Because the biotites are nearly pristine compositionally, electron microprobe analyses provide a precise geochemical fingerprint of each bed. Millbrig and Kinnekulle biotites contain more FeO* and MnO and less MgO and TiO2 than do Deicke biotites, Millbrig biotites contain more MgO and less TiO2 than Kinnekulle biotites, and Kinnekulle biotites contain appreciably more Al2O3 than either Deicke or Millbrig biotites. Each of these tephras was unmistakably the product of a gigantic explosive volcanic eruption, but the differences in phenocryst chemistry point to derivation from three compositionally different magma batches. C1 US GEOL SURVEY,NATL CTR,RESTON,VA 22092. RP HAYNES, JT (reprint author), NATL MUSEUM NAT HIST,MRC 119,SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560, USA. NR 17 TC 33 Z9 38 U1 0 U2 3 PU GEOLOGICAL SOC AMERICA PI BOULDER PA PO BOX 9140 3300 PENROSE PLACE, BOULDER, CO 80301 SN 0091-7613 J9 GEOLOGY JI Geology PD SEP PY 1995 VL 23 IS 9 BP 847 EP 850 DI 10.1130/0091-7613(1995)023<0847:COBPIO>2.3.CO;2 PG 4 WC Geology SC Geology GA RT701 UT WOS:A1995RT70100020 ER PT J AU SMITH, RW AF SMITH, RW TI THE MISSILE AND SPACE RACE - LEVINE,AJ SO ISIS LA English DT Book Review C1 JOHNS HOPKINS UNIV,DEPT HIST SCI MED & TECHNOL,BALTIMORE,MD 21218. RP SMITH, RW (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0021-1753 J9 ISIS JI Isis PD SEP PY 1995 VL 86 IS 3 BP 525 EP 526 DI 10.1086/357312 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA RZ738 UT WOS:A1995RZ73800090 ER PT J AU SMITH, RW AF SMITH, RW TI SUDDENLY, TOMORROW CAME - A HISTORY OF THE JOHNSON-SPACE-CENTER - DETHOLFF,HC SO ISIS LA English DT Book Review C1 JOHNS HOPKINS UNIV,DEPT HIST SCI MED & TECHNOL,BALTIMORE,MD 21218. RP SMITH, RW (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0021-1753 J9 ISIS JI Isis PD SEP PY 1995 VL 86 IS 3 BP 525 EP 526 DI 10.1086/357312 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA RZ738 UT WOS:A1995RZ73800089 ER PT J AU CANOUTS, V BISHOP, R AF CANOUTS, V BISHOP, R TI A HOPI TRADITION - YELLOW FIRING CERAMICS SO JOM-JOURNAL OF THE MINERALS METALS & MATERIALS SOCIETY LA English DT Article AB The famed Hopi yellow-ware vessels of the American southwest were not the product of any single technological variable, firing technique, clay, or temper. Instead, all of these factors worked together in a technological system affected by the desires, knowledge, and effectualness of the people producing the pottery. C1 SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560. RP CANOUTS, V (reprint author), NATL PK SERV,DIV ARCHAEOL ASSISTANCE,POB 37127,WASHINGTON,DC 20013, USA. NR 11 TC 0 Z9 0 U1 0 U2 1 PU MINERALS METALS MATERIALS SOC PI WARRENDALE PA 420 COMMONWEALTH DR, WARRENDALE, PA 15086 SN 1047-4838 J9 JOM-J MIN MET MAT S JI JOM-J. Miner. Met. Mater. Soc. PD SEP PY 1995 VL 47 IS 9 BP 58 EP 59 PG 2 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing SC Materials Science; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing GA RT347 UT WOS:A1995RT34700015 ER PT J AU HERKEN, G AF HERKEN, G TI ELEMENTS OF CONTROVERSY - THE ATOMIC-ENERGY COMMISSION AND RADIATION SAFETY IN NUCLEAR-WEAPONS TESTING, 1947-1974 - HACKER,BC SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review RP HERKEN, G (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGAN AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47401 SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD SEP PY 1995 VL 82 IS 2 BP 820 EP 821 DI 10.2307/2082372 PG 2 WC History SC History GA RV129 UT WOS:A1995RV12900216 ER PT J AU GREENBERG, R AF GREENBERG, R TI INSECTIVOROUS MIGRATORY BIRDS IN TROPICAL ECOSYSTEMS - THE BREEDING CURRENCY HYPOTHESIS SO JOURNAL OF AVIAN BIOLOGY LA English DT Note ID COEXISTENCE; MIGRANTS; PATTERNS; WARBLERS; FOREST; FOOD AB In many tropical habitats, the number of birds can more than double,vith the arrival of migratory birds in the autumn. This influx often occurs at a time when the total biomass of potential food resources is at an annual low. Previous food-related hypotheses have usually focused on migratory species that consume fruit or other plant products, and are more difficult to extend to insectivorous birds, which make up the bulk of tropical migrants. I hypothesize that inter-habitat and inter-seasonal variation in the size distribution of arthropods may underlie the use of habitats by migratory birds. Most habitats have a few taxa of large arthropods that serve as ''breeding'' currency. The abundance of these arthropods may not be coupled with the abundance of small arthropods during the non-breeding season. Where small arthropods are abundant during the non-breeding season and large arthropods rare during the breeding season, the surplus non-breeding food is available to the large number of small insectivorous birds that comprise most of the migratory species. RP GREENBERG, R (reprint author), NATL ZOOL PK,SMITHSONIAN MIGRATORY BIRD CTR,WASHINGTON,DC 20008, USA. NR 43 TC 36 Z9 37 U1 2 U2 10 PU MUNKSGAARD INT PUBL LTD PI COPENHAGEN PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK SN 0908-8857 J9 J AVIAN BIOL JI J. Avian Biol. PD SEP PY 1995 VL 26 IS 3 BP 260 EP 264 DI 10.2307/3677328 PG 5 WC Ornithology SC Zoology GA TE510 UT WOS:A1995TE51000013 ER PT J AU KILLION, TW AF KILLION, TW TI THE ARCHAEOLOGY OF GARDEN AND FIELD - MILLER,NF, GLEASON,KL SO JOURNAL OF FIELD ARCHAEOLOGY LA English DT Book Review RP KILLION, TW (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT ANTHROPOL,REPATRIAT OFF,WASHINGTON,DC 20560, USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU JOURNAL FIELD ARCHAEOLOGY PI BOSTON PA BOSTON UNIV 675 COMMUNWEALTH AVE, BOSTON, MA 02215 SN 0093-4690 J9 J FIELD ARCHAEOL JI J. Field Archaeol. PD FAL PY 1995 VL 22 IS 3 BP 359 EP 361 DI 10.2307/530182 PG 3 WC Archaeology SC Archaeology GA RR009 UT WOS:A1995RR00900007 ER PT J AU UBELAKER, DH HUNT, DR AF UBELAKER, DH HUNT, DR TI THE INFLUENCE OF BASS,WILLIAM,M.-III ON THE DEVELOPMENT OF AMERICAN FORENSIC ANTHROPOLOGY SO JOURNAL OF FORENSIC SCIENCES LA English DT Article DE PHYSICAL ANTHROPOLOGY; FORENSIC ANTHROPOLOGY; WILLIAM M BASS; HISTORY AB Through his teaching, research and casework over the last 33 years, William M. Bass has become a central figure in the development of the American forensic anthropology. His influence can be measured through the quantity and activity of his students in the field, the number and breadth of his publications relating to thr:field, his growing casework, his activity and important role in the development of the Physical Anthropology section of the American Academy of Forensic Sciences, and his continual willingness to lecture to interested groups. Like many of his contemporaries in physical anthropology, Bass gradually shifted his academic interests toward forensic anthropology throughout his career. This shift is reflected in all areas of his academic life. His contributions have raised professionalism acid acceptance of forensic anthropology as an integrated aspect of both forensic science and anthropology. Bass's unique style and breadth of his contributions can be traced to his education (University of Virginia, Kentucky, and Pennsylvania) and his mentors (Goon, Krogman, Stewart, Eisley and Roberts). RP UBELAKER, DH (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT ANTHROPOL,MRC 112,WASHINGTON,DC 20560, USA. NR 17 TC 0 Z9 0 U1 1 U2 6 PU AMER SOC TESTING MATERIALS PI W CONSHOHOCKEN PA 100 BARR HARBOR DR, W CONSHOHOCKEN, PA 19428-2959 SN 0022-1198 J9 J FORENSIC SCI JI J. Forensic Sci. PD SEP PY 1995 VL 40 IS 5 BP 729 EP 734 PG 6 WC Medicine, Legal SC Legal Medicine GA RX718 UT WOS:A1995RX71800008 ER PT J AU OWSLEY, DW AF OWSLEY, DW TI TECHNIQUES FOR LOCATING BURIALS, WITH EMPHASIS ON THE PROBE SO JOURNAL OF FORENSIC SCIENCES LA English DT Article DE PHYSICAL ANTHROPOLOGY; FORENSIC ARCHAEOLOGY; BURIED BODIES; FIELD TECHNIQUES ID GRAVES AB The for buried remains frequently includes visual assessment of surface features, trained dogs, and sophisticated geophysical remote sensing techniques. Nonintrusive, electronic survey equipment, such as the proton magnetometer, ground penetrating radar, and electrical resistivity, have yielded good results. However, under certain field conditions a simple, less expensive, relatively noninvasive tool-the probe-is effective. The probe, when used by an experienced investigator, provides a variety of information in a short amount of time, facilitates excavation, and minimizes damage to a burial. This paper offers examples of the application of a probe in forensic cases in urban and rural settings and in the detection of historic burials. Examples include the location of four individuals killed during the raid on the Branch Davidian Compound in Mount Carmel, Texas, and the search for burials in cemeteries that had been desecrated. RP OWSLEY, DW (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT ANTHROPOL,MRC 112,WASHINGTON,DC 20560, USA. NR 15 TC 34 Z9 36 U1 2 U2 19 PU AMER SOC TESTING MATERIALS PI W CONSHOHOCKEN PA 100 BARR HARBOR DR, W CONSHOHOCKEN, PA 19428-2959 SN 0022-1198 J9 J FORENSIC SCI JI J. Forensic Sci. PD SEP PY 1995 VL 40 IS 5 BP 735 EP 740 PG 6 WC Medicine, Legal SC Legal Medicine GA RX718 UT WOS:A1995RX71800009 ER PT J AU JANTZ, RL HUNT, DR MEADOWS, L AF JANTZ, RL HUNT, DR MEADOWS, L TI THE MEASURE AND MISMEASURE OF THE TIBIA - IMPLICATIONS FOR STATURE ESTIMATION SO JOURNAL OF FORENSIC SCIENCES LA English DT Article DE PHYSICAL ANTHROPOLOGY; TIBIA; STATURE ESTIMATION; MEASUREMENT TECHNIQUE; TROTTER AB Trotter and Gleser's stature estimation formulae, based on skeletons. of the Terry collection and on WWII casualties, have been widely used in forensic work. Our work with the Terry and WWII data yielded tibia lengths too short compared to other data sets. Using Trotter's original measurements, we discovered that she consistently mismeasured the tibia. Contrary to standard practice and her own definitions, she omitted the malleolus from the measurement. Trotter's measurements of the tibia are 10 to 12 mm shorter than they should have been, resulting in stature estimations averaging 2.5 to 3.0 cm too great when the formulae are used with properly measured tibia. We also examined tibia lengths of Korean War casualties, which were measured by technicians rather than by Trotter. Korean tibia measurements are also too short, but by a smaller amount than Terry and WWII. Since the Korean tibia are unavailable for restudy, it is unclear how they were measured. Estimation of stature from Trotter and Gleser's tibia formulae is to be avoided if possible. If necessary, the 1952 formulae could be used with tibia measured in the same manner that Trotter measured, excluding the malleolus. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT ANTHROPOL,WASHINGTON,DC 20560. RP JANTZ, RL (reprint author), UNIV TENNESSEE,DEPT ANTHROPOL,KNOXVILLE,TN 37996, USA. NR 13 TC 32 Z9 33 U1 1 U2 14 PU AMER SOC TESTING MATERIALS PI W CONSHOHOCKEN PA 100 BARR HARBOR DR, W CONSHOHOCKEN, PA 19428-2959 SN 0022-1198 J9 J FORENSIC SCI JI J. Forensic Sci. PD SEP PY 1995 VL 40 IS 5 BP 758 EP 761 PG 4 WC Medicine, Legal SC Legal Medicine GA RX718 UT WOS:A1995RX71800013 PM 7595318 ER PT J AU WELDON, PJ LETO, TL AF WELDON, PJ LETO, TL TI A COMPARATIVE-ANALYSIS OF PROTEINS IN THE SCENT GLAND SECRETIONS OF SNAKES SO JOURNAL OF HERPETOLOGY LA English DT Note C1 NIAID,HOST DEF LAB,BETHESDA,MD 20892. TEXAS A&M UNIV,DEPT BIOL,COLLEGE STN,TX 77843. SMITHSONIAN INST,CTR CONSERVAT & RES,FRONT ROYAL,VA 22630. NR 13 TC 4 Z9 5 U1 1 U2 2 PU SOC STUD AMPHIBIANS REPTILES PI OXFORD PA DEPT OF ZOOLOGY MIAMI UNIV, OXFORD, OH 45056 SN 0022-1511 J9 J HERPETOL JI J. Herpetol. PD SEP PY 1995 VL 29 IS 3 BP 474 EP 476 DI 10.2307/1565005 PG 3 WC Zoology SC Zoology GA TA491 UT WOS:A1995TA49100025 ER PT J AU BEHRENSMEYER, AK POTTS, R PLUMMER, T TAUXE, L OPDYKE, N JORSTAD, T AF BEHRENSMEYER, AK POTTS, R PLUMMER, T TAUXE, L OPDYKE, N JORSTAD, T TI THE PLEISTOCENE LOCALITY OF KANJERA, WESTERN KENYA - STRATIGRAPHY, CHRONOLOGY AND PALEOENVIRONMENTS SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE PLEISTOCENE; HOMINID; PALEOENVIRONMENT; KANJERA; EAST AFRICA; KENYA; STRATIGRAPHY; MAGNETOSTRATIGRAPHY ID PALEOMAGNETIC DATA; MATUYAMA AB Kanjera is well known as the source of controversial hominid fossils collected by L. S. B. Leakey in the 1930s. Since 1935, the context of fossils and artifacts from the locality has been in doubt, due to a claim that sediment slumping had commingled materials from stratigraphic units of different ages. A careful re-examination of the geology demonstrates that the Kanjera deposits consist of approximately 37 m of volcaniclastic, fluvial, mudflat and lacustrine sediments that we assign to three major units: the Kanjera Formation, the Apoko Formation, and the Black Cotton Soil, Outcrops cover approximately 2 km(2) in two adjacent areas, the Northern and Southern Exposures. Fossils and artifacts are found in primary contexts through much of the stratigraphic column; and extensive trenching failed to reveal any sediment slumping that would have disturbed these contexts. Faulting, rapid lateral facies changes, and an erosional unconformity between the Kanjera and Apoko Formations result in complex geological relationships. Magnetostratigraphic and faunal determinations indicate that the Kanjera Formation is approximately 1.5-0.5 Ma, the Apoko Formation younger than 0.5 Ma, and the Black Cotton Soil latest Pleistocene to Holocene. The hominid sample is derived from the Black Cotton Soil except for Leakey's Hominid 3, which probably was an intrusive burial into Kanjera Formation Bed KN-2. The Theropithecus oswaldi type specimen originated from KN-2a and is dated between 1.1 and at most 1.76 Ma. The Kanjera Formation provides the youngest known records of Metridiochoerus andrewsi and Deinotherium bozasi at about 1.0 Ma. (C) 1995 Academic Press Limited C1 SMITHSONIAN INST,DEPT ANTHROPOL,MRC,NHB 112,WASHINGTON,DC 20560. UNIV CALIF LOS ANGELES,DEPT ANTHROPOL,LOS ANGELES,CA 90024. UNIV CALIF SAN DIEGO,SCRIPPS INST OCEANOG A020,LA JOLLA,CA 92093. UNIV FLORIDA,DEPT GEOL,GAINESVILLE,FL 32611. RP BEHRENSMEYER, AK (reprint author), SMITHSONIAN INST,DEPT PALEOBIOL,MRC,NHB 121,WASHINGTON,DC 20560, USA. NR 54 TC 30 Z9 31 U1 2 U2 6 PU ACADEMIC PRESS (LONDON) LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD SEP PY 1995 VL 29 IS 3 BP 247 EP 274 DI 10.1006/jhev.1995.1059 PG 28 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA RT616 UT WOS:A1995RT61600003 ER PT J AU MCCARTHY, MC GOTTLIEB, CA THADDEUS, P AF MCCARTHY, MC GOTTLIEB, CA THADDEUS, P TI ROTATIONAL SPECTRUM AND HYPERFINE-STRUCTURE OF (CCH)-C-13 AND (CCH)-C-13 SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Note ID MILLIMETER WAVE SPECTRUM; COUPLING-CONSTANTS; VIBRONIC STRUCTURE; C2H SPECTRUM; CCH C1 HARVARD UNIV,DIV APPL SCI,CAMBRIDGE,MA 02138. RP MCCARTHY, MC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 9 TC 12 Z9 12 U1 0 U2 0 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD SEP PY 1995 VL 173 IS 1 BP 303 EP 307 DI 10.1006/jmsp.1995.1236 PG 5 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA RU652 UT WOS:A1995RU65200026 ER PT J AU KALFATOVIC, MR AF KALFATOVIC, MR TI HOPPER,EDWARD - AN INTIMATE BIOGRAPHY - LEVIN,G SO LIBRARY JOURNAL LA English DT Book Review RP KALFATOVIC, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 1 PY 1995 VL 120 IS 14 BP 171 EP 172 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA RQ788 UT WOS:A1995RQ78800047 ER PT J AU STAHL, J AF STAHL, J TI FOLLOWING BALANCHINE - GARIS,R SO LIBRARY JOURNAL LA English DT Book Review RP STAHL, J (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER ART,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 1 PY 1995 VL 120 IS 14 BP 179 EP 180 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA RQ788 UT WOS:A1995RQ78800072 ER PT J AU RILEY, S AF RILEY, S TI FLASHPOINT - HIGHTOWER,LS SO LIBRARY JOURNAL LA English DT Book Review RP RILEY, S (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 1 PY 1995 VL 120 IS 14 BP 212 EP 212 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA RQ788 UT WOS:A1995RQ78800239 ER PT J AU BROWN, P HILDEBRAND, A GREEN, D PAGE, D JACOBS, C REVELLE, D TAGLIAFERRI, E WACKER, J AF BROWN, P HILDEBRAND, A GREEN, D PAGE, D JACOBS, C REVELLE, D TAGLIAFERRI, E WACKER, J TI THE FALL OF THE ST ROBERT METEORITE - INTERPRETATION OF EYEWITNESS ACCOUNTS, SATELLITE DATA, SHORT-LIVED ISOTOPE ACTIVITY, AND INFRASOUND SO METEORITICS LA English DT Meeting Abstract C1 UNIV WESTERN ONTARIO, DEPT PHYS, LONDON, ON N6A 3K7, CANADA. GEOL SURVEY CANADA, NAT RESOSURCES CANADA, DIV CONTINENTAL GEOSCI, OTTAWA, ON K1A OY3, CANADA. SMITHSONIAN ASTROPHYS OBSERV, CAMBRIDGE, MA 02138 USA. FEDERAT ASTRONOMES AMATEURS QUEBEC, MONTREAL, PQ H2A 1K4, CANADA. SANDIA NATL LABS, ALBUQUERQUE, NM 87185 USA. LOS ALAMOS NATL LAB, LOS ALAMOS, NM 87545 USA. ET SPACE SYST, CAMARILLO, CA 93012 USA. PACIFIC NW LAB, RICHLAND, WA 99352 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORITICS JI Meteoritics PD SEP PY 1995 VL 30 IS 5 BP 492 EP 492 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RR518 UT WOS:A1995RR51800029 ER PT J AU IVANOV, AV MACPHERSON, GJ KONONKOVA, NN STROGANOV, IA AF IVANOV, AV MACPHERSON, GJ KONONKOVA, NN STROGANOV, IA TI TITANIUM-IRON-SULFUR-BEARING COMPOUNDS IN KAIDUN SO METEORITICS LA English DT Meeting Abstract C1 RUSSIAN ACAD SCI,VI VERNADSKII GEOCHEM & ANALYT CHEM INST,MOSCOW 117975,RUSSIA. SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560. NR 5 TC 2 Z9 2 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORITICS JI Meteoritics PD SEP PY 1995 VL 30 IS 5 BP 524 EP 524 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RR518 UT WOS:A1995RR51800095 ER PT J AU MARVIN, UB AF MARVIN, UB TI SIENA, 1794 - HISTORY MOST CONSEQUENTIAL METEORITE FALL SO METEORITICS LA English DT Meeting Abstract C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 0 TC 1 Z9 1 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORITICS JI Meteoritics PD SEP PY 1995 VL 30 IS 5 BP 540 EP 541 PG 2 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RR518 UT WOS:A1995RR51800131 ER PT J AU PETAEV, MI AF PETAEV, MI TI EXSOLVED FERROMAGNESIAN OLIVINE - WHY ONLY IN DIVNOE SO METEORITICS LA English DT Meeting Abstract C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 8 TC 1 Z9 1 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORITICS JI Meteoritics PD SEP PY 1995 VL 30 IS 5 BP 561 EP 561 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RR518 UT WOS:A1995RR51800171 ER PT J AU RUSSELL, SS DAVIS, AM MACPHERSON, GJ AF RUSSELL, SS DAVIS, AM MACPHERSON, GJ TI REFRACTORY INCLUSIONS IN THE CO3-LIKE CHONDRITES MACALPINE-HILLS-88107 AND MACALPINE-HILLS-87300 SO METEORITICS LA English DT Meeting Abstract C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT MINERAL SCI,WASHINGTON,DC 20560. UNIV CHICAGO,ENRICO FERMI INST,CHICAGO,IL 60637. NR 6 TC 2 Z9 2 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORITICS JI Meteoritics PD SEP PY 1995 VL 30 IS 5 BP 569 EP 570 PG 2 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RR518 UT WOS:A1995RR51800190 ER PT J AU WLOTZKA, F THACKER, R FREDRIKSSON, K AF WLOTZKA, F THACKER, R FREDRIKSSON, K TI A MAGNETITE-DOLOMITE-RICH CLAST IN ORGUEIL - DIFFERENTIATION ON THE CI PARENT BODY SO METEORITICS LA English DT Meeting Abstract ID CHONDRITES C1 SMITHSONIAN INST,WASHINGTON,DC 20560. MAX PLANCK INST CHEM,W-6500 MAINZ,GERMANY. NR 2 TC 1 Z9 1 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORITICS JI Meteoritics PD SEP PY 1995 VL 30 IS 5 BP 600 EP 600 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RR518 UT WOS:A1995RR51800251 ER PT J AU WOOD, JA AF WOOD, JA TI CHONDRITE FORMATION - A LONG MANY-STAGE PROCESS, OR FAST AND BRUTISH SO METEORITICS LA English DT Meeting Abstract C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 0 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORITICS JI Meteoritics PD SEP PY 1995 VL 30 IS 5 BP 601 EP 601 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RR518 UT WOS:A1995RR51800253 ER PT J AU PUCHNAREWICZ, EM MASON, KO SIEMIGINOWSKA, A POUNDS, KA AF PUCHNAREWICZ, EM MASON, KO SIEMIGINOWSKA, A POUNDS, KA TI THE HIGH-TEMPERATURE BIG BLUE BUMP IN THE SEYFERT-GALAXY REJ1034+396 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ACCRETION, ACCRETION DISCS; LINE, FORMATION; GALAXIES, ACTIVE; GALAXIES, INDIVIDUAL, RE J1034 + 396; GALAXIES, SEYFERT; X-RAYS, GALAXIES ID ACTIVE GALACTIC NUCLEI; CONTINUUM ENERGY-DISTRIBUTIONS; AGN ACCRETION DISKS; BROAD-LINE REGION; X-RAY-SPECTRA; OBSERVATIONAL CONSTRAINTS; LYMAN EDGES; BLACK-HOLES; QUASARS; ULTRAVIOLET AB X-ray, UV and optical spectra are presented for a rare, EUV-bright Seyfert galaxy, RE J1034 + 396 (z = 0.042). When combined, these data describe a very-high temperature big blue bump (BBB; kT(eff) similar to 100 eV) whose high energy turnover is observed in soft X-rays. The soft X-ray/UV flux ratio is extremely high, L(0.2keV)/L(1200A) similar to 10, compared to AGN in general whose ratio is usually less than 1. The optical/UV continuum betrays no trace of the BBB or the host galaxy. It rises steeply to the red, and is consistent with an underlying far-IR to X-ray power law with an index of similar to 1.3. This may represent the first direct identification of an optical power-law component in a non-blazar AGN. We compare the optical to soft X-ray spectrum of RE J1034 + 396 with three mechanisms for the production of the BBB: an optically thick accretion disc (AD); optically thin emission from a hot plasma; and reprocessing in cool clouds. A thin AD can reproduce the observed spectrum of RE J1034 + 396, but a free-free spectrum predicts too much flux in the UV. The reprocessing of a non-thermal continuum is only possible if there is a steep break between similar to 60 and 1000 Angstrom; a reprocessed free-free spectrum is an alternative. We compare the data with those of the high-redshift quasar E1346 + 266, whose BBB component is similar in shape, but 200 times stronger than that of RE J1034 + 396. A simple, thin AD is not appropriate for E1346 + 266 because of its high luminosity, but, when electron scattering is taken into account, an adequate representation is obtained for a black hole mass M = 2.3 x 10(8) M. with an accretion rate of 2.7 M. yr(-1) (L/L(Edd) similar to 2). Optically thin (T-brem = 7 x 10(6) K) emission and reprocessed free-free are also possible for E1346 + 266. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV LEICESTER, XRAY ASTRON GRP, LEICESTER LE1 7RH, LEICS, ENGLAND. RP PUCHNAREWICZ, EM (reprint author), UCL, MULLARD SPACE SCI LAB, HOLMBURY ST MARY, DORKING RH5 6NT, SURREY, ENGLAND. NR 55 TC 57 Z9 57 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 1995 VL 276 IS 1 BP 20 EP 32 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RR269 UT WOS:A1995RR26900010 ER PT J AU CODELLA, C PALUMBO, GGC PARESCHI, G SCAPPINI, F CASELLI, P ATTOLINI, MR AF CODELLA, C PALUMBO, GGC PARESCHI, G SCAPPINI, F CASELLI, P ATTOLINI, MR TI IRAS-SELECTED GALACTIC STAR-FORMING REGIONS .2. WATER MASER DETECTIONS IN THE EXTENDED SAMPLE SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE MASERS; STARS, FORMATION; ISM, MOLECULES; INFRARED, ISM, CONTINUUM; RADIO LINES, ISM ID ULTRACOMPACT HII-REGIONS; H-II REGIONS; DENSE MOLECULAR CLOUDS; H2O MASERS; DARK CLOUDS; MASSIVE STARS; POINT SOURCES; CORES; EMISSION; AMMONIA AB The results of the analysis of the occurrence of 22.2-GHz H2O maser emission in a sample of 1409 IRAS sources north of declination -30 degrees associated with star-forming regions are presented. Our sample contains all the IRAS sources that satisfy Emerson criteria for selecting molecular cores associated with the earliest evolutionary stages of the star-forming process. In a previous paper, we have reported the results of the observations of about one third of the sample. In the present paper the observations of the remaining IRAS sources are presented: 18 of them are newly detected maser sources. The results show that 20 per cent of all IRAS sources that satisfy the Wood and Churchwell criteria have H2O water masers. This is in agreement with the assumption that these criteria select objects that are connected with the early phases of the evolution of high-mass star-forming regions. Moreover, about one third of the whole sample selected according to Emerson criteria contains IRAS sources that are not associated with massive star-forming processes, but probably with molecular cores in low-mass star-forming regions. C1 UNIV BOLOGNA,DIPARTIMENTO ASTRON,I-40126 BOLOGNA,ITALY. UNIV FERRARA,DIPARTMENTO FIS,I-44100 FERRARA,ITALY. CNR,IST SPETTROSCOPIA MOLEC,I-40129 BOLOGNA,ITALY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 01218. CNR,IST TECNOL & STUDIO RADIAZ EXTRATERR,I-40129 BOLOGNA,ITALY. RP CODELLA, C (reprint author), UNIV FLORENCE,DIPARTIMENTO ASTRON & SCI SPAZIO,LARGO E FERMI 5,I-50125 FLORENCE,ITALY. NR 41 TC 49 Z9 50 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 1995 VL 276 IS 1 BP 57 EP 73 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RR269 UT WOS:A1995RR26900013 ER PT J AU ANUPAMA, GC KEMBHAVI, AK ELVIS, M EDELSON, R AF ANUPAMA, GC KEMBHAVI, AK ELVIS, M EDELSON, R TI THE INTERSTELLAR-MEDIUM IN THE SEYFERT-GALAXY NGC-7172 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE GALAXIES, ACTIVE; GALAXIES, INDIVIDUAL, NGC 7172; GALAXIES, ISM; GALAXIES, PHOTOMETRY; GALAXIES, SEYFERT; GALAXIES, STRUCTURE ID ACTIVE GALAXIES; SURFACE PHOTOMETRY; STELLAR COMPONENTS; NEUTRAL HYDROGEN; RADIO GALAXIES; NUCLEAR; SAMPLE; EMISSION; GAS; AGN AB We present aperture and surface photometry of the Seyfert galaxy NGC 7172, which is a member of the compact group HCG 90, and has a prominent equatorial dust lane. We use the observed colour excess in the dust lane, obtained from broad-band B and V images, to estimate the neutral hydrogen content as M(HI)(tot) = 2.6 x 10(8) M. and log(M(HI)/L(B)) = -1.8. We analyse the flux from NGC 7172 at various wavelengths and discuss the properties of the interstellar medium in the galaxy. Based on the results from surface photometry, and the properties of the interstellar medium, we conclude that the morphology of NGC 7172 is of type S0-Sa. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV IOWA,DEPT PHYS & ASTRON,IOWA CITY,IA 52242. RP ANUPAMA, GC (reprint author), INTERUNIV CTR ASTRON & ASTROPHYS,POST BAG 4,POONA 411007,MAHARASHTRA,INDIA. NR 40 TC 3 Z9 3 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 1995 VL 276 IS 1 BP 125 EP 132 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RR269 UT WOS:A1995RR26900017 ER PT J AU Brownell, RL Ralls, K Perrin, WF AF Brownell, RL Ralls, K Perrin, WF TI Marine mammal biodiversity - Three diverse orders encompass 119 species SO OCEANUS LA English DT Article C1 SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008. RP Brownell, RL (reprint author), NOAA,NMFS,LA JOLLA,CA 92037, USA. NR 4 TC 0 Z9 0 U1 0 U2 2 PU WOODS HOLE OCEANOGRAPHIC INST PI WOODS HOLE PA OCEANUS MAGAZINE, WOODS HOLE, MA 02543 SN 0029-8182 J9 OCEANUS JI Oceanus PD FAL-WIN PY 1995 VL 38 IS 2 BP 30 EP 33 PG 4 WC Oceanography SC Oceanography GA TQ585 UT WOS:A1995TQ58500011 ER PT J AU Hughes, NC Labandeira, CC AF Hughes, NC Labandeira, CC TI The stability of species in taxonomy SO PALEOBIOLOGY LA English DT Article C1 SMITHSONIAN INST,MUSEUM NATL HIST NAT,DEPT PALEOBIOL,WASHINGTON,DC 20560. RP Hughes, NC (reprint author), CINCINNATI MUSEUM NAT HIST,GEIR COLLECT & RES CTR,CINCINNATI,OH 45202, USA. NR 9 TC 15 Z9 15 U1 0 U2 1 PU PALEONTOLOGICAL SOC INC PI ITHACA PA 1259 TRUMANSBURG ROAD, ITHACA, NY 14850 SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD FAL PY 1995 VL 21 IS 4 BP 401 EP 403 PG 3 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA TN385 UT WOS:A1995TN38500001 ER PT J AU SILVA, ES FAUST, MA AF SILVA, ES FAUST, MA TI SMALL-CELLS IN THE LIFE-HISTORY OF DINOFLAGELLATES (DINOPHYCEAE) - A REVIEW SO PHYCOLOGIA LA English DT Article ID NAGASAKIENSE; CYCLE AB Small cells are observed in dense populations of many dinoflagellate species, both in clonal cultures and in natural bloom populations. They range in size from 0.5 to 0,16 of the normal cell volume and have reduced nucleus and cytoplasmic components. Two possible origins are considered for such small cells: unequal cell division or budding-like division, and successive 'depauperating' cell divisions. Small cells, which are reported here for 34 species, can proliferate actively in the late stages of exponential growth, and may become the dominant form in cultures when nutrients are exhausted. When new nutrients are added to the exhausted growth medium, small cells increase in size and structural components, and may give rise to forms of a more typical size, Small cells may also serve as gametes. In the sexual cycle of the species studied here, gametes were morphologically indistinguishable from vegetative small cells. Fusion was isogamous in Gymnodinium splendens Lebour, Gyrodinium instriatum Freudenthal et Lee, Alexandrium lusitanicum Balech and Coolia monotis Meunier, but anisogamy was also observed in Gyrodinium instriatum. The nuclear structure of several stages of the life history was examined, including small cells. The results agree with earlier observations: the dinoflagellate nucleus is polyploid or aneuploid and the chromosomes are polytenic. The existence of small forms may have implications for dinoflagellate taxonomy. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,MUSEUM SUPPORT CTR,SUITLAND,MD 20746. RP SILVA, ES (reprint author), INST NACL SAUDE,MICROBIOL EXPTL LAB,AV PADRE CRUZ,P-1699 LISBON,PORTUGAL. NR 44 TC 48 Z9 51 U1 1 U2 7 PU INT PHYCOLOGICAL SOC PI LAWRENCE PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0031-8884 J9 PHYCOLOGIA JI Phycologia PD SEP PY 1995 VL 34 IS 5 BP 396 EP 408 DI 10.2216/i0031-8884-34-5-396.1 PG 13 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA RX993 UT WOS:A1995RX99300005 ER PT J AU GRIFFIN, JB AF GRIFFIN, JB TI MINER,HORACE,MITCHELL (MAY-26,1912 NOVEMBER-26,1993) SO PROCEEDINGS OF THE AMERICAN PHILOSOPHICAL SOCIETY LA English DT Item About an Individual C1 UNIV MICHIGAN,MUSEUM ANTHROPOL,ANN ARBOR,MI 48109. RP GRIFFIN, JB (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 3 TC 1 Z9 1 U1 0 U2 0 PU AMER PHILOSOPHICAL SOC PI PHILADELPHIA PA 104 SOUTH FIFTH ST, PHILADELPHIA, PA 19106-3387 SN 0003-049X J9 P AM PHILOS SOC JI Proc. Amer. Philos. Soc. PD SEP PY 1995 VL 139 IS 3 BP 288 EP 292 PG 5 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA RX323 UT WOS:A1995RX32300010 ER PT J AU REINHARDT, L AF REINHARDT, L TI HISTORY OF THE UNITED-STATES-BOTANIC-GARDEN, 1816-1991 - SOLIT,KD SO PUBLIC HISTORIAN LA English DT Book Review RP REINHARDT, L (reprint author), SMITHSONIAN INST,NATL PORTRAIT GALLERY,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD FAL PY 1995 VL 17 IS 4 BP 100 EP 102 PG 3 WC History SC History GA TM877 UT WOS:A1995TM87700019 ER PT J AU PACHTER, M AF PACHTER, M TI 'BASEBALL' - A FILM BY BURNS,KEN - BURNS,K, NOVICK,L, PRODUCERS SO PUBLIC HISTORIAN LA English DT Film Review RP PACHTER, M (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD FAL PY 1995 VL 17 IS 4 BP 144 EP 146 PG 3 WC History SC History GA TM877 UT WOS:A1995TM87700039 ER PT J AU KALFATOVIC, MR AF KALFATOVIC, MR TI THE CAMBRIDGE ENCYCLOPEDIA OF RUSSIA AND THE FORMER SOVIET-UNION - BROWN,A, KASER,M, SMITH,GS SO RQ LA English DT Book Review RP KALFATOVIC, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER LIBRARY ASSN PI CHICAGO PA 50 E HURON ST, CHICAGO, IL 60611 SN 0033-7072 J9 RQ JI RQ PD FAL PY 1995 VL 35 IS 1 BP 110 EP 110 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA TD108 UT WOS:A1995TD10800017 ER PT J AU NOYES, RW AF NOYES, RW TI SOLAR AND STELLAR ACTIVITY CYCLES - WILSON,PR SO SCIENCE LA English DT Book Review RP NOYES, RW (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ADVAN SCIENCE PI WASHINGTON PA 1333 H ST NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD SEP 1 PY 1995 VL 269 IS 5228 BP 1290 EP 1291 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RR842 UT WOS:A1995RR84200043 ER PT J AU FORMAN, P AF FORMAN, P TI HALDANE DAEDALUS REVISITED - DRONAMRAJU,KR SO SCIENCE LA English DT Book Review RP FORMAN, P (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ADVAN SCIENCE PI WASHINGTON PA 1333 H ST NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD SEP 1 PY 1995 VL 269 IS 5228 BP 1291 EP 1291 DI 10.1126/science.269.5228.1291 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RR842 UT WOS:A1995RR84200045 PM 17732118 ER PT J AU LOVEJOY, TE AF LOVEJOY, TE TI EXTINCTIONS, REDUX SO SCIENCES-NEW YORK LA English DT Letter RP LOVEJOY, TE (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 E 63RD ST, NEW YORK, NY 10021 SN 0036-861X J9 SCIENCES JI Sci.-New York PD SEP-OCT PY 1995 VL 35 IS 5 BP 6 EP 6 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RZ927 UT WOS:A1995RZ92700005 ER PT J AU ALEXANDER, IC AF ALEXANDER, IC TI MONA-LISA UNMASKED SO SCIENTIFIC AMERICAN LA English DT Letter RP ALEXANDER, IC (reprint author), SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SCI AMERICAN INC PI NEW YORK PA 415 MADISON AVE, NEW YORK, NY 10017 SN 0036-8733 J9 SCI AM JI Sci.Am. PD SEP PY 1995 VL 273 IS 3 BP 10 EP 10 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RP670 UT WOS:A1995RP67000006 ER PT J AU KAN, S KHAZANOV, A KRUPNIK, I KRAUSS, M WIEHN, ER AF KAN, S KHAZANOV, A KRUPNIK, I KRAUSS, M WIEHN, ER TI UNTITLED SO SOCIETY LA English DT Letter C1 UNIV WISCONSIN,MADISON,WI. SMITHSONIAN INST,WASHINGTON,DC 20560. UNIV ALASKA,NAT LANGUAGE CTR,FAIRBANKS,AK 99701. UNIV KONSTANZ,W-7750 CONSTANCE,GERMANY. UNIV PITTSBURGH,PITTSBURGH,PA. RP KAN, S (reprint author), DARTMOUTH COLL,NAT AMER STUDIES PROGRAM,HANOVER,NH 03755, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU TRANSACTION PERIOD CONSORTIUM PI NEW BRUNSWICK PA DEPT 3091 RUTGERS-THE STATE UNIV OF NJ, NEW BRUNSWICK, NJ 08903 SN 0147-2011 J9 SOCIETY JI Society PD SEP-OCT PY 1995 VL 32 IS 6 BP 6 EP 7 PG 2 WC Social Sciences, Interdisciplinary; Sociology SC Social Sciences - Other Topics; Sociology GA RP829 UT WOS:A1995RP82900008 ER PT J AU SCHLEBECKER, JT AF SCHLEBECKER, JT TI 3 FRONTIERS, FAMILY, LAND, AND SOCIETY IN THE AMERICAN-WEST, 1850-1900 - MAY,DL SO WESTERN HISTORICAL QUARTERLY LA English DT Book Review RP SCHLEBECKER, JT (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU WESTERN HISTORY ASSOCIATION PI LOGAN PA UTAH STATE UNIV, UMC 0740, LOGAN, UT 84322 SN 0043-3810 J9 WESTERN HIST QUART JI West. Hist. Q. PD FAL PY 1995 VL 26 IS 3 BP 407 EP 408 DI 10.2307/970695 PG 2 WC History SC History GA RP079 UT WOS:A1995RP07900043 ER PT J AU PETIT, LJ PETIT, DR MARTIN, TE AF PETIT, LJ PETIT, DR MARTIN, TE TI LANDSCAPE-LEVEL MANAGEMENT OF MIGRATORY BIRDS - LOOKING PAST THE TREES TO SEE THE FOREST SO WILDLIFE SOCIETY BULLETIN LA English DT Article DE CONNECTIVITY; CORRIDORS; FOREST MANAGEMENT; LANDSCAPE; NEOTROPICAL MIGRATORY BIRDS; WILDLIFE MANAGEMENT ID AVIAN NEST PREDATION; RESOURCE-MANAGEMENT; DIVERSITY; COMMUNITIES; FRAGMENTATION; BIODIVERSITY; CONSERVATION; ECOLOGY; POPULATIONS; ECOSYSTEMS C1 NATL ZOOL PK,SMITHSONIAN MIGATORY BIRD CTR,WASHINGTON,DC 20008. SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. UNIV ARKANSAS,DEPT BIOL SCI,ARKANSAS COOPERAT FISH & WILDLIFE RES UNIT,FAYETTEVILLE,AR 72701. RI Martin, Thomas/F-6016-2011 OI Martin, Thomas/0000-0002-4028-4867 NR 67 TC 23 Z9 24 U1 0 U2 12 PU WILDLIFE SOC PI BETHESDA PA 5410 GROSVENOR LANE, BETHESDA, MD 20814-2197 SN 0091-7648 J9 WILDLIFE SOC B JI Wildl. Soc. Bull. PD FAL PY 1995 VL 23 IS 3 BP 420 EP 429 PG 10 WC Biodiversity Conservation SC Biodiversity & Conservation GA RR480 UT WOS:A1995RR48000019 ER PT J AU SEUTIN, G APANIUS, V AF SEUTIN, G APANIUS, V TI GRAY FLYCATCHER PREDATION ON A HUMMINGBIRD SO WILSON BULLETIN LA English DT Note C1 INST PARASITOL,ST ANNE BELLEVUE,PQ H9X 3V9,CANADA. RP SEUTIN, G (reprint author), SMITHSONIAN TROP RES INST,APDO 2072,UNIT 0948,BALBOA 34002,PANAMA. NR 15 TC 2 Z9 2 U1 0 U2 0 PU WILSON ORNITHOLOGICAL SOC PI ANN ARBOR PA MUSEUM OF ZOOLOGY UNIV MICHIGAN, ANN ARBOR, MI 48109 SN 0043-5643 J9 WILSON BULL JI Wilson Bull. PD SEP PY 1995 VL 107 IS 3 BP 565 EP 567 PG 3 WC Ornithology SC Zoology GA RU206 UT WOS:A1995RU20600021 ER PT J AU TONG, CYE BLUNDELL, R BUMBLE, B STERN, JA LEDUC, HG AF TONG, CYE BLUNDELL, R BUMBLE, B STERN, JA LEDUC, HG TI QUANTUM LIMITED HETERODYNE-DETECTION IN SUPERCONDUCTING NONLINEAR TRANSMISSION-LINES AT SUBMILLIMETER WAVELENGTHS SO APPLIED PHYSICS LETTERS LA English DT Article ID RECEIVERS AB A non-linear superconducting transmission line has been successfully employed in heterodyne detection of sub-millimeter waves. In our experiments an Nb/Al/AlOx/Nb tunnel junction, measuring 0.15 x 40 mu m, with a critical current density of about 2500 A/cm(2) is used as a distributed mixer element. We have demonstrated that quantum limited sensitivity can be achieved with this type of device. At 460 GHz, a Y-factor of 2.5 has been recorded, corresponding to a double-side-band receiver noise temperature of 80 K, The double-side-band conversion loss is about 1 dB and the mixer noise temperature is estimated to be 18(+/- 10) K. (C) 1995 American Institute of Physics. C1 CALTECH,JET PROP LAB,CTR SPACE MICROELECTR TECHNOL,PASADENA,CA 91109. RP TONG, CYE (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 14 TC 28 Z9 28 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD AUG 28 PY 1995 VL 67 IS 9 BP 1304 EP 1306 DI 10.1063/1.114405 PG 3 WC Physics, Applied SC Physics GA RR042 UT WOS:A1995RR04200043 ER PT J AU LEBACH, DE COREY, BE SHAPIRO, II RATNER, MI WEBBER, JC ROGERS, AEE DAVIS, JL HERRING, TA AF LEBACH, DE COREY, BE SHAPIRO, II RATNER, MI WEBBER, JC ROGERS, AEE DAVIS, JL HERRING, TA TI MEASUREMENT OF THE SOLAR GRAVITATIONAL DEFLECTION OF RADIO-WAVES USING VERY-LONG-BASE-LINE INTERFEROMETRY SO PHYSICAL REVIEW LETTERS LA English DT Article ID MILLIARCSECOND STRUCTURE; GEODESY; SYSTEM; VLBI AB We made very-long-baseline-interferometry observations of the extragalactic radio sources 3C273B and 3C279 to measure the gravitational deflection of radio waves by the Sun. Cross-correlation of data recorded at antennas in California and Massachusetts at 2, 8, and 23 GHz during a ten-day period surrounding the October 1987 solar occultation of 3C279 yielded plasma-corrected group delays, from which we obtained gamma = 0.9996 +/- 0.0017 (estimated standard error), corresponding to a gravitational deflection 0.9998 +/- 0.0008 times that predicted by general relativity. C1 NE RADIO OBSERV CORP,HAYSTACK OBSERV,WESTFORD,MA 01886. MIT,DEPT EARTH ATMOSPHER & PLANETARY SCI,CAMBRIDGE,MA 02139. RP LEBACH, DE (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 27 TC 105 Z9 108 U1 0 U2 3 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD AUG 21 PY 1995 VL 75 IS 8 BP 1439 EP 1442 DI 10.1103/PhysRevLett.75.1439 PG 4 WC Physics, Multidisciplinary SC Physics GA RP993 UT WOS:A1995RP99300003 ER PT J AU STOTT, AW EVERSHED, RP TUROSS, N AF STOTT, AW EVERSHED, RP TUROSS, N TI DELTA-C-B MEASUREMENTS OF CHOLESTEROL FROM MODERN AND ANCIENT BONES - AN ADDITIONAL SOURCE OF PALAEODIETARY INFORMATION SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 SMITHSONIAN INST,CONSERVAT & ANALYT LAB,MUSEUM SUPPORT CTR,WASHINGTON,DC 20560. UNIV BRISTOL,SCH CHEM,BRISTOL BS8 1TS,AVON,ENGLAND. RI STOTT, ANDREW /I-7920-2012 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA PO BOX 57136, WASHINGTON, DC 20037-0136 SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 20 PY 1995 VL 210 BP A0099 EP GEOC PN 1 PG 0 WC Chemistry, Multidisciplinary SC Chemistry GA RP256 UT WOS:A1995RP25601943 ER PT J AU MOULD, J HUCHRA, JP BRESOLIN, F FERRARESE, L FORD, HC FREEDMAN, WL GRAHAM, J HARDING, P HILL, R HOESSEL, JG HUGHES, SM ILLINGWORTH, GD KELSON, D KENNICUTT, RC MADORE, BF PHELPS, R STETSON, PB TURNER, A AF MOULD, J HUCHRA, JP BRESOLIN, F FERRARESE, L FORD, HC FREEDMAN, WL GRAHAM, J HARDING, P HILL, R HOESSEL, JG HUGHES, SM ILLINGWORTH, GD KELSON, D KENNICUTT, RC MADORE, BF PHELPS, R STETSON, PB TURNER, A TI LIMITS ON THE HUBBLE CONSTANT FROM THE HST DISTANCE OF M100 SO ASTROPHYSICAL JOURNAL LA English DT Article DE DISTANCE SCALE; GALAXIES, CLUSTERS, INDIVIDUAL (VIRGO); GALAXIES, DISTANCES AND REDSHIFTS; GALAXIES, INDIVIDUAL (M100); SUPERNOVAE, GENERAL ID VELOCITY-WIDTH RELATION; TULLY-FISHER RELATION; VIRGO CLUSTER; LOCAL SUPERCLUSTER; BACKGROUND-RADIATION; GALAXIES; SCALE; MOTION; FIELD; ANISOTROPY AB Because M100 is in the Virgo cluster, our recent measurement of its distance has an impact on the calibration of all of the extragalactic secondary distance indicators which reach beyond Virgo and define the expansion rate. We examine the consequences of a 17 Mpc M100 distance, questioning its consistency with supernova and other distances. The distance of M100 provides two separate constraints on the Hubble constant. First, it verifies the emissivity calculations for Type II supernovae. These models, fitted to SN 1987A, have recently been used to measure host galaxy distances beyond 10(4) km s-l recession velocity. Second, it constrains the distance of the Virgo cluster, which in spite of its apparent complex structure, provides an effective calibration for a set of reliable and well-used secondary distance indicators. Reviewing the Type II supernova distances for three galaxies with Cepheid distances, we find consistency, which supports the recent SN result H-0 = 73 +/- 11 km s(-1) Mpc(-1). This support is independent of where M100 lies in the Virgo cluster. Reviewing the Hubble recession velocity (cosmological redshift) of the Virgo cluster, we find H-0 = 81 +/- 11 km s(-1) Mpc(-1), plus an additional uncertainty arising from the extended nature of the Virgo cluster. Employing the Virgo cluster as calibrator, we obtain measurements of the Hubble constant from extant surface brightness fluctuation measurements, elliptical galaxy velocity dispersion measurements, the Tully-Fisher relation, and the Type Ia supernova standard candle. These yield H-0 = 84 +/- 16, 76 +/- 10, 82 +/- 11, and 71 +/- 10 km s(-1) Mpc(-1), respectively. All of these are consistent, but they are all subject to the additional uncertainty from Virgo's line-of-sight depth. We explore a number of simple models of the structure of the Virgo cluster; these support the recent conclusion of Freedman and coworkers that the appropriate uncertainty to attach to the Hubble constant from the Cepheid distance to Virgo is 20%. A value of H-0 = 80 +/- 17 km s(-1) Mpc(-1) is consistent with all the data discussed herein. Confidence limits with 95% significance can be assigned to the interval 50 < H-0 < 100 km s(-1) Mpc(-1). Further work in this program should be expected to identify the systematic differences between the distance indicators investigated here and constrain the Hubble constant to 10% accuracy. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. JOHNS HOPKINS UNIV,BALTIMORE,MD 21218. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. CARNEGIE INST WASHINGTON,PASADENA,CA 91101. DEPT TERR MAGNETISM,WASHINGTON,DC 20015. UNIV WISCONSIN,MADISON,WI 53706. ROYAL GREENWICH OBSERV,CAMBRIDGE CB3 0HA,ENGLAND. UNIV CALIF SANTA CRUZ,LICK OBSERV,SANTA CRUZ,CA 95064. CALTECH,CTR INFRARED PROC & ANAL,PASADENA,CA 91125. NATL RES COUNCIL CANADA,DOMINION ASTROPHYS OBSERV,HERZBERG INST ASTROPHYS,VICTORIA,BC V8X 4M6,CANADA. RP MOULD, J (reprint author), AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,INST ADV STUDIES,WESTON,ACT 2611,AUSTRALIA. NR 63 TC 58 Z9 58 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 1995 VL 449 IS 2 BP 413 EP 421 DI 10.1086/176066 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RP424 UT WOS:A1995RP42400003 ER PT J AU HENRY, JP GIOIA, IM HUCHRA, JP BURG, R MCLEAN, B MACGILLIVRAY, H CRUDDACE, RG AF HENRY, JP GIOIA, IM HUCHRA, JP BURG, R MCLEAN, B MACGILLIVRAY, H CRUDDACE, RG TI GROUPS OF GALAXIES IN THE ROSAT NORTH ECLIPTIC POLE SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, THEORY; GALAXIES, STATISTICS; SURVEYS; X-RAYS, GALAXIES ID X-RAY-EMISSION; DARK MATTER; VELOCITY DISPERSION; REDSHIFT SURVEY; CFA SURVEY; CLUSTERS; LUMINOSITY; CATALOG; FIELD AB We present the first measurement of the ensemble properties of X-ray-selected groups of galaxies. Their X-ray luminosity and temperature functions are a smooth extrapolation from rich clusters of galaxies. The X-ray-selected groups have a spiral fraction which is about a factor of 2 smaller than optically selected groups, possibly because the X-ray selection produces a more dynamically evolved sample. The binding masses of these groups and their contribution to the density of the universe is typical of those found from analyses of optically selected samples, but our estimates were derived from completely different selection criteria and mass measurements. C1 CNR,IST RADIOASTRON,I-00185 ROME,ITALY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. MAX PLANCK INST EXTRATERR PHYS,D-85740 GARCHING,GERMANY. ROYAL OBSERV,EDINBURGH EH9 3HJ,MIDLOTHIAN,SCOTLAND. USN,RES LAB,WASHINGTON,DC 20375. RP HENRY, JP (reprint author), INST ASTRON,2680 WOODLAWN DR,HONOLULU,HI 96822, USA. RI Gioia, Isabella/B-6982-2012 OI Gioia, Isabella/0000-0003-3127-498X NR 31 TC 39 Z9 39 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 1995 VL 449 IS 2 BP 422 EP 430 DI 10.1086/176067 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RP424 UT WOS:A1995RP42400004 ER PT J AU SEWARD, FD DAME, TM FESEN, RA ASCHENBACH, B AF SEWARD, FD DAME, TM FESEN, RA ASCHENBACH, B TI A ROSAT-DETECTED, NEW GALACTIC SUPERNOVA REMNANT IN SAGITTARIUS, G13.3-1.3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (G13.3-1.3); SUPERNOVA REMNANTS; X-RAYS, ISM ID EMISSION-LINE PROPERTIES; OPEN CLUSTER; MILKY-WAY; STARS; PULSARS; PLANE; CO AB Faint and diffuse soft X-ray emission, coincident with [S II] strong optical filaments, probably marks a previously unrecognized supernova remnant (SNR) in Sagittarius (l = 13.3, b = -1.3). ROSAT PSPC data show soft X-rays from an area 40' x 70' with a flux of 1.3 x 10(-11) erg cm(-2) s(-1) between 0.1-2.4 keV. Optical interference-filter images taken of the region reveal a 20' long complex of relatively bright filaments located along the south central boundary of the X-ray region which may be associated with a ridge of faint 11 cm continuum emission. Optical spectra of these filaments show strong [S II] lambda lambda 6716, 6731 emission ([S II]/H alpha = 0.85) and [O I] lambda lambda 6300, 6364 characteristic of shocked interstellar gas found in SNRs. Both X-rays and optical emissions along the source's NE extent show strong absorption by the dust regions Lynds 332, 336, and 342, indicating a location behind these nebulae. CO emission from this region has been mapped and a kinematic distance derived for absorbing material. The remnant is shown to lie between two absorbing regions located at distances of 2 and 4 kpc. C1 DARTMOUTH COLL,DEPT PHYS & ASTRON,WILDER LAB 6127,HANOVER,NH 03755. MAX PLANCK INST EXTRATERR PHYS,D-85740 GARCHING,GERMANY. RP SEWARD, FD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 33 TC 14 Z9 14 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 1995 VL 449 IS 2 BP 681 EP 687 DI 10.1086/176089 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RP424 UT WOS:A1995RP42400026 ER PT J AU MAZEH, T ZUCKER, S GOLDBERG, D LATHAM, DW STEFANIK, RP CARNEY, BW AF MAZEH, T ZUCKER, S GOLDBERG, D LATHAM, DW STEFANIK, RP CARNEY, BW TI STUDY OF SPECTROSCOPIC BINARIES WITH TODCOR .2. THE HIGHLY ECCENTRIC BINARY HD-2909 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BINARIES, SPECTROSCOPIC; STARS, INDIVIDUAL (HD 2909); STARS, ROTATION ID PROPER-MOTION STARS; TIDAL EVOLUTION; MASS-RATIO; PHOTOMETRY; SPECTRA; SYSTEMS AB TODCOR is a new two-dimensional correlation technique for analyzing observed spectra of double-lined spectroscopic binaries in order to extract the radial velocities of both components. In this paper we apply TODCOR for the first time to a real system-the highly eccentric binary HD 2909. TODCOR has derived successfully the velocities of the two components, even at phases when the velocity difference between the primary and the secondary was very small. We present an orbital solution which shows that HD 2909 is the second most eccentric spectroscopic binary known, with an eccentricity of 0.949 +/- 0.002. We discuss the tidal history of HD 2909 and show that neither the semimajor axis and the eccentricity of the orbit nor the stellar rotation have been changed by tidal interaction throughout the system lifetime. C1 TEL AVIV UNIV, RAYMOND & BEVERLY SACKLER FAC EXACT SCI, SCH PHYS & ASTRON, IL-69978 TEL AVIV, ISRAEL. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV N CAROLINA, DEPT PHYS & ASTRON, CHAPEL HILL, NC 27599 USA. RP MAZEH, T (reprint author), SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, ASTROPHYS LAB, WASHINGTON, DC 20560 USA. NR 36 TC 15 Z9 15 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 1995 VL 449 IS 2 BP 909 EP 915 DI 10.1086/176109 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RP424 UT WOS:A1995RP42400046 ER PT J AU JOY, M PRESTWICH, AH BURTON, M GUIMOND, S AF JOY, M PRESTWICH, AH BURTON, M GUIMOND, S TI EXTENDED INFRARED-EMISSION IN THE GALAXY CLUSTER 1E-1111.9-3754 - NO EVIDENCE FOR A LOW-MASS ACCRETION POPULATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; INFRARED, GALAXIES ID COOLING FLOWS; PHOTOMETRIC SYSTEM AB Optical observations of an extended red halo surrounding the galaxy 1E 1111.9-3754 sparked considerable interest as potentially the first detection of low-mass star formation in an X-ray cooling flow. To test this possibility, we obtained near-infrared surface photometry of this galaxy at J (1.25 mu m) and K (2.15 mu m) and compare this data with models of a low-mass stellar accretion population. Our surface brightness measurements are consistent with a normal r(1/4) elliptical galaxy profile and show no evidence of an extended infrared halo, which argues against the low-mass stellar accretion hypothesis. C1 SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. UNIV NEW S WALES,SCH PHYS,KENSINGTON,NSW 2033,AUSTRALIA. MONTANA STATE UNIV,DEPT PHYS,BOZEMAN,MT 59717. RP JOY, M (reprint author), NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,SPACE SCI LAB,ES84,HUNTSVILLE,AL 35812, USA. NR 11 TC 2 Z9 2 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 1995 VL 449 IS 2 BP L113 EP L115 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RP425 UT WOS:A1995RP42500004 ER PT J AU MACOMB, DJ AKERLOF, CW ALLER, HD ALLER, MF BERTSCH, DL BRUHWEILER, F BUCKLEY, JH CARTERLEWIS, DA CAWLEY, MF CHENG, KP DERMER, C FEGAN, DJ GAIDOS, JA GEAR, WK HALL, CR HARTMAN, RC HILLAS, AM KAFATOS, M KERRICK, AD KNIFFEN, DA KONDO, Y KUBO, H LAMB, RC MAKINO, F MAKISHIMA, K MARSCHER, A MCENERY, J MCHARDY, IM MEYER, DI MOORE, EM RAMOS, E ROBSON, EI ROSE, HJ SCHUBNELL, MS SEMBROSKI, G STEVENS, JA TAKAHASHI, T TASHIRO, M WEEKES, TC WILSON, C ZWEERINK, J AF MACOMB, DJ AKERLOF, CW ALLER, HD ALLER, MF BERTSCH, DL BRUHWEILER, F BUCKLEY, JH CARTERLEWIS, DA CAWLEY, MF CHENG, KP DERMER, C FEGAN, DJ GAIDOS, JA GEAR, WK HALL, CR HARTMAN, RC HILLAS, AM KAFATOS, M KERRICK, AD KNIFFEN, DA KONDO, Y KUBO, H LAMB, RC MAKINO, F MAKISHIMA, K MARSCHER, A MCENERY, J MCHARDY, IM MEYER, DI MOORE, EM RAMOS, E ROBSON, EI ROSE, HJ SCHUBNELL, MS SEMBROSKI, G STEVENS, JA TAKAHASHI, T TASHIRO, M WEEKES, TC WILSON, C ZWEERINK, J TI MULTIWAVELENGTH OBSERVATIONS OF MARKARIAN-421 DURING A TEV X-RAY FLARE SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL LACERTAE OBJECTS, GENERAL; BL LACERTAE OBJECTS, INDIVIDUAL (MARKARIAN 421) ID SIMULTANEOUS MULTIFREQUENCY OBSERVATIONS; LACERTAE OBJECT MARKARIAN-421; EMISSION AB A TeV flare from the BL Lac object Mrk 421 was detected in May of 1994 by the Whipple Observatory air Cherenkov experiment during which the flux above 250 GeV increased by nearly an order of magnitude over a 2-day period. Contemporaneous observations by ASCA showed the X-ray flux to be in a very high state. We present these results, combined with the first ever simultaneous or nearly simultaneous observations at GeV gamma-ray, UV, IR, mm, and radio energies for this nearest BL Lac object. While the GeV gamma-ray flux increased slightly, there is little evidence for variability comparable to that seen at TeV and X-ray energies. Other wavelengths show even less variability. This provides important constraints on the emission mechanisms at work. We present the multiwavelength spectrum of this gamma-ray blazar for both quiescent and flaring states and discuss the data in terms of current models of blazar emission. C1 UNIV MICHIGAN,DEPT PHYS,ANN ARBOR,MI 48109. UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. CATHOLIC UNIV AMER,WASHINGTON,DC 20064. NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,GREENBELT,MD 20771. IOWA STATE UNIV SCI & TECHNOL,DEPT PHYS & ASTRON,AMES,IA 50011. ST PATRICKS COLL,DEPT PHYS,MAYNOOTH,KILDARE,IRELAND. USN,RES LAB,DIV SPACE SCI,WASHINGTON,DC 20375. PURDUE UNIV,DEPT PHYS,W LAFAYETTE,IN 47907. ROYAL OBSERV,EDINBURGH EH9 3HJ,MIDLOTHIAN,SCOTLAND. UNIV LEEDS,DEPT PHYS,LEEDS LS2 9JT,W YORKSHIRE,ENGLAND. GEORGE MASON UNIV,CSI,INST SCI & TECHNOL,SPACE SCI PROGRAM,FAIRFAX,VA 22030. HAMPDEN SYDNEY COLL,DEPT PHYS & ASTRON,HAMPDEN SYDNEY,VA 23943. UNIV TOKYO,DEPT PHYS,BUNKYO KU,TOKYO 113,JAPAN. INST SPACE & ASTRONAUT SCI,SAGAMIHARA,KANAGAWA 229,JAPAN. BOSTON UNIV,DEPT ASTRON,BOSTON,MA 02215. UNIV SOUTHAMPTON,DEPT PHYS,SOUTHAMPTON SO9 5NH,HANTS,ENGLAND. JOINT ASTRON CTR,HILO,HI 96720. UNIV CENT LANCASHIRE,CTR ASTROPHYS,PRESTON PR1 2HE,LANCS,ENGLAND. UNIV COLL DUBLIN,DEPT PHYS,DUBLIN 4,IRELAND. HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,AMADO,AZ 85645. RP MACOMB, DJ (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771, USA. RI McEnery, Julie/D-6612-2012; Tashiro, Makoto/J-4562-2012 NR 27 TC 119 Z9 121 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 1995 VL 449 IS 2 BP L99 EP L103 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RP425 UT WOS:A1995RP42500001 ER PT J AU KOSOWSKY, A TURNER, MS AF KOSOWSKY, A TURNER, MS TI CBR ANISOTROPY AND THE RUNNING OF THE SCALAR SPECTRAL INDEX SO PHYSICAL REVIEW D LA English DT Note ID INFLATIONARY UNIVERSE; PERTURBATIONS AB Accurate (less than or equal to 1%) predictions for the anisotropy of the cosmic background radiation (CBR) are essential for using future high-resolution (less than or equal to 1 degrees) CBR maps to test cosmological models. In many inflationary models the variation (''running'') of the spectral index of the spectrum of density perturbations is a significant effect and leads to changes of around 1-10% in the CBR power spectrum. We propose a general method for taking running into account which uses the derivative of the spectral index (dn/dlnk). Conversely, high-resolution CBR maps may be able to determine dn/dlnk, giving important information about the inflationary potential. C1 HARVARD UNIV,LYMAN LAB PHYS,DEPT PHYS,CAMBRIDGE,MA 02138. UNIV CHICAGO,ENRICO FERMI INST,DEPT PHYS,CHICAGO,IL 60637. UNIV CHICAGO,ENRICO FERMI INST,DEPT ASTRON & ASTROPHYS,CHICAGO,IL 60637. FERMILAB NATL ACCELERATOR LAB,NASA,FERMILAB ASTROPHYS CTR,BATAVIA,IL 60510. RP KOSOWSKY, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 27 TC 188 Z9 188 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2821 J9 PHYS REV D JI Phys. Rev. D PD AUG 15 PY 1995 VL 52 IS 4 BP R1739 EP R1743 DI 10.1103/PhysRevD.52.R1739 PG 5 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA RQ554 UT WOS:A1995RQ55400001 ER PT J AU FIORE, F ELVIS, M SIEMIGINOWSKA, A WILKES, BJ MCDOWELL, JC MATHUR, S AF FIORE, F ELVIS, M SIEMIGINOWSKA, A WILKES, BJ MCDOWELL, JC MATHUR, S TI COMPLEX OPTICAL TO SOFT-X-RAY SPECTRUM OF LOW-REDSHIFT RADIO-QUIET QUASARS .2. COMPARISON WITH FREE-FREE AND ACCRETION DISK MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE QUASARS, GENERAL; X-RAYS, GALAXIES ID ACTIVE GALACTIC NUCLEI; COMPTON HEATED WINDS; SEYFERT-GALAXIES; ENERGY-DISTRIBUTIONS; ULTRAVIOLET; CONTINUUM; BUMP; POLARIZATION; VARIABILITY; EMISSION AB We compare the optical to soft X-ray spectral energy distributions (SEDs) of a sample of bright low-redshift (0.048 < z < 0.155), radio-quiet quasars, with a range of thermal models which have been proposed to explain the optical/UV/soft X-ray quasar emission: (1) optically thin emission from an ionized plasma, (2) optically thick emission from the innermost regions of an accretion disk in Schwarzschild and Kerr geometries. We presented ROSAT PSPC observations of these quasars in an earlier paper. Here our goals are to search for the signature of thermal emission in the quasar SEDs, and to investigate whether a single component is dominating at different frequencies. We find that isothermal optically thin plasma models can explain the observed soft X-ray color and the mean optical-ultraviolet (OUV) color. However, they predict an ultraviolet (1325 Angstrom luminosity a factor of 3 to 10 times lower than observed. Pure disk models, even in a Kerr geometry, do not have the necessary flexibility to account for the observed OUV and soft X-ray luminosities. Additional components are needed both in the optical and in the soft X-rays (e.g., a hot corona can explain the soft X-ray color). The most constrained modification of pure disk models, is the assumption of an underlying power-law component extending from the infrared (3 mu m) to the X-ray. This can explain both the OUV and soft X-ray colors and luminosities and does not exceed the 3 mu m luminosity, where a contribution from hot dust is likely to be important. We also discuss the possibility that the observed soft X-ray color and luminosity are dominated by reflection from the ionized surface of the accretion disk. While modifications of both optically thin plasma models and pure disk models might account for the observed SED, we do not find any strong evidence that the OUV bump and soft X-ray emission are one and the same component. Likewise, we do not find any strong argument which definitely argues in favor of thermal models. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OI Wilkes, Belinda/0000-0003-1809-2364; Fiore, Fabrizio/0000-0002-4031-4157 NR 79 TC 27 Z9 27 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 1995 VL 449 IS 1 BP 74 EP 85 DI 10.1086/176033 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RM555 UT WOS:A1995RM55500009 ER PT J AU WORRALL, DM BIRKINSHAW, M CAMERON, RA AF WORRALL, DM BIRKINSHAW, M CAMERON, RA TI THE X-RAY ENVIRONMENT OF THE DUMBBELL RADIO GALAXY NGC-326 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERS, INDIVIDUAL (ABELL 115); GALAXIES, INDIVIDUAL (NGC 326); GALAXIES, JETS; INTERGALACTIC MEDIUM; X-RAYS, GALAXIES ID VLA OBSERVATIONS; CLUSTERS; CATALOG; SAMPLE; JETS AB We report the first detailed X-ray observations of the dumbbell radio galaxy NGC 326. The region containing the source was imaged for 5.8 hr in soft X-rays with the ROSAT PSPC as part of a program to measure the X-ray emission in low-power radio galaxies not known to be in rich clusters. Unlike other radio galaxies measured as part of this program, NGC 326 is discovered to be embedded in bright asymmetrical X-ray-emitting cluster gas of temperature kT similar to 2 keV and 0.1-2.4 keV luminosity 3.5 x 10(36) W (H-0 = 50 km s(-1) Mpc(-1)). There is a peak in the X-ray emission consistent with the location of the radio galaxy core. Five of the 10 brightest galaxies in the region are the brightest optical objects in error circles of excess X-ray emission. In the same observation, ROSAT also detected the unrelated, more distant, cluster Abell 115 and provided its first spectral measurement: kT = 7.2(-1.9)(+9) keV. It has been suggested previously that galaxy kinematics are responsible for the apparent change in direction over time of the twin jets of the large-scale radio emission of NGC 326. This was thought to be due either to a misalignnent between the radio beam and galaxy axes or to interaction between the two galaxies which form the dumbell nucleus of NGC 326 and which are known to be passing at about 16 kpc projected separation. Our X-ray results support a different explanation: that buoyancy forces have bent the outer radio structure. RP WORRALL, DM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 40 TC 48 Z9 48 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 1995 VL 449 IS 1 BP 93 EP 104 DI 10.1086/176035 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RM555 UT WOS:A1995RM55500011 ER PT J AU LEBOURLOT, J FORETS, GPD ROUEFF, E DALGARNO, A GREDEL, R AF LEBOURLOT, J FORETS, GPD ROUEFF, E DALGARNO, A GREDEL, R TI INFRARED DIAGNOSTICS OF THE FORMATION OF H-2 ON INTERSTELLAR DUST SO ASTROPHYSICAL JOURNAL LA English DT Article DE DUST, EXTINCTION; INFRARED, ISM, LINES AND BANDS; ISM, CLOUDS; ISM, MOLECULES ID MOLECULAR-HYDROGEN GAS; ULTRAVIOLET-RADIATION; CLOUDS; H2; RECOMBINATION; EXCITATION; EMISSION; GRAINS; FIELD AB The infrared spectrum arising from the formation of molecular hydrogen in molecular clouds is calculated for three different possible mechanisms. The contribution to the spectrum arising from the excitation of molecular hydrogen by cosmic ray secondary electrons is included. Specific emission lines that may serve as diagnostics of the formation mechanism are identified. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. EUROPEAN SO OBSERV,LA SILLA OBSERV,LA SILLA,CHILE. RP LEBOURLOT, J (reprint author), OBSERV PARIS,DAEC,F-92195 MEUDON,FRANCE. NR 25 TC 32 Z9 32 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 1995 VL 449 IS 1 BP 178 EP 183 DI 10.1086/176043 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RM555 UT WOS:A1995RM55500019 ER PT J AU DEKOOL, M GREEN, PJ AF DEKOOL, M GREEN, PJ TI A MODEL FOR THE SPACE DENSITY OF DWARF CARBON STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION,; ACCRETION DISKS; BINARIES, GENERAL; STARS, CARBON; STARS, EVOLUTION; STARS, STATISTICS ID GIANT BRANCH EVOLUTION; SOLAR NEIGHBORHOOD; ORBITAL ELEMENTS; THERMAL PULSE; MASS-TRANSFER; STELLAR; ABUNDANCES; BINARIES; G77-61 AB Recent studies of faint high-latitude carbon stars have shown that a significant fraction of them are not distant asymptotic giant branch (AGB) stars but rather belong to the local population of spheroid dwarfs. In this paper we attempt a theoretical prediction of the local space density of such dwarf carbon stars (dCs) based on the assumption that they are ordinary main-sequence stars that were able to accrete enough carbon-enriched material from a binary companion on the AGB to make their C/O ratio larger than unity. A simulated population of dCs is constructed by following the evolution of a large number of binaries using simple analytic fits to detailed evolutionary calculations and determining which ones would presently contain a dC. The zero-age parameters of the sample are chosen randomly from distributions derived from the observed properties of unevolved binaries. The space density of halo dCs that we predict (similar to 2-4 x 10(-7) pc(-3)) is in agreement with current observational constraints. The predicted local space density of disk dCs (similar to 1 x 10(-6) pc(-3)) may be somewhat higher than observed. The fraction of binaries that produces dCs depends strongly on initial metallicity, and virtually no dCs are formed in systems with an initial metallicity of more than half solar. Thus, all disk dCs are predicted to be in binaries that formed in the very early phases of disk star formation, and their number depends strongly on assumptions about the age-metallicity relation during this epoch. The predictions for the halo are much less model-dependent. The simulated orbital period distributions are bimodal, with one peak between 10(3) and 10(5) days and another peak between 10(2) and 10(3) days. The shorter period component is caused by systems that have gone through a common envelope phase. The simulated period distributions bear a strong resemblance to the observed orbital period distribution of barium and CH giants, which may be the evolved descendants of the disk and halo dC populations we have modeled. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP DEKOOL, M (reprint author), MAX PLANCK INST ASTROPHYS,KARL SCHWARZSCHILD STR 1,D-85740 GARCHING,GERMANY. NR 39 TC 19 Z9 19 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 1995 VL 449 IS 1 BP 236 EP 245 DI 10.1086/176051 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RM555 UT WOS:A1995RM55500027 ER PT J AU ZUCKER, DB RAYMOND, JC SILBER, A MASON, P CURIEL, S VRTILEK, S SCHLEGEL, E AF ZUCKER, DB RAYMOND, JC SILBER, A MASON, P CURIEL, S VRTILEK, S SCHLEGEL, E TI PHASE-RESOLVED IUE AND OPTICAL OBSERVATIONS OF THE POLAR BY CAMELOPARDALIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE BINARIES, CLOSE; NOVAE; CATACLYSMIC VARIABLES; STARS, INDIVIDUAL (BY CAMELOPARDALIS); ULTRAVIOLET, STARS ID AM-HERCULIS; ULTRAVIOLET OBSERVATIONS; H0538+608 =; RAY; STATE; CYGNI AB Time-resolved IUE observations of the asynchronous polar BY Cam (H0538 + 608) over a period of 11 days show that the N v 1240 Angstrom emission-line velocity varies on the orbital period, with an amplitude of 368 +/- 27 km s(-1). The N v flux also varies on the orbital period, with maximum flux corresponding to maximum blueshift. This behavior is seen in He II 1640 Angstrom as well, although with a smaller velocity amplitude (244 +/- 26 km s(-1)). Variation on the orbital (rather than the white dwarf spin) period implies that the emission must originate outside the magnetosphere of the white dwarf, in the accretion stream, the heated face of the secondary, or some combination of the two. The rise, peak, and fall in line emission take place over similar to 0.3 of an orbit, constraining models of the system geometry; we discuss a number of potential explanations for the observed phenomena, including optically thick (in the lines) emission from the accretion stream, occultation of the emission region by the secondary, and combinations of the two processes. We also propose an alternative scenario, in which X-ray illumination from the environment of the white dwarf gives rise to anisotropic line emission from the accretion stream. Ultraviolet continuum intensities on different nights appeared to be in either low or high flux states; we obtained three nights of optical photometry during the same time period, and the optical light curves corresponding to the high and low flux states were distinct, supporting the idea that the pattern of accretion flow changes. Finally, we note that spectroscopic attempts to observe Na I lambda lambda 8183, 8194 in the photosphere of the secondary were not successful. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CASE WESTERN RESERVE UNIV,DEPT ASTRON,CLEVELAND,OH 44104. UNIV MARYLAND,DEPT ASTRON,COLLEGE PK,MD 20742. NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,UNIV SPACE RES ASSOC,GREENBELT,MD 20771. RP ZUCKER, DB (reprint author), UNIV WASHINGTON,DEPT ASTRON,FM-20,SEATTLE,WA 98195, USA. NR 36 TC 5 Z9 5 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 1995 VL 449 IS 1 BP 310 EP 319 DI 10.1086/176056 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RM555 UT WOS:A1995RM55500032 ER PT J AU GREENHILL, LJ COLOMER, F MORAN, JM BACKER, DC DANCHI, WC BESTER, M AF GREENHILL, LJ COLOMER, F MORAN, JM BACKER, DC DANCHI, WC BESTER, M TI INTERFEROMETRIC OBSERVATIONS OF THE SIO MASERS AND DUST SHELL OF VX-SAGITTARII SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; MASERS; STARS, INDIVIDUAL (VX SGR); TECHNIQUES, INTERFEROMETRIC ID LATE-TYPE STARS; SERIES INFRARED-SPECTROSCOPY; MIRA VARIABLES; EMISSION; VLBI; DIAMETER; STELLAR; SHOCK; CO AB We report the results of VLBI observations at 7 mm wavelength of the SiO maser emission (J = 1 --> 0, upsilon = 1) in the circumstellar envelope of the late-type variable star VX Sagittarii. These are the first VLBI observations that have been coordinated with mid-infrared interferometric observations of late-type stars. Synthesis images show that the maser emission at a stellar phase of about 0.4 arises from a ringlike distribution with a radius of about 1.3 R(*). The distribution of emission is asymmetric and the strongest emission arises from the redshifted center of activity that lies to the south of the star. This may indicate an asymmetry in the mass-loss or stellar atmosphere. The maser emission within 4 km s(-1) of the stellar velocity is distributed around the stellar limb and does not show evidence of systematic velocity gradients greater than a few km s(-1), The overlap of maser features is consistent with outflow (or infall) of material away from (or toward) the star of about 10 km s(-1) at 1.3 R(*), about half the velocity observed in the OH and H2O maser shells at radii of greater than 30 R(*). The arrangement of the maser emission suggests the presence of dense velocity coherent structures with characteristic sizes of similar to 0.4 AU (0.02 R(*)) in the extended atmosphere above the photosphere. However, 74% of the maser flux was resolved by these observations, as with earlier, single-baseline VLBI observations of coarser angular resolution. We speculate that the circumstellar shell also has velocity coherent cells on spatial scales of 30 to perhaps 100 AU, which give rise to SiO maser emission. The compact SiO maser emission lies well within the 4.6 R(*) inner radius of the circumstellar dust shell, as measured with the UC Berkeley Infrared Spatial Interferometer at about the same stellar minimum. The stellar radius at stellar minimum was measured to be 22 +/- 3 AU (13 +/- 2 mas). Infrared observations made close to stellar maximum show an inner radius of 6.0 R(*). The estimated density at the inner edge of the dust shell, the location of the masers, and the density at which the maser levels probably thermalize are consistent with models of atmospheric extension due to pulsation-driven shocks. C1 UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. UNIV CALIF BERKELEY,SPACE SCI LAB,BERKELEY,CA 94720. RP GREENHILL, LJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 48 TC 82 Z9 82 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 1995 VL 449 IS 1 BP 365 EP 375 DI 10.1086/176060 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RM555 UT WOS:A1995RM55500036 ER PT J AU LOEB, A SASSELOV, D AF LOEB, A SASSELOV, D TI REMOVING DEGENERACY OF MICROLENSING LIGHT CURVES THROUGH NARROW-BAND PHOTOMETRY OF GIANTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ASTROMETRY; DARK MATTER; GRAVITATIONAL LENSING ID CA-II H; EFFECTIVE TEMPERATURES; GALACTIC HALO; STARS; CHROMOSPHERES; K0 AB The standard light curve of a microlensing event provides only two constraints on the five unknown parameters of the lens. We show that narrowband photometry during a microlensing event of a giant star can in addition determine the angular radius of the Einstein ring and the proper motion of the lens. This possibility results from the fact that the extended atmospheres of giants emit the cores of resonance lines primarily from a narrow ring (limb brightening). A considerable fraction of the clump giants in the bulge have a ring radius greater than or similar to 10(12) cm, within the range of Einstein radii for subsolar mass lenses. The extended thin ring also provides a sensitive probe of possible planetary companions as it sweeps across the lens plane. The ring signature can be detected photometrically, using a narrowband filter centered on resonance lines like Ca II lambda 3933. RP LOEB, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 45 TC 50 Z9 50 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 1995 VL 449 IS 1 BP L33 EP L36 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RM556 UT WOS:A1995RM55600008 ER PT J AU MYERS, PC BACHILLER, R CASELLI, P FULLER, GA MARDONES, D TAFALLA, M WILNER, DJ AF MYERS, PC BACHILLER, R CASELLI, P FULLER, GA MARDONES, D TAFALLA, M WILNER, DJ TI GRAVITATIONAL INFALL IN THE DENSE CORES L1527 AND L483 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, MOLECULES; LINE, PROFILES; STARS, FORMATION ID SMALL-SCALE STRUCTURE; PROTOSTELLAR COLLAPSE; LINE FORMATION; DARK CLOUDS; B335; OUTFLOW; PROBE AB Lines of N2H+, C3H2, and H2CO show kinematic evidence of gravitational infall in L1527, and probably also in L483. Three trends appear to indicate infall, rather than outflow or rotation: (a) at each protostar position, line peak and centroid velocities get bluer by 0.1-0.3 km s(-1) with increasing line optical depth; (b) in maps of C3H2 and H2CO lines, peak and centroid velocities get bluer by a similar amount as positions approach each protostar; and (c) C3H2 line widths in L1527 increase as positions approach the protostar. Also, in both sources H2CO lines show the infall ''signature'' of spatially concentrated double-peaked profiles, with their blue peaks brighter than their red peaks, as seen previously in B335. Many asymmetric profiles have a single blueshifted peak with a red shoulder, or two peaks with blue/red intensity ratio greater than 3. These are hard to fit with spherical infall models, owing perhaps to the effects of the bipolar outflow. In each source, H2CO line wings show clear evidence of collimated outflow. C1 CTR ASTRON YEBES,IGN,E-19080 GUADALAJARA,SPAIN. RP MYERS, PC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Mardones, Diego/I-5719-2016 NR 31 TC 52 Z9 52 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 1995 VL 449 IS 1 BP L65 EP L68 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RM556 UT WOS:A1995RM55600015 ER PT J AU WILNER, DJ WELCH, WJ FORSTER, JR AF WILNER, DJ WELCH, WJ FORSTER, JR TI SUB-ARCSECOND IMAGING OF W3(OH) AT 87.7 GHZ SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL [W3(OH)]; STARS, FORMATION; TECHNIQUES, INTERFEROMETRIC ID RESOLUTION MAPS; OH LINES; STARS AB We report continuum observations of the W3(OH) region with the Berkeley-Illinois-Maryland array at an effective frequency of 87.7 GHz with sub-arcsecond resolution (0 ''.7 x 0 ''.5). The bright ultracompact H II region shows a shell-like morphology, consistent with an extrapolation from lower frequencies of optically thin free-free emission with no significant contribution from dust. A weak unresolved continuum source is detected 6 '' to the east of the ultracompact H II region, coincident with the elongated centimeter-wave synchrotron source associated with the Turner-Welch (TW) object. The source brightness temperature is approximately 20 K, and the spectral index between 87.7 GHz and 111 GHz is characteristic of optically thin thermal dust emission. Assuming standard dust properties, we estimate that the underlying source luminosity is 10(3)-10(4) L., and we derive a mass of 10-20 M. for the emission region. We speculate that this represents circumstellar material about to be incorporated into a newly forming star, making the TW object the high-mass equivalent of a ''class 0'' low-mass protostar. C1 UNIV CALIF BERKELEY,RADIO ASTRON LAB,BERKELEY,CA 94720. RP WILNER, DJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 28 TC 38 Z9 38 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 1995 VL 449 IS 1 BP L73 EP L76 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RM556 UT WOS:A1995RM55600017 ER PT J AU CHEUNG, ASC MOK, DKW YOSHINO, K PARKINSON, WH JAMIESON, MJ DALGAMO, A CHILD, MS AF CHEUNG, ASC MOK, DKW YOSHINO, K PARKINSON, WH JAMIESON, MJ DALGAMO, A CHILD, MS TI ISOTOPIC DEPENDENCE OF PREDISSOCIATION LINEWIDTHS IN THE SCHUMANN-RUNGE BANDS OF OXYGEN SO JOURNAL OF CHEMICAL PHYSICS LA English DT Note ID ABSORPTION-BANDS; SPECTROSCOPIC CONSTANTS; O-16 O-18; O2; O-2; NM C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV OXFORD,DEPT THEORET CHEM,OXFORD OX1 3UB,ENGLAND. UNIV GLASGOW,DEPT COMP SCI,GLASGOW G12 8QQ,LANARK,SCOTLAND. RP CHEUNG, ASC (reprint author), UNIV HONG KONG,DEPT CHEM,POKFULAM RD,HONG KONG,HONG KONG. RI Cheung, Allan/D-3059-2009; Mok, Daniel Kam-Wah/K-5826-2013 OI Mok, Daniel Kam-Wah/0000-0002-6677-2949 NR 23 TC 4 Z9 4 U1 0 U2 4 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD AUG 8 PY 1995 VL 103 IS 6 BP 2369 EP 2371 DI 10.1063/1.469660 PG 3 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA RM539 UT WOS:A1995RM53900039 ER PT J AU FORMAN, P AF FORMAN, P TI TRUST IN NUMBERS - THE PURSUIT OF OBJECTIVITY IN SCIENCE AND PUBLIC-LIFE - PORTER,TM SO SCIENCE LA English DT Book Review RP FORMAN, P (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 9 Z9 9 U1 0 U2 3 PU AMER ASSOC ADVAN SCIENCE PI WASHINGTON PA 1333 H ST NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD AUG 4 PY 1995 VL 269 IS 5224 BP 707 EP 710 DI 10.1126/science.269.5224.707 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RM702 UT WOS:A1995RM70200040 PM 17758814 ER PT J AU FORMAN, P AF FORMAN, P TI A SOCIAL-HISTORY OF TRUTH - CIVILITY AND SCIENCE IN 17TH-CENTURY ENGLAND - SHAPIN,S SO SCIENCE LA English DT Book Review RP FORMAN, P (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 9 Z9 9 U1 0 U2 3 PU AMER ASSOC ADVAN SCIENCE PI WASHINGTON PA 1333 H ST NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD AUG 4 PY 1995 VL 269 IS 5224 BP 707 EP 710 DI 10.1126/science.269.5224.707 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RM702 UT WOS:A1995RM70200039 PM 17758814 ER PT J AU UBELAKER, DH KATZENBERG, MA DOYON, LG AF UBELAKER, DH KATZENBERG, MA DOYON, LG TI STATUS AND DIET IN PRECONTACT HIGHLAND ECUADOR SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE STABLE ISOTOPES; PALEODIET; ECUADOR; MAIZE; STATUS ID BONE-COLLAGEN; ISOTOPE RATIOS; NITROGEN; N-15; ECOSYSTEMS; ABUNDANCE; ANIMALS; MARINE; MAIZE; PERU AB Excavation at the Ecuadorian highland site of La Florida in suburban Quite revealed six deep shaft tombs yielding high-status individuals (n = 9) as well as apparent sacrifices and other low-status individuals (n = 23). Determination of sex and age at death of the recovered skeletal remains resulted in a sample of 32 individuals aged from approximately 7 to 50 years of age, The sample of 18 individuals over the age of 18 years included 14 females and 4 males, Temporally, the remains are assigned to the Chaupicruz Phase (circa 100 to 450 AD) of the Regional Developmental Period. In this study, we analyze stable isotopes of carbon and nitrogen from human bone in order to compare the diets of the high- and low-status individuals. Stable carbon isotope analyses were carried out on preserved protein and biological apatite (bioapatite), and stable nitrogen isotope analyses were carried out on preserved protein. There is a statistically significant difference in delta(13)C between tween the two groups for both protein and mineral sources of carbon with evidence for the greater consumption of maize in the high-status group. There is no significant difference in delta(15)N between the two groups, nor is there a significant difference in the spacing between protein and mineral delta(13)C values between the two groups, Ethnohistorical evidence for the 16th century AD provides the expectation that the only dietary difference was the higher consumption of animal protein by the elite. There is no evidence for this based on the bone chemistry data from La Florida. Instead, the isotope data, along with the archaeological evidence, indicate that the major dietary difference during the Chaupicruz Phase was the greater intake of maize by the elite, probably in the form of beer (chicha). (C) 1995 Wiley-Liss, Inc. C1 UNIV CALGARY,DEPT ARCHAEOL,CALGARY,AB 72N 1N4,CANADA. YALE UNIV,DEPT ANTHROPOL,NEW HAVEN,CT 06520. RP UBELAKER, DH (reprint author), NATL MUSEUM NAT HIST,SMITHSONIAN INST,DEPT ANTHROPOL,MRC 112,WASHINGTON,DC 20560, USA. NR 36 TC 49 Z9 49 U1 0 U2 8 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD AUG PY 1995 VL 97 IS 4 BP 403 EP 411 DI 10.1002/ajpa.1330970407 PG 9 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA RM004 UT WOS:A1995RM00400006 PM 7485437 ER PT J AU ROSENBERGER, AL AF ROSENBERGER, AL TI MARMOSETS AND TAMARINS - SYSTEMATICS, BEHAVIOR, AND ECOLOGY - RYLANDS,AB SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Book Review RP ROSENBERGER, AL (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008, USA. NR 1 TC 0 Z9 0 U1 1 U2 2 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD AUG PY 1995 VL 97 IS 4 BP 457 EP 458 DI 10.1002/ajpa.1330970413 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA RM004 UT WOS:A1995RM00400012 ER PT J AU CHRISTY, JH AF CHRISTY, JH TI MIMICRY, MATE CHOICE, AND THE SENSORY TRAP HYPOTHESIS SO AMERICAN NATURALIST LA English DT Article ID CRICKET TELEOGRYLLUS-COMMODUS; ORIENTAL FRUIT MOTH; CRAB UCA-BEEBEI; SEXUAL SELECTION; FIDDLER CRAB; PHYSALAEMUS-PUSTULOSUS; OVIPOSITION BEHAVIOR; UTETHEISA-ORNATRIX; ANIMAL SIGNALS; ARCTIID MOTH AB Sensory traps affect mate choice when male courtship signals mimic stimuli to which females respond in other contexts and elicit female behavior that increases male fertilization rates. Because of the supernormal stimulus effect, mimetic signals may become quantitatively exaggerated relative to model stimuli. Viability selection or a decrease in responsiveness to signals that are exaggerated beyond their peak supernormal effect may limit signal elaboration. Females always benefit by responding to models and they may often benefit by responding to mimetic courtship signals. If the response as a preference is costly, it may be maintained by frequent and strong selection for the response to the model. I review five examples of courtship that illustrate the kinds of studies that can provide evidence of sensory traps. The strategic designs of mimetic courtship signals arise not from selection of responses to them but from selection for responses to models. This results from deceit by mimicry and the evolution of sensory trap responses before the signals that elicit them as preferences. RP CHRISTY, JH (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. NR 66 TC 151 Z9 153 U1 4 U2 42 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0003-0147 J9 AM NAT JI Am. Nat. PD AUG PY 1995 VL 146 IS 2 BP 171 EP 181 DI 10.1086/285793 PG 11 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA RN011 UT WOS:A1995RN01100001 ER PT J AU THOMPSON, KV AF THOMPSON, KV TI FLEHMEN AND BIRTH SYNCHRONY AMONG FEMALE SABLE ANTELOPE, HIPPOTRAGUS-NIGER SO ANIMAL BEHAVIOUR LA English DT Article ID REPRODUCTIVE SYNCHRONY; OVARIAN-FUNCTION; MALE GOATS; DOMINANCE; URINARY; HYPOTHESIS; PREGNANCY; BEHAVIOR; CYCLE AB The role of female flehmen behaviour in maintaining reproductive synchrony was investigated in 11 adult female sable antelope and their associated offspring maintained on a 13.2-ha pasture at the National Zoological Park's Conservation and Research Center near Front Royal, Virginia. All occurrences of aggression and flehmen by adult females were recorded during 274 h of observation over a 10-month period (1987), and the timing of births was recorded for four birth seasons (1986-1989). In each year, dominant females tended to give birth in temporal proximity to other females (birth clustering), while subordinates gave birth asynchronously. Flehmen frequency fluctuated seasonally, reaching highest levels just prior to the approximated time of conception. Adult, multiparous females were the primary targets of flehmen. There was positive assortment by reproductive state: pregnant females attended to urinations by other pregnant females and postpartum females responded to other postpartum females. Prepartum flehmen rates reliably predicted subsequent birth synchrony, and the degree of synchrony between a given pair of females was directly proportional to the frequency with which they sampled each other's urine in the preceding year. These results indicate that flehmen is a potential mechanism by which female sable antelope can manipulate the timing of both conception and parturition. (C) 1995 The Association for the Study of Animal Behaviour C1 UNIV MARYLAND,DEPT ZOOL,COLLEGE PK,MD 20742. SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. RI Thompson, Katerina/B-6146-2009 NR 55 TC 20 Z9 20 U1 0 U2 6 PU ACADEMIC PRESS (LONDON) LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD AUG PY 1995 VL 50 BP 475 EP 484 DI 10.1006/anbe.1995.0261 PN 2 PG 10 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA RP916 UT WOS:A1995RP91600018 ER PT J AU EBERHARD, WG AF EBERHARD, WG TI SEXUAL SELECTION - ANDERSSON,M SO ANIMAL BEHAVIOUR LA English DT Book Review C1 UNIV COSTA RICA,ESCUELA BIOL,SAN JOSE,COSTA RICA. RP EBERHARD, WG (reprint author), UNIV COSTA RICA,SMITHSONIAN TROP RES INST,CIUDAD UNIV,SAN JOSE,COSTA RICA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU ACADEMIC PRESS (LONDON) LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD AUG PY 1995 VL 50 BP 564 EP 565 PN 2 PG 2 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA RP916 UT WOS:A1995RP91600031 ER PT J AU QUINTANA, H RAMIREZ, A MELNICK, J RAYCHAUDHURY, S SLEZAK, E AF QUINTANA, H RAMIREZ, A MELNICK, J RAYCHAUDHURY, S SLEZAK, E TI THE SHAPLEY SUPERCLUSTER .1. SPECTROSCOPIC OBSERVATIONS IN THE CENTRAL REGION SO ASTRONOMICAL JOURNAL LA English DT Article ID HYDRA-CENTAURUS SUPERCLUSTER; RICH CLUSTERS; ELLIPTICAL GALAXIES; SOUTHERN CLUSTERS; X-RAY; REDSHIFT OBSERVATIONS; VELOCITY DISPERSIONS; PECULIAR VELOCITIES; RADIAL-VELOCITIES; PHOTOMETRY AB We present a new analysis of the kinematics of the Shapley supercluster based on radial velocities for 1087: galaxies in the clusters A3558 (Shapley 8), A3528 (Klemola 21), A3532 (Klemola 22), A3530, A3556 (SCI 1321-314), A3559 (CE 1327-292), A3560, A3562, SC 1329-314 and in the intercluster region of the core of the supercluster, of which 367 are new measurements. We also present accurate positions from APM and MAMA scans of the ESO/SERC Southern Sky Survey photographic plates. We obtain new velocity dispersions and estimate the masses of the member clusters, evaluating dynamical models of the supercluster. The supercluster is found to be significantly flattened. We find that for Omega(0)=0.3, H-0=75 km s(-1) Mpc(-1), the gravitational pull of the supercluster may account for up to 25% of the peculiar velocity of the Local Group required to explain the dipole anisotropy of the Cosmic Microwave Background radiation, in which case the mass of the supercluster would be dominated by intercluster dark matter. This fractional contribution would be considerably higher for combinations of significantly lower values of Omega(0) and higher values of H-0. 1995 American Astronomical Society. C1 EUROPEAN SO OBSERV,LA SILLA,CHILE. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OBSERV COTE AZUR,F-06304 NICE 4,FRANCE. ASSOC UNIV RES ASTRON INC,CERRO TOLOLO INTERAMER OBSERV,TUCSON,AZ. PONTIFICIA UNIV CATOLICA CHILE,ASTROFIS GRP,SANTIAGO,CHILE. NR 71 TC 52 Z9 52 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1995 VL 110 IS 2 BP 463 EP 476 DI 10.1086/117535 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RL500 UT WOS:A1995RL50000001 ER PT J AU MARZKE, RO GELLER, MJ DACOSTA, LN HUCHRA, JP AF MARZKE, RO GELLER, MJ DACOSTA, LN HUCHRA, JP TI PAIRWISE VELOCITIES OF GALAXIES IN THE CFA AND SSRS2 REDSHIFT SURVEYS SO ASTRONOMICAL JOURNAL LA English DT Article ID COLD DARK-MATTER; LARGE-SCALE STRUCTURE; MEAN MASS DENSITY; EXPANDING UNIVERSE; COMPLETE SAMPLE; CLUSTERS; CATALOG; DISPERSION; FIELDS; SPACE AB We combine the CfA Redshift Survey (CfA2) and the Southern Sky Redshift Survey (SSRS2) to estimate the pairwise velocity dispersion of galaxies sigma(12) on a scale of similar to 1 h(-1) Mpc. Both surveys are complete to an apparent magnitude limit B(0)=15.5. Our sample includes 12 812 galaxies distributed in a volume 1.8x10(6)h(-3) Mpc(3). We conclude: (1) The pairwise velocity dispersion of galaxies in the combined CfA2+SSRS2 redshift survey is sigma(12)=540+/-180 kms(-1). Both the estimate and the variance of sigma(12) significantly exceed the canonical values sigma(12)=340+/-40 measured by Davis and Peebles (1983) using CfA1. (2) We derive the uncertainty in sigma(12) from the variation among subsamples with volumes on the order of 7x10(5)h(-3) Mpc(3). This variation is nearly an order of magnitude larger than the formal error, 36 km s(-1) derived using least-squares fits to the CfA2+SSRS2 correlation function. This variation among samples is consistent with the conclusions of Mo ef al. (1993) for a number of smaller surveys and with the analysis of CfA1 by Zurek et al. (1994). (3) When we remove Abell clusters with R greater than or equal to 1 from our sample, the pairwise velocity dispersion of the remaining galaxies drops to 295+/-99 km s(-1). (4) The dominant source of variance in sigma(12) is the shot noise contributed by dense virialized systems. Because sigma(12) is pair weighted, the statistic is sensitive to the few richest systems in the volume. This sensitivity has two consequences. First, sigma(12) is biased low in small volumes, where the number of clusters is small. Second, we can estimate the variance in sigma(12) as a function of survey volume from the distribution of cluster and group velocity dispersions n(sigma). For either a COBE-normalized CDM universe or for the observed distribution of Abell cluster velocity dispersions, the volume required for sigma(12) to converge (delta sigma(12)/sigma(12)<0.1 is similar to 5x10(6)h(-3) Mpc(3), larger than the volume of CfA2+SSRS2. (5) The distribution of pairwise velocities is consistent with an isotropic exponential with velocity dispersion independent of scale. The inferred single-galaxy velocity distribution function is incompatible with an isotropic exponential. Thus the observed kinematics of galaxies differ from those measured in the hydrodynamic simulations of Cen & Ostriker (1993). On the other hand, our observations appear to be consistent with the velocity distribution function measured by Zurek et al. (1994) using collisionless simulations with much higher resolution than Cen & Ostriker (1993). The large dynamic range in the simulations by Zurek ef al. (1994) affords a more accurate treatment of galaxy interactions, which dramatically alter the dynamical evolution the galaxy distribution (Couchman & Carlberg 1999; Zurek et al. 1994). The agreement between the observed velocity distribution and the one predicted by these high-resolution simulations may be another clue that mergers play an important role in the evolution of galaxies and large-scale structure. (C) 1995 American Astronomical Society. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OBSERV NACL,CNPQ,DEPT ASTRON,BR-20921 RIO JANEIRO,BRAZIL. RP MARZKE, RO (reprint author), NATL RES COUNCIL CANADA,HERZBERG INST ASTROPHYS,DOMINION ASTROPHYS OBSERV,5071 W SAANICH RD,VICTORIA,BC V8X 4M6,CANADA. NR 80 TC 101 Z9 102 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1995 VL 110 IS 2 BP 477 EP 501 DI 10.1086/117536 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RL500 UT WOS:A1995RL50000002 ER PT J AU DELLANTONIO, IP GELLER, MJ FABRICANT, DG AF DELLANTONIO, IP GELLER, MJ FABRICANT, DG TI BARYON FRACTIONS FOR POOR CLUSTERS OF GALAXIES SO ASTRONOMICAL JOURNAL LA English DT Article ID ASTROPHYSICS REDSHIFT SURVEY; X-RAY; COMA CLUSTER; EINSTEIN; MASS AB We analyze x ray and optical data for six poor clusters of galaxies (MKW4, AWM4, AWM7, MKW4S, N79-299, and N67-336). For four of the systems, AWM4, AWM7, MKW4, and MKW4S, the x-ray emission is regular enough to measure the virial mass, gas mass, and temperature from the x-ray emission. We have obtained digitized plate scans for five of the poor clusters. We derive positions and photographic magnitudes for galaxies in a 30'x30' region around each group center (1.5 degrees x1.5 degrees for AWM7). From the x-ray surface brightness distribution, we construct models of the mass distribution. We use a modified V/V-max test [Avni & Bahcall, ApJ, 27, 446 (1980)] to test whether the galaxies trace the potential marked by the x-ray emitting gas. The galaxy distribution is consistent with the density distribution inferred from the x rays. The mass in galaxies is similar to 3h(-1)% of the total mass of the systems. The galaxies contribute significantly to the baryonic mass total. The ratio M(gas)/M(gal)similar to 1.4h(-1/2) similar to the value for rich clusters. The baryon fraction in rich groups is similar to 0.08 (for H-0=100), or about half that in rich clusters. This result has significant consequences for models of the formation of large-scale structure. (C) 1995 American Astronomical Society. RP DELLANTONIO, IP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 33 TC 30 Z9 30 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1995 VL 110 IS 2 BP 502 EP 512 DI 10.1086/117537 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RL500 UT WOS:A1995RL50000003 ER PT J AU PERELMUTER, JM BRODIE, JP HUCHRA, JP AF PERELMUTER, JM BRODIE, JP HUCHRA, JP TI KINEMATICS AND METALLICITY OF 25 GLOBULAR-CLUSTERS IN M81 SO ASTRONOMICAL JOURNAL LA English DT Article ID M31; SYSTEM; HALO; GALAXY; DISK; MASSES; SEARCH AB We have obtained spectra for 82 bright globular cluster candidates in the M81 field. We use the relative strengths of H delta, Ca I lambda 4227, and Fe I lambda 4045 absorption lines to distinguish stellar images of M81,globular clusters from stars in the Milky Way. We confirm 25 bona fide M81 globulars, 3 of which were previously detected by H. Harris, R. Schommer, and J. Huchra [cf. Brodie & Huchra, ApJ, 379, 157 (1991)]. The line-of-sight velocity dispersion, corrected for the observational error +/-50 km s(-1), is 152 km s(-1). The integrated mass of M81 derived by the projected mass method is M similar to 3.1+/-1.0x10(11) and thus M/L(BT)(0) similar to 19+/-6 M./L., within similar to 20 kpc. The above estimates assume an isotropic velocity ellipsoid and a spherical distribution of matter. The mean metallicity is [Fe/H]=-1.48+/-0.19. This value agrees well with the relation between the mean metallicity of a cluster system and the luminosity of the parent galaxy (BH). (C) 1995 American Astronomical Society. C1 UNIV CALIF SANTA CRUZ,UNIV CALIF OBSERV,LICK OBSERV,SANTA CRUZ,CA 95064. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP PERELMUTER, JM (reprint author), UNIV MONTREAL,DEPT PHYS,MONTREAL,PQ H3C 3J7,CANADA. NR 30 TC 42 Z9 43 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1995 VL 110 IS 2 BP 620 EP 627 DI 10.1086/117547 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RL500 UT WOS:A1995RL50000013 ER PT J AU SODERBLOM, DR JONES, BF STAUFFER, JR CHABOYER, B AF SODERBLOM, DR JONES, BF STAUFFER, JR CHABOYER, B TI EVOLUTION OF THE LITHIUM ABUNDANCES OF SOLAR-TYPE STARS .5. K-DWARFS IN THE HYADES SO ASTRONOMICAL JOURNAL LA English DT Article ID LOWER MAIN-SEQUENCE; LOW-MASS STARS; CHROMOSPHERIC EMISSION; ANGULAR-MOMENTUM; ROTATION; PLEIADES AB We have observed a dozen Hyades K dwarfs at high resolution and high signal to noise to see if they show a spread in their Li abundances like the spread seen among Pleiades K dwarfs. We cannot detect a Li feature in these stars, but we see no differences in their spectra at the Li 6708 Angstrom feature that exceed 2 m Angstrom. This suggests the Hyades K dwarfs lack the spread in Li seen in Pleiades K dwarfs, indicating a different history of Li depletion. (C) 1995 American Astronomical Society. C1 UNIV CALIF SANTA CRUZ,UNIV CALIF OBSERV,LICK OBSERV,SANTA CRUZ,CA 95064. UNIV CALIF SANTA CRUZ,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CANADIAN INST THEORET ASTROPHYS,TORONTO,ON M5S 1A7,CANADA. ASSOC UNIV RES ASTRON INC,NATL OPT ASTRON OBSERV,NATL SOLAR OBSERV,TUCSON,AZ 85726. RP SODERBLOM, DR (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. OI Chaboyer, Brian/0000-0003-3096-4161 NR 21 TC 31 Z9 31 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1995 VL 110 IS 2 BP 729 EP 732 DI 10.1086/117556 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RL500 UT WOS:A1995RL50000022 ER PT J AU LEVENSON, NA KIRSHNER, RP BLAIR, WP WINKLER, PF AF LEVENSON, NA KIRSHNER, RP BLAIR, WP WINKLER, PF TI ON THE PROPINQUITY OF SHOCK-EXCITED AND PHOTOIONIZED PLASMA - THE SUPERNOVA REMNANT AND THE H-II REGION OF N63A SO ASTRONOMICAL JOURNAL LA English DT Article ID LARGE MAGELLANIC CLOUD; NOVA REMNANTS; ABUNDANCE GRADIENTS; SOUTHERN GALAXIES; OPTICAL EMISSION; SPECTROPHOTOMETRY; SULFUR; M33 AB We present spectra covering the range lambda 3400-lambda 10100 of nebula N63A in the Large Magellanic Cloud. This object contains a supernova remnant adjacent to an H II region and thus illustrates vividly the optical and near-infrared differences between shock-ionized and photoionized emission nebulae. Species of low ionization potential, such as [S II] and [C I], predominate and emit strongly in the shock-heated region, while these elements are more highly ionized in the H II region. The gas-phase abundance of elements also affects their emission line strengths, and this depends on the particular excitation mechanism. A supernova shock can liberate calcium that is bound to interstellar grains, while photoionization does not reduce gas-phase depletion. In addition to providing a laboratory for comparison of the effects of shocks and photons on the interstellar medium, N63A is a bright object, which enables the measurement of lines that are typically too weak to observe elsewhere. In the shocked region we identify five lines of the IF multiplet of Cr II and measure lines of [Cl II] and [C I]. (C) 1995 American Astronomical Society. C1 ASSOC UNIV RES ASTRON INC,NATL OPT ASTRON OBSERV,CERRO TOLOLO INTER AMER OBSERV,TUCSON,AZ 85726. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. JOHNS HOPKINS UNIV,CTR ASTROPHYS SCI,BALTIMORE,MD 21218. MIDDLEBURY COLL,DEPT PHYS,MIDDLEBURY,VT 05753. NR 50 TC 27 Z9 27 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1995 VL 110 IS 2 BP 739 EP 746 DI 10.1086/117558 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RL500 UT WOS:A1995RL50000024 ER PT J AU RANDICH, S SCHMITT, JHMM PROSSER, CF STAUFFER, JR AF RANDICH, S SCHMITT, JHMM PROSSER, CF STAUFFER, JR TI AN X-RAY STUDY OF THE YOUNG OPEN CLUSTER IC-2602 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE OPEN CLUSTERS AND ASSOCIATIONS, INDIVIDUAL(IC 2602); STARS, CORONAE; X-RAY, STARS ID MAIN-SEQUENCE STARS; LOW-MASS STARS; T-TAURI STARS; DARK CLOUD; EINSTEIN OBSERVATIONS; PLEIADES CLUSTER; HYADES CLUSTER; ORION NEBULA; EMISSION; AGE AB We present the results of ROSAT PSPC observations of the 30 Myr old IC 2602 cluster; for the X-ray detected objects the results of a CCD photometric survey are also given. In X-rays, we detect a total of 110 objects within a 11 deg(2) area, above a threshold of typically 3-5 x 10(28) erg/sec. 68 of the detected objects have been identified with at least one optical counterpart; 44 of these are new optical candidates for cluster membership provided by our CCD photometry. Stars of all spectral types have been detected, from the very early-types to the late-M dwarfs. Soft X-ray luminosities range between about 10(29) erg/sec to a few 10(30) erg/sec, with the maximum and average L(x) decreasing with spectral type for B-V larger than similar to 0.8. Many of the stars redder than B-V similar to 0.8 show a L(X)/L(bol) ratio at about the saturation level of 10(-3). We construct X-ray luminosity distribution functions for objects in different color ranges and we compare them with those for the Pleiades. F, G, and early-K type candidates in IC 2602 appear to be more X-ray luminous than in the Pleiades, while no significant difference is seen among late-K and M dwarfs. Under the assumption that our IC 2602 sample is not severely affected by incompleteness, we argue that the above finding is related to the distribution of rotational velocities in the two clusters, with most of the late-type stars being fast rotators in both clusters, while, due to different spin-down timescales, the earlier type stars in IC 2602 are likely to rotate more rapidly than their counterparts in the Pleiades. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP RANDICH, S (reprint author), MAX PLANCK INST EXTRATERR PHYS, D-85740 GARCHING, GERMANY. NR 62 TC 89 Z9 89 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 1995 VL 300 IS 1 BP 134 EP 157 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RN774 UT WOS:A1995RN77400022 ER PT J AU HUTTEMEISTER, S WILSON, TL MAUERSBERGER, R LEMME, C DAHMEN, G HENKEL, C AF HUTTEMEISTER, S WILSON, TL MAUERSBERGER, R LEMME, C DAHMEN, G HENKEL, C TI A MULTILEVEL STUDY OF AMMONIA IN STAR-FORMING REGIONS .6. THE ENVELOPE OF SAGITTARIUS B2 (VOL 294, PG 667, 1995) SO ASTRONOMY & ASTROPHYSICS LA English DT Correction C1 MAX PLANCK INST RADIOASTRON, D-53121 BONN, GERMANY. RP HUTTEMEISTER, S (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 1 TC 2 Z9 2 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 1995 VL 300 IS 2 BP 636 EP 636 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RQ396 UT WOS:A1995RQ39600038 ER PT J AU THUM, C STRELNITSKI, VS MARTINPINTADO, J MATTHEWS, HE SMITH, HA AF THUM, C STRELNITSKI, VS MARTINPINTADO, J MATTHEWS, HE SMITH, HA TI HYDROGEN RECOMBINATION BETA-LINES IN MWC-349 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE STARS, CIRCUMSTELLAR MATTER; MASERS; STARS, MWC 349; RADIO LINES, STARS ID LEVEL POPULATIONS; MWC-349; EMISSION; MASER; STAR AB We have detected four beta-lines out of six observed in the frequency range from 100 to 400 GHz toward the radio star MWC 349A. The detected beta-lines have similar parameters as the pedestal features of the short mm alpha-lines and probably have the same origin in the ionized wind. We find that the flux ratios of beta- and alpha-line pedestals of nearly the same frequency are much smaller than expected from an optically thin plasma in LTE in all cases. We show with the help of simplified NLTE models of the recombination line emission that low beta/alpha-ratios are due to enhancement of the alpha-lines by stimulated emission. This is a natural consequence of the high free-free continuum opacity in the ionized wind ofMWC 349A. The models also predict that the beta/alpha-ratio is a sensitive probe of the electron density. For the 33 beta line emitting region the density thus derived is compatible with previous estimates, n(e) similar to 3 . 10(7) cm(-3), based on a model of the wind's continuum emission. The four newly detected beta-lines provide, together with the high frequency alpha-line pedestals, the most reliable value of the center velocity of the ionized outflow, upsilon(LSR) = 8 +/- 3 km s(-1) This value agrees well with the centroid velocity of the disk, upsilon(LSR) = 8.2 +/- .3 km s(-1), as derived from the velocities of the blue and red maser spikes, and thus represents the best estimate of the stellar velocity. H32 beta, at 366.6 GHz the highest frequency beta-line observed to date, displays on top of the pedestal two weak narrow emission features whose velocities and widths are in qualitative agreement with those of the alpha-line maser spikes. We tentatively interpret these H32 beta spikes as a weak disk maser whose estimated optical depth, \tau\ less than or equal to 1, confirms earlier estimates of the alpha-line maser gain (\tau\ similar or equal to 6). C1 SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, ASTROPHYS LAB, WASHINGTON, DC 20560 USA. CTR ASTRON YEBES, E-19080 GUADALAJARA, SPAIN. JOINT ASTRON CTR, HILO, HI 96720 USA. RP THUM, C (reprint author), INST RADIO ASTRON MILLIMETR, F-38406 ST MARTIN DHERES, FRANCE. RI Martin-Pintado, Jesus/H-6107-2015 OI Martin-Pintado, Jesus/0000-0003-4561-3508 NR 26 TC 16 Z9 16 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 1995 VL 300 IS 3 BP 843 EP 850 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RR439 UT WOS:A1995RR43900021 ER PT J AU SATYAPAL, S WATSON, DM PIPHER, JL FORREST, WJ COPPENBARGER, D RAINES, SN LIBONATE, S PICHE, F AF SATYAPAL, S WATSON, DM PIPHER, JL FORREST, WJ COPPENBARGER, D RAINES, SN LIBONATE, S PICHE, F TI HIGH-SPATIAL-RESOLUTION FABRY-PEROT IMAGING OF M82 - NEAR-INFRARED RECOMBINATION LINE OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (M82) GALAXIES, ISM; GALAXIES, NUCLEI; INFRARED, GALAXIES INFRARED, ISM, LINES AND BANDS ID INITIAL MASS FUNCTION; STARBURST GALAXIES; MOLECULAR GAS; H-I; EMISSION; NGC-7027; NEBULAE; REGION; IMAGES; STARS AB We present high spatial resolution (similar to 1 '') and moderate spectral resolution (gamma 2/Delta gamma similar or equal to 800) Pa beta and Br gamma Fabry-Perot imaging observations of the central kiloparsec of M82. These observations, in conjunction with new near-infrared broadband imaging observations, are used to examine the extinction toward the starburst region, the state of the ionized gas, and the nature of the stellar population. Enhancements in the extinction-sensitive Pa beta/Br gamma flux ratio are found to trace out the molecular lobes seen in CO, supporting the assumption that we are observing a dense torus surrounding the central stellar clusters and H II regions. Using a nonuniform foreground screen model for the Pa beta/Br gamma flux ratio, the derived extinction toward the starburst region is found to vary from A(V) similar or equal to 2 to A(V) similar or equal to 12 mag, significantly smaller than is adopted in most other studies of the stellar population in the starburst region of M82. The extinction-corrected K-magnitude in a 30 '' aperture centered on the nucleus is found to be M(K) = -22.0. This is substantially fainter than previous values adopted, amounting to as much as a reduction of a factor of similar to 3 in the intrinsic K luminosity, a difference that substantially weakens the arguments made previously for a low mass-deficient IMF for the starburst region of M82. Our recombination line images were used to estimate separately the contribution to the near-infrared continuum bandpasses from free-free and free-bound processes and the emission from dust. These sources of emission do not contribute appreciably to the total near-infrared continuum and thus it can confidently be assumed that this emission is dominated by starlight. In addition, we present narrow-band imaging observations of M82 in the 3.29 mu m unidentified dust feature. The emission is seen to be well-correlated with the Br gamma emission. The ratio of the extinction-corrected 3.29 mu m dust feature flux to extinction-corrected Br gamma flux is found to vary from 4.5 to 15 throughout most of the starburst region, with values greater than 35 near the dynamical center of the galaxy. This variation, along with other star formation diagnostics, suggests that the nucleus contains a later-type stellar population and the starburst phenomena is propagating outward. The ratio of the total far-infrared luminosity to the dereddened 3.29 mu m feature luminosity is found to be 1340 +/- 260 for M82, significantly smaller than the ratio obtained using the uncorrected 3.29 mu m feature flux (1690 +/- 200). C1 UNIV ROCHESTER, CEK MEES OBSERV, ROCHESTER, NY 14627 USA. SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, ASTROPHYS LAB, WASHINGTON, DC 20560 USA. USN, RES LAB, DIV REMOTE SENSING, WASHINGTON, DC 20375 USA. UNIV WYOMING, DEPT PHYS & ASTRON, LARAMIE, WY 82071 USA. UNIV WYOMING, WYOMING INFRARED OBSERV, LARAMIE, WY 82071 USA. RP SATYAPAL, S (reprint author), UNIV ROCHESTER, DEPT PHYS & ASTRON, ROCHESTER, NY 14627 USA. NR 40 TC 52 Z9 52 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1995 VL 448 IS 2 BP 611 EP 622 DI 10.1086/175990 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RK722 UT WOS:A1995RK72200014 ER PT J AU GOODMAN, AA JONES, TJ LADA, EA MYERS, PC AF GOODMAN, AA JONES, TJ LADA, EA MYERS, PC TI DOES NEAR-INFRARED POLARIMETRY REVEAL THE MAGNETIC-FIELD IN COLD DARK CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE DUST, EXTINCTION; INFRARED, ISM, CONTINUUM; ISM, CLOUDS; ISM, INDIVIDUAL (L1755); ISM, MAGNETIC FIELDS; POLARIZATION ID STELLAR LINEAR-POLARIZATION; WAVELENGTH DEPENDENCE; INTERSTELLAR POLARIZATION; OPTICAL POLARIZATION; MOLECULAR CLOUDS; ORION NEBULA; GRAINS; EXTINCTION; DUST; ALIGNMENT AB We present near-infrared (JHK) observations of the polarization of background starlight seen through the filamentary dark cloud L1755. The mean position angle and dispersion of the polarization vectors measured in the near-infrared, for stars along lines of sight passing through the densest portions (1 < A(V) < 10 mag) of L1755, are virtually identical to those in an optical polarization map of stars around the periphery (A(V) similar to 1 mag) of L1755. Furthermore, the percentage of polarization is not seen to increase, at all, with extinction in the near-infrared observations. We surmise that much of the dust in the dark cloud is extinguishing background starlight significantly, but not polarizing it efficiently, and thus that the polarization map of background starlight cannot reliably trace the magnetic field associated with the dense interior of the dark cloud. Our results in L1755 are remarkably similar to what we found in the dark cloud B216-217 (Goodman et al. 1992), which also shows no change in the polarization map associated with the cloud, and no rise in percentage polarization with extinction. Using our multiwavelength polarimetric observations of L1755, we have estimated the wavelength of maximum polarization, lambda(max), for most of the 53 stars in our sample. We find an unusually broad distribution of lambda(max), with a mean at 0.88 +/- 0.34 mu m. The large range of lambda(max) leads us to the hypothesis that there is a wide range of grain sizes and/or shapes along the lines of sight through L1755. We conclude that only a small subset of grains is responsible for producing the polarization of background starlight, and that these grains may be critically underrepresented in the dense interiors of cold dark. clouds. C1 UNIV MINNESOTA, SCH PHYS & ASTRON, MINNEAPOLIS, MN 55455 USA. UNIV MARYLAND, DEPT ASTRON, COLLEGE PK, MD 20742 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP GOODMAN, AA (reprint author), HARVARD UNIV, DEPT ASTRON, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 79 TC 117 Z9 117 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1995 VL 448 IS 2 BP 748 EP 765 DI 10.1086/176003 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RK722 UT WOS:A1995RK72200027 ER PT J AU GOMEZ, DO DELUCA, EE MCCLYMONT, AN AF GOMEZ, DO DELUCA, EE MCCLYMONT, AN TI NONLINEAR ENERGY-TRANSFER IN SOLAR MAGNETIC LOOPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE INSTABILITIES; MHD; SUN, CORONA; SUN, MAGNETIC FIELDS ID CORONA; FIELDS; DISSIPATION AB Active region coronal loops are widely believed to be heated by ohmic dissipation of field-aligned electric currents. These currents are driven by turbulent photospheric motions which twist and shear the magnetic footpoints of loops. Fine-scale structure in the corona is required in order to dissipate the currents rapidly enough to account for coronal heating. A long-standing controversy surrounds the question: is the fine-scale filamentation the result of magnetohydrodynamic (MI-ID) instabilities, or of dynamical nonequilibrium, or is it merely the direct product of the turbulent footpoint motions themselves? We present a simple model for the evolution of the coronal magnetic field, with no fine-scale structure in the imposed footpoint motions. The model consists of a three-mode truncation of the ''reduced'' MHD equations. One mode is driven by a stationary velocity held at the footpoints; the other two modes, of different spatial frequencies, are amplified through interaction with the driven mode. After approximately one photospheric turnover time, the coronal field loses equilibrium, and evolves rapidly to a new configuration, transferring energy to the two nondriven modes. The timescale of rapid nonequilibrium evolution is (tau(A),tau(p))(1/2), where tau(A) is the Alfven transit time along the loop and tau(p) is the photospheric turnover time. Regarding this simple model as a building block of a much more complex process, we see that dynamical nonequilibrium should be able to produce a cascade of free energy to fine spatial scales where it can be dissipated rapidly enough to account for coronal heating, as envisioned by Parker. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822. RP GOMEZ, DO (reprint author), UNIV BUENOS AIRES,FAC CIENCIAS EXACTAS & NAT,DEPT FIS,RA-1428 BUENOS AIRES,DF,ARGENTINA. RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Gomez, Daniel/0000-0002-4935-4358 NR 16 TC 7 Z9 7 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1995 VL 448 IS 2 BP 954 EP 962 DI 10.1086/176024 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RK722 UT WOS:A1995RK72200048 ER PT J AU GEHRZ, RD GREENHOUSE, MA HAYWARD, TL HOUCK, JR MASON, CG WOODWARD, CE AF GEHRZ, RD GREENHOUSE, MA HAYWARD, TL HOUCK, JR MASON, CG WOODWARD, CE TI THE INFRARED-SPECTRUM OF THE OPTICALLY THIN DUST SHELL OF V705-CASSIOPEIAE (NOVA-CASSIOPEIAE 1993) SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; DUST, EXTINCTION; INFRARED, STARS; STARS, INDIVIDUAL (V705 CASSIOPEIAE) ID HALLEY MONITORING PROGRAM; TEMPORAL DEVELOPMENT; EMISSION FEATURE; SILICATE GRAINS; COMET; PHOTOMETRY; GRAPHITE AB We report 1.25 to 18 mu m infrared photometry spectroscopy of the optically thin dust shell of V705 Cassiopeiae (Nova Cas 1993) between 330 and 418 days after the outburst. The measurements show that the dust shell, which had been optically thick until at least day approximate to 131, now shows the spectral signatures of optically thin astrophysical silicate grains at 10 and 20 mu m and hydrocarbons at 3.2-3.4 and 11.3 mu m. The 1-8 mu m continuum which is due to carbon dust is still present, although it no longer has a blackbody spectral energy distribution. We estimate mass of silicate grains required to produce the observed visual extinction and conclude that the condensible elements in the silicate grains may be overabundant with respect to hydrogen. C1 SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560. CORNELL UNIV,CTR RADIOPHYS & SPACE RES,ITHACA,NY 14853. UNIV WYOMING,DEPT PHYS & ASTRON,WYOMING INFRARED OBSERV,LARAMIE,WY 82071. RP GEHRZ, RD (reprint author), UNIV MINNESOTA,SCH PHYS & ASTRON,DEPT ASTRON,116 CHURCH ST SE,MINNEAPOLIS,MN 55455, USA. NR 37 TC 12 Z9 12 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1995 VL 448 IS 2 BP L119 EP L122 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RK720 UT WOS:A1995RK72000014 ER PT J AU HUGHES, JP BIRKINSHAW, A HUCHRA, JP AF HUGHES, JP BIRKINSHAW, A HUCHRA, JP TI A NEW X-RAY DISCOVERED CLUSTER OF GALAXIES ASSOCIATED WITH CL-0016+16 SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, OBSERVATIONS; GALAXIES, CLUSTERS, INDIVIDUAL (CL 00161+16, RX J0018.3+1618); LARGE-SCALE STRUCTURE OF UNIVERSE ID MULTICOLOR PHOTOMETRY; EXOSAT OBSERVATIONS; EVOLUTION; VELOCITY; DYNAMICS; UNIVERSE AB We have discovered a new cluster of galaxies, RX J0018.3+1618, in a deep ROSAT PSPC pointing toward the distant cluster CL 0016+16. The mean radial velocities of the new cluster (z = 0.5506) and CL 0016+16 (z = 0.5455) differ by 1000 +/- 390 km s(-1), which is comparable to their internal velocity dispersions. The angular separation of the clusters, 9'.5, corresponds to a projected linear distance of 4.2 Mpc. RX J0018.3+1618 has an X-ray luminosity in the 0.2-2 keV band of 1.3 X 10(44) ergs s(-1), which is about 10% of the luminosity of CL 0016+16. From the redshifts of seven galaxies in the new cluster, we derive a radial velocity dispersion of 540(-120)(+260) km s(-1), which establishes RX J0018.3+1618 as one of the most distant known poor clusters. Simple energetic arguments suggest that the two clusters constitute a bound system. This discovery adds considerable weight to the suggestion made by Koo in 1981 that CL 0016+16 is part of a massive large-scale structure at z similar to 0.55. C1 UNIV BRISTOL,DEPT PHYS,BRISTOL BS8 1TH,AVON,ENGLAND. RP HUGHES, JP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 23 TC 25 Z9 25 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1995 VL 448 IS 2 BP L93 EP L96 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RK720 UT WOS:A1995RK72000008 ER PT J AU HUCHRA, JP GELLER, MJ CORWIN, HG AF HUCHRA, JP GELLER, MJ CORWIN, HG TI THE CFA REDSHIFT SURVEY - DATA FOR THE NGP+36 ZONE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE GALAXIES, DISTANCES AND REDSHIFTS; GALAXIES, FUNDAMENTAL PARAMETERS; SURVEYS ID LARGE-SCALE STRUCTURE; GALAXY REDSHIFTS; LUMINOSITY FUNCTION; SPACE DISTRIBUTION; NEUTRAL HYDROGEN; CANCER CLUSTER; SURVEY SLICES; SKY SURVEY; DISPERSION; REGION AB We have assembled redshifts for a complete sample of 719 galaxies with m(ZW) less than or equal to 15.5 in the deciination range 32 degrees 5 less than or equal to delta less than or equal to 38 degrees 5 and right ascension range 8(h) less than or equal to alpha less than or equal to 17(h). We have determined morphological types for all galaxies in the magnitude limited sample by direct inspection of the POSS-O plates. 576 of the redshifts are measurements from Mount Hopkins, and 405 are new redshifts. We also include new redshifts for 77 fainter galaxies in the same strip. C1 CALTECH, IPAC, PASADENA, CA 91125 USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 87 TC 79 Z9 79 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 1995 VL 99 IS 2 BP 391 EP 403 DI 10.1086/192191 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RL641 UT WOS:A1995RL64100003 ER PT J AU STERNBERG, A DALGARNO, A AF STERNBERG, A DALGARNO, A TI CHEMISTRY IN DENSE PHOTON-DOMINATED REGIONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE GALAXIES, ISM; ISM, MOLECULES; MOLECULAR PROCESSES ID SPONTANEOUS RADIATIVE DISSOCIATION; CLUMPY PHOTODISSOCIATION REGIONS; PHOTOIONIZATION CROSS-SECTIONS; FINE-STRUCTURE EXCITATION; MOLECULAR-HYDROGEN GAS; INTERSTELLAR GAS; ULTRAVIOLET-RADIATION; STAR FORMATION; INFRARED RESPONSE; LINE EMISSION AB We present a detailed chemical model of a photon-dominated region produced in a dense molecular cloud exposed to an intense far-ultraviolet radiation field. We use it to illustrate the gas-phase processes that lead to the production of atomic and molecular species in the several distinct zones that occur in the cloud. We identify molecular diagnostics of photon-dominated chemistry in dense molecular clouds. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP STERNBERG, A (reprint author), TEL AVIV UNIV,SCH PHYS & ASTRON,IL-69978 RAMAT GAN,ISRAEL. NR 113 TC 347 Z9 347 U1 0 U2 11 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 1995 VL 99 IS 2 BP 565 EP 607 DI 10.1086/192198 PG 43 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RL641 UT WOS:A1995RL64100010 ER PT J AU JENNIONS, MD BISHOP, PJ BACKWELL, PRY PASSMORE, NI AF JENNIONS, MD BISHOP, PJ BACKWELL, PRY PASSMORE, NI TI CALL RATE VARIABILITY AND FEMALE CHOICE IN THE AFRICAN FROG, HYPEROLIUS-MARMORATUS SO BEHAVIOUR LA English DT Article ID NEOTROPICAL TREEFROG; MATE CHOICE; PHONOTAXIS; BEHAVIOR; SUCCESS; BIASES AB 1. Two-choice phonotaxis experiments were used to investigate female responses to short-term variation in call timing in the African painted reed frog, Hyperolius marmoratus. The number of calls produced per stimulus in each choice test were equalised over either 10 or 20 seconds. 2. All alternative stimuli were tested against a regular stimulus with an invariant inter-call interval (ICI = duration between the onset of successive calls). There were three categories of alternative call timing; bouts of rapid calling (short ICI) where the period of silence between bouts was shorter than the bouts of calling; bouts of rapid calling where the period of silence between bouts was longer than the bout of calling; and irregular calling (variable ICI) without prolonged periods of silence. 3. The only stimuli females discriminated against were rapid bouts of calling with prolonged periods of silence. Females showed significant differences in the number of responses when presented with two stimuli that differed in call timing over as short a period as 10 seconds. 4. We also calculated variability in the ICI of 25 males in the field. There was a significant negative relationship between mean call rate (calls/min) and variability in the ICI. Faster callers showed lower variability in ICI. 5. The phonotaxis experiments did not show a female preference for regular versus irregular call timing. So female mate choice of males with higher call rates in the field is not due to a preference for males with less variability in ICI. C1 UNIV WITWATERSRAND,DEPT ZOOL,JOHANNESBURG 2050,SOUTH AFRICA. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP JENNIONS, MD (reprint author), UNIV OXFORD,DEPT ZOOL,ABRG,S PARKS RD,OXFORD OX1 3PS,ENGLAND. RI Jennions, Michael/C-7560-2009; Backwell, Patricia/C-8883-2009 OI Jennions, Michael/0000-0001-9221-2788; NR 21 TC 6 Z9 7 U1 0 U2 4 PU E J BRILL PI LEIDEN PA PO BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0005-7959 J9 BEHAVIOUR JI Behaviour PD AUG PY 1995 VL 132 BP 709 EP 720 DI 10.1163/156853995X00108 PN 9-10 PG 12 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA RY897 UT WOS:A1995RY89700005 ER PT J AU ACUNA, HO FRANCIS, JM AF ACUNA, HO FRANCIS, JM TI SPRING AND SUMMER PREY OF THE JUAN-FERNANDEZ FUR-SEAL, ARCTOCEPHALUS-PHILIPPII SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article ID ZALOPHUS-CALIFORNIANUS; PHOCA-VITULINA; DIET; ISLAND; LIONS AB The composition of Juan Fernandez fur seal (Arctocephalus philippii) prey was assessed through analysis of 437 seats collected during five reproductive seasons (1987-1991). In total, 14 collections were analyzed and, based on 4172 fish otoliths and cephalopod beaks, 13 prey species were identified. The occurrences of fish families were as follows: Myctophidae (80.3%), Scomberesocidae (10%), Carangidae (9.5%), Engraulidae (1.0%), and Bathylagidae (0.7%). Cephalopod families included Onychoteuthidae (27.1%), Ommastrephidae (3.7%), and Tremoctopodidae (0.7%). In one year when data were available, Symbolophorus sp. B was found more frequently in subadult male and juvenile seats than in female seats (P < 0.004). Female seats contained larger numbers of the squid Onychoteuthis banksi than did subadult male and juvenile seats (P < 0.0001). When collections made in early December were compared, the occurrence of O. banksi in subadult male and juvenile seats differed significantly between years (P < 0.0001). Within-year variations in occurrence were significant only for O. banksi in 1989. The data suggest that the narrow range of species preyed upon by Juan Fernandez fur seals is unlikely to represent specialization, but is probably related to overall prey availability in the pelagic environment. Although information on marine communities in this area is limited, it is possible to relate observed prey shifts to variations in sea-surface temperature. C1 SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008. RP ACUNA, HO (reprint author), UNIV FLORIDA,DEPT ZOOL,POB 118525,GAINESVILLE,FL 32611, USA. NR 54 TC 11 Z9 12 U1 1 U2 1 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA ON K1A 0R6, CANADA SN 0008-4301 J9 CAN J ZOOL JI Can. J. Zool.-Rev. Can. Zool. PD AUG PY 1995 VL 73 IS 8 BP 1444 EP 1452 DI 10.1139/z95-170 PG 9 WC Zoology SC Zoology GA TE204 UT WOS:A1995TE20400008 ER PT J AU NAMI, HG AF NAMI, HG TI ARCHAEOLOGICAL RESEARCH IN THE ARGENTINEAN RIO-CHICO BASIN SO CURRENT ANTHROPOLOGY LA English DT Article RP NAMI, HG (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 37 TC 2 Z9 4 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0011-3204 J9 CURR ANTHROPOL JI Curr. Anthropol. PD AUG-OCT PY 1995 VL 36 IS 4 BP 661 EP 664 DI 10.1086/204413 PG 4 WC Anthropology SC Anthropology GA RT858 UT WOS:A1995RT85800009 ER PT J AU LIPSITCH, M HERRE, EA NOWAK, MA AF LIPSITCH, M HERRE, EA NOWAK, MA TI HOST POPULATION-STRUCTURE AND THE EVOLUTION OF VIRULENCE - A LAW-OF-DIMINISHING-RETURNS SO EVOLUTION LA English DT Article DE EVOLUTION; VIRULENCE; PARASITES; PATHOGENS; POPULATION STRUCTURE; PATHOGENICITY; TRANSMISSION ID PARASITE VIRULENCE; SELECTION; TRANSMISSION; COEVOLUTION; DYNAMICS; BENEVOLENCE; PATHOGENS; BACTERIA; BIOLOGY; VIRUSES AB Structure in a population of host individuals, whether spatial or temporal, can have important effects on the transmission and evolutionary dynamics of its pathogens. One of these is to limit dispersal of pathogens and thus increase the amount of contact between a given pair or within a small group of host individuals. We introduce a ''law of diminishing returns'' that predicts an evolutionary decline of pathogen virulence whenever there are on average more possibilities of pathogen transmission between the same pair of hosts. Thus, the effect of repeated contact between hosts will be to shift the balance of any trade-off between virulence and transmissibility toward lower virulence. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. UNIV OXFORD,DEPT ZOOL,OXFORD OX1 3PS,ENGLAND. RI Nowak, Martin/A-6977-2008; OI Lipsitch, Marc/0000-0003-1504-9213 NR 46 TC 61 Z9 62 U1 1 U2 16 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 SN 0014-3820 J9 EVOLUTION JI Evolution PD AUG PY 1995 VL 49 IS 4 BP 743 EP 748 DI 10.2307/2410327 PG 6 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA RZ504 UT WOS:A1995RZ50400016 ER PT J AU BARBOZA, PS AF BARBOZA, PS TI DIGESTA PASSAGE AND FUNCTIONAL-ANATOMY OF THE DIGESTIVE-TRACT IN THE DESERT TORTOISE (XEROBATES AGASSIZII) SO JOURNAL OF COMPARATIVE PHYSIOLOGY B-BIOCHEMICAL SYSTEMIC AND ENVIRONMENTAL PHYSIOLOGY LA English DT Article DE DIGESTION; FIBER; FERMENTATION; PARTICLE-SIZE; REPTILE; XEROBATES ID FATTY-ACID PRODUCTION; FRESH-WATER TURTLE; IGUANA-IGUANA; HINDGUT FERMENTATION; HERBIVOROUS LIZARDS; AEGYPTIUS AGAMIDAE; FIBER DIGESTION; WOMBATS; MARKERS; CONSEQUENCES AB The herbivorous tortoise Xerobates agassizii contends with large fluctuations in the duality and abundance of desert pastures. Responses to grass (Schismus barbatus), herbage (Sphaeralcea ambigua) and pelleted diets were studied in captive animals. Digestive anatomy was investigated in wild tortoises. Cornified esophageal epithelia and numerous mucus glands along the digestive tract indicated a resistance to abrasive diets. Gastric con tents were acidic whereas hindgut digesta were near neutral pH. The colon was the primary site of fermentation with short-chain fatty acids mainly comprised of acetate (69-84%), propionate (10-15%) and n-butyrate (1-12%). Fibre digestion was extensive and equivalent to 23-64% of digestible energy intakes. Large particles of grass (25 mm; Cr-mordants) were excreted as a pulse but retained longer than either fluids (Co-EDTA) or fine particles (2 mm; Yb). Patterns of marker excretion suggested irregular mixing of only the fluid and fine particulate digesta in the stomach and the colon. Mean retention times of Cr-mordants were 14.2-14.8 days on the grass and high-fibre pellets. Intakes of grass were low and accompanied by smaller estimates of digesta fill than for the high-fibre pellets. Digestive capacity was large and estimated at 11-21% of body mass on these diets. The capacious but simple digestive anatomy of the tortoise may provide the greatest flexibility in utilizing a variety of forages in its unreliable habitat. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. NR 53 TC 28 Z9 29 U1 1 U2 7 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0174-1578 J9 J COMP PHYSIOL B JI J. Comp. Physiol. B-Biochem. Syst. Environ. Physiol. PD AUG PY 1995 VL 165 IS 3 BP 193 EP 202 PG 10 WC Physiology; Zoology SC Physiology; Zoology GA RR505 UT WOS:A1995RR50500004 PM 7665734 ER PT J AU RALLS, K WHITE, PJ AF RALLS, K WHITE, PJ TI PREDATION ON SAN-JOAQUIN KIT FOXES BY LARGER CANIDS SO JOURNAL OF MAMMALOGY LA English DT Article DE CANIS LATRANS; VULPES MACROTIS MUTICA; COYOTE; KIT FOX; INTRAGUILD PREDATION ID VULPES-VULPES; RED FOXES; SPATIAL RELATIONSHIPS; ALOPEX-LAGOPUS; ARCTIC FOXES; COYOTES; WOLVES AB A better understanding of the relationships between endangered San Joaquin kit foxes (Vulpes macrotis mutica) and sympatric larger canids that prey on them is important for conservation efforts toward kit foxes. We used radiotelemetry to monitor the survival and cause of death of 41 San Joaquin kit foxes and 24 coyotes (Canis latrans) on the Carrizo Plain Natural Area, California, during the 1989-1991 drought. The estimated minimum-annual-survival rate for all coyotes was 0.88. Estimated annual-survival rates for juvenile foxes (0.21-0.41) were somewhat less than those for adult foxes (0.58-0.61). Survival rates for foxes were similar across years and sexes. Larger canids accounted for 78% of 23 verified deaths of kit foxes: 15 killed by coyotes; 2 by non-native red foxes (Vulpes vulpes); 1 by a domestic dog. High predation by larger canids, coupled with poor reproduction in kit foxes due to reduced prey availability during the drought, contributed to a significant decrease in density of kit foxes (from 0.24 to 0.12 foxes/km(2)) during the study. Although coyotes can have a significant impact on populations of kit foxes, larger non-native red foxes may pose a greater threat in some areas. C1 UNIV WISCONSIN,DEPT WILDLIFE ECOL,MADISON,WI 53706. RP RALLS, K (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 30 TC 102 Z9 102 U1 3 U2 20 PU AMER SOC MAMMALOGISTS PI PROVO PA BRIGHAM YOUNG UNIV, DEPT OF ZOOLOGY, PROVO, UT 84602 SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD AUG PY 1995 VL 76 IS 3 BP 723 EP 729 DI 10.2307/1382743 PG 7 WC Zoology SC Zoology GA RQ811 UT WOS:A1995RQ81100006 ER PT J AU CHANCE, KV PARK, K EVENSON, KM ZINK, LR STROH, F AF CHANCE, KV PARK, K EVENSON, KM ZINK, LR STROH, F TI FAR-INFRARED SPECTRUM OF HO2 SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article ID ASYMMETRIC-TOP MOLECULES; GROUND-STATE PARAMETERS; MICROWAVE-SPECTRUM; SPECTROSCOPY; MILLIMETER; SUBMILLIMETER; SPIN; DO2; OH; STRATOSPHERE AB We have measured the frequencies of 17 transitions in the far-infrared spectrum of the hydroperoxyl radical, HO2, from 2.5 to 5.9 THz, encompassing rotational levels up to N = 19 and K--1 = 5. These measured transition frequencies are combined with previously measured microwave and millimeter-wave transition frequencies in a complete reanalysis of the HO2 Hamiltonian for the ground vibrational state, including spin-rotation and nuclear hyperfine interactions. A revised set of molecular constants is presented. These include centrifugal distortion effects through octic dependence on the rotational angular momentum and the off-diagonal tenser component of the spin-spin dipolar interaction between the proton and the unpaired electron spin. (C) 1995 Academic Press, Inc. C1 UNIV OREGON, DEPT PHYS, EUGENE, OR 97403 USA. NATL INST STAND & TECHNOL, BOULDER, CO 80303 USA. NOAA, COOPERAT INST RES ENVIRONM SCI, BOULDER, CO 80303 USA. UNIV COLORADO, BOULDER, CO 80303 USA. FORSCHUNGSZENTRUM JULICH, FORSCHUNGSZENTRUM, INST STRATOSPHER CHEM, D-52425 JULICH, GERMANY. RP CHANCE, KV (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Stroh, Fred/A-6505-2009; OI Stroh, Fred/0000-0002-4492-2977; Chance, Kelly/0000-0002-7339-7577 NR 30 TC 14 Z9 14 U1 0 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD AUG PY 1995 VL 172 IS 2 BP 407 EP 420 DI 10.1006/jmsp.1995.1188 PG 14 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA RN476 UT WOS:A1995RN47600009 ER PT J AU KALFATOVIC, MR AF KALFATOVIC, MR TI SURREALISM IN EXILE AND THE BEGINNING OF THE NEW-YORK SCHOOL - SAWIN,M SO LIBRARY JOURNAL LA English DT Book Review RP KALFATOVIC, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD AUG PY 1995 VL 120 IS 13 BP 73 EP 73 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA RN627 UT WOS:A1995RN62700063 ER PT J AU TARR, CL AF TARR, CL TI PRIMERS FOR AMPLIFICATION AND DETERMINATION OF MITOCHONDRIAL CONTROL-REGION SEQUENCES IN OSCINE PASSERINES SO MOLECULAR ECOLOGY LA English DT Note DE CONTROL REGION; FRINGILLIDAE; MTDNA; PASSERINES; POLYMERASE CHAIN REACTION; PRIMERS C1 PENN STATE UNIV,DEPT BIOL,UNIVERSITY PK,PA 16802. RP TARR, CL (reprint author), SMITHSONIAN INST,NATL ZOOL PK,MOLEC GENET LAB,WASHINGTON,DC 20008, USA. NR 10 TC 89 Z9 91 U1 1 U2 12 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD AUG PY 1995 VL 4 IS 4 BP 527 EP 529 DI 10.1111/j.1365-294X.1995.tb00251.x PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA RU696 UT WOS:A1995RU69600019 PM 8574451 ER PT J AU ROBERTSON, DR AF ROBERTSON, DR TI COMPETITIVE ABILITY AND THE POTENTIAL FOR LOTTERIES AMONG TERRITORIAL REEF FISHES SO OECOLOGIA LA English DT Article DE CORAL REEF FISH; LOTTERY COEXISTENCE; COMPETITIVE ABILITY ID CORAL-REEF; COMMUNITY STRUCTURE; COEXISTENCE; RECRUITMENT; VARIABILITY; DAMSELFISH; SURGEONFISHES; POPULATION; AGGRESSION; SETTLEMENT AB Stegastes diencaeus and S. dorsopunicans are mutually territorial Caribbean damselfishes. S. diencaeus is larger, grows faster and fives longer than S. dorsopunicans. S. diencaeus is a habitat specialist that shares its primary habitat mainly with S. dorsopunicans. Field manipulations show that both S. diencaeus and S. dorsopunicans readily take over living space from smaller, but not larger, heterospecific neighbors. Natural changes in the use of living space by both species occur frequently and adult S. diencaeus often aggressively usurp the living areas of smaller S. dorsopunicans. Lunar and seasonal patterns of juvenile recruitment by S. diencaeus and S. dorsopunicans are similar. Large size bestows competitive superiority on S. diencaeus by giving its adults a superior ability to aggressively acquire living space, and by enabling its juveniles to quickly escape the period when they lack a size advantage. Hence they spend much of their lives as competitive dominants. There is no evidence that competitive advantages arising from large size are offset either by other adult attributes or by differences in temporal patterns of recruitment that affect priority of access to space. The lottery hypothesis for species coexistence relies on patterns of abundance being determined by patterns of recruitment to vacant space because different species have equal space-holding abilities. These data show that the existence of such a mechanism is doubtful. C1 SMITHSONIAN TROP RES INST, PANAMA CITY, FL USA. NR 55 TC 36 Z9 36 U1 1 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD AUG PY 1995 VL 103 IS 2 BP 180 EP 190 DI 10.1007/BF00329078 PG 11 WC Ecology SC Environmental Sciences & Ecology GA RN783 UT WOS:A1995RN78300007 PM 28306771 ER PT J AU WASHBURN, WE AF WASHBURN, WE TI RETAINED BY THE PEOPLE - HISTORY OF AMERICAN-INDIANS AND THE BILL-OF-RIGHTS - WUNDER,JR SO PACIFIC HISTORICAL REVIEW LA English DT Book Review RP WASHBURN, WE (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0030-8684 J9 PAC HIST REV JI Pac. Hist. Rev. PD AUG PY 1995 VL 64 IS 3 BP 438 EP 439 PG 2 WC History SC History GA RR282 UT WOS:A1995RR28200009 ER PT J AU JACOB, J GREITNER, C DRAKE, BG AF JACOB, J GREITNER, C DRAKE, BG TI ACCLIMATION OF PHOTOSYNTHESIS IN RELATION TO RUBISCO AND NONSTRUCTURAL CARBOHYDRATE CONTENTS AND IN-SITU CARBOXYLASE ACTIVITY IN SCIRPUS-OLNEYI GROWN AT ELEVATED CO2 IN THE FIELD SO PLANT CELL AND ENVIRONMENT LA English DT Article DE SCIRPUS OLNEYI; ACCLIMATION; CARBOXYLATION EFFICIENCY; ELEVATED CO2; PHOTOSYNTHESIS; RUBISCO, SOLUBLE PROTEINS; SOLUBLE SUGARS; STARCH ID CARBON-DIOXIDE CONCENTRATION; HIGH ATMOSPHERIC CO2; RIBULOSE-1,5-BISPHOSPHATE CARBOXYLASE; PLANTS; C-3; LEAVES; ACTIVATION; ENRICHMENT; RESPONSES; SUNFLOWER AB Stands of Scirpus olneyi, a native saltmarsh sedge with C-3 photosynthesis, had been exposed to normal ambient and elevated atmospheric CO2 concentrations (C-a) in their native habitat since 1987, The objective of this investigation was to characterize the acclimation of photosynthesis of Scirpus olneyi stems, the photosynthesizing organs of this species, to long-term elevated C-a treatment in relation to the concentrations of Rubisco and non-structural carbohydrates, Measurements were made on intact stems in the field under existing natural conditions and in the laboratory under controlled conditions on stems excised in the field early in the morning, Plants grown at elevated C-a had a significantly higher (30-59%) net CO2 assimilation rate (A) than those grown at ambient C-a when measurements were performed on excised stems at the respective growth C-a. However, when measurements were made at normal ambient C-a, A was smaller (45-53%) in plants grown at elevated C-a than in those grown at ambient C-a. The reductions in A at normal ambient C-a, carboxylation efficiency and in situ carboxylase activity were caused by a decreased Rubisco concentration (30-58%) in plants grown at elevated C-a; these plants also contained less soluble protein (39-52%). The Rubisco content was 43 to 58% of soluble protein, and this relationship was not significantly altered by the growth CO2 concentrations. The Rubisco activation state increased slightly, but the in situ carboxylase activity decreased substantially in plants grown at elevated C-a. When measurements were made on intact stems in the field, the elevated C-a treatment caused a greater stimulation of A (100%) and a smaller reduction in carboxylation efficiency (which was not statistically significant) than when measurements were made on excised stems in the laboratory. The possible reasons for this are discussed. Plants grown at elevated C-a contained more non-structural carbohydrates (25-53%) than those grown at ambient C-a. Plants grown at elevated C-a appear to have sufficient sink capacity to utilize the additional carbohydrates formed during photosynthesis. Overall, our results are in agreement with the hypothesis that elevated C-a leads to an increased carbohydrate concentration and the ensuing acclimation of the photosynthetic apparatus in C-3 plants results in a reduction in the protein complement, especially Rubisco, which reduces the photosynthetic capacity in plants grown at elevated C-a, relative to plants grown at normal ambient C-a. Nevertheless, when compared at their respective growth C-a, Scirpus olneyi plants grown at elevated C-a in their native habitat maintained a substantially higher rate of photosynthesis than those grown at normal ambient C-a even after 8 years of growth at elevated C-a. C1 SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. NR 40 TC 100 Z9 100 U1 1 U2 12 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0140-7791 J9 PLANT CELL ENVIRON JI Plant Cell Environ. PD AUG PY 1995 VL 18 IS 8 BP 875 EP 884 DI 10.1111/j.1365-3040.1995.tb00596.x PG 10 WC Plant Sciences SC Plant Sciences GA RN778 UT WOS:A1995RN77800005 ER PT J AU CHOI, HJ SOON, W DONAHUE, RA BALIUNAS, SL HENRY, GW AF CHOI, HJ SOON, W DONAHUE, RA BALIUNAS, SL HENRY, GW TI A STUDY OF VARIABILITY IN A SAMPLE OF G-GIANT AND K-GIANT SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID LOWER MAIN-SEQUENCE; EMISSION-LINE FLUXES; CA-II H; CHROMOSPHERIC ACTIVITY; STELLAR ROTATION; TIME VARIATIONS; COOL STARS; CONVECTION; BRAKING; SERIES AB Eight years of Ca II surface activity records from Mount Wilson Observatory measured for 12 bright G-K III stars have been analyzed in order to detect periodic variations attributable to rotation. We also present photometric V-band data for these stars from the Fairborn 0.25-m Automated Photometric Telescope (APT) that yielded a photometric period in one case and rms deviations from apparently constant brightness levels for the remaining 11 stars. The Ca II data yielded rotation periods for 10 out of 12 giant stars. We demonstrate that the photometric variability and nonvariability of these stars can be predicted from their Rossby numbers calculated from our observed rotation periods and convective turnover times scaled up from the main sequence. C1 CTR EXCELLENCE EDUC,RES SCI INST,MCLEAN,VA 22102. TENNESSEE STATE UNIV,CTR EXCELLENCE INFORMAT SYST,NASHVILLE,TN 37203. RP CHOI, HJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MCLEAN,VA 22102, USA. NR 31 TC 29 Z9 29 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD AUG PY 1995 VL 107 IS 714 BP 744 EP 750 DI 10.1086/133617 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RN590 UT WOS:A1995RN59000005 ER PT J AU KURTZ, MJ AF KURTZ, MJ TI GIANT SHOULDERS - DATA AND DISCOVERY IN ASTRONOMY SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID GALAXIES; SUPERCLUSTER; UNIVERSE AB A model is built to describe how,data and technology influence the process of discovery. A short example is given applying the model to a small project; then an extended discussion applies the model to the current state of redshift surveys. Finally the implications for data archives and information-retrieval systems are discussed. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI KURTZ, Michael /B-3890-2009 NR 66 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD AUG PY 1995 VL 107 IS 714 BP 776 EP 784 DI 10.1086/133623 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RN590 UT WOS:A1995RN59000011 ER PT J AU ERHARDT, D AF ERHARDT, D TI CORRESPONDENCE + REPLY TO PHENIX,ALAN AND STAVROUDIS,CHRIS CRITIQUES OF THE STUDY ON RESIN/BILE ACID SOAP INGREDIENTS SO STUDIES IN CONSERVATION LA English DT Letter RP ERHARDT, D (reprint author), SMITHSONIAN INST,MUSEUM SUPPORT CTR,CONSERVAT ANAL LAB,WASHINGTON,DC 20009, USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU INT INST CONSERVATION HISTORIC ARTISTIC WORKS PI LONDON PA 6 BUCKINGHAM ST, LONDON, ENGLAND WC2N 6BA SN 0039-3630 J9 STUD CONSERV JI Stud. Conserv. PD AUG PY 1995 VL 40 IS 3 BP 210 EP 211 PG 2 WC Archaeology; Art; Chemistry, Applied; Chemistry, Analytical; Spectroscopy SC Archaeology; Art; Chemistry; Spectroscopy GA RZ955 UT WOS:A1995RZ95500011 ER PT J AU BRANCO, LHZ SILVA, SMF SANTANNA, CL AF BRANCO, LHZ SILVA, SMF SANTANNA, CL TI VALIDATION OF THE NAME STICHOSIPHON MANGLE (CHROOCOCCALES, CYANOPHYTA) SO TAXON LA English DT Article AB The previously but not validly published name Stichosiphon mangle is validated by designation of a type. C1 UNIV NACL ESTADUAL SAO PAULO,IBILCE,DEPT BOT,BR-15001970 S JOSE RIO PR,SP,BRAZIL. INST BOT,SECAO FICOL,SAO PAULO,BRAZIL. RP BRANCO, LHZ (reprint author), SMITHSONIAN INST,MUSEUM NATL HIST NAT,DEPT BOT MRC166,WASHINGTON,DC 20560, USA. RI Branco, Luis Henrique/C-6756-2012 OI Branco, Luis Henrique/0000-0002-7226-4027 NR 1 TC 1 Z9 1 U1 0 U2 0 PU INT ASSN PLANT TAXONOMY PI BERLIN PA BOTANISCHER GARTEN & MUSEUM KONIGIN-LUISSE-STRASSE 6-8, W-1000 BERLIN, GERMANY SN 0040-0262 J9 TAXON JI Taxon PD AUG PY 1995 VL 44 IS 3 BP 393 EP 393 DI 10.2307/1223411 PG 1 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA RQ880 UT WOS:A1995RQ88000010 ER PT J AU JORDAN, TE CORRELL, DL WELLER, DE GOFF, NM AF JORDAN, TE CORRELL, DL WELLER, DE GOFF, NM TI TEMPORAL VARIATION IN PRECIPITATION CHEMISTRY ON THE SHORE OF THE CHESAPEAKE BAY SO WATER AIR AND SOIL POLLUTION LA English DT Article ID LONG-TERM TRENDS; ACID PRECIPITATION; ATMOSPHERIC DEPOSITION; UNITED-STATES; WATER-QUALITY; NEW-YORK; NITROGEN; ESTUARY; CHLOROPHYLL; NUTRIENTS AB We studied precipitation chemistry at the Rhode River on the western shore of the Chesapeake Bay. We sampled on an event basis, beginning in 1973 for some constituents in bulk precipitation. Beginning in 1981, we also sampled wet precipitation separately from bulk precipitation. In this report, we examine temporal variability of precipitation chemistry at different time scales. Several constituents showed long-term trends. In bulk precipitation, hydronium concentration increased by 27% of its mean concentration per decade, calcium by 67%, ammonium by 28%, and nitrate by 25%, while organic nitrogen decreased by 41%, organic phosphorus by 31%, and organic carbon by 16%. In wet precipitation, ammonium increased by 33% and calcium by 100%, while magnesium decreased by 78% per decade. Concentrations differed greatly among precipitation events, increasing as the volume of precipitation decreased and as the interval since the previous event increased. Most constituents also showed marked seasonal variation. We used a regression model to predict concentrations for each event from month, precipitation volume, and the time since the previous event. We evaluated how much of the interannual variability could be explained by these factors. The event-scale model accounted for almost half of the variability among annual means for ammonium, sodium, and magnesium in bulk precipitation, and for potassium in wet precipitation. This suggests that much of the interannual variability of concentrations may result from interannual variation in the temporal distribution of precipitation. RP JORDAN, TE (reprint author), SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037, USA. OI Weller, Donald/0000-0002-7629-5437 NR 46 TC 41 Z9 43 U1 1 U2 5 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0049-6979 J9 WATER AIR SOIL POLL JI Water Air Soil Pollut. PD AUG PY 1995 VL 83 IS 3-4 BP 263 EP 284 DI 10.1007/BF00477357 PG 22 WC Environmental Sciences; Meteorology & Atmospheric Sciences; Water Resources SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences; Water Resources GA RY462 UT WOS:A1995RY46200007 ER PT J AU FORMAN, P AF FORMAN, P TI TELLING THE TRUTH ABOUT HISTORY - APPLEBY,J, HUNT,L, JACOB,M SO SCIENCE LA English DT Book Review RP FORMAN, P (reprint author), SMITHSONIAN INST, WASHINGTON, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 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 JUL 28 PY 1995 VL 269 IS 5223 BP 565 EP 567 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RL495 UT WOS:A1995RL49500035 ER PT J AU FORMAN, P AF FORMAN, P TI RETHINKING OBJECTIVITY - MEGILL,A SO SCIENCE LA English DT Book Review RP FORMAN, P (reprint author), SMITHSONIAN INST, WASHINGTON, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 2 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 JUL 28 PY 1995 VL 269 IS 5223 BP 565 EP 567 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RL495 UT WOS:A1995RL49500034 ER PT J AU YOSHINO, K ESMOND, JR MURRAY, JE PARKINSON, WH THORNE, AP LEARNER, RCM COX, G AF YOSHINO, K ESMOND, JR MURRAY, JE PARKINSON, WH THORNE, AP LEARNER, RCM COX, G TI BAND OSCILLATOR-STRENGTHS OF THE HERZBERG-I BANDS OF O-2 SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID MOLECULAR-OXYGEN; SYSTEM AB Photoabsorption cross section measurements of the Herzberg I bands (A(3) Sigma(u)(+)-X(3) Sigma(g)(-)) of O-2 have been made by Fourier transform spectrometry with a resolution of 0.06 cm(-1) in the wavelength region 240-270 nm. Precise band oscillator strengths of the (4,0)-(11,0) bands are obtained by direct measurement, and for some of the strong bands; they are significantly higher than the previous experimental values. The rotational line strengths and the branching ratios are also presented for the same bands. The dissociation energy of O-2 is discussed. (C) 1995 American Institute of Physics. C1 UNIV LONDON IMPERIAL COLL SCI TECHNOL & MED,BLACKETT LAB,LONDON SW7 2BZ,ENGLAND. RP YOSHINO, K (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 19 TC 35 Z9 35 U1 0 U2 7 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 22 PY 1995 VL 103 IS 4 BP 1243 EP 1249 DI 10.1063/1.469800 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA RK378 UT WOS:A1995RK37800001 ER PT J AU RYAN, MJ RAND, AS AF RYAN, MJ RAND, AS TI FEMALE RESPONSES TO ANCESTRAL ADVERTISEMENT CALLS IN TUNGARA FROGS SO SCIENCE LA English DT Article ID MATE RECOGNITION; PHYLOGENETIC ANALYSES; ANIMAL COMMUNICATION; SPECIATION; DROSOPHILA; CHARACTERS; EVOLUTION; SIGNAL; MALES; TREE AB Phylogenetic techniques were used to estimate and reconstruct advertisement calls at ancestral nodes. These calls were used to investigate the degree of preference of female tungara frogs (Physalaemus pustulosus) for both extant and ancestral calls. Females did not discriminate between calls of males of their own species and calls at their most recent ancestral node. They also recognized calls of three extant species and at four ancestral nodes as the signals of appropriate mates. Both shared ancestral history, and call convergence might differentially influence call preferences. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP RYAN, MJ (reprint author), UNIV TEXAS,DEPT ZOOL,AUSTIN,TX 78712, USA. NR 22 TC 125 Z9 130 U1 0 U2 22 PU AMER ASSOC ADVAN SCIENCE PI WASHINGTON PA 1333 H ST NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD JUL 21 PY 1995 VL 269 IS 5222 BP 390 EP 392 DI 10.1126/science.269.5222.390 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RK427 UT WOS:A1995RK42700045 PM 17841263 ER PT J AU ESKRIDGE, PB FABBIANO, G KIM, DW AF ESKRIDGE, PB FABBIANO, G KIM, DW TI A MULTIPARAMETRIC ANALYSIS OF THE EINSTEIN SAMPLE OF EARLY-TYPE GALAXIES .3. COMPARISONS WITH THE KAPPA-PARAMETERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, ELLIPTIC AND LENTICULAR, CD; GALAXIES, ISM; X-RAYS, GALAXIES ID DYNAMICALLY HOT GALAXIES; ELLIPTICAL GALAXIES; X-RAY; ASTRONOMICAL DATA; STATISTICAL-ANALYSIS; UPPER LIMITS; METALLICITY; RADIO; INDICATOR; GRADIENTS AB We have extended our bivariate and multivariate statistical analysis of the Einstein sample of early-type galaxies (Fabbiano, Kim, and Trinchieri 1992; Eskridge, Fabbiano, and Rim 1995a, b) to include a consideration of the kappa-parameters defined by Bender, Burstein, and Faber (1992). The kappa-parameters are defined such that kappa(1) scales with virial mass, kappa(3) scales with inner M/L ratio, and kappa(2) is perpendicular to both kappa(1) and kappa(3). The kappa 1-kappa(3) plane is essentially edge-on to the Bender et al. (1992) formulation of the fundamental plane, and the parameter delta kappa(3) describes the scatter about that plane. We find that L(B), L(X), and L(6) are all strongly correlated with kappa(1) Partial Spearman rank analysis shows these trends to be independent of the correlations between the luminosities. There are also significant bivariate trends of both L(X) and L(6) with kappa(3). Partial Spearman rank analysis indicates that the L(X)-kappa(3), trend is the dominant one, thus arguing for a connection between the prominence of X-ray coronae and the inner M/L. This suggests that galaxies with central excesses of dark matter also have more massive extended dark matter halos, providing a mechanism for retaining larger amounts of hot interstellar medium. We find evidence for a correlation between Mg-2 and delta kappa(3) that is independent of correlations of these two parameters with sigma(v) and is enhanced when tested for constant alpha(4). The strengthening of the Mg-2-delta kappa(3) correlation when tested for contant alpha(4) indicates an underlying connection between the scatter about the fundamental plane and the Type II supernova enrichment history of the central regions of elliptical galaxies that is independent of the details of the central structure of individual galaxies. This suggests that the Mg-2-delta kappa(3) trend is not related to the Mg-2 enhancements associated with kinematically decoupled cores seen in some disky elliptical galaxies (e.g., Bender and Surma 1992). It may be that systems with higher inner M/L(e) (at a given mass) were more able to retain the metals generated in early epochs of star formation. Alternatively, systems experiencing more active or prolonged star formation may have produced an excess of baryonic dark matter from stellar remnants that is reflected in their higher M/L(e). C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CHUNGNAM NATL UNIV,DEPT ASTRON & SPACE SCI,CHUNGNAM,SOUTH KOREA. RP ESKRIDGE, PB (reprint author), UNIV ALABAMA,DEPT PHYS & ASTRON,TUSCALOOSA,AL 35487, USA. NR 34 TC 12 Z9 12 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 1995 VL 448 IS 1 BP 70 EP 83 DI 10.1086/175942 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RJ489 UT WOS:A1995RJ48900007 ER PT J AU HECKMAN, TM DAHLEM, M LEHNERT, MD FABBIANO, G GILMORE, D WALLER, WH AF HECKMAN, TM DAHLEM, M LEHNERT, MD FABBIANO, G GILMORE, D WALLER, WH TI AN X-RAY AND OPTICAL STUDY OF THE DWARF GALAXY NGC-1569 - EVIDENCE FOR A STARBURST-DRIVEN OUTFLOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, HALOS; GALAXIES, INDIVIDUAL (NGC 1569); GALAXIES, KINEMATICS AND DYNAMICS; GALAXIES, STARBURST; X-RAYS, GALAXIES ID ENHANCED GALACTIC WINDS; LOW-MASS GALAXIES; IRREGULAR GALAXIES; INTERSTELLAR-MEDIUM; STELLAR POPULATIONS; ELLIPTICAL GALAXIES; STAR FORMATION; VIRGO CLUSTER; EVOLUTION; NGC-1569 AB Supernova-driven outflows produced by intense bursts of star formation can drastically affect the structure and subsequent evolution of dwarf galaxies. Extensive mass loss from such systems may also provide an important source of chemical enrichment for the intergalactic medium. Despite the potential importance of these outflows, there is a very limited amount of direct observational evidence for their existence. One of the clearest signatures of a starburst-driven outflow is the X-ray emission from the hot gas that drives the outflow. We have therefore undertaken an X-ray imaging and optical spectroscopic investigation of the nearest and best-studied starbursting dwarf galaxy NGC 1569 using the HRI on ROSAT and the Ritchey-Chretien spectrograph on the KPNO 4 m telescope, respectively. We find that at least half the keV X-ray emission of NGC 1569 is associated with a diffuse halo that is some 3.'8 x 2.'2 similar to 2.4 x 1.5 kpc in size. Kiloparsec-scale ''spurs'' of diffuse X-ray emission extend outward along or near the optical minor axis of the galaxy. These diffuse X-ray spurs are morphologically associated with the well-known system of H alpha filaments. Previous kinematic studies have suggested that the H alpha filament system is a bipolar outflow. Our new optical spectroscopic data show that the H alpha emission comprises two kinematically distinct components: a quiescent system about 1 kpc in size responsible for about 75% of the H alpha emission and a fainter and more complex system over 2 kpc in size with radial velocities of as much as +/-200 km s(-1) relative to v(sys). The latter appears to define expanding hollow structures consisting of several kiloparsec-scale ''superbubbles.'' The dynamical age of the high-velocity system (similar to 10(7) yr) is similar to various estimates of the age of the starburst. We also see very broad wings (full width at zero intensity of 1400-2300 km s(-1)) on the H alpha emission-line profile at the location of super starcluster A, suggestive of recent supernova activity there. We argue that the starburst in NGC 1569 is driving an outflow of the interstellar medium on a global scale. Our simple models suggest that the X-ray emission is too bright to come primarily from the hot tenuous supernova-heated gas in the interior of a superbubble, unless this gas is evaporating or ablating cool dense material. This latter material may be the outer shell of the superbubble or interstellar clouds that have been engulfed by the superbubble. The high-velocity H alpha filaments probably correspond to the shocked and accelerated ambient material in the superbubble's outer walls, while the low-velocity material may be massive photoionized clouds in the starbursting galactic disk. The observed expansion speeds probably exceed the galactic escape velocity. It seems likely that the expanding material will ultimately ''blow out'' of the interstellar medium, and in so doing may allow most of the metals created by the starburst to escape from the galaxy. It is less clear whether the outflow will lead to the ejection of most or ah of this galaxy's interstellar medium, though it appears at least energetically feasible. We briefly discuss the significance of these results for ideas about the evolution of dwarf galaxies. C1 LAWRENCE LIVERMORE NATL LAB, INST GEOPHYS & PLANETARY PHYS, LIVERMORE, CA 94551 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. NASA, GODDARD SPACE FLIGHT CTR, ASTRON & SOLAR PHYS LAB, HUGHES STX CORP, GREENBELT, MD 20771 USA. RP HECKMAN, TM (reprint author), JOHNS HOPKINS UNIV, DEPT PHYS & ASTRON, BALTIMORE, MD 21218 USA. NR 100 TC 129 Z9 129 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 1995 VL 448 IS 1 BP 98 EP 118 DI 10.1086/175944 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RJ489 UT WOS:A1995RJ48900009 ER PT J AU FISHER, D FRANX, M ILLINGWORTH, G AF FISHER, D FRANX, M ILLINGWORTH, G TI LINE-STRENGTH GRADIENTS IN ELLIPTIC AND BRIGHTEST CLUSTER GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, ABUNDANCES; GALAXIES, ELLIPTIC AND LENTICULAR, CD; GALAXIES, STELLAR CONTENT ID OLD STELLAR POPULATIONS; VELOCITY DISPERSIONS; MAGNESIUM GRADIENTS; PHOTOMETRY; SPECTROSCOPY; M32; METALLICITIES; FEATURES; SPECTRA; MODELS AB Line strengths and their gradients in Mg, Fe, and H beta have been determined for seven elliptical and nine brightest cluster galaxies (BCGs) in order to study their stellar populations and investigate their relationship to one another. We find that BCGs follow the same relationship between central Mg b line strength and central velocity dispersion found for elliptical galaxies. Brightest cluster galaxies are in agreement with the known trend toward more massive elliptical galaxies having larger [Mg/Fe] ratios, while the internal gradients within our BCG and E galaxies are consistent with a roughly constant [Mg/Fe] ratio. We find that a correlation exists between the central [Mg/Fe] ratio and average H beta line strength in the sense that both BCG and elliptical galaxies with larger [Mg/Fe] ratios have lower [H beta] strengths. For our sample, H beta is the best predictor of [Mg/Fe] ratio. If the dominant contribution to the H beta feature is from turnoff stars then this relation predicts that more massive elliptical galaxies are older than less massive ones. If, however, the main source of the H beta index is from horizontal-branch stars, then the observed {[Mg/Fe],H beta} relation could be the result of more massive elliptical galaxies having flatter IMFs for high-mass stars than less massive elliptical galaxies. The [H beta] line strengths of the objects in our sample span a range of values. The BCGs generally have low global H beta line strengths, which, under the assumption that the H beta feature can be used as an age discriminant, indicates that the bulk of these systems underwent their last major episode of star formation greater than or similar to 8-10 Gyr ago. For both the elliptical galaxies and BCGs we find that within a galaxy, the H beta profile is flat for objects whose H beta absorption can be reliably measured. In the presence of a declining metallicity gradient this suggests that the centers of elliptical galaxies and BCGs are similar to 1-3 Gyr younger than their outer regions. The metal line strength gradients for the elliptical galaxies and BCGs are similar and consistent with an average gradient of Delta[Fe/H]/Delta log r = -0.25 +/- 0.1, corresponding to a reduction in the mean metallicity of the stellar population by a factor of similar to 2 over a factor of 10 in radius. No strong correlations are found between the metallicity gradient sizes and either kinematic or line strength parameters of the galaxies. For the galaxy NGC 4073, the brightest member of the poor cluster MKW 4, we find enhanced H beta absorption in the region coincident with the counterrotating stellar core. These observations are consistent with a scenario in which the accreted object was a younger system and/or a recent episode of star formation was triggered by an interaction. C1 UNIV CALIF SANTA CRUZ,UNIV CALIF OBSERV,LICK OBSERV,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP FISHER, D (reprint author), UNIV GRONINGEN,KAPTEYN ASTRON INST,POB 800,9700 AV GRONINGEN,NETHERLANDS. NR 61 TC 108 Z9 108 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 1995 VL 448 IS 1 BP 119 EP 137 DI 10.1086/175945 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RJ489 UT WOS:A1995RJ48900010 ER PT J AU DUBINSKI, J NARAYAN, R PHILLIPS, TG AF DUBINSKI, J NARAYAN, R PHILLIPS, TG TI TURBULENCE IN MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, CLOUDS; ISM, MOLECULES; TURBULENCE AB We generate random Gaussian turbulent velocity fields with a Kolmogorov spectrum and use these to obtain synthetic line-of-sight velocity profiles. The profiles are found to be similar to line profiles observed in molecular clouds. We suggest methods for analyzing measured line profiles to test whether they might arise from Gaussian Kolmogorov turbulence. C1 UNIV CALIF SANTA CRUZ,LICK OBSERV,SANTA CRUZ,CA 95064. CALTECH,DEPT PHYS,PASADENA,CA 91125. RP DUBINSKI, J (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 6 TC 58 Z9 58 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 1995 VL 448 IS 1 BP 226 EP 231 DI 10.1086/175954 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RJ489 UT WOS:A1995RJ48900019 ER PT J AU MENTEN, KM ALCOLEA, J AF MENTEN, KM ALCOLEA, J TI DETECTION OF AMMONIA EMISSION TOWARD OXYGEN-RICH EVOLVED STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; STARS, INDIVIDUAL (IK TAURI, IRC +10420, OH 231.8+4.2); STARS, LATE-TYPE; STARS, VARIABLES, OTHER (LONG-PERIOD VARIABLES) ID IRC + 10420; MASS-LOSS RATES; CIRCUMSTELLAR ENVELOPES; BEARING MOLECULES; HCN EMISSION; INTERSTELLAR AMMONIA; REFLECTION NEBULAE; VLA OBSERVATIONS; INFRARED STARS; OH-EMISSION AB Using the Effelsberg 100 m telescope, we have discovered emission in the (J, K)=(1, 1) and (2, 2) inversion transitions of ammonia (NH3) toward the circumstelIar envelopes of the Mira variable IK Tau and the OH/IR hypergiant IRC + 10420. Modeling our spectra, we find that [NH3/H-2] abundance ratios of a few times 10(-6) are required to explain the observational results. These values are of the same order as the ammonia abundances previously inferred from infrared absorption measurements toward oxygen-rich evolved stars. The high NH3 abundances implied by our observations present a challenge to models of circumstellar chemistry, which fall short of reproducing the observed values by several orders of magnitude. We also present high-quality spectra of the NH3 (1, 1), (2, 2), and (3, 3) lines toward the peculiar bipolar nebula OH 231.8+4.2, which is the only oxygen-rich (post-)AGB object with previously detected NH3 radio emission. Toward this source the (1, 1) profile looks strikingly different from the profiles of the (2, 2) and (3, 3) lines, which resemble each other closely. Similar to many millimeter-wavelength lines from other molecules, the NH3 (1, 1) line shows high-velocity emission. In contrast, the (2, 2) and (3, 3) lines have narrow line profiles that are quite different from profiles observed in spectra from any other molecule and arise from a warm (T-kin > 50 K) region dose to the central star. The high-velocity material dominating the (1, 1) spectrum is emitted from a cooler (less than or similar to 20 K), more extended region. C1 CTR ASTRON YEBES,IGN,E-19080 GUADALAJARA,SPAIN. RP MENTEN, KM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 49 TC 23 Z9 23 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 1995 VL 448 IS 1 BP 416 EP 425 DI 10.1086/175971 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RJ489 UT WOS:A1995RJ48900036 ER PT J AU DISTEFANO, R ESIN, AA AF DISTEFANO, R ESIN, AA TI BLENDING OF LIGHT IN GRAVITATIONAL MICROLENSING EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE DARK MATTER; GRAVITATIONAL LENSING; STARS, LOW-MASS, BROWN DWARFS ID OBJECTS; HALO AB When there is more than one source of light along the line of sight to a gravitationally lensed object, the characteristics of the observed light curve are influenced by the presence of the light that is not lensed. In this Letter we develop a formalism to quantify the associated effects. We find it useful to introduce the concept of a ''blended Einstein radius'' and an ''effective Einstein radius'' to describe the probability that a mass will serve as a lens or that a source will be lensed in an observable way. These considerations lead to generic predictions about the results of gravitational microlensing experiments. One example is that the optical depth for the lensing of giants is greater than that for the lensing of main-sequence stars; for any given population of sources and lenses, this effect can be quantified. We test and sharpen these predictions by performing a series of Monte Carlo simulations. We also outline general methods to (1) test whether specific events which fail to be fitted by point-mass light curves are viable candidates for blended events, (2) use the effects of blending to learn more about the lensing event than would be possible if there were no blending, and (3) include the effects of blending when inferring properties of underlying populations through the statistical study of lensing events. RP DISTEFANO, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 9 TC 41 Z9 41 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 1995 VL 448 IS 1 BP L1 EP L4 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RJ490 UT WOS:A1995RJ49000001 ER PT J AU JOHNSON, DG TRAUB, WA CHANCE, KV JUCKS, KW STACHNIK, RA AF JOHNSON, DG TRAUB, WA CHANCE, KV JUCKS, KW STACHNIK, RA TI ESTIMATING THE ABUNDANCE OF CLO FROM SIMULTANEOUS REMOTE-SENSING MEASUREMENTS OF HO2, OH, AND HOCL SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB Using a simple photochemical model we derive the mixing ratio profile of ClO in the altitude range 20-38 km from simultaneous measurements of HO2, OH, HOCl, temperature, pressure, and ozone. The measurements were made with the FIRS-2 far-infrared spectrometer during a balloon flight on September 29, 1992. We compare the derived ClO with the ClO profile obtained by the SLS instrument while flying on the same gondola. The good agreement between the two profiles validates our simple model and confirms the relevant rate constants and photolysis cross sections. C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. RP JOHNSON, DG (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Johnson, David/F-2376-2015; OI Johnson, David/0000-0003-4399-5653; Chance, Kelly/0000-0002-7339-7577 NR 9 TC 17 Z9 17 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 15 PY 1995 VL 22 IS 14 BP 1869 EP 1871 DI 10.1029/95GL01249 PG 3 WC Geosciences, Multidisciplinary SC Geology GA RK290 UT WOS:A1995RK29000008 ER PT J AU GROSSMANN, F HELLER, EJ AF GROSSMANN, F HELLER, EJ TI A SEMICLASSICAL CORRELATION-FUNCTION APPROACH TO BARRIER TUNNELING SO CHEMICAL PHYSICS LETTERS LA English DT Article ID S-MATRIX THEORY; DYNAMICS AB A time domain approach employing the semiclassical approximation to the quantum mechanical propagator, as applied to Gaussian wavepackets, is used to study the barrier penetration problem. We have observed that qualitative agreement with the exact quantum calculations for the correlation function and the transmission probability can be achieved by considering only classically allowed trajectories. The results slowly tend to the classical step function at the barrier top as a function of the wavepacket center parameter, however. We suggest that a full semiclassical calculation, including nonclassical trajectories with complex energies, would improve the results. C1 HARVARD UNIV,DEPT PHYS,CAMBRIDGE,MA 02138. HARVARD UNIV,HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RI Grossmann, Frank/A-1114-2012 NR 14 TC 79 Z9 79 U1 0 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD JUL 14 PY 1995 VL 241 IS 1-2 BP 45 EP 50 DI 10.1016/0009-2614(95)00605-4 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA RK762 UT WOS:A1995RK76200008 ER PT J AU COOKSY, AL TAO, FM KLEMPERER, W THADDEUS, P AF COOKSY, AL TAO, FM KLEMPERER, W THADDEUS, P TI STRUCTURES, ELECTRONIC-PROPERTIES, AND ISOMERIZATION OF THE HCCCO RADICAL SO JOURNAL OF PHYSICAL CHEMISTRY LA English DT Article ID MOLECULAR-ORBITAL METHODS; SPECTRUM AB The free radical HCCCO exhibits two distinct minima on the potential surface of the X(2)A' ground electronic state, corresponding to two favorable; nonequivalent canonical structures: propynonyl (acetylenic) and propadienonyl (cumulenic). The geometries at these minima and the isomerization coordinate that couples them are characterized by ab initio calculations at Hartree-Fock and configuration interaction (CISD and QCISD) levels. At the QCISD/6-311G** level, the propynonyl structure has parameters r(HCa) = 1.067 Angstrom, r(CaCb) = 1.213 Angstrom, r(CaCc) = 1.435 Angstrom, r(CcO) = 1.183 Angstrom, theta(HCC) = 176.9, theta(CCC) = 168.5 degrees, and theta(CCO) = 133.3 degrees. Coupled cluster [CCSD and CCSD(T)] calculations of the relative energies were carried out at the QCISD optimized geometries. The propynonyl structure is consistently found to be the most stable, in qualitative agreement with recent experiments [J. Chem. Phys. 1994, 101, 178]. At the highest level of theory used, the propadienonyl structure is predicted to lie 12.5 kJ mol(-1) higher in stabilization energy. The (2)A'' excited Renner-Teller state is found to be linear, with adiabatic and vertical stabilization energies of 25.6 and 165 kJ mol(-1), respectively, relative to the X(2)A' equilibrium structure. Discrepancies between the experimental geometry and predicted equilibrium geometry are tentatively ascribed to vibrational averaging on the extremely anharmonic bending potential surface. Predicted harmonic vibrational frequencies, permanent dipole moments, and Fermi contact terms are reported, with comparison to experimental results when possible. C1 HARVARD UNIV,DEPT CHEM,CAMBRIDGE,MA 02138. HARVARD UNIV,DIV APPL SCI,CAMBRIDGE,MA 02138. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP COOKSY, AL (reprint author), UNIV MISSISSIPPI,DEPT CHEM,UNIVERSITY,MS 38677, USA. NR 19 TC 14 Z9 14 U1 0 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA PO BOX 57136, WASHINGTON, DC 20037-0136 SN 0022-3654 J9 J PHYS CHEM-US JI J. Phys. Chem. PD JUL 13 PY 1995 VL 99 IS 28 BP 11095 EP 11100 DI 10.1021/j100028a009 PG 6 WC Chemistry, Physical SC Chemistry GA RK018 UT WOS:A1995RK01800009 ER PT J AU SARAZIN, CL BURNS, JO ROETTIGER, K MCNAMARA, BR AF SARAZIN, CL BURNS, JO ROETTIGER, K MCNAMARA, BR TI COMPARISON OF THE RADIO, OPTICAL, AND X-RAY STRUCTURES OF THE CD GALAXY IN ABELL-2597 SO ASTROPHYSICAL JOURNAL LA English DT Article DE COOLING FLOWS; GALAXIES, CLUSTERS, INDIVIDUAL (ABELL 2597); GALAXIES, ELLIPTIC AND LENTICULAR, CD; RADIO CONTINUUM, GALAXIES; X-RAYS, GALAXIES ID CLUSTER COOLING FLOWS; EMISSION-LINE NEBULAE; BL LACERTAE OBJECTS; ELECTRON-SCATTERING; INTRACLUSTER GAS; STAR FORMATION; CONSTRAINTS; REDSHIFT; ALIGNMENT; STABILITY AB We present new, high spatial resolution X-ray and radio observations of the cD galaxy in A2597. The X-ray observations confirm that this is a cooling flow with a cooling rate of r(cool) approximate to 327 M. yr(-1) within a radius of r(cool) approximate to 130 kPc The central X-ray emission is elongated parallel to the major axis of the cD galaxy. Our radio observations are the first to resolve the structure of the small, powerful radio source PKS 2322-122 associated with the central cD. The radio source consists of unresolved nuclear emission, a strongly bent radio jet to the southwest of the nucleus, and two diffuse lobes to the northeast and southwest of the nucleus. The radio source has a steep spectral index of alpha approximate to - 1.35 for the entire source and alpha approximate to -1.5 for the diffuse lobes. The minimum nonthermal pressures of the diffuse lobes are in very good agreement with the measured pressure of the ambient X-ray-emitting gas. The diffuse morphology of the radio lobes, their steep spectral indices, and the apparent pressure equilibrium with the ambient gas all indicate that the radio lobes are confined by the ambient hot gas. The radio jets emerge perpendicular to the elongation in the inner X-ray structure. We suggest that the X-ray-emitting gas forms an inflowing disk which feeds the radio source. The radio jet to the southeast is disrupted and turned through a large projected angle roughly 1 '' away from the nucleus. We suggest that the jet was bent either by ram pressure due to motions in the ambient thermal gas or due to a collision with a dense, massive cloud. Both of the radio lobes have been deflected in the same direction in which the jet is bent; this is more consistent with ram pressure from motions of the ambient gas. The cD galaxy in A2597 has two blue optical lobes located on either side of the nucleus (McNamara & O'Connell 1993), The radio observations show that the lobes cannot be due to synchrotron or inverse Compton emission. The lobes are aligned with the initial directions of the radio jet. This morphology and the brightness of the jets are in agreement with a model in which the lobes are scattered light from an anisotropically beamed nucleus. It is also possible that the lobes might be produced by stars formed recently by interactions of the radio jets with the ambient gas. C1 NEW MEXICO STATE UNIV,DEPT ASTRON,LAS CRUCES,NM 88003. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP SARAZIN, CL (reprint author), UNIV VIRGINIA,DEPT ASTRON,POB 3818,CHARLOTTESVILLE,VA 22903, USA. NR 52 TC 51 Z9 51 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1995 VL 447 IS 2 BP 559 EP 571 DI 10.1086/175899 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF788 UT WOS:A1995RF78800010 ER PT J AU FABBIANO, G SCHWEIZER, F AF FABBIANO, G SCHWEIZER, F TI ROSAT PSPC OBSERVATIONS OF 2 DYNAMICALLY YOUNG ELLIPTIC GALAXIES - NGC-4125 AND NGC-3610 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, ELLIPTIC AND LENTICULAR, CD; GALAXIES, INDIVIDUAL (NGC 3610, NGC 4125); GALAXIES, INTERACTIONS; X-RAYS ID X-RAY-SPECTRA; MOLECULAR GAS; INTERSTELLAR-MEDIUM; STARBURST GALAXIES; FINE-STRUCTURE; IRAS GALAXIES; EMISSION; RADIO; EVOLUTION; COLORS AB We present the results of ROSAT PSPC X-ray observations of NGC 4125 and NGC 3610. These two galaxies are among the best representatives of a newly recognized class of elliptical galaxies that may be the product of recent mergers, NGC 4125 shows two plumes or disks crossing at right angles; NGC 3610 has the richest fine structure of all elliptical galaxies cataloged by Schweizer and Seltzer. Our X-ray observations show that these galaxies do not retain large gaseous halos, contrary to the suggested link between merging and X-ray brightness. Their X-ray luminosities (0.1-2 keV) are in the range 10(40-41) ergs s(-1), low compared with those of hot gas-rich elliptical galaxies. The X-ray to optical ratio of NGC 3610 is in the range of those of X-ray faint elliptical galaxies, consistent with the value found for the bulge of M31, where the X-ray emission is dominated by low-mass binaries; its X-ray spectrum is also comparable with those of X-ray faint elliptical galaxies, presenting significant very soft excess emission. The X-ray to optical ratio of NGC 4125 is larger and might suggest the presence of some hot interstellar medium. This suggestion is supported by the spectrum of NGC 4125, which shows evidence of Fe L emission. This spectrum can be fitted with either a low-abundance single-temperature Raymond model or with a two-temperature model with solar abundances. Further work is needed to firmly resolve the question of gaseous versus stellar X-ray emission in NGC 4125. C1 CARNEGIE INST WASHINGTON,DEPT TERR MAGNETISM,WASHINGTON,DC 20015. RP FABBIANO, G (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 49 TC 37 Z9 37 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1995 VL 447 IS 2 BP 572 EP 581 DI 10.1086/175900 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF788 UT WOS:A1995RF78800011 ER PT J AU YUNGELSON, L LIVIO, M TUTUKOV, A KENYON, SJ AF YUNGELSON, L LIVIO, M TUTUKOV, A KENYON, SJ TI A MODEL FOR THE GALACTIC POPULATION OF SYMBIOTIC STABS WITH WHITE-DWARF ACCRETORS SO ASTROPHYSICAL JOURNAL LA English DT Review DE BINARIES, SYMBIOTIC; GALAXY, STELLAR CONTENT; NOVAE, CATACLYSMIC VARIABLES; STARS, STATISTICS; WHITE DWARFS ID COLLIDING WINDS; BINARY-SYSTEMS; I SUPERNOVAE; STABILITY ANALYSIS; PLANETARY-NEBULAE; MASS-DISTRIBUTION; DEGENERATE DWARF; GIANT BRANCH; INITIAL MASS; STARS AB By means of a population synthesis code, we investigate the formation of symbiotic systems in which the hot components are assumed to be white dwarfs which are either burning hydrogen steadily or are in a post-nova ''plateau'' phase, in the evolution of exploding white dwarfs. Our estimate for the total number of symbiotic systems in the Galaxy, similar to 3000-30,000 (depending on different model assumptions), is compatible with observational estimates. The crucial parameter for the determination of the birthrate and number of symbiotic stars is the mass of the hydrogen layer which the white dwarf can accumulate prior to hydrogen ignition. We model the distributions of symbiotic stars over orbital periods, masses of the components, mass-loss rates by the cool components, and brightness of components, and we obtain a reasonable agreement with observations. We show that in systems which are the most efficient in producing the symbiotic phenomenon, the accretors have to capture up to similar to 30% of the matter lost by the cool component via a stellar wind. If the fraction of captured matter is significantly lower, it becomes impossible to explain even the lowest observational estimates of the number of symbiotic stars. The theoretical estimate of the average rate of symbiotic novae is similar to 0.1 yr(-1), compatible with the observed one. The apparent normal chemical composition of symbiotic novae can be explained if the white dwarfs in these systems, which have systematically lower masses than in cataclysmic binaries, manage to preserve ''buffer'' helium layers between their CO cores and the accreted hydrogen envelopes. Mass exchange in symbiotic systems does not lead to SN Ia's via the accumulation of a Chandrasekhar mass. However, if sub-Chandrasekhar-mass, double-detonation models indeed produce SN Ia's, then symbiotic systems can be the progenitors of less than or similar to 1/3 of the events. According to the model, SN Ia's in symbiotic binaries belong to young and intermediate-age populations (t less than or similar to 6 x 10(9) yr). C1 SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 129 TC 103 Z9 103 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1995 VL 447 IS 2 BP 656 EP 679 DI 10.1086/175908 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF788 UT WOS:A1995RF78800019 ER PT J AU MAOZ, E AF MAOZ, E TI A STRINGENT CONSTRAINT ON ALTERNATIVES TO A MASSIVE BLACK-HOLE AT THE CENTER OF NGC-4258 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; GALAXIES, INDIVIDUAL (NGC 4258); GALAXIES, NUCLEI; MASERS ID RANDOM GRAVITATIONAL ENCOUNTERS; SPHERICAL SYSTEMS; EVOLUTION; GALAXY; M31 AB There is now dynamical evidence for massive dark objects at the center of several galaxies, but suggestions that these are supermassive black holes are based only on indirect astrophysical arguments. As emphasized by Kormendy and Richstone, large M/L ratios and gas motions of order approximate to 10(3) km s(-1) do not uniquely imply a massive black hole (BH), and it is possible that the central dark objects in these galaxies are massive clusters of stellar remnants, brown dwarfs, low-mass stars, or halo dark matter. The recent unprecedented measurement of the rotation curve of maser emission sources at the center of NGC 4258, and the remarkable discovery that it is Keplerian to high precision, provide us with a unique opportunity for testing alternatives to a BH. We use a conservative upper limit on the systematic deviation from a Keplerian rotation curve to constrain the mass distribution at the galaxy center. Based on evaporation and physical collision timescale arguments, we show that a central cluster is firmly ruled out, unless the cluster consists of extremely dense objects with mass less than or similar to 0.03 M. (e.g., low-mass BHs or elementary particles). Since both of these dynamically allowed systems are very improbable for other astrophysical reasons, we conclude that a central dense cluster at the center of NGC 4258 is very improbable, thus leaving the alternative possibility of a massive BH. We also show that the mass of the BH must be greater than or similar to 98% of the mass enclosed within the inner edge of the masering disk (3.6 x 10(7) M.). A substantial contribution to that mass from a density cusp in the background mass distribution is excluded. RP MAOZ, E (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MS 51,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 19 TC 74 Z9 75 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 1995 VL 447 IS 2 BP L91 EP L94 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF790 UT WOS:A1995RF79000008 ER PT J AU PRADHAN, AD KIRBY, KP DALGARNO, A AF PRADHAN, AD KIRBY, KP DALGARNO, A TI THEORETICAL-STUDY OF HCL+ - POTENTIAL CURVES, RADIATIVE LIFETIMES, AND PHOTODISSOCIATION CROSS-SECTIONS (VOL 95, PG 9009, 1991) SO JOURNAL OF CHEMICAL PHYSICS LA English DT Correction, Addition C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP PRADHAN, AD (reprint author), NASA,AMES RES CTR,MS 230-3,MOFFETT FIELD,CA 94035, USA. NR 1 TC 2 Z9 2 U1 1 U2 6 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 8 PY 1995 VL 103 IS 2 BP 864 EP 864 DI 10.1063/1.470739 PG 1 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA RH105 UT WOS:A1995RH10500040 ER PT J AU BERTULANI, CA CANTO, LF HUSSEIN, MS AF BERTULANI, CA CANTO, LF HUSSEIN, MS TI A COUPLED-CHANNELS STUDY OF BE-11 COULOMB-EXCITATION SO PHYSICS LETTERS B LA English DT Article AB We study the effects of channel coupling in the excitation of Be-11 projectiles incident on heavy targets. The contribution to the excitation from the Coulomb and the nuclear fields in peripheral collisions are considered. Our results are compared with recent data on the excitation of the 1/2(-) state in Be-11 projectiles. We show that the experimental results cannot be explained, unless very unusual parameters are used. C1 MIT,CTR THEORET PHYS,NUCL SCI LAB,CAMBRIDGE,MA 02139. MIT,DEPT PHYS,CAMBRIDGE,MA 02139. HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. UNIV SAO PAULO,INST FIS,BR-01498 SAO PAULO,BRAZIL. RP BERTULANI, CA (reprint author), FED UNIV RIO DE JANEIRO,INST FIS,CX POSTAL 68528,BR-21945970 RIO JANEIRO,RJ,BRAZIL. RI Canto, Luiz /I-3733-2012 NR 11 TC 28 Z9 28 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-2693 J9 PHYS LETT B JI Phys. Lett. B PD JUL 6 PY 1995 VL 353 IS 4 BP 413 EP 416 DI 10.1016/0370-2693(95)00595-C PG 4 WC Astronomy & Astrophysics; Physics, Nuclear; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA RJ453 UT WOS:A1995RJ45300001 ER PT J AU BIDDLE, W AF BIDDLE, W TI OLD BOY NETWORK - RALLY ROUND THE B-2 SO NATION LA English DT Article AB Congress is seeking to stuff some $533 million into the FY96 defense budget in order to keep open the production line for B-2 Stealth bombers, which the Pentagon concluded were superfluous in a major study this spring. The following letter, dated January 4, was sent to President Clinton by seven former Defense Secretaries urging the government to buy more of these planes. It was released by the alexis de Tocqueville Institution's Committee for the Common Defense, a Virginia-based lobby founded and chaired by former Republican Representative Jim Courter of New Jersey, which promotes government funding of the weapons business. I have supplied annotations of interest to taxpayers. RP BIDDLE, W (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATION CO INC PI NEW YORK PA 72 FIFTH AVE, NEW YORK, NY 10011 SN 0027-8378 J9 NATION JI Nation PD JUL 3 PY 1995 VL 261 IS 1 BP 19 EP 19 PG 1 WC Political Science SC Government & Law GA RD870 UT WOS:A1995RD87000013 ER PT J AU BARBER, JG AF BARBER, JG TI WHOS WHO + HOW TO DETERMINE WHETHER A PICTURE IS AUTHENTIC AND WHY THAT AUTHENTICITY MATTERS IN THE STUDY OF HISTORIC PORTRAITS SO AMERICAN HERITAGE LA English DT Article RP BARBER, JG (reprint author), SMITHSONIAN INST,NATL PORTRAIT GALLERY,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER HERITAGE SUBSCRIPTION DEPT PI NEW YORK PA FORBES BUILDING 60 FIFTH AVE, NEW YORK, NY 10011 SN 0002-8738 J9 AM HERITAGE JI Am. Herit. PD JUL-AUG PY 1995 VL 46 IS 4 BP 76 EP & PG 0 WC History SC History GA RC748 UT WOS:A1995RC74800016 ER PT J AU DAI, YS POST, JE AF DAI, YS POST, JE TI CRYSTAL-STRUCTURE OF HILLEBRANDITE - A NATURAL ANALOG OF CALCIUM SILICATE HYDRATE (CSH) PHASES IN PORTLAND-CEMENT SO AMERICAN MINERALOGIST LA English DT Article ID GEL; TOBERMORITE AB The crystal structure of hillebrandite, Ca2SiO3(OH)(2), was solved and refined in space group Cmc2(1), a = 3.6389, b = 16.311, c = 11.829 Angstrom, to R = 0.041 using single-crystal X-ray data. The structure consists of a three-dimensional network of Ca-O polyhedra that accommodates wollastonite-type Si-O tetrahedral chains. Each of the wollastonite-type chains is an average of two symmetrically equivalent chains related by the mirror plane perpendicular to a. In a given structural channel of the Ca-O polyhedral network, only one chain orientation can be occupied to give reasonable Si-O distances. The O3 and O4 sites corresponding to each vacant Si2 site are occupied by OH groups to achieve charge balance. The wollastonite-type Si-O tetrahedral chains in the hillebrandite structure resemble those reported for many calcium silicate hydrate (CSH) phases. C1 SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560. RP DAI, YS (reprint author), HARBISON WALKER REFRACTORIES,GARBER RES CTR,1001 PITTSBURGH MCKEESPORT BLVD,W MIFFILIN,PA 15122, USA. NR 16 TC 26 Z9 27 U1 0 U2 4 PU MINERALOGICAL SOC AMER PI WASHINGTON PA 1130 17TH ST NW SUITE 330, WASHINGTON, DC 20036 SN 0003-004X J9 AM MINERAL JI Am. Miner. PD JUL-AUG PY 1995 VL 80 IS 7-8 BP 841 EP 844 PG 4 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA RN609 UT WOS:A1995RN60900020 ER PT J AU CRONE, MM GELLER, MJ AF CRONE, MM GELLER, MJ TI RECENT EVOLUTION IN CLUSTER VELOCITY DISPERSIONS SO ASTRONOMICAL JOURNAL LA English DT Article ID COLD DARK MATTER; GAUSSIAN FLUCTUATIONS; GALAXY CLUSTERS; RICH CLUSTERS; UNIVERSE; DISTANT; AMPLITUDE; CATALOG C1 UNIV MICHIGAN,DEPT PHYS,ANN ARBOR,MI 48109. RP CRONE, MM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 42 TC 23 Z9 23 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 1995 VL 110 IS 1 BP 21 EP 31 DI 10.1086/117494 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RE741 UT WOS:A1995RE74100002 ER PT J AU BLAIR, WP VANCURA, O LONG, KS AF BLAIR, WP VANCURA, O LONG, KS TI VOYAGER-2 UVS SPECTRA OF THE VELA SUPERNOVA REMNANT SO ASTRONOMICAL JOURNAL LA English DT Article ID HOPKINS-ULTRAVIOLET-TELESCOPE; CYGNUS LOOP; EINSTEIN OBSERVATIONS; FAR-ULTRAVIOLET; ABSORPTION-LINES; NOVA REMNANT; EMITTING GAS; SHOCK-WAVE; EMISSION; SPECTROMETER C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. NR 39 TC 14 Z9 14 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 1995 VL 110 IS 1 BP 312 EP 317 DI 10.1086/117521 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RE741 UT WOS:A1995RE74100029 ER PT J AU GEHRZ, RD JONES, TJ MATTHEWS, K NEUGEBAUER, G WOODWARD, CE HAYWARD, TL GREENHOUSE, MA AF GEHRZ, RD JONES, TJ MATTHEWS, K NEUGEBAUER, G WOODWARD, CE HAYWARD, TL GREENHOUSE, MA TI THE NEON NOVA .3. THE INFRARED LIGHT CURVES OF NOVA QU VULPECULAE (NOVA-VUL 1984 NUMBER-2) SO ASTRONOMICAL JOURNAL LA English DT Article ID CLASSICAL NOVAE; CORONAL LINES; AQUILAE 1982; CYGNI 1975; EMISSION; DUST; SPECTROSCOPY; CONDENSATION; PHOTOMETRY; SPECTRUM C1 CALTECH, PALOMAR OBSERV, PASADENA, CA 91125 USA. UNIV WYOMING, WYOMING INFRARED OBSERV, DEPT PHYS & ASTRON, LARAMIE, WY 82071 USA. CORNELL UNIV, CTR RADIOPHYS & SPACE RES, ITHACA, NY 14853 USA. SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, ASTROPHYS LAB, WASHINGTON, DC 20260 USA. RP UNIV MINNESOTA, SCH PHYS & ASTRON, DEPT ASTRON, 116 CHURCH ST SE, MINNEAPOLIS, MN 55455 USA. NR 48 TC 10 Z9 10 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUL PY 1995 VL 110 IS 1 BP 325 EP 335 DI 10.1086/117523 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RE741 UT WOS:A1995RE74100031 ER PT J AU KENYON, SJ MIKOLAJEWSKA, J AF KENYON, SJ MIKOLAJEWSKA, J TI SPECTROSCOPIC ORBITS FOR SYMBIOTIC BINARIES .3. ECLIPSES OF THE HOT COMPONENT IN RW HYDRAE SO ASTRONOMICAL JOURNAL LA English DT Article ID INHOMOGENEOUS-MEDIUM; HM-SGE; STARS; EMISSION; WINDS; LINES; ACCRETION; COLLISION; SPECTRA; CYGNI C1 NICHOLAS COPERNICUS ASTRON CTR,PL-00716 WARSAW,POLAND. RP KENYON, SJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 66 TC 20 Z9 20 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 1995 VL 110 IS 1 BP 391 EP 397 DI 10.1086/117529 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RE741 UT WOS:A1995RE74100037 ER PT J AU DUPREE, AK SMITH, GH AF DUPREE, AK SMITH, GH TI SPECTROSCOPY OF THE CA-II LINE IN METAL-POOR FIELD RED GIANTS .2. NORTHERN-HEMISPHERE OBSERVATIONS SO ASTRONOMICAL JOURNAL LA English DT Article ID H-ALPHA EMISSION; SOLAR-TYPE STARS; MAGNETIC-STRUCTURE; COOL STARS; MASS-LOSS; CHROMOSPHERIC ACTIVITY; STELLAR CHROMOSPHERES; K-LINE; EVOLUTION; PROFILES C1 UNIV CALIF OBSERV,LICK OBSERV,SANTA CRUZ,CA 95064. RP DUPREE, AK (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 76 TC 32 Z9 32 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 1995 VL 110 IS 1 BP 405 EP 419 DI 10.1086/117531 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RE741 UT WOS:A1995RE74100039 ER PT J AU GANGUI, A PERIVOLAROPOULOS, L AF GANGUI, A PERIVOLAROPOULOS, L TI COSMIC STRINGS AND COSMIC VARIANCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMIC MICROWAVE BACKGROUND; COSMIC STRINGS; COSMOLOGY, THEORY; LARGE-SCALE STRUCTURE OF UNIVERSE ID MICROWAVE BACKGROUND FLUCTUATIONS; LARGE-SCALE STRUCTURE; NUMERICAL-SIMULATION; PECULIAR VELOCITIES; EVOLUTION; RADIATION; WAKES; COBE; ANISOTROPIES; STATISTICS AB By using a simple analytical model based on counting random multiple impulses inflicted on photons by a network of cosmic strings we show how to construct the general q-point temperature correlation function of the cosmic microwave background radiation. Our analysis is especially sensible for large angular scales where the Kaiser-Stebbins effect is dominant. Then we concentrate on the four-point function and, in particular, on its zero-lag limit, namely, the excess kurtosis parameter, for which we obtain a predicted value of similar to 10(-2). In addition, we estimate the cosmic variance for the kurtosis due to a Gaussian fluctuation field, showing its dependence on the primordial spectral index of density fluctuations n and finding agreement with previous published results for the particular case of a flat Harrison-Zel'dovich spectrum. Our value for the kurtosis compares well with previous analyses but falls below the threshold imposed by the cosmic variance when commonly accepted parameters from string simulations are considered. In particular the non-Gaussian signal is found to be inversely proportional to the scaling number of defects, as could be expected by the central limit theorem. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,DIV THEORET ASTROPHYS,CAMBRIDGE,MA 02138. RP GANGUI, A (reprint author), SISSA,SCH ADV INT STUDIES,VIA BEIRUT 2-4,I-34013 TRIESTE,ITALY. NR 51 TC 9 Z9 9 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1995 VL 447 IS 1 BP 1 EP 7 DI 10.1086/175851 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF079 UT WOS:A1995RF07900001 ER PT J AU MOHR, JJ EVRARD, AE FABRICANT, DG GELLER, MJ AF MOHR, JJ EVRARD, AE FABRICANT, DG GELLER, MJ TI COSMOLOGICAL CONSTRAINTS FROM OBSERVED CLUSTER X-RAY MORPHOLOGIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, THEORY; GALAXIES, CLUSTERS, GENERAL; METHODS, NUMERICAL; X-RAYS, GALAXIES ID FLUX-LIMITED SAMPLE; ABELL CLUSTERS; RICH CLUSTERS; COOLING FLOWS; N-BODY; GALAXIES; EINSTEIN; DYNAMICS; SUBSTRUCTURE; FLUCTUATIONS AB We use a representative sample of 65 galaxy dusters observed with the Einstein IPC to constrain the range of cluster X-ray morphologies. We develop and apply quantitative and reproducible measures of cluster X-ray morphologies to constrain the intrinsic distributions of (1) emission-weighted centroid variation w(x), (2) emission-weighted axial ratio eta, (3) emission-weighted orientation theta(0), and (4) measures of the radial falloff, cr and beta. For each cluster we use a Monte Carlo procedure to determine the effects of Poisson noise, detector imperfections, and foreground/background X-ray point sources. We then use the range of cluster X-ray morphologies to constrain three generic cosmological models (Omega = 1, Omega(0) = 0.2, and Omega(0) = 0.2 and lambda(0) = 0.8). For each of these models, we evolve eight sets of Gaussian random initial conditions consistent with an effective power spectrum P(k) proportional to k(-1) on cluster scales. Using this sample of 24 numerical cluster simulations which include gravity and gas physics (but no cooling or ejection from galaxies), we compare the X-ray morphologies of the observed and simulated clusters. Specifically, we build artificial ensembles with the same distributions in the number of cluster photons, X-ray temperature, and cluster redshift as the Einstein ensemble; we then compare the observed and simulated distributions in w(x), eta, and alpha. The comparisons indicate that (1) these three morphological characteristics are sensitive to the underlying cosmological model and (2) galaxy clusters with the observed range of X-ray morphologies are very unlikely in low-Omega(0) cosmologies. The analysis favors the Omega = 1 model, though some discrepancies remain. We discuss the effects of changing the initial conditions and of including additional physics in the simulations. C1 UNIV MICHIGAN,DEPT PHYS,ANN ARBOR,MI 48109. RP MOHR, JJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Evrard, August/0000-0002-4876-956X NR 44 TC 187 Z9 187 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1995 VL 447 IS 1 BP 8 EP 22 DI 10.1086/175852 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF079 UT WOS:A1995RF07900002 ER PT J AU CHEN, GH KOCHANEK, CS HEWITT, JN AF CHEN, GH KOCHANEK, CS HEWITT, JN TI THE MASS-DISTRIBUTION OF THE LENS GALAXY IN MG-1131+0456 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (MG 1131+0456); GALAXIES, STRUCTURE; GRAVITATIONAL LENSING; RADIO CONTINUUM, GALAXIES ID GRAVITATIONAL LENS; EINSTEIN RING; ELLIPTIC GALAXIES; DARK HALOS; ALGORITHM; MODELS; MG-1131+0456; MG1131+0456; IMAGES AB We present the results of modeling 5, 8, and 15 GHz maps of the gravitational lens MG 1131+0456 using the LensClean algorithm. Two models for the mass distribution in the lens were fitted: a de Vaucouleurs model and a model with the two-dimensional potential phi = b(2-alpha)(r(2) + s(2))(alpha/2)/alpha, both in an external shear field. The best-fit de Vaucouleurs model has an effective radius of R(e) = 0''.83 +/- 0''.13, larger than that measured at optical wavelengths. The best-fit ''alpha-model'' has alpha = 0.6 +/- 0.2 and a core radius of s = 0''.19 +/- 0''.07. An isothermal model (alpha = 1) is inconsistent with the data. The best alpha-model fits the 8 GHz map significantly better than the best de Vaucouleurs model, and it is a good fit at all three frequencies. Although the peak residuals in the best reconstructions are less than 5% of the map peak and it is difficult to distinguish visually the original image and the reconstructions, none of the models is statistically consistent with the data. Experiments on the effects of using Clean maps suggest that systematic errors are not the source of the discrepancy. We believe the primary problem is that an external shear is an inadequate model for the angular structure of the lens galaxy. The finite core radius in the models is required by the structure of the extended ring, so we confirm that the central component in the 8 GHz map is a central, lensed image of the source rather than the lens galaxy. Two galaxies 3'' from the ring add an external shear to the lens model that is within 3 degrees of the fitted model. The alignment is remarkable, but the two galaxies cannot account for the magnitude of the shear unless the effective ratio of their luminosity to the primary lens galaxy is 25 times larger than the measured ratio. The model lens positions, the position angle of the shear, and the mass interior to the ring are determined very precisely by the lens models. The time delay between the compact components is predicted with an uncertainty we estimate to be at most +/-9%; the formal uncertainty is +/-4%. C1 MIT, ELECTR RES LAB, CAMBRIDGE, MA 02139 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. HARVARD UNIV, COLL OBSERV, DEPT ASTRON, CAMBRIDGE, MA 02138 USA. RP MIT, DEPT PHYS, CAMBRIDGE, MA 02139 USA. NR 37 TC 21 Z9 21 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 JUL 1 PY 1995 VL 447 IS 1 BP 62 EP 81 DI 10.1086/175857 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF079 UT WOS:A1995RF07900007 ER PT J AU KOO, BC KIM, KT SEWARD, FD AF KOO, BC KIM, KT SEWARD, FD TI ROSAT OBSERVATIONS OF THE SUPERNOVA REMNANT W51C SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (W51); RADIO CONTINUUM, ISM; SUPERNOVA REMNANTS; X-RAYS, ISM ID 11 CM WAVELENGTH; GALACTIC-PLANE; PULSAR; REGION AB We have carried out ROSAT X-ray observations of the W51C supernova remnant (SNR). The SNR appears as an elongated (50' x 38') structure along the east-west direction. In contrast to its shell-type morphology in radio continuum, the SNR has both center-filled and shell-type morphologies in X-ray structure. The boundary of the radio structure matches well with that of the X-ray in the southeast. To the west, the X-ray structure appears to extend beyond the radio continuum shell. High-resolution (40 '') interferometric 21 cm continuum observation shows a thin shell located within the X-ray structure. The thin shell appears to surround the central X-ray-bright region. The X-ray spectrum of the SNR becomes systematically harder toward the west. By comparing the spectral hardness with the distribution of molecular gas in this region, we have found that the spectral hardening is due to the selective absorption by intervening interstellar gas. The W51C SNR is considered to be behind the ''high-velocity molecular stream'' at a mean distance of 5.6 kpc. The average X-ray spectrum of the SNR can be fitted well by the Raymond-Smith thermal model with T-e = 3.4 x 10(6) K. We apply the Sedov and evaporative (White and Long 1991) models to derive the SNR parameters. Both models yield an age of similar to 3 x 10(4) yr and an explosion energy of 3.6 x 10(51) ergs, which is larger than the canonical value of a single supernova explosion. We discuss the implications of the large energy requirement and the complex X-ray and radio morphologies. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP KOO, BC (reprint author), SEOUL NATL UNIV,DEPT ASTRON,SEOUL 151742,SOUTH KOREA. NR 29 TC 44 Z9 44 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1995 VL 447 IS 1 BP 211 EP 219 DI 10.1086/175867 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF079 UT WOS:A1995RF07900017 ER PT J AU DANEN, RM GWINN, CR BLOEMHOF, EE AF DANEN, RM GWINN, CR BLOEMHOF, EE TI THE SUBARCSECOND 10 MICRON-SIZE OF LKH-ALPHA-101 - CONSTRAINTS ON CIRCUMSTELLAR DUST SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; INFRARED, STARS; RADIATIVE TRANSFER; STARS, EMISSION-LINE, BE; STARS, INDIVIDUAL (LKH-ALPHA 101); STARS, PRE-MAIN-SEQUENCE ID T-TAURI STARS; YOUNG STELLAR OBJECTS; HERBIG AE/BE STARS; AMORPHOUS-CARBON; INTERSTELLAR GRAINS; OPTICAL-PROPERTIES; INFRARED-SPECTRA; MASS-LOSS; DISKS; LKH-ALPHA-101 AB Operating slightly beyond the formal diffraction limit of a 3 m telescope, we have obtained lambda = 10 mu m images with subarcsecond spatial resolution of the pre-main-sequence emission-line star LkH alpha 101. Our measurements show that mid-infrared radiation emanates from within 135 AU of the star, on the same spatial scale as a strong ionized wind deduced from radio observations. The point-spread function of our infrared instrument, at the 3 m Shane Telescope, has FWHM 0 ''.740 +/- 0 ''.022, as measured for the unresolved star alpha Tau. Raw images of the core component of LkH alpha 101 have FWHM 0 ''.768 +/- 0 ''.021; after deconvolution, we set a 95% confidence upper limit of 0 ''.34 (270 AU) for the FWHM diameter of the core. Our measured flux density of 325 +/- 27 Jy for the unresolved core accounts for most of the 10 mu m emission from the central arcminute of LkHa alpha 101. Our observation implies that approximate to 12% of the total luminosity of LkH alpha 101 is radiated by this unresolved core; thus, the unresolved core emission must be either optically thin, or anisotropically distributed about the star. For optically thin emission from dust, graphite or glassy carbon grains with radii less than a approximate to 0.15 mu m can be excluded as contributing significantly to the unresolved 10 mu m emission based on our upper limit of the source size and our measurement of the flux density, along with the observed spectrum. Similarly, silicate grains with radii less than a approximate to 0.3 mu m can be excluded; although, based on the spectrum, silicate grains of any size are unlikely a dominant source of the mid-infrared core emission, if optically thin. The observation of an ionized stellar wind suggests as a model for the unresolved core a spherically symmetric, optically thin envelope of dust with an r(-2) density distribution (characteristic of a uniform outflow). This model is consistent with our observations and with the spectral energy distribution, if the dust grains are graphite or glassy carbon and have radii a confined to the range 0.3 less than or similar to a less than or similar to 0.5 mu m. An optically thin r(-2) distribution composed primarily of other sizes of graphite and glassy carbon grains, or some other forms of carbon grains, would be inconsistent with the size we measure or the spectral energy distribution of the source. Alternatively, isothermal concentrations of dust of any size and composition that are optically thick even at lambda = 10 mu m, distributed anisotropically around the star, could produce the mid-infrared core emission. This dust cannot lie in a circumstellar disk because the near- to mid-infrared spectrum of LkH alpha 101 is inconsistent with that expected for a disk. If the unresolved 10 mu m emission is produced by isothermal concentrations of dust optically thick at lambda = 10 mu m, then the concentrations must lie near a single radius from the star. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP DANEN, RM (reprint author), UNIV CALIF SANTA BARBARA,DEPT PHYS,SANTA BARBARA,CA 93106, USA. NR 51 TC 3 Z9 3 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1995 VL 447 IS 1 BP 391 EP 400 DI 10.1086/175882 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF079 UT WOS:A1995RF07900032 ER PT J AU WANG, Y NOYES, RW TARBELL, TD TITLE, AM AF WANG, Y NOYES, RW TARBELL, TD TITLE, AM TI VORTICITY AND DIVERGENCE IN THE SOLAR PHOTOSPHERE SO ASTROPHYSICAL JOURNAL LA English DT Article DE HYDRODYNAMICS; SUN, ATMOSPHERE; SUN, GRANULATION ID SURFACE; FLOW; SUN AB We have studied an outstanding sequence of continuum images of the solar granulation from Pic du Midi Observatory. We have calculated the horizontal vector flow field using a correlation tracking algorithm, and from this determined three scalar fields: the vertical component of the curl, the horizontal divergence, and the horizontal flow speed. The divergence field has substantially longer coherence time and more power than does the curl field. Statistically, curl is better correlated with regions of negative divergence-that is, the vertical vorticity is higher in downflow regions, suggesting excess vorticity in intergranular lanes. The average value of the divergence is largest (i.e., outflow is largest) where the horizontal speed is large; we associate these regions with exploding granules. A numerical simulation of general convection also shows similar statistical differences between curl and divergence. Some individual small bright points in the granulation pattern show large local vorticities. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. LOCKHEED PALO ALTO RES LABS, PALO ALTO, CA 94304 USA. RP HARVARD UNIV, DEPT ASTRON, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 18 TC 32 Z9 32 U1 0 U2 0 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 JUL 1 PY 1995 VL 447 IS 1 BP 419 EP 427 DI 10.1086/175886 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF079 UT WOS:A1995RF07900036 ER PT J AU UITENBROEK, H BRIAND, C AF UITENBROEK, H BRIAND, C TI THE MG I LAMBDA-285.21 NANOMETER LINE - AN EXAMPLE OF NON-LTE LINE FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE LINE, FORMATION; SUN, UV RADIATION ID PARTIAL REDISTRIBUTION; HELIOSEISMOLOGY LINES; SOLAR CHROMOSPHERE; OSCILLATOR-STRENGTHS; RESONANCE LINES; EMISSION-LINES; MAGNESIUM; MODEL; ATMOSPHERE; RADIATION AB We discuss how the Mg I lambda 285.21 nm line is formed in the context of standard plane-parallel modeling. The line appears to be very sensitive to the nonlocal radiation field determining the balance between neutral and singly ionized magnesium. We resolve between conflicting results in earlier lambda 285.21 nm line modeling by showing that, in the quite Sun, the line forms at sufficiently low density for partial frequency redistribution to take effect and give rise to small emission reversals in the core. We find this to be true only if we take proper account of UV line blanketing at the relevant Mg I ionization edges. In this case there is good agreement between theoretical line profiles and spatially averaged spectra from the Solar Maximum Mission (SMM) Ultraviolet Spectrometer and Polarimeter (UVSP) and from the French RASOLBA balloon experiment. Spatially resolved spectra obtained with the latter instrument show considerable variation in the line core, with emission present only in some locations and absent in others. C1 CTR UNIV ORSAY, INST ASTROPHYS SPATIALE, F-91405 ORSAY, FRANCE. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 61 TC 5 Z9 5 U1 0 U2 0 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 JUL 1 PY 1995 VL 447 IS 1 BP 453 EP 463 DI 10.1086/175889 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF079 UT WOS:A1995RF07900039 ER PT J AU CAMERON, AGW HOFLICH, P MYERS, PC CLAYTON, DD AF CAMERON, AGW HOFLICH, P MYERS, PC CLAYTON, DD TI MASSIVE SUPERNOVAE, ORION GAMMA-RAYS, AND THE FORMATION OF THE SOLAR-SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE GAMMA RAYS, THEORY; SOLAR SYSTEM, FORMATION; SUPERNOVAE, GENERAL ID STARS; MODELS AB We discuss the source of the enhanced carbon and oxygen low-energy cosmic-ray flux in the Orion star-forming region and attribute it to the acceleration of the surface layers of a massive supernova, probably of Type Ib. The gamma rays from Orion are produced by that fast CO ejecta. In this model there would be few Orion-like gamma-ray sources in the Galaxy at any one time. We also postulate that a massive supernova produced the short-lived extinct radioactivities injected into the molecular cloud core that produced the solar system. We find that relative to Al-26 the other short-lived extinct radioactivities are excessively produced in massive supernovae but are likely to be more attenuated by postexplosion fallback than Al-26. This is a revival of the supernova trigger hypothesis; to obtain the correct dilutions of the extinct radioactivities, the distance from the supernova to the impacted molecular cloud core must be a few parsecs, and the effective projected collecting area of the cloud must be significantly less than normal core radii. C1 CLEMSON UNIV,DEPT PHYS & ASTRON,CLEMSON,SC 29634. RP CAMERON, AGW (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 28 TC 90 Z9 91 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1995 VL 447 IS 1 BP L53 EP L57 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF081 UT WOS:A1995RF08100014 ER PT J AU PUN, CSJ KIRSHNER, RP SONNEBORN, G CHALLIS, P NASSIOPOULOS, G ARQUILLA, R CRENSHAW, DM SHRADER, C TEAYS, T CASSATELLA, A GILMOZZI, R TALAVERA, A WAMSTEKER, W AF PUN, CSJ KIRSHNER, RP SONNEBORN, G CHALLIS, P NASSIOPOULOS, G ARQUILLA, R CRENSHAW, DM SHRADER, C TEAYS, T CASSATELLA, A GILMOZZI, R TALAVERA, A WAMSTEKER, W TI ULTRAVIOLET OBSERVATIONS OF SN 1987A WITH THE IUE SATELLITE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE ULTRAVIOLET, STARS; STARS, INDIVIDUAL (SN 1987A) ID LARGE MAGELLANIC CLOUD; OPTICAL SPECTROPHOTOMETRIC ATLAS; BOLOMETRIC LIGHT-CURVE; SUPERNOVA 1987A; INTERSTELLAR EXTINCTION; UBVRI PHOTOMETRY; CERRO-TOLOLO; NEUTRINO BURST; SPECTRAL-LINES; CCD PHOTOMETRY AB Ultraviolet (lambda: 1150-3300 Angstrom) observations of SN 1987A with the IUE satellite provide a unique data set. Observations started the day after discovery, 1987 February 24 (day 1.6), and a total of 751 spectra were obtained through 1992 June 9 (day 1567). The data have been processed to generate a complete catalog of SN 1987A ultraviolet spectra. The data reduction procedure includes careful line-by-line extraction, removing hits and hot pixels, and, most importantly, a scrupulous subtraction of the contribution from stars near SN 1987A within the IUE aperture. In addition to processing the data, we have also extracted light curves, and combined them with the ground-based optical data and HST observations (day 1278 to 2431) to extend the study in both wavelength and time. The data-processing procedures of our IUE study produce results that are consistent with the HST data where they overlap, but not with the IUE study by Sanz Fernandez de Cordoba (1993) because of its incorrect background subtraction. The IUE data are consistent with the ground-based Walraven VBLUW photometry, while we found that flux scale of the Soviet ASTRON satellite spectroscopic data is low by similar to 15%. The UV flux plummeted during the earliest days of observations because of the drop in the photospheric temperature and the increase in opacity. However, after reaching a minimum of 0.04% on day 44, the UV flux increased by 175 times in its contribution to 7% of the total UVOIR bolometric luminosity at day 800. A revised set of bolometric data has been constructed which includes the contribution of UV from day 1 to day 1352. Studies of the UV colors show that the supernova started to get bluer in UV around the time when dust started to form in the ejecta. Our results are consistent with the possibility that the dust condensed may be metal-rich. C1 NASA, GODDARD SPACE FLIGHT CTR, ASTRON & SOLAR PHYS LAB, GREENBELT, MD 20771 USA. NASA, GODDARD SPACE FLIGHT CTR, COMP SCI CORP, GREENBELT, MD 20771 USA. VILSPA, ESA IUE OBSERV, E-28080 MADRID, SPAIN. STOCKHOLM OBSERV, S-13336 SALTSJOBADEN, SWEDEN. SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. UNIV SPACE RES ASSOC, WASHINGTON, DC USA. UNIV CATANIA, CATANIA, ITALY. RP PUN, CSJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 139 TC 56 Z9 57 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 1995 VL 99 IS 1 BP 223 EP 261 DI 10.1086/192185 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RD575 UT WOS:A1995RD57500009 ER PT J AU Winker, K AF Winker, K TI Autumn stopover on the isthmus of Tehuantepec by woodland Nearctic-Neotropic migrants SO AUK LA English DT Article ID BODY SIZE; BIRDS AB The Isthmus of Tehuantepec in southern Mexico seems to cause a concentration of Nearctic-Neotropic migrant landbirds during migration. Despite its possible importance as an area for fat deposition, almost nothing is known about how this area is used by migrants. Of 11 small passerine species examined, 6 showed significant diurnal increases in body condition in relation to time of capture. All six showed gains suggesting low to moderate levels of fat deposition, concordant with the concept of the Isthmus as an important source of stopover resources. The area is not used in the same manner by all of these common species, however. The migrants at this site in autumn probably have not arrived via a long-distance, trans-Gulf migration. Comparison with data from other sources suggests that the energetic costs of molt are important at northerly stopover sites, and that modifications are needed in our concepts of Middle American migration routes. RP Winker, K (reprint author), SMITHSONIAN INST,CONSERVAT & RES CTR,NZP,FRONT ROYAL,VA 22630, USA. RI Winker, Kevin/M-2042-2014 OI Winker, Kevin/0000-0002-8985-8104 NR 39 TC 43 Z9 43 U1 1 U2 1 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0004-8038 J9 AUK JI AUK PD JUL PY 1995 VL 112 IS 3 BP 690 EP 700 PG 11 WC Ornithology SC Zoology GA TZ356 UT WOS:A1995TZ35600013 ER PT J AU Elzanowski, A BrettSurman, MK AF Elzanowski, A BrettSurman, MK TI Avian premaxilla and tarsometatarsus from the uppermost Cretaceous of Montana SO AUK LA English DT Article C1 GEORGE WASHINGTON UNIV,DEPT GEOL,WASHINGTON,DC 20052. RP Elzanowski, A (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT VERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 14 TC 8 Z9 8 U1 1 U2 3 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0004-8038 J9 AUK JI AUK PD JUL PY 1995 VL 112 IS 3 BP 762 EP 767 PG 6 WC Ornithology SC Zoology GA TZ356 UT WOS:A1995TZ35600022 ER PT J AU BROWN, JL WILDT, DE GRAHAM, LH BYERS, AP COLLINS, L BARRETT, S HOWARD, JG AF BROWN, JL WILDT, DE GRAHAM, LH BYERS, AP COLLINS, L BARRETT, S HOWARD, JG TI NATURAL VERSUS CHORIONIC GONADOTROPIN-INDUCED OVARIAN RESPONSES IN THE CLOUDED LEOPARD (NEOFELIS-NEBULOSA) ASSESSED BY FECAL STEROID ANALYSIS SO BIOLOGY OF REPRODUCTION LA English DT Article ID INTRAUTERINE ARTIFICIAL-INSEMINATION; PUMA FELIS-CONCOLOR; SEXUAL-BEHAVIOR; REPRODUCTIVE PHYSIOLOGY; CIRCULATING HORMONES; CAT; PROGESTERONE; PREGNANCY; PSEUDOPREGNANCY; ESTRADIOL AB The clouded leopard (Neofelis nebulosa) is an endangered species difficult to propagate in captivity because of sexual incompatibility between paired individuals. Fecal estradiol (E(2)) and progesterone (P-4) metabolites were quantified in 14 females to noninvasively monitor seasonal reproductive patterns and compare ovarian responses to natural mating vs. exogenous gonadotropins. Increased E(2) excretion was associated with behavioral estrus or eCG treatment, whereas elevated P-4 metabolites were observed during natural and hCG-induced pregnant and nonpregnant luteal phases, On the basis of fecal E(2) profiles, duration of the estrous cycle was 24 +/- 2 days, with estrus lasting 6 +/- 1 days. Mean gestation length was 89 +/- 2 days, whereas duration of the nonpregnant luteal phase was 47 +/- 2 days. Females experienced a seasonal anestrus during the late summer and early fall. One female demonstrated a lactational anestrus after the birth of three cubs. On nine occasions, clouded leopards ovulated spontaneously (based on elevated fecal P-4 metabolite concentrations) in the absence of mating. Patterns of eCG-stimulated E(2) excretion were similar to those associated with natural estrus and were unaffected by eCG dosage (25, 50, or 100 IU). In contrast, post-hCG P-4 metabolite profiles varied considerably, with responses including anovulation, attenuated luteal P-4 metabolite production, and hyperstimulated luteal function. in some females, compromised luteal function after ovulation induction appeared to be due to the presence of mature CL from previous spontaneous (without copulation) ovulations at the time of gonadotropin treatment. Duration of post-hCG P-4 metabolite excretion was reduced similar to 40% in these individuals compared to females with no evidence of active luteal activity. In sum, these are the first data describing the ovarian cycle of this endangered species. The information is important because it is based on the longitudinal assessment of multiple females using a completely atraumatic approach, thereby eliminating the potential confounding impact of stress, Data indicate that spontaneous ovulations and the presence of active luteal tissue on the ovary can profoundly affect ovarian responses to exogenous gonadotropin therapy. Therefore, fecal steroid monitoring can serve as a useful adjunct to developing assisted reproduction techniques, especially the hormonal induction of ovulation for planned artificial insemination. C1 CONSERVAT BREEDING SPECIALIST GRP,APPLE VALLEY,MN. NASHVILLE ZOO,JOELTON,TN. RP BROWN, JL (reprint author), SMITHSONIAN INST,NATL ZOOL PK,CONSERVAT & RES CTR,1500 REMOUNT RD,FRONT ROYAL,VA 22630, USA. NR 41 TC 55 Z9 63 U1 1 U2 17 PU SOC STUDY REPRODUCTION PI MADISON PA 1526 JEFFERSON ST, MADISON, WI 53711-2106 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD JUL PY 1995 VL 53 IS 1 BP 93 EP 102 DI 10.1095/biolreprod53.1.93 PG 10 WC Reproductive Biology SC Reproductive Biology GA RC850 UT WOS:A1995RC85000012 PM 7669862 ER PT J AU LOSOS, E HAYES, J PHILLIPS, A WILCOVE, D ALKIRE, C AF LOSOS, E HAYES, J PHILLIPS, A WILCOVE, D ALKIRE, C TI TAXPAYER-SUBSIDIZED RESOURCE EXTRACTION HARMS SPECIES - DOUBLE JEOPARDY SO BIOSCIENCE LA English DT Article C1 STANFORD UNIV,SCH EARTH SCI,EARTH SYST PROGRAM,STANFORD,CA 94305. UNIV MICHIGAN,SCH NAT RESOURCES & ENVIRONM,ANN ARBOR,MI 48109. ENVIRONM DEF FUND,WASHINGTON,DC 20009. WILDERNESS SOC,WASHINGTON,DC 20006. RP LOSOS, E (reprint author), SMITHSONIAN TROP RES INST,CTR TROP FOREST SCI,900 JEFFERSON DR,SUITE 2207,WASHINGTON,DC 20560, USA. NR 43 TC 20 Z9 21 U1 3 U2 8 PU AMER INST BIOL SCI PI WASHINGTON PA 730 11TH STREET, NW, WASHINGTON, DC 20001-4521 SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD JUL-AUG PY 1995 VL 45 IS 7 BP 446 EP 455 DI 10.2307/1312788 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA RF560 UT WOS:A1995RF56000005 ER PT J AU RICE, ME PIRAINO, J REICHARDT, HF AF RICE, ME PIRAINO, J REICHARDT, HF TI A SURVEY OF THE SIPUNCULA OF THE INDIAN-RIVER LAGOON SO BULLETIN OF MARINE SCIENCE LA English DT Article; Proceedings Paper CT Biodiversity of the Indian River Lagoon Conference CY FEB 15-16, 1994 CL HARBOR BRANCH OCEANOG OMST, FT PIERCE, FL SP Indian River Lagoon, Natl Estuary Program HO HARBOR BRANCH OCEANOG OMST ID THEMISTE-LAGENIFORMIS AB From 22 stations in the Indian River Lagoon, ranging from Haulover Canal in the north to St. Lucie Inlet in the south, 18 species of sipunculans are reported. Habitats include oyster beds, subtidal and intertidal sand, seagrass beds, and sea walls. The greatest number of species occurs near inlets: Sebastian, Fort Pierce, and St. Lucie. The most widely distributed sipunculan in the Indian River Lagoon is Phascolion cryptum, averaging 3 cm in length. Usually buried in the upper 5 cm of sandy sediments associated with seagrass beds, it inhabits discarded gastropod shells in shallow waters throughout the lagoon. Development is direct, a crawling vermiform stage hatching from egg coverings within 2 days. The second most widely distributed sipunculan is Themiste lageniformis, attaining a maximum extended length of 4 cm. Occurring most commonly near the inlets of Fort Pierce and Saint Lucie, it is associated either with oyster beds, where it lives in and among the shells, or with the encrusting fauna on sea walls, among the vermetid snails, sponges, and tunicates. In oyster beds near Fort Pierce it occurs in densities as great as 2,100 . m(2). This species is parthenogenic; its development includes a short-lived non-feeding pelagic larval stage. Other species, found mostly in relatively small numbers near the inlets, are characterized generally by developmental patterns with long-lived feeding pelagic larvae. Whether they establish breeding populations in the Indian River Lagoon has not been determined. RP RICE, ME (reprint author), SMITHSONIAN MARINE STN LINK PORT,5612 OLD DIXIE HIGHWAY,FT PIERCE,FL 34946, USA. NR 13 TC 4 Z9 4 U1 0 U2 4 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD JUL PY 1995 VL 57 IS 1 BP 128 EP 135 PG 8 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA RH265 UT WOS:A1995RH26500014 ER PT J AU KENSLEY, B NELSON, WG SCHOTTE, M AF KENSLEY, B NELSON, WG SCHOTTE, M TI MARINE ISOPOD BIODIVERSITY OF THE INDIAN-RIVER LAGOON, FLORIDA SO BULLETIN OF MARINE SCIENCE LA English DT Article; Proceedings Paper CT Biodiversity of the Indian River Lagoon Conference CY FEB 15-16, 1994 CL HARBOR BRANCH OCEANOG OMST, FT PIERCE, FL SP Indian River Lagoon, Natl Estuary Program HO HARBOR BRANCH OCEANOG OMST ID SEAGRASS AB Twenty-one species of free-living isopods, and six species of parasitic bopyrids are recorded from the Indian River Lagoon. The distribution of this fauna bears out the zoogeographically transitional nature of the area, but also emphasizes its strong subtropical affinities. The seasonal abundance of the three most common species in Halodule seagrass beds, viz. Erichsonella attenuata, Harrieta faxoni, and Edotea montosa suggests that the various regions of the Indian River Lagoon are not biologically closely coupled, and that seasonal predation pressure may account for lowered numbers during the summer months. C1 FLORIDA INST TECHNOL,DIV MARINE & ENVIRONM SYST,OCEANOG PROGRAM,MELBOURNE,FL 32901. RP KENSLEY, B (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 14 TC 17 Z9 17 U1 1 U2 5 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD JUL PY 1995 VL 57 IS 1 BP 136 EP 142 PG 7 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA RH265 UT WOS:A1995RH26500015 ER PT J AU KLAPPER, G OLIVER, WA AF KLAPPER, G OLIVER, WA TI THE DETROIT RIVER GROUP IS MIDDLE DEVONIAN - DISCUSSION ON EARLY DEVONIAN AGE OF THE DETROIT RIVER GROUP, INFERRED FROM ARCTIC STROMATOPOROIDS SO CANADIAN JOURNAL OF EARTH SCIENCES LA English DT Discussion C1 SMITHSONIAN INST, NATL MUSEUM NAT HIST E-305, DEPT PALEOBIOL, WASHINGTON, DC 20560 USA. UNIV IOWA, DEPT GEOL, IOWA CITY, IA 52242 USA. NR 21 TC 9 Z9 9 U1 0 U2 0 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA SN 0008-4077 EI 1480-3313 J9 CAN J EARTH SCI JI Can. J. Earth Sci. PD JUL PY 1995 VL 32 IS 7 BP 1070 EP 1073 DI 10.1139/e95-088 PG 4 WC Geosciences, Multidisciplinary SC Geology GA RZ634 UT WOS:A1995RZ63400020 ER PT J AU LITTLER, MM LITTLER, DS TAYLOR, PR AF LITTLER, MM LITTLER, DS TAYLOR, PR TI SELECTIVE HERBIVORE INCREASES BIOMASS OF ITS PREY - A CHITON-CORALLINE REEF-BUILDING ASSOCIATION SO ECOLOGY LA English DT Article DE ACCRETION; BIOMASS; CARIBBEAN; CHIRON-CORALLINE ASSOCIATION; CHONEPLAX LATA; HERBIVORY; POROLITHON PACHYDERMUM; REEF-BUILDING ID ALGAL CRUSTS; SUCCESSION; PREDATION; COMMUNITY; PRODUCTIVITY; MUTUALISM; GROWTH; FACILITATION; DISTURBANCE; POROLITHON AB The intimate association between a selective herbivore (the chiton Choneplax lata) and its primary prey (the crustose coralline alga Porolithon pachydermum) results in increased biomass and accretion of the alga. This process, over ecological and geological time scales, comprises a major component of Caribbean reef-building systems. Manipulative experiments showed that as the chiton grazes the alga it stimulates new meristematic activity and removes sporlings of the competitively superior frondose and filamentous algae, thereby increasing the survival rate of P. pachydermum on the intertidal reef crest. Furthermore, in the absence of C. into, overgrowths of frondose and filamentous epiphytes provide an attractive food source for parrotfishes (Scaridae), which accelerates bioerosion of the coralline reef-crest structure due to the deep rasping action of feeding activity. Algal removal experiments suggest that the role of P. pachydermum is to provide a predictable food source and refuge substratum, which increases survivorship of the burrowing chiton by minimizing expenditure of energy during foraging and risk to predation. The chiton/coralline alga association is abundant throughout tropical western Atlantic islands and augments reef-building processes on the shallow algal crest portion of Caribbean reefs. Cover of the Choneplax/Porolithon association in the Belize Barrier Reef cost averages 13% (maximum to 70%) with a mean chiton density of 664 individuals/m(2) within the association. On average, the extensive networks of interconnected chiton burrows extend between 6 and 10 cm deep and contain one C. lata for every six openings, with the majority of animals (66%) ranging from 16 to 30 mm in length. Gut contents of the chiton consist predominantly of P. pachydermum (51%), followed by bacterial detritus (30%), Cyanophyta (13%), Bacillariophyta (3%), and fleshy microalgae (3%). The close SEM (scanning electron microscope) match between radular morphology of C. lata and grazing scars on the thallus surface of P. pachydermum shows how the chiton regularly feeds on the coralline alga without causing mortality. Virtually all P. pachydermum in the vicinity of C., lata burrows contain radular track scars of approximate to 10 mu m in depth, whereas the photosynthetic, meristematic, and reproductive tissues of the coralline lie below 20 mu m P. pachydermum under intense chiton grazing is photosynthetically competent with 0.1 mg C fixed . g(-1) organic dry mass . h(-1), which is not significantly different from ungrazed material and within the range of rates for other crustose coralline algae. The result is continuous net accretion at a mean rate of 2.3 mm/yr. C1 NATL SCI FDN,BIOL OCEANOG PROGRAM,ARLINGTON,VA 22230. RP LITTLER, MM (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,WASHINGTON,DC 20560, USA. NR 71 TC 75 Z9 75 U1 1 U2 19 PU ECOLOGICAL SOC AMER PI TEMPE PA ARIZONA STATE UNIV CENTER ENVIRONMENTAL STUDIES, TEMPE, AZ 85287 SN 0012-9658 J9 ECOLOGY JI Ecology PD JUL PY 1995 VL 76 IS 5 BP 1666 EP 1681 DI 10.2307/1938167 PG 16 WC Ecology SC Environmental Sciences & Ecology GA RE892 UT WOS:A1995RE89200027 ER PT J AU WCISLO, WT AF WCISLO, WT TI A FALSE ANTITHESIS AND EVOLUTIONARY PSYCHOLOGY SO ETHOLOGY AND SOCIOBIOLOGY LA English DT Letter C1 SMITHSONIAN TROP RES INST,PANAMA CITY,FL. NR 7 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCIENCE PUBL CO INC PI NEW YORK PA 655 AVENUE OF THE AMERICAS, NEW YORK, NY 10010 SN 0162-3095 J9 ETHOL SOCIOBIOL JI Ethol.Sociobiol. PD JUL PY 1995 VL 16 IS 4 BP 343 EP 344 DI 10.1016/0162-3095(95)00054-O PG 2 WC Psychology, Biological; Behavioral Sciences; Social Sciences, Biomedical; Sociology; Zoology SC Psychology; Behavioral Sciences; Biomedical Social Sciences; Sociology; Zoology GA TB978 UT WOS:A1995TB97800003 ER PT J AU ZOTZ, G HARRIS, G KONIGER, M WINTER, K AF ZOTZ, G HARRIS, G KONIGER, M WINTER, K TI HIGH-RATES OF PHOTOSYNTHESIS IN THE TROPICAL PIONEER TREE, FICUS-INSIPIDA WILLD SO FLORA LA English DT Article DE CO2 EXCHANGE; FICUS; PHOTOSYNTHESIS; TREE PHYSIOLOGY; TROPICAL FOREST ID FOREST CANOPY; LEAVES; PLANTS; CLUSIA AB Diurnal courses of CO2 and water-vapour exchange of canopy leaves of mature trees of Ficus insipida WILLD. (Moraceae) were studied under natural conditions in the tropical dry forest of Parque Metropolitano near Panama City, Republic of Panama. Measurements were conducted from early January 1993 (dry season) until July 1993 (wet season). Rates of net CO2 uptake were high throughout the study period, with up to 33.1 mu mol m(-2) s(-1) in the early dry season. During the dry season, gas exchange was characterized by strong reductions (''midday-depressions'') of net CO2 uptake and stomatal conductance at noon. However, daily carbon gain and diurnal water-use efficiency of CO2 uptake did not differ between seasons. East-exposed leaves that received direct sunlight during early morning hours showed higher CO2 uptake rates and lost less water per CO2 fixed than west-exposed leaves. As previously demonstrated for several canopy species from a tropical moist forest, the maximum rate of net CO2 uptake was a good predictor of daily carbon gain. C1 WELLESLEY COLL,DEPT BIOL,WELLESLEY,MA 02181. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP ZOTZ, G (reprint author), UNIV WURZBURG,LEHRSTUHL BOT 2,JULIUS VON SACHS INST BIOWISSENSCH,MITTLERER DALLENBERGWEG 64,D-97082 WURZBURG,GERMANY. NR 26 TC 49 Z9 50 U1 0 U2 11 PU GUSTAV FISCHER VERLAG JENA PI JENA PA VILLENGANG 2, D-07745 JENA, GERMANY SN 0367-2530 J9 FLORA JI Flora PD JUL PY 1995 VL 190 IS 3 BP 265 EP 272 PG 8 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA RP521 UT WOS:A1995RP52100008 ER PT J AU MEECH, KJ KNOPP, GP FARNHAM, TL GREEN, D AF MEECH, KJ KNOPP, GP FARNHAM, TL GREEN, D TI THE SPLIT NUCLEUS OF COMET WILSON-(C/1986-P1=1987-VII) SO ICARUS LA English DT Article ID PHOTOMETRIC STANDARD STARS; CELESTIAL EQUATOR; DUST; P/HALLEY; PRECESSION; ASTEROIDS; 1987VII; SIZE AB We present CCD observations of Comet Wilson (C/1986 P1 = 1987 VII) from 26 nights during the time period 1986 October to 1991 February, which brackets perihelion. During the observing run of 1988 February, the comet was observed to have split into two fragments. Our broadband CCD photometry, along with photometry from the international Cometary Quarterly, shows a steady decline in brightness of Comet Wilson post-perihelion, with an outburst between heliocentric distances r = 2.8 and 3.3 AU during 1987 October and November. By r approximate to 7 AU, the fragment had faded with respect to the parent and was no longer centrally condensed. A brightness limit of m(R) approximate to 25, when the comet was at r = 12.65 AU, constrains the primary nucleus to have a maximum radius between 5 and 7 km, assuming an albedo of 0.04. The accuracy of direct orbital solutions for the parent body and fragment to determine the time of splitting was limited by the presence of significant nongravitational forces and the limited fragment orbital coverage. We used the relative position of the fragment with respect to the parent to calculate a time of splitting which was consistent with the time of the observed outburst. We discuss the possible causes of the splitting. The coma of Comet Wilson was observed to have a surface-brightness profile which fell off as p(-1) (characteristic of a canonical steady-state coma under the influence of radiation pressure) for all of the data with the exception of the data taken during 1987 November when the gradient was p(-1.3). This steeper slope was probably caused by the injection of new material into the coma during the outburst. During 1986 October, there was a break in the surface-brightness profile slope which may be interpreted as the distance at which grains are swept into the tail. The profiles suggested grain velocities of a few x 10(2) to 10 m sec(-1) for grains between 1 and a few hundred micrometers. Finson-Probstein dust modeling showed that ejection of grains began preperihelion at r > 6 AU, peaking near perihelion with a very rapid decline thereafter, with an outburst occurring roughly 170 days post-perihelion. We found no evidence for the existence of discrete features in the coma. Both the primary and fragment nuclei grew redder with time, with the fragment being redder than the parent, consistent with the picture of smaller grains leaving the field of view of the aperture more quickly than larger grains. (C) 1995 Academic Press, Inc. C1 SMITHSONIAN OBSERV,CAMBRIDGE,MA 02138. UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822. NR 62 TC 14 Z9 14 U1 0 U2 0 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD JUL PY 1995 VL 116 IS 1 BP 46 EP 76 DI 10.1006/icar.1995.1113 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RJ716 UT WOS:A1995RJ71600004 ER PT J AU WILLIAMS, IP OCEALLAIGH, DP FITZSIMMONS, A MARSDEN, BG AF WILLIAMS, IP OCEALLAIGH, DP FITZSIMMONS, A MARSDEN, BG TI THE SLOW-MOVING OBJECTS 1993-SB AND 1993-SC SO ICARUS LA English DT Article ID SHORT-PERIOD COMETS; ORIGIN AB The results are reported of a search that was carried out in September 1993 for slow moving objects in the Solar System that may be potential members of the Kuiper belt of comets. Two objects, 1993 SB and 1993 SC were discovered and an analysis of all the images allows a possible rotation rate for 1993 SC to be determined. An estimate, based on the limiting magnitudes of the images, is made of the likely space density of such objects. (C) 1995 Academic Press, Inc. C1 QUEENS UNIV BELFAST,DEPT PURE & APPL PHYS,BELFAST,ANTRIM,NORTH IRELAND. HARVARD UNIV,HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP WILLIAMS, IP (reprint author), UNIV LONDON QUEEN MARY & WESTFIELD COLL,ASTRON UNIT,MILE END RD,LONDON E1 4NS,ENGLAND. OI Williams, Iwan Prys/0000-0002-8069-1344 NR 20 TC 43 Z9 43 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD JUL PY 1995 VL 116 IS 1 BP 180 EP 185 DI 10.1006/icar.1995.1119 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RJ716 UT WOS:A1995RJ71600010 ER PT J AU GODDARD, I AF GODDARD, I TI PRINCIPLES AND METHODS IN HISTORICAL PHONOLOGY - FROM PROTO-ALGONQUIAN TO ARAPAHO - PICARD,M SO INTERNATIONAL JOURNAL OF AMERICAN LINGUISTICS LA English DT Book Review RP GODDARD, I (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 18 TC 1 Z9 1 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0020-7071 J9 INT J AM LINGUIST JI Int. J. Am. Linguist. PD JUL PY 1995 VL 61 IS 3 BP 328 EP 334 DI 10.1086/466259 PG 7 WC Linguistics; Language & Linguistics SC Linguistics GA RZ746 UT WOS:A1995RZ74600004 ER PT J AU CULVER, SJ BUZAS, MA AF CULVER, SJ BUZAS, MA TI THE EFFECTS OF ANTHROPOGENIC HABITAT DISTURBANCE, HABITAT DESTRUCTION, AND GLOBAL WARMING ON SHALLOW MARINE BENTHIC FORAMINIFERA SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article; Proceedings Paper CT Annual Cushman-Foundation Symposium on Human Problems, Foraminiferal Solutions CY OCT, 1993 CL BOSTON, MA SP Cushman Fdn ID BIOLOGICAL DIVERSITY; CLIMATE CHANGE; CONSEQUENCES; PATTERNS; OCEAN; CONSERVATION; CIRCULATION; PERSPECTIVE; VEGETATION; POLLUTION AB Protists such as benthic foraminifera are not immune to the effects of global warming or to shallow marine environmental degradation and destruction caused by the activities of humans. Increasing environmental stresses are likely to lead, in the near future, to disruption and dynamic restructuring of communities, localized extinctions of both rare and abundant species, and total extinction of rare species (and, perhaps, abundant species) in the shallow marine environment. Low latitude and/or developed coastal environments and communities are likely to experience the greatest changes. The role of benthic foraminifera in the trophic structure of shallow marine communities dictates that many other organisms will be affected by changes in the structure and diversity of shallow marine foraminiferal populations. C1 SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL,WASHINGTON,DC 20560. RP CULVER, SJ (reprint author), NAT HIST MUSEUM,DEPT PALAEONTOL,CROMWELL RD,LONDON SW7 5BD,ENGLAND. NR 132 TC 31 Z9 32 U1 1 U2 5 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD JUL PY 1995 VL 25 IS 3 BP 204 EP 211 PG 8 WC Paleontology SC Paleontology GA RQ547 UT WOS:A1995RQ54700003 ER PT J AU GRANT, RE AF GRANT, RE TI UPPER PERMIAN BRACHIOPODS OF THE SUPERFAMILY ORTHOTETOIDEA FROM HYDRA ISLAND, GREECE SO JOURNAL OF PALEONTOLOGY LA English DT Article AB Permian Orthotetoidea on Hydra belong to the genera Cyndalia Grant (1993a), Goniarina Cooper and Grant (1969), Derbyia Waagen (1884), Diplanus Stehli (1954), Schuchertella Girty (1904), Sicelia Merla (1934), and Tropidelasma Cooper and Grant (1969). Hydra has the most complete Permian section in the Western Tethys, 500 m thick and ranging in age from Asselian to Dorashamian. These are the youngest silicified Permian brachiopods west of China. RP GRANT, RE (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,WASHINGTON,DC 20560, USA. NR 50 TC 13 Z9 14 U1 0 U2 2 PU PALEONTOLOGICAL SOC INC PI ITHACA PA 1259 TRUMANSBURG ROAD, ITHACA, NY 14850 SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD JUL PY 1995 VL 69 IS 4 BP 655 EP 670 PG 16 WC Paleontology SC Paleontology GA RK703 UT WOS:A1995RK70300004 ER PT J AU WOOD, TC BYERS, AP JENNETTE, BD WILDT, DE AF WOOD, TC BYERS, AP JENNETTE, BD WILDT, DE TI INFLUENCE OF PROTEIN AND HORMONE SUPPLEMENTATION ON IN-VITRO MATURATION AND FERTILIZATION OF DOMESTIC CAT EGGS SO JOURNAL OF REPRODUCTION AND FERTILITY LA English DT Article ID FOLLICLE-STIMULATING-HORMONE; OOCYTES MATURED INVITRO; BOVINE OOCYTES; MEIOTIC MATURATION; ZONA-PELLUCIDA; MOUSE OOCYTES; DEVELOPMENTAL CAPACITY; LUTEINIZING-HORMONE; MAMMALIAN OOCYTES; CULTURED INVITRO AB Immature eggs were recovered from freshly excised ovaries from domestic cats, and initially 931 eggs with a compact cumulus and uniform cytoplasm were cultured in I of 15 treatments. Eagle's minimum essential medium containing, glutamine and pyruvate was supplemented with 5% (v/v) fetal calf serum (FCS), 4 mg bovine serum albumin (BSA) ml(-1) or 2 mg polyvinyl alcohol ml(-1) (PVA; non-protein control). Within each of these supplement groups, eggs were cultured with: no hormone; LH+FSH; LH+FSH+oestradiol; or LH+FSH+oestradiol+progesterone. After incubation for 52 h, eggs were inseminated with conspecific fresh spermatozoa, cultured and examined for stage of meiotic maturation and in vitro fertilization (IVF). There were fewer (P < 0.05) eggs maturing to metaphase II in vitro in FCS compared with BSA or PVA, the last two treatments producing similar (P < 0.05) results. Gonadotrophins in concert with oestradiol or oestradiol+progesterone improved the incidence of maturation (P less than or equal to 0.01) compared with no added hormones. The incidence of fertilization and cleavage in vitro ranged from 5.2 to 33.9% and varied (P < 0.05) with hormone subtreatment. Adding FSH+LH+oestradiol consistently increased the incidence of IVF approximately twofold compared with controls with no added hormones. Although it inhibited the ability of eggs to reach metaphase II, FCS in the presence of gonadotrophins and oestradiol allowed > 60% of mature eggs to fertilize in vitro (P < 0.05, compared with PVA and BSA). Inhibitory effects on egg maturation were further evaluated by testing four FCS batches from three commercial sources against BSA. All FCS batches were clearly inhibitory, as 60.7% of treated eggs arrested at the germinal vesicle stage (21.1% of BSA-treated eggs, P < 0.001). Dialysis of FCS eliminated a significant proportion of the inhibition; 69 of 158 eggs (43.7%) matured compared with 22 of 135 (16.3%) in complete or 23 of 160 (14.4%) in recombined serum. In summary, FCS appears to exert a paradoxical effect in this system, inhibiting maturation in vitro (apparently due to small molecular weight components), but promoting IVF of mature eggs if gonadotrophins and oestradiol are present. Although hormone supplementation enhanced the ability of in vitro matured eggs to fertilize and cleave, neither protein source nor the hormone treatments tested here appear responsible for the consistently low incidence of fertilization in cat eggs matured in vitro. C1 GEORGE MASON UNIV,DEPT BIOL,FAIRFAX,VA 22030. RP WOOD, TC (reprint author), SMITHSONIAN INST,NATL ZOOL PK,CONSERVAT & RES CTR,WASHINGTON,DC 20008, USA. NR 52 TC 60 Z9 65 U1 3 U2 4 PU J REPROD FERTIL INC PI CAMBRIDGE PA 22 NEWMARKET RD, CAMBRIDGE, ENGLAND CB5 8DT SN 0022-4251 J9 J REPROD FERTIL JI J. Reprod. Fertil. PD JUL PY 1995 VL 104 IS 2 BP 315 EP 323 PG 9 WC Reproductive Biology SC Reproductive Biology GA RM978 UT WOS:A1995RM97800020 PM 7473424 ER PT J AU VALLANCE, JW SIEBERT, L ROSE, WI GIRON, JR BANKS, NG AF VALLANCE, JW SIEBERT, L ROSE, WI GIRON, JR BANKS, NG TI EDIFICE COLLAPSE AND RELATED HAZARDS IN GUATEMALA SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article ID VOLCANO; ERUPTION; FUEGO; AVALANCHES; COMPLEX; HISTORY AB Guatemalan volcanoes have at least seven debris-avalanche deposits, associated with Cerro Quemado, Fuego, Pacaya, Tecuamburro and an unidentified volcano. The deposits range in size from less than 0.1 to in excess of 9 km(3) and from 2.5 to in excess of 300 km(2). The avalanches traveled 3 to 50 km from their sources in the Guatemalan highlands. Three of the avalanches occurred in Late Pleistocene time and four in Holocene time-two of them within the last 2000 years, The avalanches occurred at both andesitic and basaltic stratovolcanoes and at dacitic dome complexes, Laterally directed phreatic or magmatic pyroclastic explosions were associated with two of the debris avalanches. An evaluation of factors that might lead to an edifice collapse in Guatemala is based on the case studies presented in this report and a survey of the literature. Edifice collapses are more apt to occur if zones of weakness exist within the volcanic edifices, such as unwelded pyroclastic rocks and pervasively altered rocks, Further, the trench-ward side of volcano pairs like Fuego and Atitlan may be more likely to fail because it may have weak zones along the contact with the older back-are volcano. The direction of failure may be influenced by regional slopes, which in Guatemala generally trend southward toward the oceanic trench, and by such structural factors as multiple vents or overly steep slopes reflecting previous activity or erosion, Debris avalanches are more likely to occur in drainages which have headwaters at two or more volcanoes, Domes ate especially apt to produce small- to moderate-sized debris avalanches, and, further, if the domes form a coalescing chain, are most likely to fail in a direction normal to the chain. These factors are used at seventeen major volcanic centers in Guatemala to assess their potential for edifice collapse and most probable direction of failure. C1 SMITHSONIAN INST,GLOBAL VOLCANISM PROGRAM,WASHINGTON,DC 20560. INSIVUMEH,SECC VULCANOL,GUATEMALA CITY,GUATEMALA. US GEOL SURVEY,VANCOUVER,WA 98661. RP VALLANCE, JW (reprint author), MICHIGAN TECHNOL UNIV,DEPT GEOL ENGN & SCI,HOUGHTON,MI 49931, USA. RI Rose, William/A-7923-2009 NR 47 TC 46 Z9 47 U1 1 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD JUL PY 1995 VL 66 IS 1-4 BP 337 EP 355 DI 10.1016/0377-0273(94)00076-S PG 19 WC Geosciences, Multidisciplinary SC Geology GA RU458 UT WOS:A1995RU45800026 ER PT J AU SIEBERT, L BEGET, JE GLICKEN, H AF SIEBERT, L BEGET, JE GLICKEN, H TI THE 1883 AND LATE-PREHISTORIC ERUPTIONS OF AUGUSTINE VOLCANO, ALASKA SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article ID MOUNT-ST-HELENS; DEBRIS AVALANCHES; DEPOSITS; WASHINGTON; FLOW; STRATIGRAPHY; CHRONOLOGY; CREEK AB The eruptive history of Augustine volcano has been characterized by cycles of growth and destruction of the volcano. Repeated failure of 5-10% of the edifice has produced mobile debris avalanches that reached the sea on all sides. High lava extrusion rates rapidly restore the volcano to its pre-failure configuration. This equilibrium between constructive and destructive processes has resulted in a relatively low lava-dome complex surrounded by an apron of volcaniclastic debris three times the volume of the dome complex. The most recent edifice collapse occurred in 1883, producing the 0.3 km(3) Purr Point debris-avalanche deposit. Three major slide blocks extended the shoreline up to 2 km and produced a tsunami that swept across Cook Inlet. Hummock morphologies change from a proximal radial orientation to a dominantly transverse alignment reflecting deceleration and compression of the avalanches as they enter the sea. The breached crater formed by collapse was then largely filled by a 0.09 km(3) lava dome and a 0.04 km(3) lava flow travelled down the north flank. Lithic block-and-ash flows and pyroclastic surges reached the coast. The Burr Point avalanche deposit partially overlaps the Rocky Point debris-avalanche deposit to the west that was probably emplaced 200-400 years B.P. A major collapse event at ca. 1540 +/- 110 A.D. produced the West Island debris avalanche, ending a period of expansion of the western side of the island. An accompanying lateral blast overtopped the avalanche, covering a 40 degrees sector of the west flank. The plinian tephra layer B may also have been erupted at the time of the West Island eruption. Today Augustine volcano has rebuilt itself to a size similar to that which preceded the last edifice failure in 1883. The frequency of past collapses (three in the last 500 years) suggests that summit collapse is a possibility during any future eruption. The next major collapse is expected to involve 0.1-0.5 km(3) of the summit; the ensuing debris avalanche would likely reach the coast, producing a tsunami that could impact populated areas of the Kenai Peninsula. The largest tsunami would result from collapse in directions other than to the north or west. Tsunami magnitude is contingent on failure volume, direction and timing with respect to tides. C1 UNIV ALASKA FAIRBANKS,DEPT GEOL & GEOPHYS,FAIRBANKS,AK 99775. UNIV ALASKA FAIRBANKS,ALASKA VOLCANO OBSERV,FAIRBANKS,AK 99775. RP SIEBERT, L (reprint author), SMITHSONIAN INST,GLOBAL VOLCANISM PROGRAM,WASHINGTON,DC 20560, USA. NR 68 TC 41 Z9 41 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD JUL PY 1995 VL 66 IS 1-4 BP 367 EP 395 DI 10.1016/0377-0273(94)00069-S PG 29 WC Geosciences, Multidisciplinary SC Geology GA RU458 UT WOS:A1995RU45800028 ER PT J AU SCHWARTZ, CC MONFORT, SL DENNIS, PH HUNDERTMARK, KJ AF SCHWARTZ, CC MONFORT, SL DENNIS, PH HUNDERTMARK, KJ TI FECAL PROGESTAGEN CONCENTRATION AS AN INDICATOR OF THE ESTROUS-CYCLE AND PREGNANCY IN MOOSE SO JOURNAL OF WILDLIFE MANAGEMENT LA English DT Article DE ALASKA; ALCES ALCES; ESTRUS; FECES; GESTATION; MOOSE; PROGESTAGEN; REPRODUCTION ID WHITE-TAILED DEER; STEROIDS; URINARY AB We established a noninvasive technique for monitoring the estrous cycle and pregnancy in moose (Alces alces). We collected fecal samples daily from nonpregnant yearling females (n = 3) for the duration of 3-4 estrous cycles, and weekly throughout gestation from 3 pregnant adult cows. We analyzed samples by radioimmunoassay (RIA) to quantify the concentration of progestagen metabolites. Peak luteal phase concentrations of progestagens were 4.5 +/- 0.9 (SD) mu g/g compared with 0.5 +/- 0.1 mu g/g during the follicular phase. Observed (n = 7) and suspected (n = 2) matings all occurred within +/-2 days of the nadir in progestagen excretion. Fecal progestagens were above peak luteal phase concentrations by the eighth week of gestation (>7 mu g/g of feces, P < 0.001), permitting accurate pregnancy detection by this time. Relative concentrations of fecal progestagens during the follicular phase, luteal phase, and pregnancy were 1:10:35, respectively. Monitoring fecal progestagen is a useful noninvasive technique for tracking ovarian activity and pregnancy in moose. C1 SMITHSONIAN INST,DEPT ANIM HLTH,NATL ZOOL PK,FRONT ROYAL,VA 22630. SMITHSONIAN INST,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630. RP SCHWARTZ, CC (reprint author), ALASKA DEPT FISH & GAME,MOOSE RES CTR,34828 KALIFORNSKY BEACH RD,SUITE B,SOLDOTNA,AK 99669, USA. NR 19 TC 24 Z9 26 U1 2 U2 8 PU WILDLIFE SOC PI BETHESDA PA 5410 GROSVENOR LANE, BETHESDA, MD 20814-2197 SN 0022-541X J9 J WILDLIFE MANAGE JI J. Wildl. Manage. PD JUL PY 1995 VL 59 IS 3 BP 580 EP 583 DI 10.2307/3802466 PG 4 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA RH455 UT WOS:A1995RH45500020 ER PT J AU KALFATOVIC, MR AF KALFATOVIC, MR TI THE SUNNY SIDE OF THE ALPS - YEAR-ROUND DELIGHTS IN SOUTH TYROL AND THE DOLOMITES - HOFMANN,P SO LIBRARY JOURNAL LA English DT Book Review RP KALFATOVIC, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD JUL PY 1995 VL 120 IS 12 BP 108 EP 108 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA RH984 UT WOS:A1995RH98400279 ER PT J AU MIKHAILOVA, MV BEMIS, DL WISE, ML GERWICK, WH NORRIS, JN JACOBS, RS AF MIKHAILOVA, MV BEMIS, DL WISE, ML GERWICK, WH NORRIS, JN JACOBS, RS TI STRUCTURE AND BIOSYNTHESIS OF NOVEL CONJUGATED POLYENE FATTY-ACIDS FROM THE MARINE GREEN-ALGA ANADYOMENE STELLATA SO LIPIDS LA English DT Article ID PERFORMANCE LIQUID-CHROMATOGRAPHY; SELECTIVELY INHIBITS 5-LIPOXYGENASE; BEE VENOM PHOSPHOLIPASE-A2; NATURAL PRODUCT; ARACHIDONIC-ACID; INACTIVATION; MANOALIDE; METABOLISM; FUSCOSIDE; MECHANISM AB Novel polyunsaturated fatty acids with four conjugated double bonds were found in extracts of the green macroalga, Anadyomene stellata. The isolation of five of these with different chain lengths and varying degrees of unsaturation-16:5, 18:4, 20:5, 20:6, and 22:7-was accomplished by organic extraction followed by a combination of vacuum and high-performance liquid chromatography. One of these that was a novel substance (22:7) was characterized as 4Z,7Z,9E,11E,13Z,16Z,19Z-docosaheptaenoic acid and assigned the trivial name stellaheptaenoic acid. The structure of this new compound, isolated as its methyl ester derivative, was deduced from detailed nuclear magnetic resonance, gas chromatography/mass spectrometry (GC/MS), and other spectroscopic methods. Incubation of a chloroplast preparation, isolated from a crude algal homogenate by differential centrifugation, with six unsaturated fatty acids (palmitoleic, 6Z,9Z,12Z,15Z-octadecatetraenoic acid, arachidonic acid, eicosapentaenoic acid, 7Z,10Z,13Z,16Z-docosatetraenoic acid, and 4Z,7Z,10Z,13Z,16Z,19Z-docosahexaenoic acid) resulted in substantially increased synthesis of unique tetraene compounds as detected by ultraviolet spectrophotometry and tentatively identified by GC/MS. C1 UNIV CALIF SANTA BARBARA, INST MARINE SCI, SANTA BARBARA, CA 93106 USA. OREGON STATE UNIV, COLL PHARM, CORVALLIS, OR 97331 USA. OREGON STATE UNIV, DEPT BIOCHEM & BIOPHYS, CORVALLIS, OR 97331 USA. SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT BOT, WASHINGTON, DC 20560 USA. NR 26 TC 42 Z9 43 U1 0 U2 2 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0024-4201 EI 1558-9307 J9 LIPIDS JI Lipids PD JUL PY 1995 VL 30 IS 7 BP 583 EP 589 DI 10.1007/BF02536993 PG 7 WC Biochemistry & Molecular Biology; Nutrition & Dietetics SC Biochemistry & Molecular Biology; Nutrition & Dietetics GA RK293 UT WOS:A1995RK29300001 PM 7564911 ER PT J AU CAMERON, AGW AF CAMERON, AGW TI TRYING TO MAKE SENSE OF AL-26 ABUNDANCES SO METEORITICS LA English DT Editorial Material RP CAMERON, AGW (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORITICS JI Meteoritics PD JUL PY 1995 VL 30 IS 4 BP 363 EP 364 PG 2 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RM357 UT WOS:A1995RM35700002 ER PT J AU MACPHERSON, GJ DAVIS, AM ZINNER, EK AF MACPHERSON, GJ DAVIS, AM ZINNER, EK TI THE DISTRIBUTION OF AL-26 IN THE EARLY SOLAR-SYSTEM - A REAPPRAISAL SO METEORITICS LA English DT Review ID MURCHISON CARBONACEOUS CHONDRITE; AL-RICH INCLUSIONS; UNUSUAL ALLENDE INCLUSION; TRACE-ELEMENT ABUNDANCES; LARGE ISOTOPIC ANOMALIES; B REFRACTORY INCLUSION; GAMMA-RAY LINE; ION MICROPROBE; PRIMITIVE METEORITES; INTERSTELLAR GRAINS AB A compilation of over 1500 Mg-isotopic analyses of Al-rich material from primitive solar system matter (meteorites) shows clearly that Al-26 existed live in the early Solar System. Excesses of Mg-26 observed in refractory inclusions are not the result of mixing of ''fossil'' interstellar (26)M,Ig with normal solar system Mg. Some material was present that contained little or no Al-26, but it was a minor component of solar system matter in the region where CV3 and CO3 carbonaceous chondrites accreted and probably was a minor component in the accretion regions of CM chondrites as well. Data for other chondrite groups are too scanty to make similar statements. The implied long individual nebular histories of CAIs and the apparent gap of one or more million years between the start of CAI formation and the start of chondrule formation require the action of some nebular mechanism that prevented the CAIs from drifting into the Sun. Deciding whether Al-26 was or was not the agent of heating that caused melting in the achondrite parent bodies hinges less on its widespread abundance in the nebula than it does on the timing of planetesimal accretion relative to the formation of the CAIs. C1 UNIV CHICAGO,ENRICO FERMI INST,CHICAGO,IL 60637. WASHINGTON UNIV,MCDONNELL CTR SPACE SCI,ST LOUIS,MO 63130. WASHINGTON UNIV,DEPT PHYS,ST LOUIS,MO 63130. RP MACPHERSON, GJ (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT MINERAL SCI,MRC NHB 119,WASHINGTON,DC 20560, USA. OI Davis, Andrew/0000-0001-7955-6236 NR 181 TC 381 Z9 383 U1 3 U2 15 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORITICS JI Meteoritics PD JUL PY 1995 VL 30 IS 4 BP 365 EP 386 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RM357 UT WOS:A1995RM35700003 ER PT J AU BENSON, L AF BENSON, L TI BENEFIT CUT SO NEW SCIENTIST LA English DT Letter RP BENSON, L (reprint author), COMPUTERWORLD SMITHSONIAN AWARDS,BOSTON,MA, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU NEW SCIENTIST PUBL EXPEDITING INC PI ELMONT PA 200 MEACHAM AVE, ELMONT, NY 11003 SN 0262-4079 J9 NEW SCI JI New Sci. PD JUL 1 PY 1995 VL 147 IS 1984 BP 50 EP 50 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RG914 UT WOS:A1995RG91400050 ER PT J AU Melder, K AF Melder, K TI Margaret Fuller's New-York journalism: A biographical essay and key writings - Mitchell,CC SO NEW YORK HISTORY LA English DT Book Review RP Melder, K (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU NEW YORK STATE HIST ASSN PI COOPERSTOWN PA PO BOX 800, COOPERSTOWN, NY 13326-0800 SN 0146-437X J9 NEW YORK HIST JI N. Y. Hist. PD JUL PY 1995 VL 76 IS 3 BP 323 EP 325 PG 3 WC History SC History GA WD652 UT WOS:A1995WD65200005 ER PT J AU BROWN, ED HOPKINS, MJG AF BROWN, ED HOPKINS, MJG TI A TEST OF POLLINATOR SPECIFICITY AND MORPHOLOGICAL CONVERGENCE BETWEEN NECTARIVOROUS BIRDS AND RAIN-FOREST TREE FLOWERS NEW-GUINEA SO OECOLOGIA LA English DT Article DE POLLINATION; NECTARIVORY; RAIN-FOREST; HONEYEATERS; NEW GUINEA ID NECTAR-FEEDING BIRDS; HONEYEATER COMMUNITY; FORAGING BEHAVIOR; BANKSIA-MENZIESII; POLLEN DISPERSAL; SOUTH-AUSTRALIA; HUMMINGBIRDS; FOREST; ORGANIZATION; COEVOLUTION AB Interactions between flowering trees in a representative sample of vegetation, and the birds that fed at their flowers, were studied for 2 years in lowland tropical hill forest in New Guinea. All 2,200 trees in a 3-ha plot were tagged, identified, mapped, and monitored monthly. Approximately 60% of all individual trees flowered during the study; all species that these flowering individuals belonged to were evaluated for bird visitation. Approximately 13% of the 164 resident species of New Guinea avifauna at the study site, especially honey eaters and parrots, visited flowers. In the forest inventory plot, approximately 15-22% of all 86 tree species that flowered during the study were visited by birds; most of these tree species were canopy species. Results showed that there was no statistically significant correlation between bird species grouped by bill morphology and flower species grouped as morphotypes and ranked by nectar accessibility, although strong but unexpected bird/plant associations were evident. These associations may be related to variables such as body mass or perch size. These results are discussed in comparison with results from the Neotropics and Australia, and in terms of morphological convergence and pollinator specificity in pollination systems. C1 NYZS,WILDLIFE CONSERVAT SOC,BRONX,NY. UNIV PAPUA NEW GUINEA,DEPT BIOL,PORT MORESBY,PAPUA N GUINEA. RP BROWN, ED (reprint author), NATL MUSEUM NAT HIST,SMITHSONIAN INST,DIV BIRDS,WASHINGTON,DC 20560, USA. NR 56 TC 21 Z9 23 U1 2 U2 15 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JUL PY 1995 VL 103 IS 1 BP 89 EP 100 DI 10.1007/BF00328429 PG 12 WC Ecology SC Environmental Sciences & Ecology GA RJ294 UT WOS:A1995RJ29400012 PM 28306949 ER PT J AU MARINESCU, M DALGARNO, A AF MARINESCU, M DALGARNO, A TI DISPERSION FORCES AND LONG-RANGE ELECTRONIC-TRANSITION DIPOLE-MOMENTS OF ALKALI-METAL DIMER EXCITED-STATES SO PHYSICAL REVIEW A LA English DT Article ID RESOLVED LASER SPECTROSCOPY; ATOMS; POLARIZABILITIES; LITHIUM; SODIUM; COEFFICIENTS; LIFETIME; LI RP MARINESCU, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 30 TC 187 Z9 189 U1 0 U2 18 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUL PY 1995 VL 52 IS 1 BP 311 EP 328 DI 10.1103/PhysRevA.52.311 PG 18 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA RH932 UT WOS:A1995RH93200041 ER PT J AU ALPERT, Y AF ALPERT, Y TI DID SAGDEEV DISGUISE SOVIET SYSTEMS SINS SO PHYSICS TODAY LA English DT Letter RP ALPERT, Y (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD JUL PY 1995 VL 48 IS 7 BP 15 EP & DI 10.1063/1.2808087 PG 0 WC Physics, Multidisciplinary SC Physics GA RG350 UT WOS:A1995RG35000004 ER PT J AU BIRCHARD, GF WALSH, T ROSSCOE, R REIBER, CL AF BIRCHARD, GF WALSH, T ROSSCOE, R REIBER, CL TI OXYGEN-UPTAKE BY KOMODO-DRAGON (VARANUS-KOMODOENSIS) EGGS - THE ENERGETICS OF PROLONGED DEVELOPMENT IN A REPTILE SO PHYSIOLOGICAL ZOOLOGY LA English DT Article ID AVIAN EMBRYOS; METABOLISM; ONTOGENY; CONSUMPTION; TEMPERATURE AB Oxygen consumption was measured during incubation in the eggs of the Komodo dragon (Varanus komodoensis), a reptile that exhibits prolonged embryonic development. Oxygen consumption of eggs (mean mass 175 g) showed a sigmoidal pattern over the course of an incubation period, averaging 235.6 d at 29 degrees C. The rate Of oxygen consumption during the plateau prior to hatching averaged 151.1 mL/d. The incubation time was 210% greater and the peak oxygen consumption 53.2% less than predicted by existing allometric equations Analysis of incubation time data indicates that the Komodo dragon is not unique in having prolonged incubation times relative to those of previously studied reptiles that do not undergo diapause. The cost of development in dragons averaged 329.4 kJ (1.88 kJ/g egg mass), which is significantly higher than predicted. These results are consistent with those predicted from models of developmental energetics based on avian species. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT HERPETOL,WASHINGTON,DC 20008. UNIV NEVADA,DEPT BIOL SCI,LAS VEGAS,NV 89154. RP BIRCHARD, GF (reprint author), GEORGE MASON UNIV,DEPT BIOL,FAIRFAX,VA 22030, USA. NR 18 TC 15 Z9 16 U1 1 U2 13 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0031-935X J9 PHYSIOL ZOOL JI Physiol. Zool. PD JUL-AUG PY 1995 VL 68 IS 4 BP 622 EP 633 PG 12 WC Physiology; Zoology SC Physiology; Zoology GA RK543 UT WOS:A1995RK54300005 ER PT J AU FROESCHNER, RC AF FROESCHNER, RC TI KORMILEV,NICHOLAS,A - A LIST OF HIS ENTOMOLOGICAL PUBLICATIONS AND PROPOSED TAXA SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Item About an Individual DE KORMILEV; LISTS; PUBLICATIONS; TAXA; HETEROPTERA; NEUROPTERA AB A list of the 231 entomological publication titles and the taxonomic names proposed, alone or in coauthorship, by Nicholas A. Kormilev from 1936 to 1992 is given. Names proposed in two orders of insects-for Heteroptera: 1 family; 2 subfamilies; 6 tribes; 105 genera and subgenera; and 1182 species and subspecies; for Neuroptera: 1 generic name; 1 subspecies name. RP FROESCHNER, RC (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,NHB 127,WASHINGTON,DC 20560, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 1995 VL 97 IS 3 BP 515 EP 547 PG 33 WC Entomology SC Entomology GA RX791 UT WOS:A1995RX79100005 ER PT J AU RAO, N MATHIS, WN AF RAO, N MATHIS, WN TI A REVISION OF THE SHORE-FLY GENUS RHYSOPHORA CRESSON (DIPTERA, EPHYDRIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE DIPTERA; EPHYDRIDAE; SHORE FLIES; RHYSOPHORA; PHYLOGENY AB The New World genus Rhysophora Cresson, now placed in the tribe Discomyzini (subfamily Discomyzinae), is revised. Four species, including R. griseola (type locality: Costa Pica. Guanacaste: Colorado), which is newly described, are included. The phylogenetic relationships of the species of Rhysophora are reanalyzed, and brief comments are provided on the relationships of the genus within the tribe. A key to the genera of the tribe is included. RP RAO, N (reprint author), SMITHSONIAN INST,DEPT ENTOMOL,NHB 169,WASHINGTON,DC 20560, USA. NR 0 TC 3 Z9 4 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 1995 VL 97 IS 3 BP 666 EP 688 PG 23 WC Entomology SC Entomology GA RX791 UT WOS:A1995RX79100019 ER PT J AU Lorenzini, EC Borgonovi, C Cosmo, ML AF Lorenzini, EC Borgonovi, C Cosmo, ML TI Passive attitude stabilization of small satellites SO SPACE TECHNOLOGY-INDUSTRIAL AND COMMERCIAL APPLICATIONS LA English DT Article; Proceedings Paper CT 45th Congress of the International-Astronautical-Federation CY OCT 09-14, 1994 CL ISRAEL SOC AERONAUT & ASTRONAUT, JERUSALEM, ISRAEL SP Int Astronaut Federat, Int Acad Astronaut, Int Inst Space Law HO ISRAEL SOC AERONAUT & ASTRONAUT AB Passive stabilization can drastically simplify the design of attitude control systems of Earth-oriented satellites with moderate pointing requirements. Long tethers are attractive for passive attitude stabilization because, at the expense of a small mass increment, they provide strong restoring torques about the roll and pitch axes of the satellite. Consequently, reaction wheels and thrusters for pitch and roll control can be eliminated, thereby saving propellant mass in direct proportion to the mission duration. The attainable pointing accuracies, the masses and inertia ratios required for passive attitude stabilization are analyzed and discussed in this paper. Numerical results are derived for low and geostationary Earth's orbits for a class of small satellites. C1 UNIV ROMA LA SAPIENZA,ROME,ITALY. RP Lorenzini, EC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0892-9270 J9 SPACE TECHNOL JI Space Tech.-Ind. Comm. Appl. PD JUL PY 1995 VL 15 IS 4 BP 215 EP 221 PG 7 WC Engineering, Aerospace SC Engineering GA TM410 UT WOS:A1995TM41000006 ER PT J AU WELLER, SG WAGNER, WL SAKAI, AK AF WELLER, SG WAGNER, WL SAKAI, AK TI A PHYLOGENETIC ANALYSIS OF SCHIEDEA AND ALSINIDENDRON (CARYOPHYLLACEAE, ALSINOIDEAE) - IMPLICATIONS FOR THE EVOLUTION OF BREEDING SYSTEMS SO SYSTEMATIC BOTANY LA English DT Article ID SECT PARVIFLORAE LAMIACEAE; OUTCROSSED PROGENY; SEED PLANTS; DIOECY; GYNODIOECY; FITNESS; HYPOTHESES; SEQUENCES; ISLANDS; TREES AB Phylogenetic analysis of Schiedea and Alsinidendron (Caryophyllaceae), a monophyletic lineage endemic to the Hawaiian Islands, produced six equally most parsimonious trees with 132 steps using morphological characters. Four major clades were found in all trees. Breeding system characters were excluded from the analysis because of the likelihood that dimorphism (gynodioecy, subdioecy, dioecy) has evolved in parallel in Schieden, although subsequent inclusion of these characters had little effect on topology. Dimorphism is found in the two clades occurring primarily in dry habitats. Mapping of breeding systems on the phylogeny suggests that dimorphism has probably evolved on two or more occasions, depending on the number of character states and whether the character is treated as ordered or unordered. One to several reversals from dimorphism to hermaphroditism have also occurred. Dimorphic species occur only in dry habitats, but mapping of habitat on the phylogeny suggests that hermaphroditic species originally may have invaded dry habitats without evolving a dimorphic breeding system. Ecological shifts to very wet habitats appear to have favored the evolution of autogamy, which has occurred independently in the two clades largely restricted to mesic or wet habitats. The striking variation in breeding systems found in Schiedea and Alsinidendron appears to result in large part from the invasion of diverse habitats in the Hawaiian Islands following colonization by the ancestor of this lineage. C1 SMITHSONIAN INST, NATL MUSEUM NAT HIST, DEPT BOT, MRC 166, WASHINGTON, DC 20560 USA. RP WELLER, SG (reprint author), UNIV CALIF IRVINE, DEPT ECOL & EVOLUT BIOL, IRVINE, CA 92717 USA. NR 45 TC 63 Z9 66 U1 0 U2 4 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD JUL-SEP PY 1995 VL 20 IS 3 BP 315 EP 337 DI 10.2307/2419498 PG 23 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA RV220 UT WOS:A1995RV22000006 ER PT J AU SHEPARD, MK BRACKETT, RA ARVIDSON, RE AF SHEPARD, MK BRACKETT, RA ARVIDSON, RE TI SELF-AFFINE (FRACTAL) TOPOGRAPHY - SURFACE PARAMETERIZATION AND RADAR SCATTERING SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID IMAGES AB Starting with the assumption that planetary surfaces are self-affine (fractal) over the scales applicable to radar scattering, we derive various surface parameters, e.g., rms slopes and autocorrelation functions, and examine the implications for radar scattering models. The results of this work provide several new insights of interest to planetary geologists and others using radar to study surface features. First, the unidirectional slope histograms of self-affine surfaces are Gaussian, and the adirectional slope histograms are Rayleigh. Normalization of the adirectional histogram by solid angle results in a Gaussian adirectional slope density function and therefore a Gaussian quasi-specular angular scattering function. Next, the wavelength dependent behavior of surface roughness inferred from lunar radar observations is consistent with self-affine topography. Finally, surface rms height measurements are functions of profile length. Therefore, when determining the applicability of the small perturbation model to a surface based on those measurements, it is necessary to consider the length of the profile with respect to the sampling wavelength. C1 SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, CTR EARTH & PLANETARY STUDIES, WASHINGTON, DC 20560 USA. WASHINGTON UNIV, DEPT EARTH & PLANETARY SCI, ST LOUIS, MO 63130 USA. NR 25 TC 47 Z9 49 U1 0 U2 5 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 JUN 25 PY 1995 VL 100 IS E6 BP 11709 EP 11718 DI 10.1029/95JE00664 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RF728 UT WOS:A1995RF72800001 ER PT J AU ROBINSON, CA THORNHILL, GD PARFITT, EA AF ROBINSON, CA THORNHILL, GD PARFITT, EA TI LARGE-SCALE VOLCANIC ACTIVITY AT MAAT-MONS - CAN THIS EXPLAIN FLUCTUATIONS IN ATMOSPHERIC CHEMISTRY OBSERVED BY PIONEER-VENUS SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID DYNAMICS; CLOUDS AB Magellan (and Pioneer Venus Orbiter (PVO)) found high mountain terrains on Venus (similar to 2.5 km above 6051 km planetary radius) exhibit anomalously low radiothermal emissivity. This is thought to result from weathering of primary Venus rock, which at high altitudes produces a distinctive high-dielectric-constant mineral assemblage. Deviations from the nominal altitude-emissivity pattern have been used as a crude chronometric tool with which to date Venusian landforms. This technique indicates Maat Mons (an unusually large shield volcano, standing 9.17 km above 6051 km planetary radius, at 2.1 degrees N, 194.3 degrees E) has undergone a ''recent'' episode of large-scale volcanic activity, a deduction also implied morphologically. The present paper investigates whether a plinian eruption at Maat Mons could explain the enhanced concentrations of SO2 gas in the upper atmosphere of Venus that were detected by the Pioneer Venus UV spectrometer. The results show for a minimum vent radius of 156 m, a minimum eruption temperature of 1200 K, and a magmatic volatile content of similar to 5 wt%, a plinian eruption at the summit of Maat Mons can explain the anomalous concentration of SO2 gas. This would mean Maat Mons is an active volcano. C1 BROWN UNIV,DEPT GEOL,PROVIDENCE,RI 02912. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 20 TC 11 Z9 11 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 25 PY 1995 VL 100 IS E6 BP 11755 EP 11763 DI 10.1029/95JE00147 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RF728 UT WOS:A1995RF72800004 ER PT J AU MAXWELL, TA CRADDOCK, RA AF MAXWELL, TA CRADDOCK, RA TI AGE RELATIONS OF MARTIAN HIGHLAND DRAINAGE BASINS SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID GEOLOGIC EVOLUTION; MARS; TERRESTRIAL; VOLCANISM; CHANNELS; CRATERS; WATER; EARTH; VENUS AB Dendritic valley patterns in the equatorial highlands of Mars show evidence of internal drainage into restricted basins, which are interpreted to be floored with sedimentary fill. Based on crater frequency characteristics of six areas of enclosed basins, the origin of these intercrater plains fill units ranges from middle to late Noachian. In contrast, the age of modification of the same plains units derived from the frequency of fresh craters occupies a relatively narrow range centered on the Noachian/Hesperian boundary. In half the areas studied the timing of highlands and plains crater modification is consistent with a sedimentary origin for basin fill materials. The other plains units most likely consist of interlayered sedimentary and volcanic materials. Relations between the age of stability of these internally drained highland units and their elevation are not as distinct as prior studies suggested; a trend of decreasing age with decreasing elevation for the plains materials is not matched by similarly derived ages of the dissected highlands. Remapping and age dating of the dissected highlands and associated basins suggest that volcanic plains may be more extensive than those used in past models for magma and Volatile evolution, and support local volcanism rather than a global-scale magmatic head model for highlands plains formation. RP MAXWELL, TA (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,CTR EARTH & PLANETARY STUDIES,WASHINGTON,DC 20560, USA. RI Craddock, Robert/B-3884-2013 NR 32 TC 13 Z9 13 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 25 PY 1995 VL 100 IS E6 BP 11765 EP 11780 DI 10.1029/95JE00940 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RF728 UT WOS:A1995RF72800005 ER PT J AU FERRARI, FD AF FERRARI, FD TI 6 COPEPODID STAGES OF RIDGEWAYIA-KLAUSRUETZLERI, A NEW SPECIES OF COPEPOD CRUSTACEAN (RIDGEWAYIIDAE, CALANOIDA) FROM THE BARRIER-REEF IN BELIZE, WITH COMMENTS ON APPENDAGE DEVELOPMENT SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID DIOITHONA-OCULATA AB Ridgewayia klausruetzleri from the barrier reef in Belize differs from the five other Atlantic species of Ridgewayia in the morphology of the female genital complex and fifth leg of both females and males. Developmental patterns of setation suggest that there are six enditic lobes associated with the syncoxa and basis of maxilla 2, and that the ramal segments are exopodal. The maxilliped has a distomedial lobe on its basis and five endopodal segments, three of which are added proximally from the penultimate segment during the copepodid phase of development. The first through fourth legs exhibit the common, and presumed ancestral, pattern of segmental development. Left and right endopods of the male fifth leg are one-segmented, a condition resulting from developmental convergence for the two rami. The male fifth leg also exhibits setal loss during development of the right endopod and both exopods. RP FERRARI, FD (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL MRC534,WASHINGTON,DC 20560, USA. NR 21 TC 43 Z9 46 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 22 PY 1995 VL 108 IS 2 BP 180 EP 200 PG 21 WC Biology SC Life Sciences & Biomedicine - Other Topics GA RF863 UT WOS:A1995RF86300002 ER PT J AU RODRIGUEZALMARAZ, GA BOWMAN, TE AF RODRIGUEZALMARAZ, GA BOWMAN, TE TI SPHAEROLANA KARENAE, A NEW SPECIES OF HYPOGEAN ISOPOD CRUSTACEAN FROM NUEVO-LEON, MEXICO SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Sphaerolana karenae is described from two localities in Nuevo Leon, Mexico. It is the third known species of Sphaerolana Cole and Minckley, 1970 and differs from the two previously known species in having three rather than two pleonites visible dorsally, in having the telson pointed rather than rounded, and in having only one rather than two retinacula on the endite of the maxilliped. C1 SMITHSONIAN INST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560. RP RODRIGUEZALMARAZ, GA (reprint author), UNIV AUTONOMA NUEVO LEON,FAC CIENCIAS BIOL,AP POSTAL 105-F,CIUDAD UNIV,SAN NICOLAS GARZAS,NUEVO LEON,MEXICO. NR 2 TC 4 Z9 5 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 22 PY 1995 VL 108 IS 2 BP 207 EP 211 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA RF863 UT WOS:A1995RF86300004 ER PT J AU WILLIAMS, AB DOBBS, FC AF WILLIAMS, AB DOBBS, FC TI A NEW GENUS AND SPECIES OF CARIDEAN SHRIMP (CRUSTACEA, DECAPODA, BRESILIIDAE) FROM HYDROTHERMAL VENTS ON LOIHI SEAMOUNT, HAWAII SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID VOLCANO AB Opaepele loihi, new genus and species, is described from hydrothermal vents on Loihi Seamount, Hawaii, a mid-plate, hot-spot volcano at 18 degrees 55'N, 155 degrees 16'W, 980 m depth. This new form is related to several other bresiliid shrimps associated with hydrothermal vents, brine and hydrocarbon seeps. It has a laterally broadened triangular rostrum inconspicuously toothed on dorsal and ventral margins, carapace with pterygostomian spine present, and eyes reduced and fused mesially. This combination of characters places it in an intermediate position between a group of species in the genus Alvinocaris Williams & Chace with well developed compressed toothed rostrum, carapace with pterygostomian spine present, and eyes on separate movable stalks, and a group of species with rostrum absent (genus Rimicaris Williams) or much reduced (genus Chorocaris Martin & Hessler), carapace with pterygostomian spine absent, and eyestalks reduced and fused mesially. Only two of the vent/seep bresiliid species are now known from depths less than 1000 m, A. stactophila Williams, from hydrocarbon seeps at 5 34 m in the Gulf of Mexico, and the present new species at 980 m. C1 OLD DOMINION UNIV,DEPT OCEANOG,NORFOLK,VA 23529. RP WILLIAMS, AB (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,SYSTEMAT LAB,NATL MARINE FISHERIES SERV,WASHINGTON,DC 20560, USA. NR 13 TC 26 Z9 28 U1 1 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 22 PY 1995 VL 108 IS 2 BP 228 EP 237 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA RF863 UT WOS:A1995RF86300007 ER PT J AU MANNING, RB FELDER, DL AF MANNING, RB FELDER, DL TI DESCRIPTION OF THE GHOST SHRIMP SERGIO-MERICEAE, A NEW SPECIES FROM SOUTH FLORIDA, WITH REEXAMINATION OF S-GUASSUTINGA (CRUSTACEA, DECAPODA, CALLIANASSIDAE) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID THALASSINIDEA; SCHMITT; MEXICO AB Sergio mericeae is here described from intertidal sandflats of the Atlantic coast of Florida, where it shares habitats with Neocallichirus rathbunae and N. grandimana. This new species, formerly identified with the Brazilian species, Sergio guassutinga (until recently assigned to Neocallichirus), bears a strong resemblance to its Brazilian counterpart in body size, the unique dactylar dentition of the major chela, and most other morphological features. However, these apparent sibling species can be distinguished on the basis of body coloration and subtle but consistent differences in the third maxilliped and major cheliped. Immature specimens from Louisiana, Texas and Tamaulipas, Mexico, strongly resemble topotypic juveniles from Fort Pierce, Florida, and suggest that S. mericeae ranges into the western Gulf of Mexico. C1 UNIV SW LOUISIANA,DEPT BIOL,LAFAYETTE,LA 70504. RP MANNING, RB (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 21 TC 10 Z9 13 U1 1 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 22 PY 1995 VL 108 IS 2 BP 266 EP 280 PG 15 WC Biology SC Life Sciences & Biomedicine - Other Topics GA RF863 UT WOS:A1995RF86300011 ER PT J AU ROSS, CA MAYER, GC BOUR, R AF ROSS, CA MAYER, GC BOUR, R TI DESIGNATION OF A LECTOTYPE FOR CROCODILUS-SIAMENSIS SCHNEIDER, 1801 (REPTILIA, CROCODYLIA) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Schneider (1801) named Crocodilus siamensis on the basis of three specimens from Slam that were described and figured (but not named) in an earlier publication (Anon. 1688). None of the three specimens are known to have been preserved. Cuvier (1807) considered the syntypical series composite and proposed the replacement name Crocodilus galeatus for one of the included species. Cuvier's (1807) replacement name is assessed and rejected as unjustified. In the interest of nomenclatural stability, a lectotype of C. siamensis Schneider is designated. The type locality of C. siamensis is shown to be Louvo, Slam (= Ayutthaya, Thailand). C1 UNIV WISCONSIN PARKSIDE,DEPT BIOL SCI,KENOSHA,WI 53141. MUSEUM NATL HIST NAT,ZOOL REPTILES & AMPHIBIENS LAB,F-75005 PARIS,FRANCE. RP ROSS, CA (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 21 TC 0 Z9 0 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 22 PY 1995 VL 108 IS 2 BP 298 EP 301 PG 4 WC Biology SC Life Sciences & Biomedicine - Other Topics GA RF863 UT WOS:A1995RF86300014 ER PT J AU CARLETON, MD MUSSER, GG AF CARLETON, MD MUSSER, GG TI SYSTEMATIC STUDIES OF ORYZOMYINE RODENTS (MURIDAE, SIGMODONTINAE) - DEFINITION AND DISTRIBUTION OF OLIGORYZOMYS-VEGETUS (BANGS, 1902) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID MORPHOLOGICAL EVOLUTION; MUROID RODENTS; ZYGODONTOMYS; PATTERNS AB Morphological and distributional evidence is presented to document the specific stature of Oligoryzomys vegetus (Bangs, 1902) and to clarify its identification with respect to Central American populations of O. fulvescens. The geographic range of O. vegetus covers not only the mountains of western Panama but also the cordilleras de Tilaran, Central, and Talamanca of Costa Pica, generally above 1000 meters elevation and within lower montane and montane biotic zones. Within southern Central America, populations of O. fulvescens usually occur from sea level to 1000 meters in wet tropical and subtropical associations, but numerous instances of sympatry with O. vegetus are recorded in the 1000-1500 meter zone. Two species-group taxa, both described from Costa Pica, are allocated to subjective junior synonymy under O. vegetus, namely Oryzomys fulvescens creper Goodwin, 1945 and Oryzomys fulvescens reventazoni Goodwin, 1945. With improved understanding of its taxonomy and geographic range, Oligoryzomys vegetus emerges as another species of small terrestrial mammal restricted to the highlands of Costa Rica and western Panama, a region which has formed a modest center for mammalian endemism in southern Central America. C1 AMER MUSEUM NAT HIST,DEPT MAMMAL,NEW YORK,NY 10024. RP CARLETON, MD (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DIV MAMMALS,WASHINGTON,DC 20560, USA. NR 57 TC 22 Z9 25 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 22 PY 1995 VL 108 IS 2 BP 338 EP 369 PG 32 WC Biology SC Life Sciences & Biomedicine - Other Topics GA RF863 UT WOS:A1995RF86300017 ER PT J AU CASELLI, P MYERS, PC AF CASELLI, P MYERS, PC TI THE LINE WIDTH-SIZE RELATION IN MASSIVE CLOUD CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, CLOUDS; ISM, KINEMATICS AND DYNAMICS; ISM, MOLECULES; STARS, FORMATION ID ORION MOLECULAR CLOUD; STAR-FORMING REGIONS; DENSE CORES; DARK CLOUDS; AMMONIA OBSERVATIONS; BIPOLAR OUTFLOW; IRAS SOURCES; NGC-2071; L1641; (CO)-C-13 AB We report (CO)-C-13 and (CO)-O-18 line observations and maps in Orion A (L1641) and B (L1630). Together with already published observations, these data are used to study the line width-map size relation in massive star-forming regions. The nonthermal component of the line width (Delta upsilon(NT)) in Orion cores follows the trend Delta upsilon(NT)similar to R(q) with q = 0.21 +/- 0.03, significantly different from q = 0.53 +/- 0.07 found in low-mass cores. These relations are analyzed in the context of an equilibrium model of a spherically symmetric dense core which incorporates both thermal and nonthermal (''TNT'') motions. The internal consistency of the TNT model and Delta upsilon(NT)-R data is shown. We present general formulae for the TNT model and apply them to the observational data. Differences in the slope and in the intercept of the log Delta upsilon(NT)-log R relation between massive and low-mass cores imply significant differences in density structure, pressure profile, mass infall rate, and probably in the masses of stars which form. In particular, massive cores are denser and have steeper density profiles than low-mass cores. Visual extinction values predicted by the TNT model for low mass and massive cores (3.3 and 16 mag, respectively) are in good agreement with available observational estimates for similar objects. The higher density and pressure in massive cores lead to values for the infall time for 1 M. of similar to 7 x 10(4) yr, similar to 6 times shorter than in low-mass cores. Massive dense cores associated with embedded young stellar objects have physical properties almost identical to neighboring massive starless cores. Thus, the formation of a star or a small group of stars does not significantly affect the initial physical conditions of the associated molecular cloud core. On the other hand, line widths of ammonia cores become narrower as the distance from embedded young stellar clusters increases. In particular, the massive core farthest away from embedded clusters is mostly thermal and its kinetic temperature is similar to 10 K, similar to 2 times lower than the typical kinetic temperature of massive cores. RP CASELLI, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 60 TC 184 Z9 185 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1995 VL 446 IS 2 BP 665 EP 686 DI 10.1086/175825 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RC755 UT WOS:A1995RC75500022 ER PT J AU MAUCHE, CW RAYMOND, JC MATTEI, JA AF MAUCHE, CW RAYMOND, JC MATTEI, JA TI EUVE OBSERVATIONS OF THE ANOMALOUS 1993 AUGUST OUTBURST OF SS CYGNI SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; NOVAE, CATACLYSMIC VARIABLES; STARS, INDIVIDUAL (SS CYGNI); ULTRAVIOLET, STARS ID X-RAY-EMISSION; CATACLYSMIC VARIABLE-STARS; DWARF-NOVA OUTBURSTS; VW-HYDRI; ACCRETION DISKS; EXOSAT OBSERVATIONS; BOUNDARY-LAYER; OPTICAL OBSERVATIONS; IUE OBSERVATIONS; WX HYDRI AB Target-of-opportunity observations of the dwarf nova SS Cygni were made by the Extreme Ultraviolet Explorer (EUVE) satellite between 1993 August 17.1 and 23.6 UT (MJD 9216.6 and 9223.1). The observations cover the rise and plateau phases of an anomalous outburst which began on August 15.5 and which reached maximum at V similar to 8.3 on August 20.5. During the observations, the brightness of the source as measured by the Deep Survey instrument rose from similar to 0.015 counts s(-1) to similar to 5 counts s(-1). A delay of similar to 3 days was initially observed between the EUV and optical light curves, but this delay decreased to zero as the light curves approached maximum. During the interval August 17.3 to 23.6 UT, the 72-130 Angstrom flux as measured by the Short Wavelength Spectrometer rose from similar to 6 x 10(-13) to similar to 6.7 x 10(-11) ergs cm(-2) s(-1), while the 72-90 Angstrom to 90-130 Angstrom count ratio remained constant at 1.39 +/- 0.05. Parameterizing the EUV spectrum with a blackbody absorbed by a column of cold neutral material, we derive the luminosity L(bl) and fractional emitting area f = L(bl)/4 pi R(wd)(2) sigma T-4 of the boundary layer as a function of temperature kT. For kT = 30 eV, N-H similar to 4.4 x 10(19) cm(-2), L(bl) similar to 5 x 10(32) ergs s(-1) and f similar to 1 x 10(-4). For kT = 20 eV, N-H similar to 7.0 x 10(19) cm(-2), L(bl) similar to 2 x 10(33) ergs s(-1), and f similar to 3 x 10(-3). The optical through far-UV luminosity of the accretion disk in outburst is L(disk) similar to 3 x 10(34) ergs s(-1). Therefore, while simple theory predicts that the luminosities of the boundary layer and accretion disk should be comparable unless the white dwarf is rotating very rapidly, zeta = L(bl)/L(disk) similar to 1, we find that zeta less than or similar to 0.07. The most interesting and enigmatic aspect of these observations is the EUV spectrum, which evolved homologously over roughly two orders of magnitude in luminosity. The constancy of the EUV spectrum over such a wide range of brightness seems impossible to reconcile with the standard picture of boundary layer emission. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. AMER ASSOC VARIABLE STAR OBSERVERS, CAMBRIDGE, MA 02138 USA. RP MAUCHE, CW (reprint author), LAWRENCE LIVERMORE NATL LAB, EXPTL ASTROPHYS LAB, L-41, POB 808, LIVERMORE, CA 94550 USA. NR 63 TC 46 Z9 46 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1995 VL 446 IS 2 BP 842 EP 851 DI 10.1086/175842 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RC755 UT WOS:A1995RC75500039 ER PT J AU GREDEL, R DALGARNO, A AF GREDEL, R DALGARNO, A TI INFRARED RESPONSE OF H-2 TO X-RAYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE MOLECULAR PROCESSES; X-RAYS, GENERAL ID THRESHOLD VIBRATIONAL-EXCITATION; MOLECULAR-HYDROGEN GAS; ELECTRON-IMPACT; ULTRAVIOLET-RADIATION; STARBURST GALAXIES; SUPERNOVA-REMNANTS; INTERSTELLAR H2; LINE EMISSION; SEYFERT; CLOUDS AB The rates of population of the rovibrational levels of H-2 by the impact of energetic photoelectrons produced by the absorption of X-rays are calculated. Population occurs by excitation of electronically excited states of H-2 followed by cascading and by direct impact excitation of the lowest vibrational level. The resulting infrared spectra are presented. The emission from high vibrational levels is similar to that from ultraviolet pumping. Emission from the v = 1 and 2 vibrational levels in a gas of low fractional ionization is dominated by direct electron impact excitation. The intensity ratio of the S(1)(2-1) and S(1)(1-0) lines is 0.06 in a gas of low fractional ionization and 0.54 in a gas of high fractional ionization. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP GREDEL, R (reprint author), EUROPEAN SO OBSERV,CASILLA 19001,SANTIAGO 19,CHILE. NR 23 TC 35 Z9 35 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1995 VL 446 IS 2 BP 852 EP 859 DI 10.1086/175843 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RC755 UT WOS:A1995RC75500040 ER PT J AU TRAUB, WA JUCKS, KW JOHNSON, DG CHANCE, KV AF TRAUB, WA JUCKS, KW JOHNSON, DG CHANCE, KV TI SUBSIDENCE OF THE ARCTIC STRATOSPHERE DETERMINED FROM THERMAL EMISSION OF HYDROGEN-FLUORIDE SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID WINTER AB We determine subsidence in the Arctic stratospheric vortex from measurements of the column density of hydrogen fluoride, using a rotational line in thermal emission. The data were obtained with the far-infrared spectrometer on board the NASA DC-8 aircraft during the Arctic Airborne Stratospheric Expedition, from January through Mai ch 1992. A wide range of meteorological conditions was sampled, both inside and outside the polar vortex region. The measured values of subsidence are analyzed as a function of time of year and potential vorticity. From this analysis we draw the following conclusions: (1) Subsidence is strongly correlated with potential vorticity. However, there appear to be other factors, including meteorological conditions, which play a lesser role. (2) The gradient of subsidence with respect to potential vorticity is large and approximately constant across the Vortex wall and is small elsewhere. The gradient of subsidence with respect to horizontal distance is dramatically large across the vortex wall. (3) There appears to be substantial descent in the early winter vortex, from the evidence of the observed subsidence in January and the assumption of zero subsidence at the fall equinox. (4) Descent continues to occur in late winter, with measured vertical velocities similar to that inferred for early winter. The average early and late winter vertical velocity at a representative altitude of 18 km is 0.052(+/-0.013) cm s(-1). (5) At the measured rate of subsidence the time required to flush the stratosphere by one scale height is about 6 months. RP TRAUB, WA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, MS-19, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Johnson, David/F-2376-2015 OI Johnson, David/0000-0003-4399-5653 NR 13 TC 12 Z9 12 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 JUN 20 PY 1995 VL 100 IS D6 BP 11261 EP 11267 DI 10.1029/95JD00619 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA RF051 UT WOS:A1995RF05100018 ER PT J AU HABBAL, SR ESSER, R GUHATHAKURTA, M FISHER, RR AF HABBAL, SR ESSER, R GUHATHAKURTA, M FISHER, RR TI FLOW PROPERTIES OF THE SOLAR-WIND DERIVED FROM A 2-FLUID MODEL WITH CONSTRAINTS FROM WHITE-LIGHT AND IN-SITU INTERPLANETARY OBSERVATIONS SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CORONAL HOLE; DYNAMICS AB We derive the flow properties of the solar wind in coronal holes using a two-fluid model constrained by density profiles inferred from simultaneous space-based SPARTAN 201-01 and ground-based Mauna Loa White Light coronagraph observations, and by in situ interplanetary measurements. Also used as a guide is the hydrostatic temperature profile derived from the density gradient. Density profiles are inferred between 1.16 and 5.5 R(s), for two different density structures observed along the line of sight in a polar coronal hole. The model computations that fit remarkably well the empirical constraints yield a supersonic flow at 2.3 R(s) for the less dense ambient coronal hole, and at 3.4 R(s) for the denser structures. The novel result that emerges from these fits is a proton temperature twice as large as the electron temperature in the inner corona, reaching a peak of 2 x 10(6) K at 2 R(s). C1 NASA, GODDARD SPACE FLIGHT CTR, GREENBELT, MD USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, MS-15, CAMBRIDGE, MA 02138 USA. NR 14 TC 108 Z9 108 U1 0 U2 1 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 JUN 15 PY 1995 VL 22 IS 12 BP 1465 EP 1468 PG 4 WC Geosciences, Multidisciplinary SC Geology GA RE528 UT WOS:A1995RE52800001 ER PT J AU FRIEDSON, AJ HOFFMANN, WF GOGUEN, JD DEUTSCH, LK ORTON, GS HORA, JL DAYAL, A SPITALE, JN WELLS, WK FAZIO, GG AF FRIEDSON, AJ HOFFMANN, WF GOGUEN, JD DEUTSCH, LK ORTON, GS HORA, JL DAYAL, A SPITALE, JN WELLS, WK FAZIO, GG TI THERMAL INFRARED LIGHTCURVES OF THE IMPACT OF COMET SHOEMAKER-LEVY-9 FRAGMENT-R SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB The impact of fragment R was observed at thermal infrared wavelengths of 7.85, 10.3 and 12.2 mu m from the NASA/Infrared Telescope Facility on July 21 UT, using the MIRAC2 mid-infrared array camera. Thermal emission at the three wavelengths was sampled sequentially using a 1.8% circular variable filter, with an average time interval of 17 seconds between observations at different wavelengths. Continuous imaging of Jupiter in this mode began at 5:08 UT and extended to 5:55 UT. We present calibrated lightcurves for the three wavelengths. Clear evidence for enhanced emission from the impact region first appears at 5:41 UT, with the peak in emission at all three wavelengths occurring similar to 3.5 minutes later. The information content of the data is presented in terms of plots of the product of emissivity times angular size versus source temperature for each wavelength. Assuming that the peak in the lightcurves is due to rotation of the hot impact site into view from Earth, we estimate a diameter of similar to 1900 km for the source emitting area at 5:44:30 UT and estimate a lower limit on the source temperature at this time of similar to 1350 K. This lower limit drops to 800 K if the diameter of the emitting region was actually a factor of two larger. C1 UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ. UNIV MASSACHUSETTS,FCAD,AMHERST,MA. UNIV HAWAII,INST ASTRON,HONOLULU,HI. CALTECH,PASADENA,CA. UNIV ARIZONA,LUNAR & PLANETARY LAB,TUCSON,AZ. SMITHSONIAN ASTROPHYS OBSERV,BOSTON,MA. RP FRIEDSON, AJ (reprint author), CALTECH,JET PROP LAB,MS 169-237,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 6 TC 8 Z9 8 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 15 PY 1995 VL 22 IS 12 BP 1569 EP 1572 DI 10.1029/95GL00359 PG 4 WC Geosciences, Multidisciplinary SC Geology GA RE528 UT WOS:A1995RE52800028 ER PT J AU NICHOLSON, PD GIERASCH, PJ HAYWARD, TL MCGHEE, CA MOERSCH, JE SQUYRES, SW VANCLEVE, J MATTHEWS, K NEUGEBAUER, G SHUPE, D WEINBERGER, A MILES, JW CONRATH, BJ AF NICHOLSON, PD GIERASCH, PJ HAYWARD, TL MCGHEE, CA MOERSCH, JE SQUYRES, SW VANCLEVE, J MATTHEWS, K NEUGEBAUER, G SHUPE, D WEINBERGER, A MILES, JW CONRATH, BJ TI PALOMAR OBSERVATIONS OF THE R-IMPACT OF COMET SHOEMAKER-LEVY-9 .1. LIGHT CURVES SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB We present near-infrared observations from Palomar observatory of the impact of fragment R of comet Shoemaker-Levy 9 with Jupiter on 21 July 1994. Two instruments were used to image the event at 3.2 and 4.5 microns simultaneously. The lightcurves from these image sequences both show two faint precursor flashes, a bright main peak, and several oscillations over the following hour. We identify the precursor flashes with the entry of the bolide into Jupiter's upper atmosphere, and with the post-impact ejecta plume rising above the planet's limb. The main peak is due to the re-entry of the collapsing plume into Jupiter's atmosphere and the resultant shock heating. C1 CALTECH,PALOMAR OBSERV,DOWNS LAB 320 47,PASADENA,CA 91125. SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP NICHOLSON, PD (reprint author), CORNELL UNIV,CTR RADIOPHYS & SPACE RES,SPACE SCI BLDG,ITHACA,NY 14853, USA. RI Moersch, Jeffrey/F-7189-2010; OI Weinberger, Alycia/0000-0001-6654-7859 NR 9 TC 20 Z9 20 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 15 PY 1995 VL 22 IS 12 BP 1613 EP 1616 DI 10.1029/95GL01179 PG 4 WC Geosciences, Multidisciplinary SC Geology GA RE528 UT WOS:A1995RE52800039 ER PT J AU NICHOLSON, PD GIERASCH, PJ HAYWARD, TL MCGHEE, CA MOERSCH, JE SQUYERS, SW VANCLEVE, J MATTHEWS, K NEUGEBAUER, G SHUPE, D WEINBERGER, A MILES, JW CONRATH, BJ AF NICHOLSON, PD GIERASCH, PJ HAYWARD, TL MCGHEE, CA MOERSCH, JE SQUYERS, SW VANCLEVE, J MATTHEWS, K NEUGEBAUER, G SHUPE, D WEINBERGER, A MILES, JW CONRATH, BJ TI PALOMAR OBSERVATIONS OF THE R IMPACT OF COMET SHOEMAKER-LEVY-9 .2. SPECTRA SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID INTERSTELLAR AB We present mid-infrared spectroscopic observations from Palomar observatory of the impact of fragment R of comet P/Shoemaker-Levy 9 with Jupiter on 21 July 1994. Low-resolution 8-13 mum spectra taken near the peak of the lightcurve show a broad emission feature that resembles the silicate feature commonly seen in comets and the interstellar medium. We use this feature to estimate the dust content of the impact plume. The overall infrared spectral energy distribution at the time of peak brightness is consistent with emission from an optically-thin layer of small particles at approximate to 600 K. Integrating over the spectrum and the lightcurve, we obtain a total radiated energy from the R impact of greater than or equal to 2x10(25) ergs and a plume mass of greater than or equal to 3x10(13) g. C1 CALTECH,PALOMAR OBSERV,DOWNS LAB 320-47,PASADENA,CA 91125. SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP NICHOLSON, PD (reprint author), CORNELL UNIV,CTR RADIOPHYS & SPACE RES,SPACE SCI BLDG,ITHACA,NY 14853, USA. RI Moersch, Jeffrey/F-7189-2010; OI Weinberger, Alycia/0000-0001-6654-7859 NR 9 TC 21 Z9 21 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 15 PY 1995 VL 22 IS 12 BP 1617 EP 1620 DI 10.1029/95GL01067 PG 4 WC Geosciences, Multidisciplinary SC Geology GA RE528 UT WOS:A1995RE52800040 ER PT J AU KALFATOVIC, MR AF KALFATOVIC, MR TI ART AND MONEY - SHELL,M SO LIBRARY JOURNAL LA English DT Book Review RP KALFATOVIC, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 15 PY 1995 VL 120 IS 11 BP 69 EP 69 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA RC370 UT WOS:A1995RC37000049 ER PT J AU NAIM, A LAHAV, O BUTA, RJ CORWIN, HG DEVAUCOULEURS, G DRESSLER, A HUCHRA, JP VANDENBERGH, S RAYCHAUDHURY, S SODRE, L STORRIE-LOMBARDI, MC AF NAIM, A LAHAV, O BUTA, RJ CORWIN, HG DEVAUCOULEURS, G DRESSLER, A HUCHRA, JP VANDENBERGH, S RAYCHAUDHURY, S SODRE, L STORRIE-LOMBARDI, MC TI A COMPARATIVE-STUDY OF MORPHOLOGICAL CLASSIFICATION OF APM GALAXIES SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE METHODS, DATA ANALYSIS; GALAXIES, GENERAL; GALAXIES STRUCTURE AB We investigate the consistency of visual morphological classifications of galaxies by comparing classifications for 831 galaxies from six independent observers. The galaxies were classified on laser print copy images or on computer screen using scans made with the Automated Plate Measuring (APM) machine. Classifications are compared using the Revised Hubble numerical type index T. We find that individual observers agree with one another with rms combined dispersions of between 1.3 and 2.3 type units, typically about 1.8 units. The dispersions tend to decrease slightly with increasing angular diameter and, in some cases, with increasing axial ratio (b/a). The agreement between independent observers is reasonably good but the scatter is nonnegligible. In spite of the scatter, the Revised Hubble T system can be used to train an automated galaxy classifier, e.g. an artificial neural network, to handle the large number of galaxy images that are being compiled in the APM and other surveys. C1 UNIV ALABAMA, DEPT PHYS & ASTRON, TUSCALOOSA, AL 35487 USA. CALTECH, PASADENA, CA 91125 USA. UNIV TEXAS, DEPT ASTRON, AUSTIN, TX 78712 USA. CARNEGIE OBSERV, PASADENA, CA 91101 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. DOMINION ASTROPHYS OBSERV, VICTORIA, BC V8X 4M6, CANADA. UNIV SAO PAULO, INST ASTRON & GEOFIS, BR-01065970 SAO PAULO, BRAZIL. RP NAIM, A (reprint author), UNIV CAMBRIDGE, INST ASTRON, MADINGLEY RD, CAMBRIDGE CB3 0HA, ENGLAND. RI Sodre, Laerte/P-6045-2016 OI Sodre, Laerte/0000-0002-3876-268X NR 27 TC 76 Z9 77 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 15 PY 1995 VL 274 IS 4 BP 1107 EP 1125 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RE235 UT WOS:A1995RE23500014 ER PT J AU COLLURA, A MICELA, G SCIORTINO, S HARNDEN, FR ROSNER, R AF COLLURA, A MICELA, G SCIORTINO, S HARNDEN, FR ROSNER, R TI AN OBJECTIVE MULTICOLOR METHOD FOR THE CHARACTERIZATION OF LOW-RESOLUTION X-RAY-SPECTRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE X-RAYS, GALAXIES; X-RAYS, STARS ID STARS AB We describe a new technique for the characterization of low-resolution X-ray spectra, based on generalized colors defined by means of a principal component analysis. Application of the method to a sample of optically and radio-selected Einstein Observatory X-ray sources yields groups that are dominated either by stars or by extragalactic sources. The method thereby provides an immediate interpretation in terms of differences in the physics of the emission processes dominating the objects studied. The principal advantages of the method are that it provides an objective means of classifying source spectra and that it provides an objective means of obtaining the minimal set of spectral classification parameters. Though the method does not significantly improve results obtained with previously employed techniques when applied to Einstein data, its objective operation should prove powerful in aiding source classification in the more recent medium spectral resolution X-ray surveys based on the ROSAT and ASCA mission. C1 SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. UNIV CHICAGO,DEPT ASTRON & ASTROPHYS,CHICAGO,IL 60637. IST OSSERVATORIO ASTRON,I-90134 PALERMO,ITALY. RP COLLURA, A (reprint author), CNR,IST APPL INTERDISCIPLINARI FIS,VIA ARCHIRAFI 36,PALERMO,ITALY. OI collura, alfonso/0000-0001-9534-1235 NR 18 TC 5 Z9 5 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1995 VL 446 IS 1 BP 108 EP 114 DI 10.1086/175772 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF810 UT WOS:A1995RF81000012 ER PT J AU KUIJKEN, K AF KUIJKEN, K TI AN AXISYMMETRICAL DISTRIBUTION FUNCTION FOR THE GALACTIC BULGE SO ASTROPHYSICAL JOURNAL LA English DT Article DE CELESTIAL MECHANICS, STELLAR DYNAMICS; GALAXY, HALO; GALAXY, KINEMATICS AND DYNAMICS; GALAXY, STRUCTURE; METHODS, NUMERICAL ID SPACELAB INFRARED TELESCOPE; SURFACE MASS DENSITY; ELLIPTIC GALAXIES; MILKY-WAY; KINEMATICS; SYSTEMS; MODELS; LIGHT; DISK; BAR AB We describe a method for parameterizing two-integral distribution functions, based on triangular tessellations of the integral plane. We apply the method to the axisymmetric isotropic rotator model for the Galactic bulge of Kent (1992), and compute the projected distributions of radial velocities and proper motions expected for this model in order to allow a detailed comparison with observations. This type of analysis yields complete model predictions, significantly stronger than the velocity moments that can be calculated from the Jeans equations. In spite of strong evidence from surface photometry and from study of the gas kinematics that the Galactic bulge is not axisymmetric, the stellar kinematics in Baade's window art very similar to those of an isotropic oblate rotator. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV BASQUE COUNTRY,DEPT THEORET PHYS,BILBAO,SPAIN. NR 32 TC 22 Z9 22 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1995 VL 446 IS 1 BP 194 EP 202 DI 10.1086/175778 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF810 UT WOS:A1995RF81000018 ER PT J AU SABBEY, CN SASSELOV, DD FIELDUS, MS LESTER, JB VENN, KA BUTLER, RP AF SABBEY, CN SASSELOV, DD FIELDUS, MS LESTER, JB VENN, KA BUTLER, RP TI ON SPECTRAL-LINE FORMATION AND MEASUREMENT IN CEPHEIDS - IMPLICATIONS TO DISTANCE DETERMINATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE CEPHEIDS; LINE, FORMATION; LINE, PROFILES; STARS, DISTANCES; TECHNIQUES, RADIAL VELOCITIES ID HYDRODYNAMIC MODELS; CLASSICAL CEPHEIDS; BRIGHT CEPHEIDS; VELOCITY; RADII; PHOTOMETRY; ATMOSPHERE; VARIABLES; NGC-129 AB The formation and measurement of Cepheid photospheric spectral lines are explored to understand better the systematic effects involved in radial and pulsation velocity determination, and hence to help secure Cepheid distance scale calibrations that depend on Cepheid velocities (e.g., the Baade-Wesselink method). Using high-resolution optical and infrared spectra and synthetic line profiles, we examine techniques for measuring the position of line center and the amount of asymmetry of Cepheid absorption line profiles. The line asymmetry is observed to be a specific function of pulsation phase and to correlate with line center measurements, thus (1) the conversion factor between radial and pulsation velocity (p-factor) may not be assumed constant with phase and (2) there is a systematic offset of about 1 km s(-1) in the center-of-mass velocity. Our Cepheid models, which employ non-LTE radiative hydrodynamics, reproduce and describe (as an opacity effect) the observed unequal line asymmetry magnitudes during contraction and expansion stages. The models also allow us to study the phase dependence of the p-factor and its influence on Baade-Wesselink radius calculations. We conclude that in order to reach an accuracy of better than 7% (0.15 mag) in the zero point of the Cepheid distance scale, these systematic effects should be taken into account. C1 YALE UNIV,DEPT ASTRON,NEW HAVEN,CT 06520. UNIV TORONTO,DEPT ASTRON,TORONTO,ON,CANADA. UNIV TORONTO,ERINDALE COLL,DEPT ASTRON,MISSISSAUGA,ON L5L 1C6,CANADA. UNIV TEXAS,DEPT ASTRON,AUSTIN,TX 78712. UNIV STERNWARTE,INST ASTRON,D-81925 MUNICH,GERMANY. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. SAN FRANCISCO STATE UNIV,DEPT PHYS & ASTRON,SAN FRANCISCO,CA 94132. RP SABBEY, CN (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Butler, Robert/B-1125-2009 NR 53 TC 66 Z9 67 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1995 VL 446 IS 1 BP 250 EP 260 DI 10.1086/175783 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF810 UT WOS:A1995RF81000023 ER PT J AU DAMIANI, F MICELA, G SCIORTINO, S HARNDEN, FR AF DAMIANI, F MICELA, G SCIORTINO, S HARNDEN, FR TI EINSTEIN OBSERVATIONS OF T-TAURI STARS IN TAURUS-AURIGA .1. PROPERTIES OF X-RAY-EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, ACTIVITY; STARS, PRE-MAIN-SEQUENCE; X-RAYS, STARS ID MAIN-SEQUENCE STARS; DARK CLOUD; STELLAR POPULATION; ASTRONOMICAL DATA; ORION POPULATION; UPPER LIMITS; SEARCH; VARIABILITY; ROTATION; PLEIADES AB We present a systematic reanalysis of the Einstein IPC X-ray data on the pre-main-sequence stars in the Taurus-Auriga star formation region. We consider all cataloged stars in this region which have been observed with the IPC; of these, 52 out of 68 can be identified with X-ray sources; upper limits on the X-ray luminosity have been evaluated in the remaining cases. We derive an X-ray luminosity function and argue that its median L(x) is representative of the population intrinsic value, in spite of incompleteness of the sample and possible ambiguities in the X-ray source identifications. As a result, it is confirmed that the known steady increase in the average level of X-ray emission toward younger ages can be extended to the pre-main-sequence phase. By using the line equivalent width as the relevant parameter, a statistically significant difference is found between the distributions of X-ray luminosities of stars with and without strong emission lines. No such difference is found instead between stars with and without strong infrared excess at 25 mu m. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP DAMIANI, F (reprint author), IST OSSERVATORIO ASTRON PALERMO, PIAZZA PARLAMENTO 1, I-90134 PALERMO, ITALY. OI Damiani, Francesco/0000-0002-7065-3061 NR 66 TC 36 Z9 36 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1995 VL 446 IS 1 BP 331 EP 340 DI 10.1086/175791 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RF810 UT WOS:A1995RF81000031 ER PT J AU ELOSEGUI, P DAVIS, JL JALDEHAG, RTK JOHANSSON, JM NIELL, AE SHAPIRO, II AF ELOSEGUI, P DAVIS, JL JALDEHAG, RTK JOHANSSON, JM NIELL, AE SHAPIRO, II TI GEODESY USING THE GLOBAL POSITIONING SYSTEM - THE EFFECTS OF SIGNAL SCATTERING ON ESTIMATES OF SITE POSITION SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID AIR AB Analysis of Global Positioning System (GPS) data from two sites separated by a horizontal distance of only similar to 2.2 m yielded phase residuals exhibiting a systematic elevation angle dependence. One of the two GPS antennas was mounted on an similar to 1-m-high concrete pillar, and the other was mounted on a standard wooden tripod. We performed elevation angle cutoff tests with these data and established that the estimate of the vertical coordinate of site position was sensitive to the minimum elevation angle (elevation cutoff) of the data analyzed. For example, the estimate of the vertical coordinate of site position changed by 9.7+/-0.8 mm when the minimum elevation angle was increased from 10 degrees to 25 degrees. We performed simulations based on a simple (ray tracing) multipath model with a single horizontal reflector which demonstrated that the results from the elevation angle cutoff tests and the pattern of the residuals versus elevation angle could be qualitatively reproduced if the reflector were located 0.1-0.2 m beneath the antenna phase center. We therefore hypothesized that the elevation-angle-dependent error was caused by scattering from the horizontal surface of the pillar, located a distance of similar to 0.2 m beneath the antenna phase center. We tested this hypothesis by placing microwave absorbing material between the antenna and the pillar in a number of configurations and by analyzing the changes in apparent position of the antenna. The results indicate that (1) the horizontal surface of the pillar is indeed the main scatterer, (2) both the concrete and the metal plate embedded in the pillar are significant sources of scattering, and (3) the scattering can be reduced greatly by the use of microwave absorbing materials. These results have significant implications for the accuracy of global GPS geodetic tracking networks which use pillar-antenna configurations identical or similar to the one used for this study at the Westford WFRD GPS site. C1 CHALMERS UNIV TECHNOL, ONSALA SPACE OBSERV, S-43992 ONSALA, SWEDEN. MIT, HAYSTACK OBSERV, WESTFORD, MA 01886 USA. RP ELOSEGUI, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, MAIL STOP 42, CAMBRIDGE, MA 02138 USA. RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 29 TC 104 Z9 104 U1 2 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD JUN 10 PY 1995 VL 100 IS B6 BP 9921 EP 9934 DI 10.1029/95JB00868 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RC486 UT WOS:A1995RC48600010 ER PT J AU MATHEWS, PM BUFFETT, BA SHAPIRO, II AF MATHEWS, PM BUFFETT, BA SHAPIRO, II TI LOVE NUMBERS FOR DIURNAL TIDES - RELATION TO WOBBLE ADMITTANCES AND RESONANCE EXPANSIONS SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID INNER CORE DYNAMICS; FORCED NUTATIONS; GRAVITY CHANGES; CHANDLER-WOBBLE; EARTH DYNAMICS; OCEAN TIDE; MODEL; INTERFEROMETRY; PARAMETERS; MECHANISMS AB Wobble-related centrifugal and gravitational forces result in contributions to the Love numbers that are proportional to wobble admittances of the Earth and its core regions. We examine the nature of such forces on the basis of the recent work of Buffett et al. (1993) and present expressions relating the Love numbers to the wobble admittances. These expressions are qualitatively different from those of Sasao et al. (1980). By using a semianalytic theory for wobbles, we obtain a corresponding theory for the Love numbers and resonance formulae to describe their frequency dependence in the diurnal tidal band. In this formulation, the Earth's properties enter through a set of basic parameters (ellipticities, compliances: etc., of the whole Earth and its core regions). This analytic structure offers, for the first time, possibilities for the estimation of such parameters from data on nutation amplitudes and tides in a mutually consistent fashion. It also assures that use of a ''modified preliminary reference Earth model (modifed PREM)'' set of values for the basic parameters, which yields a free core nutation period in agreement with estimates from very long baseline interferometry (VLBI) data, will lead to resonances in the Love numbers at the corresponding nearly diurnal free wobble (NDFW) eigenfrequency. No other method is currently available for placing the resonance at the observed frequency. We present and discuss tables of values of (1) the parameters occurring in the resonance formulae for the wobbles and the Love numbers and (2) the wobble admittances and the Love numbers at various frequencies in the diurnal band, all computed using modified PREM in an approximation which takes account of all wobble-related effects but treats the Earth otherwise as spherical and static. Such detailed information on the admittances of wobbles, of the outer and inner cores, in particular, is not available elsewhere in the literature. We present comparisons of other workers' and our values for the Love numbers, to help to elucidate the sources of the differences among them. The influence of the NDFW eigenfrequency implied by the model used is notable: for the psi(1) tide which is nearest this eigenfrequency, we obtain k = 0.5382, h = 1.0812, and l = 0.0687;, while the Wahr (1981b) values, for model 1066A, which has an NDFW eigenfrequency differing significantly from the VLBI estimate, are k = 0.466, h = 0.937, 1 = 0.0736. C1 UNIV BRITISH COLUMBIA, DEPT GEOPHYS & ASTRON, VANCOUVER, BC V6T 1Z4, CANADA. RP MATHEWS, PM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 54 TC 14 Z9 17 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD JUN 10 PY 1995 VL 100 IS B6 BP 9935 EP 9948 DI 10.1029/95JB00670 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RC486 UT WOS:A1995RC48600011 ER PT J AU LUHR, JF ARANDAGOMEZ, JJ HOUSH, TB AF LUHR, JF ARANDAGOMEZ, JJ HOUSH, TB TI SAN-QUINTIN VOLCANIC FIELD, BAJA-CALIFORNIA-NORTE, MEXICO - GEOLOGY, PETROLOGY, AND GEOCHEMISTRY SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article; Proceedings Paper CT Symposium on Cenozoic Magmatism in the Colorado River Extensional Corridor and Adjacent Areas, at the Geological-Society-of-America Cordilleran/Rocky-Mountain-Section Meeting CY 1993 CL RENO, NV SP GEOL SOC AMER, CORDILLERAN ROCKY MT SECT ID LATE CENOZOIC EXTENSION; JAGUEY-MAAR COMPLEX; SPINEL-LHERZOLITE; NORTHWEST SCOTLAND; NORTHERN MEXICO; MAGMA GENESIS; UPPER MANTLE; LUIS-POTOSI; OLIVINE; EVOLUTION AB The San Quintin Volcanic Field (SQVF) is unique for the Baja California peninsula as the only known location of intraplate-type mafic alkalic volcanism and the only known source of peridotitic and granulitic xenoliths. It consists of 10 distinct Quaternary volcanic complexes. The oldest cones mainly erupted primitive magmas (Mg # >64)(Mg # = 100 x Mg/(Mg + (0.85 x Fe-Total))), which carried occasional small xenoliths. As the SQVF evolved with time, differentiated magmas (Mg # <64) became increasingly common, but primitive magmas, virtually devoid of xenoliths and unusually rich in olivine phenocrysts, dominanted at the youngest cones. Abundances of incompatible elements declined during evolution of the SQVF, implying a temporal increase in the extent of partial melting in the mantle, or progressive exhaustion of these elements in the source. Samples from two cones, Maze and Ceniza, show relatively low Ce/Pb, epsilon(Nd), and Pb-206/Pb-204 and high Sr-87/Sr-86, which we interpret as evidence for crustal contamination of these magmas. Small isotopic variations for the other cones are collectively interpreted to reflect involvement of at least three mantle components beneath the SQVF. Ranges in isotopic composition overlap for primitive and differentiated rocks, supporting fractional crystallization as the mechanism for deriving the latter from the former. Most differentiated rocks can be successfully modeled by fractional crystallization of olivine, plagioclase, clinopyroxene, and spinel from primitive parents. The largest and most abundant xenoliths were carried by differentiated magmas, indicating that fractional crystallization took place within the mantle, below the level of peridotite entrainment, and reflecting the importance of fractionation-elevated volatile contents for driving these differentiated magmas rapidly to the surface. Primitive rocks of the SQVF are unusual compared to other reported intraplate-type mafic alkalic suites from around the world in having relatively high Al2O3 and Yb, as well as low La/Yb and CaO/Al2O3. These characteristics and trends of rising Al2O3 and falling CaO with decreasing incompatible element abundances are all consistent with origins for the SQVF primitive magmas by progressive partial melting of spinel Iherzolite at unusually shallow levels in the mantle. C1 UNIV NACL AUTONOMA MEXICO, INST GEOL, ESTAC REG CTR, GUANAJUATO, MEXICO. UNIV TEXAS, DEPT GEOL SCI, AUSTIN, TX 78712 USA. RP LUHR, JF (reprint author), SMITHSONIAN INST, DEPT MINERAL SCI, NHB-119, WASHINGTON, DC 20560 USA. NR 75 TC 63 Z9 66 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD JUN 10 PY 1995 VL 100 IS B6 BP 10353 EP 10380 DI 10.1029/95JB00037 PG 28 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA RC486 UT WOS:A1995RC48600038 ER PT J AU GARGAS, A DEPRIEST, PT GRUBE, M TEHLER, A AF GARGAS, A DEPRIEST, PT GRUBE, M TEHLER, A TI MULTIPLE ORIGINS OF LICHEN SYMBIOSES IN FUNGI SUGGESTED BY SSU RDNA PHYLOGENY SO SCIENCE LA English DT Article ID CLADISTIC OUTLINE AB Phylogenetic hypotheses provide a context for examining the evolution of heterotrophic lifestyles. The lichen lifestyle, which is the symbiotic association of fungi with algae, is found in various representatives of Dicaryomycotina, both Ascomycetes and Basidiomycetes. A highly resolved parsimony analysis of small subunit ribosomal DNA (SSU rDNA) sequences suggests at least five independent origins of the lichen habit in disparate groups of Ascomycetes and Basidiomycetes. Because lichen associations arose from parasitic, mycorrhizal, or free-living saprobic fungi, neither mutualism nor parasitism should be construed as endpoints in symbiont evolution. C1 GRAZ UNIV,INST BOT,A-8010 GRAZ,AUSTRIA. UNIV STOCKHOLM,INST BOT,S-10691 STOCKHOLM,SWEDEN. RP GARGAS, A (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,NHB-166,WASHINGTON,DC 20560, USA. RI DePriest, Paula/K-6633-2015; OI Grube, Martin/0000-0001-6940-5282 NR 32 TC 214 Z9 220 U1 4 U2 32 PU AMER ASSOC ADVAN SCIENCE PI WASHINGTON PA 1333 H ST NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD JUN 9 PY 1995 VL 268 IS 5216 BP 1492 EP 1495 DI 10.1126/science.7770775 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RC190 UT WOS:A1995RC19000039 PM 7770775 ER PT J AU WASHBURN, WE AF WASHBURN, WE TI KILLING CUSTER - THE BATTLE OF THE LITTLE-BIGHORN AND THE FATE OF THE PLAINS-INDIANS - WELCH,J, STEKLER,P SO TLS-THE TIMES LITERARY SUPPLEMENT LA English DT Book Review RP WASHBURN, WE (reprint author), SMITHSONIAN INST,AMER STUDIES PROGRAM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU TIMES NEWSPAPERS LTD PI LONDON PA PO BOX 479 VIRGINIA ST, LONDON, ENGLAND E1 9XU SN 0307-661X J9 TLS-TIMES LIT SUPPL JI TLS-Times Lit. Suppl. PD JUN 9 PY 1995 IS 4810 BP 9 EP 9 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA RD969 UT WOS:A1995RD96900007 ER PT J AU WASHBURN, WE AF WASHBURN, WE TI CUSTER LAST STAND - THE ANATOMY OF AN AMERICAN MYTH - DIPPIE,BW SO TLS-THE TIMES LITERARY SUPPLEMENT LA English DT Book Review RP WASHBURN, WE (reprint author), SMITHSONIAN INST,AMER STUDIES PROGRAM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU TIMES NEWSPAPERS LTD PI LONDON PA PO BOX 479 VIRGINIA ST, LONDON, ENGLAND E1 9XU SN 0307-661X J9 TLS-TIMES LIT SUPPL JI TLS-Times Lit. Suppl. PD JUN 9 PY 1995 IS 4810 BP 9 EP 9 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA RD969 UT WOS:A1995RD96900006 ER PT J AU LONG, W DIXON, W AF LONG, W DIXON, W TI THE WISDOM OF THE BLUES, DEFINING BLUES AS THE TRUE FACTS OF LIFE - A INTERVIEW WITH DIXON,WILLIE SO AFRICAN AMERICAN REVIEW LA English DT Editorial Material RP LONG, W (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AFRICAN AMERICAN REVIEW PI TERRE HAUTE PA DEPT ENGLISH, INDIANA STATE UNIV, TERRE HAUTE, IN 47809 SN 1062-4783 J9 AFR AM REV JI Afr. Am. Rev. PD SUM PY 1995 VL 29 IS 2 BP 207 EP 212 DI 10.2307/3042292 PG 6 WC Literature, American SC Literature GA RR947 UT WOS:A1995RR94700005 ER PT J AU ROSENBERGER, AL AF ROSENBERGER, AL TI KINZEY,WARREN,GLENFORD (1935-1994) - OBITUARY SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Item About an Individual RP ROSENBERGER, AL (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008, USA. NR 1 TC 0 Z9 0 U1 0 U2 4 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD JUN PY 1995 VL 97 IS 2 BP 207 EP 211 DI 10.1002/ajpa.1330970213 PG 5 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA RB108 UT WOS:A1995RB10800012 PM 7653509 ER PT J AU CHOE, JC AF CHOE, JC TI COURTSHIP FEEDING AND REPEATED MATING IN ZOROTYPUS-BARBERI (INSECTA, ZORAPTERA) SO ANIMAL BEHAVIOUR LA English DT Article ID CRYPTIC FEMALE CHOICE; BEHAVIOR; GENITALIA; COPULATION; EVOLUTION; SELECTION; DIPTERA AB The mating behaviour of Zorotypus barberi Gurney (Insecta: Zoraptera) involves courtship feeding and repeated mating. The male performs an elaborate sequence of pre-copulatory courtship, during which he secretes a liquid substance from the cephalic gland and uses it as a courtship gift to entice females to mate. The female allows the male to copulate with her, only after she has successfully obtained the gift. Females continue to assess the mate quality even after genitalic intromission has begun and mate rejection by females is common during copulation as well as during pre-copulatory courtship. The majority of prematurely terminated copulations occur before sperm are transferred. Mating pairs usually copulate three or more times in succession and the entire sequence of courtship is repeated prior to each copulation. Females that mated three or more times lay considerably more eggs than those mated only once or twice, suggesting that sufficient sperm supplies are required for females to achieve full fecundity. By copulating repeatedly with the same male, females could obtain courtship gifts at a greater rate than mating multiply with different males because the courtship duration with the same male decreases significantly after the first copulation. Observations on females that mated with multiple males suggest that such females may copulate repeatedly with a preferred male in order to dilute the sperm from inferior males and thus affect the paternity of offspring. C1 HARVARD UNIV,DEPT ORGANISM & EVOLUTIONARY BIOL,BIOL LABS,CAMBRIDGE,MA 02138. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 34 TC 23 Z9 25 U1 0 U2 5 PU ACADEMIC PRESS (LONDON) LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD JUN PY 1995 VL 49 IS 6 BP 1511 EP 1520 DI 10.1016/0003-3472(95)90072-1 PG 10 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA RE987 UT WOS:A1995RE98700010 ER PT J AU HAHN, DC FLEISCHER, RC AF HAHN, DC FLEISCHER, RC TI DNA FINGERPRINT SIMILARITY BETWEEN FEMALE AND JUVENILE BROWN-HEADED COWBIRDS TRAPPED TOGETHER SO ANIMAL BEHAVIOUR LA English DT Article ID DISPERSION; BEHAVIOR AB This DNA fingerprinting study investigates whether females of the brood parasite brown-headed cowbird, Molothrus ater, associate with their own juvenile offspring at feeding sites more often than would be expected by chance. Cowbirds lay their eggs in the nests of a variety of host species and, as far as is known, leave them to the care of foster parents. Using baited walk-in funnel traps, 36 adult female-juvenile pairs (or trios) of cowbirds were trapped. Blood samples were collected from these individuals to conduct DNA fingerprinting analyses, calculate similarity indices, and to compare S-values for the 11 comparisons of juveniles and the females with which they were caught with S-values of random pairings of juveniles and the females in adjacent gel lanes with which they were not caught. Overall band-sharing was significantly higher for the individuals trapped together than for the random pairings. These associations between juvenile cowbirds and their mothers could occur as a result of female cowbirds monitoring the development of their young in the nests where they have laid. Alternatively, nestling cowbirds in the nest could become familiar visually and vocally with a female parent that is frequently present in their territory and could follow her when she departs for feeding grounds. In either case these data suggest that adult cowbirds associate with juveniles, in some cases their own offspring, and that offspring may learn to function as cowbirds in part from this association. C1 SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008. RP HAHN, DC (reprint author), PATUXENT WILDLIFE RES CTR,NATL BIOL SERV,LAUREL,MD 20708, USA. NR 19 TC 26 Z9 26 U1 1 U2 6 PU ACADEMIC PRESS (LONDON) LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD JUN PY 1995 VL 49 IS 6 BP 1577 EP 1580 DI 10.1016/0003-3472(95)90079-9 PG 4 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA RE987 UT WOS:A1995RE98700017 ER PT J AU RAND, H AF RAND, H TI DELACROIX 'WOMEN OF ALGIERS' SO ARTNEWS LA English DT Article RP RAND, H (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ARTNEWS ASSOCIATES PI NEW YORK PA 48 WEST 38TH STREET, NEW YORK, NY 10018 SN 0004-3273 J9 ART NEWS JI Artnews PD SUM PY 1995 VL 94 IS 6 BP 75 EP 76 PG 2 WC Art SC Art GA RC009 UT WOS:A1995RC00900032 ER PT J AU DIAFERIO, A GELLER, MJ RAMELLA, M AF DIAFERIO, A GELLER, MJ RAMELLA, M TI THE FORMATION OF COMPACT-GROUPS OF GALAXIES .2. X-RAY-PROPERTIES SO ASTRONOMICAL JOURNAL LA English DT Article ID DARK MATTER; CLUSTERS; EVOLUTION; EMISSION; GAS; SIMULATIONS; DYNAMICS C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OSSERV ASTRON TRIESTE,I-34131 TRIESTE,ITALY. RP DIAFERIO, A (reprint author), UNIV PAVIA,DIPARTIMENTO FIS NUCL & TEOR,VIA BASSI 6,I-27100 PAVIA,ITALY. NR 46 TC 29 Z9 29 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 1995 VL 109 IS 6 BP 2293 EP 2304 DI 10.1086/117452 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RA978 UT WOS:A1995RA97800001 ER PT J AU THORSTENSEN, JR KURTZ, MJ GELLER, MJ RINGWALD, FA WEGNER, G AF THORSTENSEN, JR KURTZ, MJ GELLER, MJ RINGWALD, FA WEGNER, G TI REDSHIFTS FOR FAINTER GALAXIES IN THE FIRST CFA SLICE .3. TO THE ZWICKY CATALOG LIMIT SO ASTRONOMICAL JOURNAL LA English DT Article ID LUMINOSITY FUNCTION; IRAS GALAXIES; BOOTES; SUPERCLUSTER; MORPHOLOGY; UNIVERSE C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. DARTMOUTH COLL,DEPT PHYS & ASTRON,HANOVER,NH 03755. RP THORSTENSEN, JR (reprint author), DARTMOUTH COLL,DEPT PHYS & ASTRON,HANOVER,NH 03755, USA. RI KURTZ, Michael /B-3890-2009; OI Kurtz, Michael/0000-0002-6949-0090 NR 25 TC 15 Z9 15 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 1995 VL 109 IS 6 BP 2368 EP 2375 DI 10.1086/117457 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RA978 UT WOS:A1995RA97800006 ER PT J AU MATHIEU, RD ADAMS, FC FULLER, GA JENSEN, ELN KOERNER, DW SARGENT, AI AF MATHIEU, RD ADAMS, FC FULLER, GA JENSEN, ELN KOERNER, DW SARGENT, AI TI SUBMILLIMETER CONTINUUM OBSERVATIONS OF THE T-TAURI SPECTROSCOPIC BINARY GW-ORIONIS SO ASTRONOMICAL JOURNAL LA English DT Article ID ECCENTRIC GRAVITATIONAL INSTABILITIES; INTERMEDIATE-MASS STARS; YOUNG STELLAR OBJECTS; PROTOSTELLAR DISKS; CIRCUMSTELLAR DISKS; ACCRETION DISKS; EMISSION; FRAGMENTATION; EVOLUTION; SYSTEMS C1 UNIV MICHIGAN,DEPT PHYS,ANN ARBOR,MI 48109. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NATL RADIO ASTRON OBSERV,TUCSON,AZ 85721. CALTECH,DIV GEOL & PLANETARY SCI,PASADENA,CA 91125. CALTECH,DIV PHYS MATH & ASTRON,PASADENA,CA 91125. RP MATHIEU, RD (reprint author), UNIV WISCONSIN,DEPT ASTRON,MADISON,WI 53706, USA. NR 55 TC 30 Z9 30 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 1995 VL 109 IS 6 BP 2655 EP 2669 DI 10.1086/117479 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RA978 UT WOS:A1995RA97800028 ER PT J AU BAUDRY, A MENTEN, KM AF BAUDRY, A MENTEN, KM TI VLA OBSERVATIONS OF HIGHLY EXCITED OH ABSORPTION TOWARD W3(OH) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE HII REGIONS; MASERS; STAR FORMATION; ISM, W3(OH); RADIO CONTINUUM, ISM; RADIO LINES, ISM ID VLBI SYNTHESIS OBSERVATIONS; GHZ METHANOL MASERS; RESOLUTION MAPS; W3 OH; EMISSION; REGIONS; LINES; SPECTRUM AB We have used the Very Large Array (VLA) to map the two main hyperfine lines of the highly excited (II3/2)-I-2, J = 9/2 level of OH toward the ultracompact HII region W3(OH) with high angular (0 ''.33) and spectral (0.62 km s(-1)) resolution. These transitions have frequencies near 23.8 GHz and, with energies around 500 K above the ground-state, probe hot gas in the molecular environment of the ultracompact HII region. Both lines are seen in absorption against the western half of the HII region with an angular extent and a clumpy structure similar to that of OH transitions in the (II1/2)-I-2 energy ladder, which have been previously observed with the VLA at comparable resolution. In contrast to the latter, we find for most of the area over which the OH lines are detected that the excitation of the J = 9/2 level apparently does not show strong deviations from LTE, except for a compact region near its northeastern boundary, where we tentatively detect weak maser emission in the F = 4 --> 4 transition. We have also produced a 23.8 GHz continuum map of W3(OH) that is in good agreement with previous VLA maps at similar frequencies. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP BAUDRY, A (reprint author), OBSERV BORDEAUX, BP 89, F-33270 FLOIRAC, FRANCE. NR 30 TC 14 Z9 14 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 1995 VL 298 IS 3 BP 905 EP 912 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RG130 UT WOS:A1995RG13000027 ER PT J AU KOCHANEK, CS AF KOCHANEK, CS TI EVIDENCE FOR DARK-MATTER IN MG-1654+134 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, KINEMATICS AND DYNAMICS; GALAXIES, STRUCTURE; GRAVITATIONAL LENSING ID GRAVITATIONAL LENS SYSTEM; ELLIPTICAL GALAXIES; STELLAR POPULATION; STATISTICS; ALGORITHM; IMAGES; MODELS; QUASAR; HALOS AB The radio ring lens MG 1654 + 134 strongly constrains the structure and mass of the 19 mag lens galaxy at its center. The best-fit effective radius for a de Vaucouleurs model of the lens galaxy is R(e) = 2''.0 (1''.5 < R(e) < 3''.0) marginally consistent with fits to the observed lens galaxy. The B band mass-to-light ratio interior to the ring that the galaxy would have today is (M/L)(B) = (20.4 +/- 2.8)(f(e)/1.4)h, where a passively evolving early type galaxy fades by a factor of f(e) similar or equal to 1.4 between the lens redshift and the present. This (M/L)(B) is inconsistent with stellar dynamical models of nearby ellipticals, but it is consistent with estimates from the statistics of gravitational lens numbers and separations. Isothermal models fit the ring with a halo velocity dispersion of sigma(DM) = (216 +/- 2) km s(-1), consistent with the fundamental plane, the stellar dynamics of ellipticals in dark matter halos [predicted dispersion (212 +/- 12)(f(e)/1.4)(-0.29) km s(-1)], and the statistics of gravitational lenses. This strongly supports the conclusion from lens statistics that early type galaxies do not have constant mass-to-light ratios even on scales comparable to the effective radius. Density distributions with rho proportional to (r(2) + s(2))((alpha) (-) (3)/2) fit the data only in the restricted range 0.9 less than or similar to alpha less than or similar to 1.1 where alpha = 1 is an isothermal model. Centrally concentrated models such as the Plummer or modified Hubble models require large, finite core radii (800 h(-1) and 600 h(-1) pc, respectively) but fail to fit the structure of the ring. Isothermal models only have upper limits of order 100 h(-1) pc on the core radius. The major axis of the mass distribution is 7 degrees +/- 10 degrees from the major axis of the luminosity distribution. The models clearly distinguish between different angular structures for the lens model, and a quadrupole expansion of an ellipsoidal density distribution fits the data better than a similar monopole in an external shear. RP KOCHANEK, CS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 46 TC 112 Z9 112 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 1995 VL 445 IS 2 BP 559 EP 577 DI 10.1086/175721 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RA625 UT WOS:A1995RA62500005 ER PT J AU DAVID, LP JONES, C FORMAN, W AF DAVID, LP JONES, C FORMAN, W TI COSMOLOGICAL IMPLICATIONS OF ROSAT OBSERVATIONS OF GROUPS AND CLUSTERS OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, THEORY; GALAXIES, CLUSTERS, GENERAL; GALAXIES, FUNDAMENTAL PARAMETERS; X-RAYS, GALAXIES ID COLD DARK-MATTER; LARGE-SCALE STRUCTURE; X-RAY-CLUSTERS; COMA CLUSTER; INTRACLUSTER MEDIUM; EVOLUTION; DYNAMICS; GAS; EFFICIENCY; ABUNDANCE AB We have combined ROSAT PSPC and optical observations of a sample of groups and clusters of galaxies to determine the fundamental parameters of these systems (e.g., the dark matter distribution, gas mass fraction, baryon mass fraction, mass-to-light ratio, and the ratio of total-to-luminous mass). Imaging X-ray spectroscopy of groups and clusters show that the gas is essentially isothermal beyond the central region, indicating that the total mass density (mostly dark matter) scales as rho(dark) proportional to r(-2). The density profile of the hot X-ray-emitting gas is fairly flat in groups with rho(gas) proportional to r(-1.0) and becomes progressively steeper in hotter richer systems, with rho(gas) proportional to r(-2.0) in the richest clusters. These results show, that in general, the hot X-ray-emitting gas is the most extended mass component in groups and clusters, the galaxies are the most centrally concentrated component, and the dark matter is intermediate between the two. The flatter density profile of the hot gas compared to the dark matter produces a gas mass fraction that increases with radius within each object. There is also a clear trend of increasing gas mass fraction (from 2% to 30%) between elliptical galaxies and rich clusters due to the greater detectable extent of the X-ray emission in richer systems. For the few systems in which the X-ray emission can be traced to the viriaI radius (where the overdensity delta approximate to 200), the gas mass fraction (essentially the baryon mass fraction) approaches a roughly constant value of 30%, suggesting that this is the true primordial value. Based on standard big bang nucleosynthesis, the large baryon mass fraction implies that Omega = 0.1-0.2. The antibiased gas distribution suggests that feedback from galaxy formation and hydrodynamics play important roles in the formation of structure on the scale of galaxies to rich clusters. All the groups and clusters in our sample have mass-to-light ratios of M/L(v) similar to 100-150 M./L., which strongly contrasts with the traditional view that the mass-to-light ratio of rich clusters is significantly greater than individual galaxies or groups with M/L(v) similar to 250-300 M./L.. We also show that M/L(v) is essentially constant within the virial radius of clusters (where delta greater than or similar to 200), which is consistent with the peaks formalism of biased galaxy formation. While the mass-to-light ratios of groups and clusters are comparable (indicating a constant mass fraction of optically luminous material), the ratio of the total mass-to-luminous mass (gas plus stars) monotonically decreases between galaxies and clusters. The decrease in M(tot)/M(lum) arises from two factors: (1) the composition of baryonic matter varies from a predominance of optically luminous material (stars) on the scale of galaxies (similar to 10 kpc) to a predominance of X-ray luminous material (hot gas) on the scale of rich clusters (similar to 1 Mpc), and (2) the hot gas has a more extended spatial distribution than the gravitating matter. The observed decrease in M(tot)/M(lum) between galaxies and clusters indicates that the universe actually becomes ''brighter'' on mass scales between 10(12) and 10(15) M., in the sense that a greater fraction of the gravitating mass is observable. RP DAVID, LP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, SMITHSONIAN ASTROPHYS OBSERV, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 66 TC 233 Z9 233 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 1995 VL 445 IS 2 BP 578 EP 590 DI 10.1086/175722 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RA625 UT WOS:A1995RA62500006 ER PT J AU GREBENEV, SA FORMAN, W JONES, C MURRAY, S AF GREBENEV, SA FORMAN, W JONES, C MURRAY, S TI WAVELET TRANSFORM ANALYSIS OF THE SMALL-SCALE X-RAY STRUCTURE OF THE CLUSTER ABELL-1367 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERS, GENERAL; GALAXIES, CLUSTERS, INDIVIDUAL (ABELL 1367); GALAXIES, STRUCTURE; METHODS, DATA ANALYSIS; X-RAYS, GALAXIES ID EARLY-TYPE GALAXIES; GAS AB We have developed a new technique based on a wavelet transform analysis to quantify the small-scale (less than a few arcminutes) X-ray structure of clusters of galaxies. We apply this technique to the ROSAT position sensitive proportional counter (PSPC) and Einstein high-resolution imager (HRI) images of the central region of the cluster Abell 1367 to detect sources embedded within the diffuse intracluster medium. In addition to detecting sources and determining their fluxes and positions, we show that the wavelet analysis allows a characterization of the source extents. In particular, the wavelet scale at which a given source achieves a maximum signal-to-noise ratio in the wavelet images provides an estimate of the angular extent of the source. To account for the widely varying point response of the ROSAT PSPC as a function of off-axis angle requires a quantitative measurement of the source size and a comparison to a calibration derived from the analysis of a Deep Survey image. Therefore, we assumed that each source could be described as an isotropic two-dimensional Gaussian and used the wavelet amplitudes, at different scales, to determine the equivalent Gaussian FWHM (and its uncertainty) appropriate for each source. In our analysis of the ROSAT PSPC image, we detect 31 X-ray sources above the diffuse cluster emission (within a radius of 24'), 16 of which are apparently associated with cluster galaxies and two with serendipitous, background quasars. We find that the angular extents of 11 sources exceed the nominal width of the PSPC point-spread function. Four of these extended sources were previously detected by Bechtold et al. (1983) as 1'' scale features using the Einstein HRI. The same wavelet analysis technique was applied to the Einstein HRI image. We detect 28 sources in the HRI image, of which nine are extended. Eight of the extended sources correspond to sources previously detected by Bechtold et al. Overall, using both the PSPC and the HRI observations, we detect 16 extended features, of which nine have galaxies coincident with the X-ray-measured positions (within the positional error circles). These extended sources have luminosities lying in the range (3-30) x 10(40) ergs s(-1) and gas masses of approximately (1-30) x 10(9) M., if the X-rays are of thermal origin. We confirm the presence of extended features in A1367 first reported by Bechtold ct al. (1983). The nature of these systems remains uncertain. The luminosities are large if the emission is attributed to single galaxies, and several of the extended features have no associated galaxy counterparts. The extended features may be associated with galaxy groups, as suggested by Canizares, Fabbiano, and Trinchieri (1987), although the number required is large. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP GREBENEV, SA (reprint author), RUSSIAN ACAD SCI,SPACE RES INST,84-32 PROFSOYUZNAYA,MOSCOW 117810,RUSSIA. NR 30 TC 46 Z9 46 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 1995 VL 445 IS 2 BP 607 EP 623 DI 10.1086/175725 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RA625 UT WOS:A1995RA62500009 ER PT J AU MENTEN, KM REID, MJ AF MENTEN, KM REID, MJ TI WHAT IS POWERING THE ORION KLEINMANN-LOW INFRARED NEBULA SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL, BECKLIN-NEUGEBAUER; ISM INDIVIDUAL, ORION KLEINMANN-LOW; ISM, INDIVIDUAL, IRC2; MASERS; STARS, FORMATION ID MOLECULAR CLOUD; SIO MASERS; KL NEBULA; EMISSION; RESOLUTION; OUTFLOW; REGION; IRC2; STAR; LINE AB We used the Very Large Array to observe the Orion BN/KL region simultaneously at frequencies of 8.4 and 43.1 GHz with 0''.25 resolution. At 8.4 GHz we detect a rich cluster of compact radio continuum sources, some of which are coincident with infrared sources while others do not have known infrared counterparts. At 43.1 GHz we observed continuum emission together with the v = 1, J = 1 --> 0 SiO maser line, allowing precise registration of radio continuum relative to SiO emission. We find that the radio continuum emission from one of the radio sources, I, coincides with the centroid of the SiO maser distribution. Our SiO maser maps show intricate velocity structure indicative of ordered motions that must have a rotating and expanding (or contracting) component. Since source I powers an SiO maser, it must have a high luminosity, most likely exceeding 10(4) L.. Precise astrometry shows that it does not coincide with the mid-infrared source IRc2. Given that the radio emission from source I is not affected by dust extinction, it locates the central (proto)star powering the IRc2 complex. This suggests that the location and morphology of the infrared emission from ''IRc2'' is determined by inhomogeneities of the dust envelope surrounding the central star. Furthermore, this brings into question all previous luminosity estimates of IRc2 and opens the possibility that other sources contribute significantly to the energetics of the Orion KL region. In particular, we suggest that another infrared source, n, which is coincident with a peculiar double radio source, may be responsible for at least some of the energetic phenomena observed in the region. RP MENTEN, KM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 25 TC 97 Z9 97 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 1995 VL 445 IS 2 BP L157 EP L160 DI 10.1086/187913 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RA626 UT WOS:A1995RA62600022 ER PT J AU RIESS, AG PRESS, WH KIRSHNER, RP AF RIESS, AG PRESS, WH KIRSHNER, RP TI DETERMINING THE MOTION OF THE LOCAL GROUP USING TYPE-IA SUPERNOVAE LIGHT-CURVE SHAPES SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, OBSERVATIONS; LARGE-SCALE STRUCTURE OF UNIVERSE; LOCAL GROUP; SUPERNOVAE, GENERAL ID GALAXIES AB We have measured our Galaxy's motion relative to distant galaxies in which Type Ia supernovae (SNe Ia) have been observed. The effective recession velocity of this sample is 7000 km s(-1), which approaches the depth of the survey of brightest cluster galaxies by Lauer & Postman (1994). We use the light curve shape (LCS) method for deriving distances to SNe Ia, providing relative distance estimates to individual supernovae with a precision of similar to 5% (Riess, Press, & Kirshner 1995). Analyzing the distribution on the sky of velocity residuals from a pure Hubble flow for 13 recent SNe Ia drawn primarily from the Calan/Tololo survey (Hamuy 1993a, 1994, 1995a, b; Maza et al. 1994), we find the best solution for the motion of the Local Group in this frame is 600 +/- 350 km s(-1) in the direction l = 260 degrees, b = +54 degrees, with a 1 sigma error ellipse that measures 90 degrees x 25 degrees. This solution is consistent with the rest frame of the cosmic microwave background (CMB) as determined by the COBE measurement of the dipole temperature anisotropy, and also with many plausible bulk hows expected to accompany observed density variations. It is inconsistent with the velocity observed by Lauer & Postman. RP RIESS, AG (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 28 TC 76 Z9 76 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 1995 VL 445 IS 2 BP L91 EP L94 DI 10.1086/187897 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RA626 UT WOS:A1995RA62600006 ER PT J AU BICAY, MD KOJOIAN, G SEAL, J DICKINSON, DF MALKAN, MA AF BICAY, MD KOJOIAN, G SEAL, J DICKINSON, DF MALKAN, MA TI A MULTIFREQUENCY RADIO-CONTINUUM AND IRAS FAINT SOURCE SURVEY OF MARKARIAN GALAXIES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE GALAXIES, SEYFERT; GALAXIES, STARBURST; INFRARED, GALAXIES; RADIO CONTINUUM, GALAXIES SURVEYS ID EMISSION-LINE OBJECTS; INFRARED-EMISSION; MULTIPLE NUCLEI; POSITIONS AB Results are presented from a multifrequency radio continuum survey of Markarian galaxies (MRKs) and are supplemented by IRAS infrared data from the Faint Source Survey. Radio data are presented for 899 MRKs observed at nu = 4.755 GHz with the NRAO-Green Bank 300 foot(91 m) telescope, including nearly 88% of those objects in Markarian lists VI-XIV. In addition, 1.415 GHz measurements of 258 MRKs, over 30% of the MRKs accessible from NAIC-Arecibo, are reported. Radio continuum observations of smaller numbers of MRKs were made at 10.63 GHz and at 23.1 GHz and are also presented. The ( 1.415 GHz, 4.755 GHz) percentages of ''probable'' detections were found to be (37%, 15%) for the MRK sample as a whole. These detection rates increased to (49%, 33%) among Seyfert MRKs, and to (73%, 42%) for those classified as having starburst nuclei. The vast majority of radio-detected MRKs have radio luminosities h(2)P(1.415) < 10(23) W HZ(-1) characteristic of ''normal galaxies.'' Infrared data from the IRAS Faint Source Survey (Ver. 2) are presented for 944 MRKs, with reasonably secure identifications extracted from the NASA/IPAC Extragalactic Database. MRKs exhibit the same canonical infrared characteristics as those reported for various other galaxy samples, that is, the well-known enhancement of the 25 mu m/60 mu m color ratio among Seyfert MRKs, and a clear tendency for MRKs with warmer 60 mu m/100 mu m colors to also possess cooler 12 mu m/25 mu m colors. In addition, non-Seyfert MRKs are found to obey the well-documented infrared/radio luminosity correlation, with the tightest correlation seen for starburst MRKs. Linear regression fits to the infrared/radio correlations yield these relationships: log L(FIR) = 0.77 log P-1.415 + 19.95 (r = 0.96) and log L(FIR) = 0.89 log P-4.755 + 17.51 (r = 0.90). Mean values of the infrared/radio ratios are consistent with those derived for various optically selected galaxy samples. The FIR/radio ratios for starburst MRKs are enhanced by a factor of 3 over those for Seyfert MRKs. There is no statistically significant difference between the infrared/radio ratios of single-nucleus and multiple-nucleus MRKs, although the analysis is complicated by small sample sizes. C1 CALTECH,JET PROP LAB,DIV EARTH & SPACE SCI,PASADENA,CA 91125. NASA HEADQUARTERS,DIV ASTROPHYS,WASHINGTON,DC 20546. UNIV WISCONSIN,DEPT PHYS & ASTRON,EAU CLAIRE,WI 54702. CAMBRIDGE RES,CHAMPAIGN,IL 61821. LOCKHEED PALO ALTO RES LABS,PALO ALTO,CA 94304. UNIV CALIF LOS ANGELES,DEPT ASTRON,LOS ANGELES,CA 90024. RP BICAY, MD (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20546, USA. NR 55 TC 34 Z9 34 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 1995 VL 98 IS 2 BP 369 EP 440 DI 10.1086/192168 PG 72 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QZ758 UT WOS:A1995QZ75800001 ER PT J AU GOLDSWORTHY, SD AF GOLDSWORTHY, SD TI DIFFERENTIAL EXPENDITURE OF MATERNAL RESOURCES IN ANTARCTIC FUR SEALS, ARCTOCEPHALUS-GAZELLA, AT HEARD-ISLAND, SOUTHERN INDIAN-OCEAN SO BEHAVIORAL ECOLOGY LA English DT Article DE ANTARCTIC FUR SEAL; ARCTOCEPHALUS-GAZELLA; DIFFERENTIAL EXTRACTION; MATERNAL EXPENDITURE; PARENT OFFSPRING CONFLICT; SEX ALLOCATION AB Maternal expenditure in lactating Antarctic fur seals (Arctocephalus gazella) was studied at Heard Island in the 1987 to 1988 summer/autumn. The mean birth mass, growth rate, and mass at 60 days of sons were significantly greater than those of daughters. Maternal foraging trips lasted on average 5.9 days, and attendance bouts lasted 1.5 days. Over the course of this study, foraging trip duration increased from 5.0 to 7.0 days, and attendance duration declined from 2.0 to 1.5 days. Pups lost 3.2% of their body mass/day while their mothers foraged at sea, but gained mass rapidly during periods of maternal attendance. Sons gained significantly more body mass (1.9 kg) compared with daughters (1.3 kg) during maternal attendance, suggesting that sons consume more milk. Sex differences in mass gain were unrelated to pup age or body mass. During 2-day maternal attendance bouts, sons gained most of their mass (71%) during the first day, and daughters increased mass at almost the same rate each day. The increase in mass by sons during maternal attendance was significantly positively related to both the duration of their mothers' preceding and subsequent foraging trips. In contrast, mass gained by daughters was positively related to the duration of their mothers' attendance. Mass at 60 days age was negatively related to birth date in sons, and positively related to birth mass in daughters. These data indicate that (1) greater maternal resources are expended on sons than on daughters, (2) sons receive greater maternal resources because they are male, and not because of their greater birth mass and body size, (3) different factors appear to be important in determining high postnatal growth in sons and daughters, and (4) demand for resources by sons can influence maternal behavior and ultimately the level of resources received. RP GOLDSWORTHY, SD (reprint author), SMITHSONIAN INST,DEPT ZOOL RES,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 0 TC 32 Z9 32 U1 0 U2 9 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 SN 1045-2249 J9 BEHAV ECOL JI Behav. Ecol. PD SUM PY 1995 VL 6 IS 2 BP 218 EP 228 DI 10.1093/beheco/6.2.218 PG 11 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA RD051 UT WOS:A1995RD05100015 ER PT J AU WINDSOR, DM DEMACEDO, MV SIQUEIRACAMPOS, AD AF WINDSOR, DM DEMACEDO, MV SIQUEIRACAMPOS, AD TI FLOWER FEEDING BY SPECIES OF ECHOMA CHEVROLAT (COLEOPTERA, CHRYSOMELIDAE, CASSIDINAE) ON MIKANIA (ASTERACEAE) IN PANAMA AND BRAZIL SO COLEOPTERISTS BULLETIN LA English DT Article AB We observed Echoma sp. nr. bonfilsi (Boheman) males competing for mates and copulating while females oviposited within fresh inflorescences of Mikania guaco H. and B. (Asteraceae) in Panama. Adults and all larval instars fed exclusively upon unopened and recently opened florets of this plant. This is the first record of flower feeding among tortoise beetles (Chrysomelidae, Cassidinae) and the first host plant record for any Echoma species. Observations of Echoma marginata (L.), in Brazil confirm that larvae and adults of this species also feed upon unopened hewers of an asteraceous host, Mikania stipulacea Willd. The incubation period for eggs and the overall developmental period for the immature stages in these two species is shorter than in several leaf feeding species of the same tribe (Stolaini). RP WINDSOR, DM (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA ANCON,PANAMA. NR 0 TC 5 Z9 6 U1 0 U2 1 PU COLEOPTERISTS SOC PI NATCHEZ PA P.O. BOX 767, NATCHEZ, MS 39121 SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD JUN PY 1995 VL 49 IS 2 BP 101 EP 108 PG 8 WC Entomology SC Entomology GA RE815 UT WOS:A1995RE81500001 ER PT J AU PEKARIK, A AF PEKARIK, A TI JAPANESE DESIGN, A SURVEY SINCE 1950 SO DESIGN ISSUES LA English DT Art Exhibit Review RP PEKARIK, A (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU MIT PRESS PI CAMBRIDGE PA 55 HAYWARD ST JOURNALS DEPT, CAMBRIDGE, MA 02142 SN 0747-9360 J9 DES ISSUES JI Des. Iss. PD SUM PY 1995 VL 11 IS 2 BP 71 EP 84 DI 10.2307/1511760 PG 14 WC Architecture SC Architecture GA RG648 UT WOS:A1995RG64800006 ER PT J AU TISSUE, DT WRIGHT, SJ AF TISSUE, DT WRIGHT, SJ TI EFFECT OF SEASONAL WATER AVAILABILITY ON PHENOLOGY AND THE ANNUAL SHOOT CARBOHYDRATE CYCLE OF TROPICAL FOREST SHRUBS SO FUNCTIONAL ECOLOGY LA English DT Article DE PANAMA; PSYCHOTRIA; REPRODUCTION; STORED CARBON; TROPICAL RAIN FOREST ID SUBGENUS PSYCHOTRIA RUBIACEAE; DROUGHT ACCLIMATION; CLIMATE TREES; UNDERSTORY; REVISION; PATTERNS; STORAGE; PLANTS AB 1. The effect of seasonal water availability on phenology and shoot total non-structural carbohydrate (TNC) of three Psychotria species was investigated by irrigating two large plots of mature tropical forest in Panama during the dry season for five consecutive years. This study reports results for the fifth and final year of irrigation. 2. Irrigation did not affect total production of leaves, inflorescences or infructescenes but did advance the timing of leaf production in all Psychotria, and advanced the timing of inflorescence production in P. furcata and P. marginata and infructescence production in P. furcata. Irrigation also reduced shoot TNC levels. 3. Shoot TNC levels in all three species of Psychotria showed similar depressions at the end of the dry season and maximum levels near the end of the wet season. Depletion of shoot TNC occurred just before or during peak leaf production but did not coincide with production of inflorescences or infructescences. Therefore, we hypothesize that shoot TNC supported part of the cost of new leaf production but production of inflorescences and infructescences was most likely supported by current photosynthate. 4. Tropical plants generally show less seasonal variation in TNC than plants from more variable climates but stored carbon still plays an important role in the growth of Psychotria, although its direct role in reproduction appears limited. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RI Wright, Stuart/M-3311-2013; Tissue, David/H-6596-2015 OI Wright, Stuart/0000-0003-4260-5676; Tissue, David/0000-0002-8497-2047 NR 43 TC 112 Z9 120 U1 0 U2 17 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD JUN PY 1995 VL 9 IS 3 BP 518 EP 527 DI 10.2307/2390018 PG 10 WC Ecology SC Environmental Sciences & Ecology GA RF969 UT WOS:A1995RF96900022 ER PT J AU JOHNSON, DG TRAUB, WA CHANCE, KV JUCKS, KW AF JOHNSON, DG TRAUB, WA CHANCE, KV JUCKS, KW TI DETECTION OF HBR AND UPPER LIMIT FOR HOBR - BROMINE PARTITIONING IN THE STRATOSPHERE SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB We determine mixing ratio profiles for HBr and upper limits for HOBr in the stratosphere with precisions up to 1.7 and 4.8 parts per trillion, respectively, using the combined data from 7 flights of our far-infrared spectrometer. The measurements suggest that in the range 22-34 km the average mixing ratio of HBr is 2.0 +/- 0.8, and that the average mixing ratio of HOBr is less than 2.8 ppt. Our measurements of HBr are in reasonable agreement with a photochemical model which includes 0 or 2% production of HBr through the reaction of BrO with HO2, but in strong disagreement with a model including 5 or 10% HBr production. RP JOHNSON, DG (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Johnson, David/F-2376-2015; OI Johnson, David/0000-0003-4399-5653; Chance, Kelly/0000-0002-7339-7577 NR 15 TC 44 Z9 44 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 1 PY 1995 VL 22 IS 11 BP 1373 EP 1376 DI 10.1029/95GL01349 PG 4 WC Geosciences, Multidisciplinary SC Geology GA RB550 UT WOS:A1995RB55000015 ER PT J AU STONER, R BEKEFI, G AF STONER, R BEKEFI, G TI A 70-PERIOD HIGH-PRECISION MICROWIGGLER FOR FREE-ELECTRON LASERS SO IEEE JOURNAL OF QUANTUM ELECTRONICS LA English DT Article ID UNDULATOR; PERFORMANCE; WIGGLER AB We have designed, constructed, and operated a 70-period microwiggler for free electrons lasers (FEL's), The device is a pulsed ferromagnetic core electromagnet with a period of 8.8 mm, which generates an on-aids peak magnetic field of 4.2 kG. The pulses, of 0.5 ms duration, are generated at a rate of 0.5 Hz, Each field peak is independently tunable, We employed a novel tuning regimen to reduce the RMS spread in the peak amplitudes to 0.12%, the lowest value thus far attained in a sub cm-period periodic magnetic field. C1 MIT,ELECTR RES LAB,CAMBRIDGE,MA 02139. SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. RP STONER, R (reprint author), MIT,DEPT PHYS,CAMBRIDGE,MA 02139, USA. OI Stoner, Richard/0000-0001-7949-6747 NR 14 TC 14 Z9 14 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017-2394 SN 0018-9197 J9 IEEE J QUANTUM ELECT JI IEEE J. Quantum Electron. PD JUN PY 1995 VL 31 IS 6 BP 1158 EP 1165 DI 10.1109/3.387055 PG 8 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA QZ924 UT WOS:A1995QZ92400023 ER PT J AU POST, RC AF POST, RC TI SANDOW THE MAGNIFICENT - SANDOW,EUGENE AND THE BEGINNINGS OF BODYBUILDING - CHAPMAN,DL SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review RP POST, RC (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGAN AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47401 SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD JUN PY 1995 VL 82 IS 1 BP 283 EP 283 DI 10.2307/2082059 PG 1 WC History SC History GA RD316 UT WOS:A1995RD31600147 ER PT J AU PISANO, DA AF PISANO, DA TI HEROES WITHOUT LEGACY - AMERICAN AIRWOMEN, 1912-1944 - JAROS,D SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review RP PISANO, DA (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGAN AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47401 SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD JUN PY 1995 VL 82 IS 1 BP 305 EP 305 DI 10.2307/2082085 PG 1 WC History SC History GA RD316 UT WOS:A1995RD31600174 ER PT J AU BUNCH, LG AF BUNCH, LG TI THEY HAD A DREAM - THE STORY OF AFRICAN-AMERICAN ASTRONAUTS - PHELPS,JA SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review RP BUNCH, LG (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGAN AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47401 SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD JUN PY 1995 VL 82 IS 1 BP 361 EP 361 DI 10.2307/2082153 PG 1 WC History SC History GA RD316 UT WOS:A1995RD31600244 ER PT J AU STARK, MT CLARK, JJ ELSON, MD AF STARK, MT CLARK, JJ ELSON, MD TI CAUSES AND CONSEQUENCES OF MIGRATION IN THE 13TH-CENTURY TONTO BASIN SO JOURNAL OF ANTHROPOLOGICAL ARCHAEOLOGY LA English DT Review ID STYLE; TECHNOLOGY; ANTHROPOLOGY; ETHNICITY AB Archaeological evidence for migration into the Tonto Basin during the early Classic period (ca. A.D. 1150-1350) is examined in this study. The Tonto Basin, located in central Arizona, provides an ideal setting for investigating prehistoric migration for several reasons: (1) it is located in an interstitial zone in both environmental and cultural terms; (2) an enormous amount of archaeological information is now available for the Classic period; and (3) migrant groups can be differentiated from the local population based on material remains. In this study, concepts from the anthropology of technology are applied to architectural and ceramic data to examine migration patterns in the 13th-century Tonto Basin. The effects of migration on the sociopolitical organization of the local population are also discussed. (C) 1995 Academic Press, Inc. C1 CTR DESERT ARCHAEOL,TUCSON,AZ. RP STARK, MT (reprint author), SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560, USA. OI Stark, Miriam/0000-0003-1700-4406 NR 124 TC 17 Z9 17 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 SN 0278-4165 J9 J ANTHROPOL ARCHAEOL JI J. Anthropol. Archaeol. PD JUN PY 1995 VL 14 IS 2 BP 212 EP 246 DI 10.1006/jaar.1995.1012 PG 35 WC Anthropology; Archaeology SC Anthropology; Archaeology GA RG544 UT WOS:A1995RG54400008 ER PT J AU CHEN, ZY STANLEY, DJ AF CHEN, ZY STANLEY, DJ TI QUATERNARY SUBSIDENCE AND RIVER CHANNEL MIGRATION IN THE YANGTZE DELTA PLAIN, EASTERN CHINA SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE CHANNEL MIGRATION; DELTA PLAIN; EAST CHINA SEA; FLUVIAL SAND TYPES; PROVENANCE; QUATERNARY STRATIGRAPHY; SUBSIDENCE; TAIHU LAKE; YANGTZE DELTA; YELLOW SEA ID EVOLUTION AB The Yangtze delta's fluvial channel system and overall depocenter configuration have been controlled largely by movement of active subsurface structures during most of the Quaternary. Data from numerous borings reveal marked variations in lithic distribution and thickness of Pleistocene and Holocene sequences across the delta plain. These stratigraphic differences record shifts in the Yangtze's depocenter through time and are in large part a direct response to the interaction of land motion with sea level variations and fluvial and oceanographic professes. Delta plain subsidence has progressed from north to south since early Quaternary time, and this has induced a southward shift of the Yangtze river channel from the early Pleistocene to the present. During much of Quaternary time, the Yangtze river flowed across the northern part of the delta's plain. This is primarily the results of two factors: differential subsidence of the northern sector from the upper Tertiary to the late Pleistocene; and a ''topographic barrier effect'' produced by highlands which blocked the Yangtze from Bowing to and across the southern sector of the plain. Thus, fluvial Quaternary deposits in the southern plain were not derived from the Yangtze river but from proximal highlands west of the southern delta plain. Stratal cofiguration, texture and composition serve to distinguish Yangtze river deposits concentrated in the north from the more proximal fluvial channel sediments in the south. Our investigation suggests that tectonically induced channel migration and southward shift, of the Yangtze deltaic depocenter are continuing at present. These ongoing depositional changes related to differential subsidence have potentially serious ramifications for this low-lying, densely populated delta plain area. Hence, accurate measurements of land subsidence are needed throughout the plain, and particularly in the lower reaches of the Yangtze river. C1 SMITHSONIAN INST,NMNH E206,DELTAS GLOBAL CHANGE PROGRAM,WASHINGTON,DC 20560. RP CHEN, ZY (reprint author), E CHINA NORMAL UNIV,DEPT GEOG,SHANGHAI 200062,PEOPLES R CHINA. NR 51 TC 46 Z9 61 U1 4 U2 8 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD SUM PY 1995 VL 11 IS 3 BP 927 EP 945 PG 19 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA RN670 UT WOS:A1995RN67000033 ER PT J AU GOODWAY, M AF GOODWAY, M TI THE TRADITIONAL USE OF AN ORE MINERAL AS AN ABRASIVE SO JOURNAL OF FIELD ARCHAEOLOGY LA English DT Note AB Chalcopyrite (CuFeS2) was identified as the main constituent of Trent sand, and naturally-occurring abrasive that until the last few years was traditionally employed in the Birmingham (England) Jewellery Quarter for buffing metal. Since chalcopyrite is one of the chief ores of copper and has not heretofore been identified in an abrasive, the possibility exists that excavated particulate chalcopyrite used as a polishing material may be misinterpreted as dressed ore. The same possibility of misinterpretation holds true of black-smiths' ''iron scale'' as well. RP GOODWAY, M (reprint author), SMITHSONIAN INST,CONSERVAT ANALYT LAB,MRC 534,WASHINGTON,DC 20560, USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU JOURNAL FIELD ARCHAEOLOGY PI BOSTON PA BOSTON UNIV 675 COMMUNWEALTH AVE, BOSTON, MA 02215 SN 0093-4690 J9 J FIELD ARCHAEOL JI J. Field Archaeol. PD SUM PY 1995 VL 22 IS 2 BP 255 EP 256 DI 10.2307/530328 PG 2 WC Archaeology SC Archaeology GA RE728 UT WOS:A1995RE72800010 ER PT J AU FLEISCHER, RC TARR, CL AF FLEISCHER, RC TARR, CL TI PLAIN WREN DESTROYS EGG OF DUSKY ANTBIRD SO JOURNAL OF FIELD ORNITHOLOGY LA English DT Article AB A Plain Wren was observed to pierce one of two eggs in the nest of a Dusky Antbird in Gamboa, Panama Province, Republic of Panama. This is the first report of egg destruction by a tropical wren species. RP FLEISCHER, RC (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 5 TC 2 Z9 2 U1 1 U2 3 PU ASSOC FIELD ORNITHOLOGISTS PI BELOIT PA BELOIT COLLEGE, DEPT BIOLOGY, 700 COLLEGE ST, BELOIT, WI 53511 SN 0273-8570 J9 J FIELD ORNITHOL JI J. Field Ornithol. PD SUM PY 1995 VL 66 IS 3 BP 404 EP 405 PG 2 WC Ornithology SC Zoology GA RL134 UT WOS:A1995RL13400012 ER PT J AU HEYER, WR GASCON, C AF HEYER, WR GASCON, C TI COLLECTION NOTES AND CALL CHARACTERISTICS FOR ISCHNOCNEMA-QUIXENSIS AND PHYZELAPHRYNE-MIRIAMAE (AMPHIBIA, ANURA, LEPTODACTYLIDAE) SO JOURNAL OF HERPETOLOGY LA English DT Note C1 INST NACL PESQUISAS,PROJECTO DINAM BIOL FRAGMENTOS FLORESTAIS ECOL,BR-69083 MANAUS,AMAZONAS,BRAZIL. RP HEYER, WR (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,DEPT VERTEBRATE ZOOL,MRC 162,WASHINGTON,DC 20560, USA. NR 6 TC 5 Z9 5 U1 0 U2 1 PU SOC STUD AMPHIBIANS REPTILES PI OXFORD PA DEPT OF ZOOLOGY MIAMI UNIV, OXFORD, OH 45056 SN 0022-1511 J9 J HERPETOL JI J. Herpetol. PD JUN PY 1995 VL 29 IS 2 BP 304 EP 307 DI 10.2307/1564574 PG 4 WC Zoology SC Zoology GA TA490 UT WOS:A1995TA49000023 ER PT J AU FAUST, MA MORTON, SL AF FAUST, MA MORTON, SL TI MORPHOLOGY AND ECOLOGY OF THE MARINE DINOFLAGELLATE OSTREOPSIS-LABENS SP-NOV (DINOPHYCEAE) SO JOURNAL OF PHYCOLOGY LA English DT Article DE BELIZE, CORAL REEF; DINOPHYCEAE; EAST CHINA SEA; ECOLOGY; IRIOMOTE ISLAND, JAPAN; LIGHT MICROSCOPY; MAN OF WAR CAY; BELIZE; OSHIGAKI ISLAND, JAPAN ID GAMBIERDISCUS; TOXICITY AB A new species, Ostreopsis labens Faust et Morton sp. nov., is described from three marine habitats: lagoonal water and Lagoonal sand from the barrier reef of Belize, and associated with macroalgae from coral reef habitats of Oshigaki and Iriomote Islands, Japan. Dimensions of Ostreopsis labens cells are 60-86 mu m long, 70-80 mu m wide, and 81-110 mu m in dorsoventral depth. Cells are broadly ovoid, anterioposteriorly compressed bearing a spherical nucleus and many chloroplasts. The epitheca is convex and composed of three apical plates, seven precingular plates, and an apical pore plate. The cingulum is composed of six plates. The hypotheca is constructed of five posticugular plates, one posterior intercalary and two antapical plates. The sulcus is small, recessed, and hidden and exhibits a ventral pore and a ridged, curved plate. The thecal arrangement of O. labens is P-o, 3', 7 '' 6C, 6S(?), V-p, R(p), 5, 1p, 2 ''''. Only one sulcal list is present. The thecal plates have a smooth surface with distinct round pores. The intercalary band between the thecal plates is smooth. A row of marginal pores line the lipped cingulum. Ostreopsis species are anteroposteriorly flattened, photosynthetic, benthic dinoflagellates that are more diverse in ecology than previously known. Ostreopsis labens is capable of living in three, marine habitats: in the water column, in sand, and on macroalgal surfaces. It was most numerous in sand and less in lagoonal waters, and only a few cells were associated with macroalgae. Light and scanning electron microscopy studies revealed engulfed cells within O. labens, which indicates mixotrophic/phagotrophic behavior. A ventral opening situated in the cinglum of O. labens exhibits size variability; It may serve as an opening for engulfing food particles because it varies in size. We propose that ingestion of prey by O. labens occurs through the ventral opening the proposed feeding apparatus of this species, which is similar to the function of the peduncle-bike structure of mixotrophic dinoflagellates. The behavior of O. labens appears similar to that previously described for Dinophysis species. C1 SO ILLINOIS UNIV,DEPT PLANT BIOL,CARBONDALE,IL 62901. RP FAUST, MA (reprint author), SMITHSONIAN INST,MUSEUM NATL HIST NAT,DEPT BOT,4201 SILVER HILL RD,SUITLAND,MD 20746, USA. NR 20 TC 35 Z9 37 U1 0 U2 9 PU PHYCOLOGICAL SOC AMER INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD JUN PY 1995 VL 31 IS 3 BP 456 EP 463 DI 10.1111/j.0022-3646.1995.00456.x PG 8 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA RF344 UT WOS:A1995RF34400018 ER PT J AU KURIN, R AF KURIN, R TI CULTURAL POLICY THROUGH PUBLIC DISPLAY + PUBLIC-FOLKLORE SO JOURNAL OF POPULAR CULTURE LA English DT Article RP KURIN, R (reprint author), SMITHSONIAN INST,CTR FOLKLIFE PROGRAM,WASHINGTON,DC 20560, USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU POPULAR CULTURE ASSN PI BOWLING GREEN PA BOWLING GREEN STATE UNIV, BOWLING GREEN, OH 43403 SN 0022-3840 J9 J POP CULT JI J. Pop. Cult. PD SUM PY 1995 VL 29 IS 1 BP 3 EP & PG 0 WC Humanities, Multidisciplinary; Cultural Studies SC Arts & Humanities - Other Topics; Cultural Studies GA UC084 UT WOS:A1995UC08400001 ER PT J AU BECKER, MA WILLMAN, P TUROSS, NC AF BECKER, MA WILLMAN, P TUROSS, NC TI THE UNITED-STATES FIRST-LADIES GOWNS, A BIOCHEMICAL STUDY OF SILK PRESERVATION SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Article C1 SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560. SMITHSONIAN INST,ANAL LAB,WASHINGTON,DC 20560. RP BECKER, MA (reprint author), NATL INST SERICULTURAL & ENTOMOL SCI,TSUKUBA,JAPAN. NR 25 TC 15 Z9 17 U1 0 U2 1 PU AMER INST CONSERVATION HISTORIC ARTISTIC WORKS PI WASHINGTON PA 1717 K ST, NW, STE 301, WASHINGTON, DC 20006 SN 0197-1360 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD SUM PY 1995 VL 34 IS 2 BP 141 EP 152 DI 10.2307/3179736 PG 12 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA TU095 UT WOS:A1995TU09500005 ER PT J AU RILEY, S AF RILEY, S TI SKINS - LOUIS,AC SO LIBRARY JOURNAL LA English DT Book Review RP RILEY, S (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 1995 VL 120 IS 10 BP 164 EP 164 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA RA269 UT WOS:A1995RA26900217 ER PT J AU STANLEY, DJ AF STANLEY, DJ TI A GLOBAL SEA-LEVEL CURVE FOR THE LATE QUATERNARY - THE IMPOSSIBLE DREAM SO MARINE GEOLOGY LA English DT Article AB In view of the vulnerability of heavily populated, low-lying coastal areas to sea-level rise and marine incursion, an improved late Quaternary global sea-level curve is sorely needed as a gauge for measuring changing sea-level positions. Contrary to the prevailing view, it is proposed that such a global sea-level curve can be derived from observations compiled in widely diverse continental margin and coastal settings. Needed are a larger number of more precisely dated elevation points, with minimal relation to land motion and climatic variation, which can serve as a basis for a curve defining global sea level, particularly for the late Pleistocene and Holocene. Such a curve will not be made from any one type section or locality but, rather, from observation of contemporaneous events compiled in widely diverse settings. Rather than simply defending a contentious view, this essay solicits new and more precise data and a reconsideration of viable approaches. RP STANLEY, DJ (reprint author), SMITHSONIAN INST,DELTAS GLOBAL CHANGE PROGRAM,E-206 NMNH,WASHINGTON,DC 20560, USA. NR 13 TC 27 Z9 28 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0025-3227 J9 MAR GEOL JI Mar. Geol. PD JUN PY 1995 VL 125 IS 1-2 BP 1 EP 6 DI 10.1016/0025-3227(95)00057-6 PG 6 WC Geosciences, Multidisciplinary; Oceanography SC Geology; Oceanography GA RM342 UT WOS:A1995RM34200001 ER PT J AU STUART, J AF STUART, J TI UNIFIED STYLE IN CHINESE PAINTING AND PORCELAIN IN THE 18TH-CENTURY SO ORIENTAL ART LA English DT Article C1 SMITHSONIAN INST,ARTHUR M SACKLER GALLERY,WASHINGTON,DC 20560. RP STUART, J (reprint author), SMITHSONIAN INST,FREER GALLERY ART,WASHINGTON,DC 20560, USA. NR 28 TC 1 Z9 1 U1 0 U2 0 PU ORIENTAL ART MAGAZINE LTD PI RICHMOND PA 12 ENNERDALE RD, RICHMOND, SURREY, ENGLAND TW9 3PG SN 0030-5278 J9 ORIENTAL ART JI Orient. Art PD SUM PY 1995 VL 41 IS 2 BP 32 EP 46 PG 15 WC Art; Asian Studies SC Art; Asian Studies GA RQ262 UT WOS:A1995RQ26200005 ER PT J AU LEWENSTEIN, M CIRAC, JI ZOLLER, P AF LEWENSTEIN, M CIRAC, JI ZOLLER, P TI MASTER EQUATION FOR SYMPATHETIC COOLING OF TRAPPED-PARTICLES SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATION; POLARIZED ATOMIC-HYDROGEN; DOPPLER LIMIT C1 UNIV CASTILLA LA MANCHA, DEPT FIS APLICADA, E-13071 CIUDAD REAL, SPAIN. UNIV INNSBRUCK, INST THEORET PHYS, A-6020 INNSBRUCK, AUSTRIA. POLISH ACAD SCI, CTR FIZ TEORET, PL-02668 WARSAW, POLAND. RP LEWENSTEIN, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOLEC PHYS, 60 GARDEN ST, MAIL STOP 14, CAMBRIDGE, MA 02138 USA. RI Zoller, Peter/O-1639-2014; Lewenstein, Maciej/I-1337-2014 OI Zoller, Peter/0000-0003-4014-1505; Lewenstein, Maciej/0000-0002-0210-7800 NR 61 TC 17 Z9 18 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUN PY 1995 VL 51 IS 6 BP 4617 EP 4627 DI 10.1103/PhysRevA.51.4617 PG 11 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA RC541 UT WOS:A1995RC54100041 ER PT J AU YOU, L LEWENSTEIN, M COOPER, J AF YOU, L LEWENSTEIN, M COOPER, J TI QUANTUM-FIELD THEORY OF ATOMS INTERACTING WITH PHOTONS .2. SCATTERING OF SHORT LASER-PULSES FROM TRAPPED BOSONIC ATOMS SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATION; 2-LEVEL SYSTEM DRIVEN; RESONANCE FLUORESCENCE; SMOOTH PULSE; HYDROGEN; SPECTRA C1 UNIV COLORADO,JILA,BOULDER,CO 80309. NATL INST STAND & TECHNOL,BOULDER,CO 80309. POLISH ACAD SCI,CTR FIZ TEORETYCZNEJ,PL-02668 WARSAW,POLAND. RP YOU, L (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,MS 14,CAMBRIDGE,MA 02138, USA. RI Lewenstein, Maciej/I-1337-2014 OI Lewenstein, Maciej/0000-0002-0210-7800 NR 43 TC 62 Z9 77 U1 0 U2 3 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUN PY 1995 VL 51 IS 6 BP 4712 EP 4727 DI 10.1103/PhysRevA.51.4712 PG 16 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA RC541 UT WOS:A1995RC54100052 ER PT J AU FARRELLY, D HUMPHERYS, J AF FARRELLY, D HUMPHERYS, J TI SIGNATURE OF CLASSICAL CHAOS ON QUANTUM TUNNELING - COMMENT SO PHYSICAL REVIEW E LA English DT Letter ID HARMONIC BATH; DOUBLE-WELL C1 UTAH STATE UNIV,DEPT CHEM & BIOCHEM,LOGAN,UT 84322. UTAH STATE UNIV,DEPT MATH & STAT,LOGAN,UT 84322. RP FARRELLY, D (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1063-651X J9 PHYS REV E JI Phys. Rev. E PD JUN PY 1995 VL 51 IS 6 BP 6313 EP 6315 DI 10.1103/PhysRevE.51.6313 PN B PG 3 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA RE080 UT WOS:A1995RE08000048 ER PT J AU HATTORI, M NAKABAYASHI, T LIM, YA MIYASHIRO, H KUROKAWA, M SHIRAKI, K GUPTA, MP CORREA, M PILAPITIYA, U AF HATTORI, M NAKABAYASHI, T LIM, YA MIYASHIRO, H KUROKAWA, M SHIRAKI, K GUPTA, MP CORREA, M PILAPITIYA, U TI INHIBITORY EFFECTS OF VARIOUS AYURVEDIC AND PANAMANIAN MEDICINAL-PLANTS ON THE INFECTION OF HERPES-SIMPLEX VIRUS-1 IN-VITRO AND IN-VIVO SO PHYTOTHERAPY RESEARCH LA English DT Article DE ANTIVIRAL AGENT; HERPES SIMPLEX; AYURVEDIC MEDICINE; PANAMANIAN PLANT ID RNA TUMOR-VIRUS; REVERSE-TRANSCRIPTASE; TRADITIONAL MEDICINES; EXTRACTS; TANNINS; PREVENTION; INVITRO; MICE AB Extracts of 40 Ayurvedic medicines and 39 Panamanian medicinal plants were screened for their inhibitory activity on the plaque formation of herpes simplex virus type I (HSV-1) in cultured cells, The extracts of II plant species showed potent inhibitory activity at a concentration of 100 mu g/mL, while those of ten species showed moderate activities, Repeated oral administration of each extract of Rhus acuminata (galls), Saraca indica (bark), Strychnos potatrum (seeds) appreciably suppressed the development of typical skin lesions induced by infection of HSV-1 in BALB/c mice, The extract of S. potatrum prolonged both development of skin lesion and mean survival time. This indicates that S. potatrum is a possible candidate for therapeutic application for HSV-1 infection. C1 TOYAMA MED & PHARMACEUT UNIV,FAC MED,SUGITANI,TOYAMA 93001,JAPAN. UNIV PANAMA,COLL PHARM,PHARMACOGNOSY RES CTR PANAMANIAN FLORA,PANAMA CITY,PANAMA. UNIV PANAMA,HERBARIUM,PANAMA CITY,PANAMA. SMITHSONIAN TROP RES INST,PANAMA CITY,PANAMA. BANDARANAYAKE MEM AYURVED RES INST,COLOMBO,SRI LANKA. RP HATTORI, M (reprint author), TOYAMA MED & PHARMACEUT UNIV,WAKAN YAKU RES INST,SUGITANI,TOYAMA 93001,JAPAN. OI Gupta, Mahabir/0000-0002-9302-7864 NR 30 TC 18 Z9 20 U1 0 U2 1 PU JOHN WILEY & SONS LTD PI W SUSSEX PA BAFFINS LANE CHICHESTER, W SUSSEX, ENGLAND PO19 1UD SN 0951-418X J9 PHYTOTHER RES JI Phytother. Res. PD JUN PY 1995 VL 9 IS 4 BP 270 EP 276 DI 10.1002/ptr.2650090408 PG 7 WC Chemistry, Medicinal; Pharmacology & Pharmacy SC Pharmacology & Pharmacy GA RF629 UT WOS:A1995RF62900007 ER PT J AU FIELD, CR AF FIELD, CR TI A QUEST FOR GRANDEUR - MOORE,CHARLES AND THE FEDERAL-TRIANGLE - TOMPKINS,SK SO PUBLIC HISTORIAN LA English DT Book Review RP FIELD, CR (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 1 Z9 1 U1 0 U2 0 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD SUM PY 1995 VL 17 IS 3 BP 132 EP 135 PG 4 WC History SC History GA TA755 UT WOS:A1995TA75500035 ER PT J AU FIELD, CR AF FIELD, CR TI A PLAN WHOLLY NEW - LENFANT,PIERRE,CHARLES PLAN OF THE CITY OF WASHINGTON - STEPHENSON,RW SO PUBLIC HISTORIAN LA English DT Book Review RP FIELD, CR (reprint author), SMITHSONIAN INST,OFF ARCHITECTURAL HIST & HIST PRESERVATION,WASHINGTON,DC 20560, USA. NR 1 TC 1 Z9 1 U1 0 U2 0 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD SUM PY 1995 VL 17 IS 3 BP 132 EP 135 PG 4 WC History SC History GA TA755 UT WOS:A1995TA75500034 ER PT J AU TORRES, G AF TORRES, G TI A VISUAL-SPECTROSCOPIC ORBIT FOR THE BINARY SIGMA-248 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID STELLAR MASSES AB Spectroscopic studies of visual binaries with angular separations less than about 1'' have so far had great difficulty in providing the individual radial velocities for the components, because of the small velocity differences that are typical in these systems. The recent introduction of TODCOR, a two-dimensional cross-correlation technique (Zucker and Mazeh, ApJ, 420, 806 1994), promises to change the situation, bridging the gap between the wider pairs resolvable at the telescope, and the classical double-lined spectroscopic binaries, with large velocity amplitudes. We present the first example of an application of TODCOR to such a case: the study of the close visual pair Sigma248. We report our high-resolution low signal-to-noise spectroscopic observations of the system over the past seven years, which happen to cover the periastron passage. Using TODCOR, we are able to disentangle the light from the two stars in our composite spectra and obtain radial velocities for both components despite the small velocity difference. By combining our velocities with all available astrometric observations of the pair we derive for the first time a visual-spectroscopic orbital solution, with a period of about 310 yr. We obtain also the orbital parallax of the system, corresponding to a distance of 60 pc, as well as the individual masses, which are consistent with early K-type dwarfs. RP TORRES, G (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 20 TC 8 Z9 8 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUN PY 1995 VL 107 IS 712 BP 524 EP 530 DI 10.1086/133587 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RC140 UT WOS:A1995RC14000005 ER PT J AU ESKRIDGE, PB AF ESKRIDGE, PB TI IC-1613-X-1 - A GALAXY CLUSTER AT Z-APPROXIMATE-TO-0.2 BEHIND A LOCAL GROUP DWARF GALAXY SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID MEDIUM-SENSITIVITY SURVEY; X-RAY-SPECTRA; ACTIVE GALACTIC NUCLEI; MAGELLANIC CLOUD; NEARBY GALAXIES; QUASARS; IC-1613; DEPENDENCE; EVOLUTION; EMISSION AB Based on Einstein IPC imaging and spectroscopy, optical spectroscopy, and optical imaging, I argue that the X rays seen in the direction of the Local Group dwarf irregular galaxy IC 1613 are mainly due to emission from a previously uncataloged cluster of galaxies (CL B0102 + 0146) at a redshift of z almost-equal-to 0.2 and of richness class approximately 3, centered at the IPC X-ray position. The Einstein data are not adequate to determine if the X rays are due to cluster emission or an AGN. However, both the available optical data, and the nondetection of this object in deep radio surveys argue that a hot intracluster medium is the source of the X-ray emission. The X-ray flux of this cluster in the Einstein IPC band (0.2-4.0 keV) is higher than 78% of the clusters in the Einstein Extended Medium Sensitivity Survey sample of Gioia et al. (1990). It is thus likely that only its position behind IC 1613 prevented its earlier identification. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 40 TC 5 Z9 5 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUN PY 1995 VL 107 IS 712 BP 561 EP 565 DI 10.1086/133592 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RC140 UT WOS:A1995RC14000010 ER PT J AU KALFATOVIC, MR AF KALFATOVIC, MR TI ENCYCLOPEDIA OF TRADITIONAL EPICS - JACKSON,GM SO RQ LA English DT Book Review RP KALFATOVIC, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER LIBRARY ASSN PI CHICAGO PA 50 E HURON ST, CHICAGO, IL 60611 SN 0033-7072 J9 RQ JI RQ PD SUM PY 1995 VL 34 IS 4 BP 517 EP 517 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA RF866 UT WOS:A1995RF86600032 ER PT J AU DONAHUE, RA KEIL, SL AF DONAHUE, RA KEIL, SL TI THE SOLAR SURFACE DIFFERENTIAL ROTATION FROM DISK-INTEGRATED CHROMOSPHERIC FLUXES SO SOLAR PHYSICS LA English DT Article ID MAIN-SEQUENCE STARS; EMISSION-LINE FLUXES; STELLAR ROTATION; K-EMISSION; TIME VARIATIONS; SERIES AB Disk-integrated solar chromospheric Ca II K-line (3933.68 Angstrom) fluxes have been measured almost daily at Sacramento Peak Observatory since 1977. Using observing windows selected to mimic seasonal windows for chromospheric measurements of lower Main-Sequence stars such as those observed by Mount Wilson Observatory's HK Project, we have measured the solar rotation from the modulation of the Ca it K-line flux. We track the change of rotation period from the decline of cycle 21 through the maximum of cycle 22. This variation in rotation period is shown to behave as expected from the migration of active regions in latitude according to Maunder's 'butterfly diagram', including an abrupt change in rotation period at the transition from cycle 21 to cycle 22. These results indicate the successful detection of solar surface differential rotation from disk-integrated observations. We argue that the success of our study compared to previous investigations of the solar surface differential rotation from disk-integrated fluxes lies primarily with the choice of the length of the time-series window. Our selection of 200 days is shorter than in previous studies whose windows are typically on the order of one year. The 200-day window is long enough to permit an accurate determination of the rotation period, yet short enough to avoid complications arising from active region evolution. Thus, measurements of the variation of rotation period in lower Main-Sequence stars, especially those that appear to be correlated with long-term changes in chromospheric activity (i.e., cycles), are probably evidence for stellar surface differential rotation. C1 NATL SOLAR OBSERV,SUNSPOT,NM 88349. RP DONAHUE, RA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 33 TC 22 Z9 22 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JUN PY 1995 VL 159 IS 1 BP 53 EP 62 DI 10.1007/BF00733031 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RJ187 UT WOS:A1995RJ18700005 ER PT J AU GRAVES, GR AF GRAVES, GR TI SEQUENCE OF PLUMAGE EVOLUTION IN THE STANDARDWING BIRD-OF-PARADISE SO WILSON BULLETIN LA English DT Note RP GRAVES, GR (reprint author), NATL MUSEUM NAT HIST,SMITHSONIAN INST,DEPT VERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 12 TC 0 Z9 0 U1 5 U2 9 PU WILSON ORNITHOLOGICAL SOC PI ANN ARBOR PA MUSEUM OF ZOOLOGY UNIV MICHIGAN, ANN ARBOR, MI 48109 SN 0043-5643 J9 WILSON BULL JI Wilson Bull. PD JUN PY 1995 VL 107 IS 2 BP 371 EP 373 PG 3 WC Ornithology SC Zoology GA RC272 UT WOS:A1995RC27200015 ER PT J AU WARKENTIN, IG MORTON, ES AF WARKENTIN, IG MORTON, ES TI ROOSTING BEHAVIOR OF PROTHONOTARY WARBLERS IN THE NON-BREEDING SEASON SO WILSON BULLETIN LA English DT Note C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. NR 9 TC 5 Z9 5 U1 0 U2 1 PU WILSON ORNITHOLOGICAL SOC PI ANN ARBOR PA MUSEUM OF ZOOLOGY UNIV MICHIGAN, ANN ARBOR, MI 48109 SN 0043-5643 J9 WILSON BULL JI Wilson Bull. PD JUN PY 1995 VL 107 IS 2 BP 374 EP 376 PG 3 WC Ornithology SC Zoology GA RC272 UT WOS:A1995RC27200016 ER PT J AU BUZAS, MA AF BUZAS, MA TI THE CHALLENGER FORAMINIFERA - JONES,RW SO SCIENCE LA English DT Book Review RP BUZAS, MA (reprint author), SMITHSONIAN INST,DEPT PALEOBIOL,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 1 U2 2 PU AMER ASSOC ADVAN SCIENCE PI WASHINGTON PA 1333 H ST NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD MAY 26 PY 1995 VL 268 IS 5214 BP 1208 EP 1209 DI 10.1126/science.268.5214.1208-a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RA604 UT WOS:A1995RA60400055 PM 17840641 ER PT J AU GELLER, M AF GELLER, M TI CARNEGIE ATLAS OF GALAXIES - SANDAGE,A, BEDKE,J SO SCIENCE LA English DT Book Review RP GELLER, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ADVAN SCIENCE PI WASHINGTON PA 1333 H ST NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD MAY 26 PY 1995 VL 268 IS 5214 BP 1214 EP 1214 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA RA604 UT WOS:A1995RA60400059 ER PT J AU CHARTAS, G FALCO, E FORMAN, W JONES, C SCHILD, R SHAPIRO, I AF CHARTAS, G FALCO, E FORMAN, W JONES, C SCHILD, R SHAPIRO, I TI ROSAT OBSERVATIONS OF THE GRAVITATIONALLY LENSED SYSTEM-0957+561 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GRAVITATIONAL LENSING; QUASARS, INDIVIDUAL (0957 + 561); X-RAYS, GALAXIES ID TIME-DELAY; X-RAY; Q0957+561; ABSORPTION; QUASARS AB Observations of 0957+561 with the Einstein High Resolution Imager (HRI) in 1979 May and 1979 November and with the ROSAT HRI in 1991 May and 1992 October reveal large variations in the X-ray fluxes for images A and B which significantly differ from simultaneously observed changes of the corresponding optical continuum emission. Most striking was the apparent increase by over fivefold in the flux of image B from the late 1970's to the early 1990's. Further, in the 1990's the X-ray flux for image A increased by a factor of 1.7 +/- 0.3 and that of B by a factor of 1.9 +/- 0.2 between the two ROSAT observations (separated by 540 days), whereas optical measurements showed nearly no changes for A and B between these epochs. No significant changes in X-ray emission were observed on timescales of hours to days. If we adopt 1.5 yr as the difference between the propagation times from the quasar to us via the two images (''time delay''), then the ratio of the X-ray flux of image B for the 1992 October epoch to that of A for the 1991 May epoch is 2.7 +/- 0.4. This ratio is significantly greater than the ratio of 1.05 +/- 0.03 observed in the optical R band, 0.75 in the broad line region (BLR), and 0.76 +/- 0.03 in the radio (VLBI lambda 13 cm core) for approximately the same epoch. The wavelength dependence in the ratio of the fluxes of the two images suggests that either microlensing may be significant for the X-ray band or the time delay is substantially different from 1.5 yr (and the intrinsic variation of the quasar emission were significant within an interval comparable to the uncertainty of the time delay), or both. A ROSAT Position Sensitive Proportional Counter (PSPC) spectrum of 0957+561 is fitted well with a power law of energy index 1.1 +/- 0.2 plus a Raymond-Smith thermal plasma model with a temperature of 0.22 +/- 0.17 keV in the source frame. The estimated unmagnified X-ray luminosity of the thermal component is 3 x 10(44) ergs s(-1) (if the magnification of the thermal component by the lens is 14). This thermal emission may be a result of a strong cooling flow in the vicinity of the quasar. There is no evidence for excess absorption above that attributed to our galaxy for the relatively high-redshift quasar. We place an upper limit of 6(-4)(+3) x 10(20) atoms cm(-2) (90% confidence) on absorption at the redshift z = 1.391 of a known damped Lyman-alpha absorber and provide upper and lower bounds of 30 h(50)(-1) kpc and 0.2 h(50)(-1) kpc, respectively, for the spatial extent of this H I region. For the cluster of galaxies around the primary lensing galaxy, G1, the 3 sigma upper limit on the X-ray luminosity within a 0.5 Mpc radius over the energy range 2-10 keV (PSPC frame) is 4.1 x 10(44) ergs s(-1) for a cluster core radius of 0.1 Mpc and 1.7 x 10(44) ergs s(-1) for a core radius of 0.25 Mpc. Similarly the limit on the X-ray luminosity of a cluster around the galaxy G5 is found to be 2.8 x 10(43) ergs s(-1). Based on the relation of cluster X-ray luminosity to gas temperature and system mass, we estimate the 3 sigma upper limits on the mass of the clusters that contain the galaxies G1 and G5 within 1 Mpc to be 1.5 x 10(14) and 1 x 10(14) M., respectively. RP CHARTAS, G (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Forman, William/0000-0002-9478-1682 NR 29 TC 13 Z9 13 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 1995 VL 445 IS 1 BP 140 EP 147 DI 10.1086/175679 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QY129 UT WOS:A1995QY12900014 ER PT J AU DURIC, N GORDON, SM GOSS, WM VIALLEFOND, F LACEY, C AF DURIC, N GORDON, SM GOSS, WM VIALLEFOND, F LACEY, C TI THE RELATIVISTIC ISM IN M33 - ROLE OF THE SUPERNOVA-REMNANTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCELERATION OF PARTICLES; GALAXIES, INDIVIDUAL (M33); GALAXIES, ISM; RADIO CONTINUUM, ISM; STARS, STATISTICS; SUPERNOVA REMNANTS ID COSMIC-RAYS; PARTICLE-ACCELERATION; SPIRAL GALAXIES; RADIO; EMISSION; ORIGIN; SHOCKS AB The role of supernova remnants in producing and maintaining the relativistic interstellar medium is investigated for the case of the nearby galaxy M33. Analysis of a radio continuum sample of supernova remnants (SNRs) has led to the following results. (1) The SNRs use roughly 1%-10% of their blast energy to produce relativistic particles. (2) The currently observed SNR population contains between 0.1% and 1% of the relativistic particle energy of the entire interstellar medium of M33, which leads to reasonable values of the particle residence time in the disk. (3) The distribution of synchrotron spectral indices indicates that the particle populations of the observed SNRs have energy spectra with power-law indices of 2.2 +/- 0.4, consistent with values predicted by diffusive shock acceleration theory. Taken together, the three results favor the hypothesis that SNRs account for the bulk of M33's relativistic medium. It is further shown that, as a consequence of these results, the predicted SN rate is 1 per 140-250 yr, in general agreement with independent estimates of the SN rate and the absence of historical supernovae. C1 QUEENS UNIV,DEPT PHYS,KINGSTON,ON K71 3N6,CANADA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NATL RADIO ASTRON OBSERV,SOCORRO,NM 87801. OBSERV PARIS,SECT MEUDON,F-92190 MEUDON,FRANCE. RP DURIC, N (reprint author), UNIV NEW MEXICO,INST ASTROPHYS,ALBUQUERQUE,NM 87106, USA. NR 37 TC 36 Z9 36 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 1995 VL 445 IS 1 BP 173 EP 181 DI 10.1086/175683 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QY129 UT WOS:A1995QY12900018 ER PT J AU BILLER, SD AKERLOF, CW BUCKLEY, J CAWLEY, MF CHANTELL, M FEGAN, DJ FENNELL, S GAIDOS, JA HILLAS, AM KERRICK, AD LAMB, RC LEWIS, DA MEYER, DI MOHANTY, G OFLAHERTY, KS PUNCH, M REYNOLDS, PT ROSE, HJ ROVERO, AC SCHUBNELL, MS SEMBROSKI, G WEEKES, TC WILSON, C AF BILLER, SD AKERLOF, CW BUCKLEY, J CAWLEY, MF CHANTELL, M FEGAN, DJ FENNELL, S GAIDOS, JA HILLAS, AM KERRICK, AD LAMB, RC LEWIS, DA MEYER, DI MOHANTY, G OFLAHERTY, KS PUNCH, M REYNOLDS, PT ROSE, HJ ROVERO, AC SCHUBNELL, MS SEMBROSKI, G WEEKES, TC WILSON, C TI AN UPPER LIMIT TO THE INFRARED BACKGROUND FROM OBSERVATIONS OF TEV GAMMA-RAYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMIC RAYS; DIFFUSE RADIATION; INFRARED, GENERAL ID LIGHT AB An upper bound to the energy density of infrared background radiation is derived from considering the effect of gamma-gamma interactions on the observed TeV gamma-ray spectrum of the active galaxy Markarian 421. This upper bound proves to be the most restrictive for the wavelength range of 10-12 mu m. These constraints are presently limited by the uncertainty of extrapolating the source spectrum from 5 to 500 GeV. Observations in the regime less than 100 GeV would significantly improve these limits, allowing for a wide range of IR production models to be constrained. C1 UNIV MICHIGAN,DEPT PHYS,RANDALL LAB,ANN ARBOR,MI 48109. ST PATRICKS COLL,MAYNOOTH,KILDARE,IRELAND. HARVARD SMITHSONIAN CTR ASTROPHYS,FRED LAWRENCE WHIPPLE OBSERV,AMADO,AZ 85645. NATL UNIV IRELAND UNIV COLL DUBLIN,DUBLIN 4,IRELAND. PURDUE UNIV,DEPT PHYS,W LAFAYETTE,IN 47907. IOWA STATE UNIV SCI & TECHNOL,DEPT PHYS & ASTRON,AMES,IA 50011. NO KENTUCKY UNIV,DEPT PHYS,HIGHLAND HTS,KY 41076. EUROPEAN SPACE AGCY,ESTEC,DIV ASTROPHYS,2200 AG NOORDWIJK,NETHERLANDS. ECOLE POLYTECH,LPNHE,F-91128 PALAISEAU,FRANCE. RTC,DEPT PHYS,DUBLIN 24,IRELAND. RP BILLER, SD (reprint author), UNIV LEEDS,DEPT PHYS,LEEDS LS2 9JT,W YORKSHIRE,ENGLAND. OI Punch, Michael/0000-0002-4710-2165 NR 26 TC 40 Z9 40 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 1995 VL 445 IS 1 BP 227 EP 230 DI 10.1086/175689 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QY129 UT WOS:A1995QY12900024 ER PT J AU GAGNE, M CAILLAULT, JP STAUFFER, JR AF GAGNE, M CAILLAULT, JP STAUFFER, JR TI DEEP ROSAT HRI OBSERVATIONS OF THE ORION NEBULA REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (ORION NEBULA); STARS, PRE-MAIN-SEQUENCE; X-RAYS, STARS ID T-TAURI STARS; X-RAY SURVEY; MAIN-SEQUENCE STARS; EMISSION-LINE STARS; SOLAR-TYPE STARS; DARK CLOUD; EINSTEIN OBSERVATIONS; ASSOCIATION REGION; STELLAR POPULATION; TRAPEZIUM CLUSTER AB We present results from three deep ROSAT high-resolution imager observations of the Orion Nebula star-forming region. The X-ray images contain over 1500 cataloged stars in a roughly 0.8 deg(2) region centered on the Trapezium. In all 389 distinct X-ray sources have been detected, at least two-thirds of which are associated with a single proper-motion cluster member. X-ray emission is detected from stars of all spectral types, from the massive O- and B-type components of the Trapezium to the coolest, low-mass pre-main-sequence (PMS) stars. In this paper we focus primarily on X-ray emission from the late-type PMS stars. Of the similar to 100 late-type cluster members with measured spectral types, approximately three-fourths have been detected; we have derived X-ray luminosity upper limits for the remaining stars. We found coronal X-ray emission turns on around spectral type F6, with the upper envelope of activity increasing with decreasing effective temperature. When plotted in an X-ray luminosity versus bolometric luminosity diagram, late-type PMS stars lie below a ''saturation'' line corresponding to L(X)/L(bol)similar to 10(-3). For approximately solar-mass PMS stars, we find a median X-ray luminosity similar to 1 x 10(30) ergs s(-1). The late G, K, and M stars exhibit nearly a two order of magnitude spread in X-ray luminosity and in L(X)/L(bol) at a given effective temperature. Plots of X-ray activity versus v sin i rotational velocity and rotational period appear to show no clear dependence of activity on rotation. However, because only a small fraction of late-type PMS stars in the Orion Nebula have measured v sin i or P-rot and because of uncertainties in L(X) and L(X)/L(bol), we believe the data are not conclusive on this point. Light curves of the detected X-ray sources have revealed at least 10 strong X-ray flares with characteristic rise times greater than or similar to 1 hr and decay times ranging from similar to 2 to 12 hr. All the flares have X-ray energies in excess of 3 x 10(35) ergs. Many of the X-ray sources associated with late-type cluster members have been observed in more than one ROSAT HRI exposure, allowing us to look for variability on the similar to 1 yr timescale between HRI observations. A statistical analysis of the resulting count rate ratios suggests that at least one-fourth of the late-type cluster stars are significantly variable on this timescale. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP GAGNE, M (reprint author), UNIV GEORGIA, DEPT PHYS & ASTRON, ATHENS, GA 30602 USA. RI Gagne, Marc/C-1130-2013 NR 91 TC 83 Z9 83 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 1995 VL 445 IS 1 BP 280 EP 313 DI 10.1086/175694 PN 1 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QY129 UT WOS:A1995QY12900029 ER PT J AU CHEN, H MYERS, PC LADD, EF WOOD, DOS AF CHEN, H MYERS, PC LADD, EF WOOD, DOS TI BOLOMETRIC TEMPERATURE AND YOUNG STARS IN THE TAURUS AND OPHIUCHUS COMPLEXES SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, FUNDAMENTAL PARAMETERS; STARS, PRE-MAIN-SEQUENCE ID SPECTRAL ENERGY-DISTRIBUTIONS; AURIGA MOLECULAR CLOUD; IRAS POINT SOURCES; T-TAURI; DARK CLOUD; STELLAR OBJECTS; CORES; PROTOSTARS; REGIONS; IDENTIFICATION AB We calculated bolometric temperature (T-bol) and luminosity (L(bol)) for 128 young stellar objects (YSOs) in Taurus, 74 in the Ophiuchus ''core,'' and 33 in the Ophiuchus ''off-core'' region. We have constructed the bolometric luminosity-temperature (BLT) diagram, the log-log plot of L(bol) versus T-bol, for the three samples. T-bol is defined as the temperature of a blackbody having the same frequency as the observed continuum spectrum. It measures the redness (or coldness) of an astronomical source. The BLT diagram is analogous to the H-R diagram and allows for a direct and quantitative comparison of YSOs at a wide variety of evolutionary states, ranging from the most deeply embedded stars to T Tauri stars nearly on the main sequence. We found (1) T-bol increases monotonically from embedded sources (similar to 60-500 K) to classical T Tauri stars (similar to 1000-3000 K) to weak-line T Tauri stars (similar to 2000-5000 K); (2) T-bol correlates reasonably well with the age inferred from the evolutionary models of pre-main-sequence stars and protostars for embedded ''protostars'' and weak-line T Tauri stars. There is no significant correlation for the classical T Tauri stars. These results can be understood in terms of dissipation of circumstellar dust envelope and disk during the early stages of stellar evolution. Sources in the three regions have different distributions in the BLT diagram. The Ophiuchus core has the highest fraction of cold sources among the three regions. These cold sources are also more luminous than the YSOs in the other regions. The Ophiuchus off-core sample is dominated by the more evolved pre-main-sequence stars. The Taurus sources have distributions intermediate in L(bol), T-bol, and age between the Ophiuchus core and off-core distributions. These may suggest differences in the star formation history, and possibly in the stellar masses and mass accretion rates in these star-forming regions. C1 UNIV MASSACHUSETTS,FIVE COLL RADIO ASTRON OBSERV,AMHERST,MA 01003. NATL RADIO ASTRON OBSERV,SOCORRO,NM 87801. RP CHEN, H (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 60 TC 211 Z9 211 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 1995 VL 445 IS 1 BP 377 EP 392 DI 10.1086/175703 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QY129 UT WOS:A1995QY12900038 ER PT J AU BACHILLER, R FUENTE, A TAFALLA, M AF BACHILLER, R FUENTE, A TAFALLA, M TI AN EXTREMELY HIGH-VELOCITY MULTIPOLAR OUTFLOW AROUND IRAS-20050+2720 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (IRAS 20050+2027); ISM, JETS AND OUTFLOWS; ISM, MOLECULES; RADIO LINES, ISM; STARS, FORMATION ID MOLECULAR OUTFLOWS; JET; REGION; L723 AB We report high angular resolution maps in the CO 2 --> 1 and CS 3 --> 2 lines of the molecular gas around the embedded object IRAS 20050+2027. This is a 260 L. source located in the Cygnus Rift at 700 pc from the Sun. The CS data uncover a dense core of size 0.3 pc and 80 M. centered on the IRAS object. The CO map reveals a remarkable molecular outflow consisting of three pairs of lobes emanating from the close vicinity of the IRAS source. One of the lobe pairs is a highly collimated jet of extremely high velocity emission (LSR velocities up to +70 km s(-1)) containing molecular ''bullets.'' We briefly examine different possibilities to explain the complex structure of the multipolar outflow. A single outflow appears unable to explain all the CO observations, so we suggest that two or three independent outflows emanate from different young sources embedded within the core. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP BACHILLER, R (reprint author), CTR ASTRON YEBES,IGN,APARTADO 148,E-19080 GUADALAJARA,SPAIN. RI Fuente, Asuncion/G-1468-2016 OI Fuente, Asuncion/0000-0001-6317-6343 NR 17 TC 28 Z9 28 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 1995 VL 445 IS 1 BP L51 EP L54 DI 10.1086/187887 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QY132 UT WOS:A1995QY13200013 ER PT J AU KALFATOVIC, MR AF KALFATOVIC, MR TI SLOAN,JOHN - PAINTER AND REBEL - LOUGHERY,J SO LIBRARY JOURNAL LA English DT Book Review RP KALFATOVIC, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 15 PY 1995 VL 120 IS 9 BP 68 EP 68 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA QX750 UT WOS:A1995QX75000107 ER PT J AU GRAHAM, JB DUDLEY, R AGUILAR, NM GANS, C AF GRAHAM, JB DUDLEY, R AGUILAR, NM GANS, C TI IMPLICATIONS OF THE LATE PALEOZOIC OXYGEN PULSE FOR PHYSIOLOGY AND EVOLUTION SO NATURE LA English DT Article ID TERRESTRIAL VERTEBRATES; MASS EXTINCTION; FOSSIL RECORD; ATMOSPHERE; PHYLOGENY; DIVERSITY; TETRAPODS; INSECTA; ORIGIN; MODEL AB The late Palaeozoic was marked by significant changes in atmospheric chemistry and biotic composition. Geochemical models suggest a marked increase and then decline of atmospheric oxygen and associated shifts in the concentration of carbon dioxide. Although the actual magnitude of these changes is uncertain, the pulse of oxygen concentration may have reached a maximum of 35% and then dropped to 15% (compared with the present 21%). This oxygen pulse may have influenced the evolution of major groups of organisms. C1 UNIV CALIF SAN DIEGO,SCRIPPS INST OCEANOG,CTR MARINE BIOTECHNOL & BIOMED,LA JOLLA,CA 92093. UNIV TEXAS,DEPT ZOOL,AUSTIN,TX 78712. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. UNIV MICHIGAN,DEPT BIOL,ANN ARBOR,MI 48109. RP GRAHAM, JB (reprint author), UNIV CALIF SAN DIEGO,SCRIPPS INST OCEANOG,DIV MARINE BIOL RES,LA JOLLA,CA 92093, USA. NR 85 TC 181 Z9 186 U1 4 U2 33 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD MAY 11 PY 1995 VL 375 IS 6527 BP 117 EP 120 DI 10.1038/375117a0 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA QX741 UT WOS:A1995QX74100041 ER PT J AU TUCKER, WH TANANBAUM, H REMILLARD, RA AF TUCKER, WH TANANBAUM, H REMILLARD, RA TI A SEARCH FOR FAILED CLUSTERS OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERS, GENERAL; GALAXIES, FORMATION; X-RAYS, GALAXIES ID REDSHIFT SURVEY SLICES; LARGE-SCALE STRUCTURE; X-RAY; COMA CLUSTER; GAS CLOUDS; FRAGMENTATION; EFFICIENCY; STARS AB We describe a search for a new type of object-large clouds of hot gas with no visible galaxies-which we call failed clusters of galaxies. We calculate the expected X-ray luminosity, temperature, and angular diameter of such objects as a function of total cloud mass and convert the results to expected X-ray fluxes from failed clusters at different redshifts. Using the Einstein Imaging Proportional Counter (IPC) database, we establish a strategy to search for candidate failed clusters. From this initial screening of 1435 IPC fields, 17 candidates are selected for more detailed analysis, which indicates that 10 of these are very probably extended X-ray sources. Optical follow-up on the 10 prime candidates finds eight dusters of galaxies (including six reported for the first time in this paper), one stellar identification, and one without an obvious optical counterpart (the candidate with the weakest evidence for X-ray extent). Investigation of several candidates with less evidence for X-ray extent yields two additional new clusters of galaxies. A conservative comparison of our results with the Einstein Extended Medium Sensitivity Survey demonstrates that failed clusters are at most one-sixth as common as clusters of galaxies (98.3% confidence level). Therefore we conclude that failed clusters are a relatively unimportant contributor to the mass density of the universe. Our inability to find failed clusters is consistent with the hierarchical clustering scenario for the formation of galaxies and clusters. C1 MIT,CAMBRIDGE,MA 02139. UNIV CALIF SAN DIEGO,SAN DIEGO,CA 92103. RP TUCKER, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 34 TC 47 Z9 47 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 1995 VL 444 IS 2 BP 532 EP 547 DI 10.1086/175627 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QV701 UT WOS:A1995QV70100004 ER PT J AU DAVIS, DS MUSHOTZKY, RF MULCHAEY, JS WORRALL, DM BIRKINSHAW, M BURSTEIN, D AF DAVIS, DS MUSHOTZKY, RF MULCHAEY, JS WORRALL, DM BIRKINSHAW, M BURSTEIN, D TI DIFFUSE HOT GAS IN THE NGC-4261 GROUP OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERS OF; GALAXIES, INDIVIDUAL (NGC 4261, NGC 4264, NGC 4273); INTERGALACTIC MEDIUM; X-RAYS, GALAXIES ID X-RAY-EMISSION; SPIRAL GALAXIES; COMPACT-GROUPS; DARK MATTER; CLUSTERS; EINSTEIN AB We have found diffuse X-ray gas in the group of galaxies containing the elliptical galaxy NGC 4261. This galaxy along with its associated companions are behind the Virgo cluster in the W-cloud. A recent analysis of the velocity structure in the Virgo region indicates that the W-cloud has similar to 30 members, most of which are low luminosity dwarfs. The hot X-ray emitting gas is centered about halfway between NGC 4261 and NGC 4264 and extends out to a radius of similar to 40' (620 kpc). The spectral data for the diffuse component are well fitted with a Raymond-Smith plasma model with a temperature of 0.85(-0.16)(+0.21) keV and abundance <0.08 times the solar value. Under the assumption that the diffuse gas is in hydrostatic equilibrium the total mass within 40' is 1.9 x 10(13) M(.). We estimate that the total baryonic mass of the hot gas and the galaxies is 20%-34% of the total mass in the central 40' radius of this group. This group of galaxies contains NGC 4273 which exhibits a ''bow shock'' morphology similar to that of NGC 2276, This is thought to occur when the ram pressure from the intragroup gas significantly perturbs the interstellar medium in a late-type galaxy. We show that this is unlikely in this group. C1 NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. ARIZONA STATE UNIV,DEPT PHYS & ASTRON,TEMPE,AZ 85287. UNIV MARYLAND,DEPT ASTRON,COLLEGE PK,MD 20742. NR 26 TC 22 Z9 22 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 1995 VL 444 IS 2 BP 582 EP 589 DI 10.1086/175632 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QV701 UT WOS:A1995QV70100009 ER PT J AU KETO, ER WELCH, WJ REID, MJ HO, PTP AF KETO, ER WELCH, WJ REID, MJ HO, PTP TI LINE BROADENING IN THE W3(OH) CHAMPAGNE FLOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II REGIONS; ISM, INDIVIDUAL (W3); ISM, JETS AND OUTFLOWS; RADIO LINES, ISM; STARS, FORMATION ID H-II REGIONS; RADIATION-DRIVEN IMPLOSION; GRAVITATIONAL COLLAPSE; OB CLUSTERS; RECOMBINATION; OH; RESOLUTION; EXPANSION; HYDROGEN; MASERS AB High angular resolution H92 alpha recombination-line and 18 cm continuum observations of the ultracompact H II region W3(OH) indicate a supersonic champagne flow: a 12 km s(-1) gradient in the recombination-line velocities across the H II region measures the acceleration of the ionized gas, while low-level continuum emission traces the extent of the outflow to the northeast away from the compact core. The previously observed progressive blueshifting of lower frequency recombination lines may be due to variations in electron impact line broadening in the champagne flow. This systematic shifting of the recombination-line velocities can occur because the line broadening is coupled to the gas density through electron collisions while the gas velocity is also coupled to the density through mass flux conservation. Interpretation of observations of H II regions within the context of the champagne flow model rather than the ionization bounded nebula model has implications for theories of the sequential formation of massive stars in clusters and the dynamical evolution of molecular gas around newly formed stars. C1 UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP KETO, ER (reprint author), LAWRENCE LIVERMORE NATL LAB,POB 808 L-59,LIVERMORE,CA 94550, USA. NR 31 TC 21 Z9 22 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 1995 VL 444 IS 2 BP 765 EP 769 DI 10.1086/175649 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QV701 UT WOS:A1995QV70100026 ER PT J AU GRAHAM, JR LEVENSON, NA HESTER, JJ RAYMOND, JC PETRE, R AF GRAHAM, JR LEVENSON, NA HESTER, JJ RAYMOND, JC PETRE, R TI AN X-RAY AND OPTICAL STUDY OF THE INTERACTION OF THE CYGNUS-LOOP SUPERNOVA REMNANT WITH AN INTERSTELLAR CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (CYGNUS LOOP); SUPERNOVA REMNANTS; X-RAYS, ISM ID INTER-STELLAR MEDIUM; EINSTEIN OBSERVATIONS; WAVE; PRECURSORS; EMISSION AB We have used the ROSAT high-resolution imager and optical emission line data to study the structure of a bright optical knot on the southeastern rim of the Cygnus Loop supernova remnant. This knot has been identified as an encounter between the blast wave and a small isolated cloud. The knot appears in projection just behind the blast wave, which is traced by Balmer line filaments which bound the X-ray emission. The knot is a prominent X-ray feature, consisting of a number of filaments which are correlated with the optical line emission. These data permit a detailed view of the blast wave interaction. By combining the optical and X-ray data it is possible to trace the blast wave as a continuous surface from its southern edge around the western side of the cloud that then continues on to the north. The southeastern knot is an indentation on the surface of the blast wave. Thus the southeastern knot is not a small cloud that has been overrun by the blast wave, but the tip of a larger cloud. Bright X-ray emission is associated with bright radiative filaments. The location of this emission, upstream of the radiative shocks, implies that the enhanced X-rays come from a reverse shock. The presence of a reverse shock is further evidence that the southeastern knot represents an early stage of a blast wave encountering a large cloud. A consistent picture of the Cygnus Loop as an explosion within a preexisting cavity is emerging. These observations agree with that picture. C1 ARIZONA STATE UNIV,DEPT PHYS & ASTRON,TEMPE,AZ 85287. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP GRAHAM, JR (reprint author), UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720, USA. NR 32 TC 45 Z9 45 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 1995 VL 444 IS 2 BP 787 EP 795 DI 10.1086/175651 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QV701 UT WOS:A1995QV70100028 ER PT J AU HUGHES, JP HAYASHI, I HELFAND, D HWANG, U ITOH, M KIRSHNER, R KOYAMA, K MARKERT, T TSUNEMI, H WOO, J AF HUGHES, JP HAYASHI, I HELFAND, D HWANG, U ITOH, M KIRSHNER, R KOYAMA, K MARKERT, T TSUNEMI, H WOO, J TI ASCA OBSERVATIONS OF THE LARGE MAGELLANIC CLOUD SUPERNOVA REMNANT SAMPLE - TYPING SUPERNOVAE FROM THEIR REMNANTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (LARGE MAGELLANIC CLOUD); NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES; SUPERNOVA REMNANTS; X-RAYS, ISM ID NOVA REMNANTS; X-RAY; MODELS AB We present our first results from a study of the supernova remnants (SNRs) in the Large Magellanic Cloud (LMC) using data from ASCA. The three remnants we have analyzed to date, 0509-67.5, 0519-69.0, and N103B, are among the smallest, and presumably also the youngest, in the Cloud. The X-ray spectra of these SNRs show strong K alpha emission lines of silicon, sulfur, argon, and calcium with no evidence for corresponding lines of oxygen, neon, or magnesium. The dominant feature in the spectra is a broad blend of emission lines around 1 keV which we attribute to L-shell emission lines of iron. Model calculations (Nomoto, Thielemann, and Yokoi 1984) show that the major products of nucleosynthesis in Type Ia supernovae (SNs) are the elements from silicon to iron, as observed here. The calculated nucleosynthetic yields from Type Ib and II SNs are shown to be qualitatively inconsistent with the data. We conclude that the SNs which produced these remnants were of Type Ia. This finding also confirms earlier suggestions that the class of Balmer-dominated remnants arise from Type Ia SN explosions. Based on these early results from the LMC SNR sample, we find that roughly one-half of the SNRs produced in the LMC within the last similar to 1500 yr came from Type Ia SNs. C1 KYOTO UNIV,DEPT PHYS,SAKYO KU,KYOTO 606,JAPAN. COLUMBIA UNIV,DEPT ASTRON,NEW YORK,NY 10027. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. INST SPACE & ASTRONAUT SCI,SAGAMIHARA,KANAGAWA 229,JAPAN. MIT,CTR SPACE RES,CAMBRIDGE,MA 02139. MIT,DEPT PHYS,CAMBRIDGE,MA 02139. OSAKA UNIV,DEPT PHYS,TOYONAKA,OSAKA 560,JAPAN. RP HUGHES, JP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 23 TC 80 Z9 80 U1 2 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 1995 VL 444 IS 2 BP L81 EP L84 DI 10.1086/187865 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QV709 UT WOS:A1995QV70900006 ER PT J AU LESSIOS, HA ALLEN, GR WELLINGTON, GM BERMINGHAM, E AF LESSIOS, HA ALLEN, GR WELLINGTON, GM BERMINGHAM, E TI GENETIC AND MORPHOLOGICAL EVIDENCE THAT THE EASTERN PACIFIC DAMSELFISH ABUDEFDUF DECLIVIFRONS IS DISTINCT FROM A-CONCOLOR (POMACENTRIDAE) SO COPEIA LA English DT Article ID DNA; PANAMA; ISTHMUS; DROSOPHILA; POLYMERASE; EVOLUTION; DISTANCE; PROTEIN AB No consensus exists in the systematic literature about whether the Mexican night-sergeant, Abudefduf declivifrons, from Baja California and the Sea of Cortez, is distinct from the Panamic night-sergeant, Abudefduf concolor, from the rest of the tropical eastern Pacific. We present evidence from electrophoretic comparisons of proteins, nucleotide sequence comparisons of the cytochrome oxidase I gene of mitochondrial DNA, and quantitative comparisons of morphology. All agree that the two nominal species are distinct. Based on analysis of isozyme and mitochondrial DNA data from the Caribbean species of night-sergeant, Abudefduf taurus, we suggest that A. declivifrons split from the lineage leading to A. concolor and A. taurus before the Pliocene rise of the Isthmus of Panama. The two night-sergeants from the eastern Pacific differ significantly in body, snout, and caudal peduncle depth and can be distinguished by the condition of the suborbital margin (adnate in A. concolor, semi-adnate or exposed in A. declivifrons). C1 WESTERN AUSTRALIAN MUSEUM,PERTH,WA 6000,AUSTRALIA. UNIV HOUSTON,DEPT BIOL,HOUSTON,TX 77204. RP LESSIOS, HA (reprint author), SMITHSONIAN TROP RES INST,BOX 2072,BALBOA,PANAMA. NR 36 TC 22 Z9 24 U1 0 U2 2 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS BUSINESS OFFICE PI CARBONDALE PA SOUTHERN ILLINOIS UNIV, DEPT ZOOLOGY, CARBONDALE, IL 62901-6501 SN 0045-8511 J9 COPEIA JI Copeia PD MAY 3 PY 1995 IS 2 BP 277 EP 288 PG 12 WC Zoology SC Zoology GA QX933 UT WOS:A1995QX93300002 ER PT J AU ZUG, GR BALAZS, GH WETHERALL, JA AF ZUG, GR BALAZS, GH WETHERALL, JA TI GROWTH IN JUVENILE LOGGERHEAD SEATURTLES (CARETTA-CARETTA) IN THE NORTH PACIFIC PELAGIC HABITAT SO COPEIA LA English DT Note ID SOUTHERN BAHAMAS; CHELONIA-MYDAS; GREEN TURTLES; SEA-TURTLES; RATES; AGE C1 NOAA,NATL MARINE FISHERIES SERV,SW FISHERIES CTR,HONOLULU LAB,HONOLULU,HI 96822. RP ZUG, GR (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT VERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 19 TC 39 Z9 46 U1 0 U2 6 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS BUSINESS OFFICE PI CARBONDALE PA SOUTHERN ILLINOIS UNIV, DEPT ZOOLOGY, CARBONDALE, IL 62901-6501 SN 0045-8511 J9 COPEIA JI Copeia PD MAY 3 PY 1995 IS 2 BP 484 EP 487 PG 4 WC Zoology SC Zoology GA QX933 UT WOS:A1995QX93300028 ER PT J AU LATHAM, DW SODERBLOM, DR AF LATHAM, DW SODERBLOM, DR TI SETI TARGET SELECTION SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 44th Congress of the International-Astronautical-Federation CY OCT 16, 1993 CL GRAZ, AUSTRIA SP Int Astron Federat AB The NASA High Resolution Microwave Survey consists of two complementary elements: a Sky Survey of the entire sky to a moderate level of sensitivity; and a Targeted Search of nearby stars, one at a time, to a much deeper level of sensitivity. In this paper we propose strategies for target selection. We have two goals: to improve the chances of successful detection of signals from technical civilizations that inhabit planets around solar-type stars, and to minimize the chances of missing signals From unexpected sites. For the main Targeted Search survey of approximately 1000 nearby solar-type stars, we argue that the selection criteria should be heavily biased by what we know about the origin and evolution of life here on Earth. We propose that observations of stars with stellar companions orbiting near the habitable zone should be de-emphasized, because such companions would prevent the formation of habitable planets. We also propose that observations of stars younger than about three billion years should be de-emphasized in favor of older stars, because our own technical civilization took longer than three billion years to evolve here on Earth. To provide the information needed for the preparation of specific target lists, we have undertaken an inventory of a large sample of solar-type stars out to a distance of 60 pc, with the goal of characterizing the relevant astrophysical properties of these stars, especially their ages and companionship. To complement the main survey, we propose that a modest sample of the nearest stars should be observed without any selection biases whatsoever. Finally, we argue that efforts to identify stars with planetary systems should be expanded. If found, such systems should receive intensive scrutiny. RP LATHAM, DW (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD MAY-JUN PY 1995 VL 35 IS 9-11 BP 741 EP 744 DI 10.1016/0094-5765(95)00028-X PG 4 WC Engineering, Aerospace SC Engineering GA RK466 UT WOS:A1995RK46600020 PM 11540737 ER PT J AU THOMSEN, JL FROHLICH, B AF THOMSEN, JL FROHLICH, B TI DRUG-ABUSE AND INTOXICATION IN ALCOHOLICS SO ALCOHOL AND ALCOHOLISM LA English DT Article AB The frequency of drug, alcohol and combined alcohol/drug intoxication in forensic autopsy material is described. Alcoholics had frequently abused drugs; the cause of death was drug intoxication in 12%, combined alcohol/drug intoxication in 13%, and alcohol intoxication only in 4%. The manner of death was different in the various groups as it was almost equally stated as accident, suicide and unascertainable, respectively, with only drugs involved, whereas accidents were the predominant features in the combined alcohol/drug intoxication among alcoholics. In controls, accidents predominated on both types of intoxication. The alcoholics seemed to be more 'deliberately' choosing suicide with drugs, while both alcoholics and controls need more information with regard to the dangers of mixing alcohol and drugs. The frequency of combined alcohol and drug intoxication was much higher in alcoholics. C1 UNIV COPENHAGEN,INST FORENS PATHOL,COPENHAGEN,DENMARK. SMITHSONIAN INST,DEPT ANTHROPOL,WASHINGTON,DC 20560. RP THOMSEN, JL (reprint author), ODENSE UNIV,INST FORENS MED,WINSLOWPK 17,DK-5000 ODENSE C,DENMARK. NR 7 TC 7 Z9 7 U1 0 U2 0 PU OXFORD UNIV PRESS UNITED KINGDOM PI OXFORD PA WALTON ST JOURNALS DEPT, OXFORD, ENGLAND OX2 6DP SN 0735-0414 J9 ALCOHOL ALCOHOLISM JI Alcohol Alcohol. PD MAY PY 1995 VL 30 IS 3 BP 379 EP 383 PG 5 WC Substance Abuse SC Substance Abuse GA RL141 UT WOS:A1995RL14100013 PM 7545993 ER PT J AU ERCIT, TS WISE, MA CERNY, P AF ERCIT, TS WISE, MA CERNY, P TI COMPOSITIONAL AND STRUCTURAL SYSTEMATICS OF THE COLUMBITE GROUP SO AMERICAN MINERALOGIST LA English DT Article ID ORDERED COLUMBITE; PEGMATITE AB The systematics of the columbite group have been studied to quantify variations in composition and structure. Multiple regression methods involving 89 heated samples and five synthetic equivalents of columbite-group minerals give equations that permit prediction of the effects of composition on unit-cell parameters for fully ordered samples. The results are: a(0) = 14.258 + 0.166Mn/(Mn + Fe) + 0.0072Ta/(Ta + Nb) - 0.06Ti - 0.02Sn + 0.05Sc; b(0) = 5.7296 + 0.031Mn/(Mn + Fe) + 0.0024Ta/(Ta + Nb) - 0.024Ti - 0.009Sn + 0.02Sc; c(0) = 5.0495 + 0.033Mn/(Mn + Fe) + 0.011Ta/(Ta + Nb) - 0.004Ti, where a(0), b(0), and c(0) are the cell parameters (Angstrom) calculated from unit-cell concentrations of elements. With these equations, crystal-chemical trends, the effects of heating experiments, the degree of cation order, and the structural effects of heterovalent cation substitution can be predicted for samples of columbite-group minerals. C1 SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560. UNIV MANITOBA,DEPT GEOL SCI,WINNIPEG,MB R3T 2N2,CANADA. RP ERCIT, TS (reprint author), CANADIAN MUSEUM NAT,DIV RES,POB 3443 STN D,OTTAWA,ON K1P 6P4,CANADA. NR 19 TC 42 Z9 44 U1 1 U2 3 PU MINERALOGICAL SOC AMER PI WASHINGTON PA 1130 17TH ST NW SUITE 330, WASHINGTON, DC 20036 SN 0003-004X J9 AM MINERAL JI Am. Miner. PD MAY-JUN PY 1995 VL 80 IS 5-6 BP 613 EP 619 PG 7 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA RF781 UT WOS:A1995RF78100019 ER PT J AU HAGEDORN, M AF HAGEDORN, M TI THE ELECTRIC FISH HYPOPOMUS-OCCIDENTALIS CAN RAPIDLY MODULATE THE AMPLITUDE AND DURATION OF ITS ELECTRIC ORGAN DISCHARGES SO ANIMAL BEHAVIOUR LA English DT Note RP HAGEDORN, M (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 15 TC 30 Z9 31 U1 0 U2 2 PU ACADEMIC PRESS (LONDON) LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD MAY PY 1995 VL 49 IS 5 BP 1409 EP 1413 DI 10.1006/anbe.1995.0174 PG 5 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA QZ999 UT WOS:A1995QZ99900026 ER PT J AU EGGERTSSON, O LAEYENDECKER, D AF EGGERTSSON, O LAEYENDECKER, D TI A DENDROCHRONOLOGICAL STUDY OF THE ORIGIN OF DRIFTWOOD IN FROBISHER BAY, BAFFIN-ISLAND, NWT, CANADA SO ARCTIC AND ALPINE RESEARCH LA English DT Article ID ICE AB Archaeological sites in Frobisher Bay, located far above the treeline, yielded large amounts of wooden remains. Questions were raised about the source of that wood. Forty driftwood samples were collected from the shares and analyzed by dendrochronological and wood-anatomical methods to determine their origins and ages. Four Picea logs are cross-dated via tree-ring chronologies from the Yukon River drainage in Alaska and two Pinus samples are cross-dated with a tree-ring chronology from the Yenisey River in Siberia. The Picea driftwood and some Larix driftwood were eroded naturally from river terraces, while most Pinus and Larix wood escaped logging and floating operations along Russian rivers. We propose that wood on the shores of Frobisher Bay drifted from the Arctic Ocean via Fram Strait, between Greenland and Svalbard, and around the southern tip of Greenland rather than through the Canadian Arctic Archipelago. C1 SMITHSONIAN INST,CTR ARCTIC STUDIES,DEPT ANTHROPOL,WASHINGTON,DC 20560. RP EGGERTSSON, O (reprint author), LUND UNIV,DEPT QUATERNARY GEOL,TORNAVAGEN 13,S-22363 LUND,SWEDEN. NR 27 TC 13 Z9 13 U1 0 U2 1 PU INST ARCTIC ALPINE RES PI BOULDER PA UNIV COLORADO, BOULDER, CO 80309 SN 0004-0851 J9 ARCTIC ALPINE RES JI Arct. Alp. Res. PD MAY PY 1995 VL 27 IS 2 BP 180 EP 186 DI 10.2307/1551900 PG 7 WC Environmental Sciences; Geography SC Environmental Sciences & Ecology; Geography GA RD300 UT WOS:A1995RD30000009 ER PT J AU MORSE, JA WINKLER, PF KIRSHNER, RP AF MORSE, JA WINKLER, PF KIRSHNER, RP TI SPATIALLY-RESOLVED KINEMATICS AND LONGSLIT SPECTROSCOPY OF THE YOUNG, OXYGEN-RICH SUPERNOVA REMNANT N132D IN THE LARGE MAGELLANIC CLOUD SO ASTRONOMICAL JOURNAL LA English DT Article ID NOVA REMNANT; BOW SHOCK; X-RAY; OPTICAL-EMISSION; MACH DISK; PUPPIS-A; CASSIOPEIA; SPECTROPHOTOMETRY; VARIABILITY; DISCOVERY C1 SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. MIDDLEBURY COLL,DEPT PHYS,MIDDLEBURY,VT 05753. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 58 TC 44 Z9 44 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 1995 VL 109 IS 5 BP 2104 EP 2120 DI 10.1086/117436 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QV645 UT WOS:A1995QV64500018 ER PT J AU GIOIA, IM HENRY, JP LUPPINO, GA CLOWE, DI BOHRINGER, H BRIEL, UG VOGES, W HUCHRA, JP MACGILLIVRAY, H AF GIOIA, IM HENRY, JP LUPPINO, GA CLOWE, DI BOHRINGER, H BRIEL, UG VOGES, W HUCHRA, JP MACGILLIVRAY, H TI DISCOVERY OF A LARGE GRAVITATIONAL ARC IN THE X-RAY-CLUSTER A2280 SO ASTRONOMY & ASTROPHYSICS LA English DT Letter DE GALAXIES, CLUSTERING; PHOTOMETRY, CLUSTERS OF GALAXIES, INDIVIDUAL ABELL 2280, COSMOLOGY, OBSERVATIONS; GRAVITATIONAL LENSING, X-RAYS, GENERAL ID MEDIUM-SENSITIVITY SURVEY; RICH CLUSTERS; GALAXIES; EVOLUTION; SAMPLE AB This Letter presents the serendipitous discovery of a large are in an X-ray selected cluster detected in the ROSAT North Ecliptic Pole (NEP) survey. The cluster, associated with Abell 2280, is identified as the optical counterpart of the X-ray source RX J1743.51+6341. This object is a medium-distant (z=0.326) and luminous (L(0.5-2kev)=5.06x10(44) ergs s(-1)) cluster dominated by a central bright galaxy. The are is located similar to 14 '' to the North-West of the cD and it is detected in the R and I bands but not in the B band. Photometric and spectroscopic observations of the cluster and of the are are presented. Other similar discoveries in the course of imaging and spectroscopic surveys of ROSAT are expected in the future. C1 CNR, IST RADIOASTRON, I-40129 BOLOGNA, ITALY. MAX PLANCK INST EXTRATERR PHYS, D-85748 GARCHING, GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. ROYAL OBSERV, EDINBURGH EH9 3HJ, MIDLOTHIAN, SCOTLAND. RP GIOIA, IM (reprint author), UNIV HAWAII, INST ASTRON, 2680 WOODLAWN DR, HONOLULU, HI 96822 USA. RI Gioia, Isabella/B-6982-2012 OI Gioia, Isabella/0000-0003-3127-498X NR 30 TC 8 Z9 8 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 1995 VL 297 IS 3 BP L75 EP L78 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RA532 UT WOS:A1995RA53200002 ER PT J AU MAGGIO, A SCIORTINO, S COLLURA, A HARNDEN, FR AF MAGGIO, A SCIORTINO, S COLLURA, A HARNDEN, FR TI ROSAT PSPC SPECTRAL FITTING SIMULATIONS WITH ONE-TEMPERATURE AND 2-TEMPERATURE MODELS OF OPTICALLY-THIN PLASMAS SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article DE METHODS, DATA ANALYSIS; METHODS, STATISTICAL; X-RAYS, GENERAL ID CORONAL TEMPERATURES; PARAMETER-ESTIMATION; ASTRONOMY AB We present results from an extensive number of PSPC spectral fitting simulations, performed with the aim to ascertain the dependence of the quality of the fit on photon counting statistics. In particular, we investigate the reliability of the results and their sensitivity to the assumed model in the case of X-ray emission from optically thin plasmas in thermal equilibrium, typical of stellar coronae and supernova remnants. We consider both single-temperature and two-temperature Raymond-Smith emission models, and the effects of contamination from either low or relatively high diffuse X-ray background. We explore the relative errors on the fitted temperatures derived from the simulations, and discuss constraints on the inferences that can be drawn regarding the existence of two components with different temperatures and emission measures in the observed spectrum. We also discuss the possibility that the presence of two components could be erroneously inferred from the analysis of a single-temperature spectrum. Moreover, we address the issue of the statistical independence of the spectral bins used in the fit by testing the agreement of the distribution of chi(2) values obtained from the simulations with the theoretical distribution. Finally, we briefly investigate advantages and drawbacks of using the C statistics as an alternative to the chi(2) statistics. C1 CNR,IST APPLICAZ INTERDISCIPLINARI FIS,I-90100 PALERMO,ITALY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MAGGIO, A (reprint author), IST OSSERV ASTRON,PALAZZO NORMANNI,I-90134 PALERMO,ITALY. RI Maggio, Antonio/P-5700-2015 OI Maggio, Antonio/0000-0001-5154-6108 NR 15 TC 3 Z9 3 U1 0 U2 0 PU EDITIONS PHYSIQUE PI LES ULIS CEDEX PA Z I DE COURTABOEUF AVE 7 AV DU HOGGAR, BP 112, 91944 LES ULIS CEDEX, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD MAY PY 1995 VL 110 IS 3 BP 573 EP 582 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QW812 UT WOS:A1995QW81200010 ER PT J AU GILBERT, AM PERIVOLAROPOULOS, L AF GILBERT, AM PERIVOLAROPOULOS, L TI SPECTRA AND STATISTICS OF COSMIC-STRING PERTURBATIONS ON THE MICROWAVE BACKGROUND - A MONTE-CARLO APPROACH SO ASTROPARTICLE PHYSICS LA English DT Article ID LARGE-SCALE STRUCTURE; WAKES; EVOLUTION AB Using Monte Carlo simulations of perturbations induced by cosmic strings on the microwave background, we demonstrate the scale invariance of string fluctuation patterns. By comparing string-induced fluctuation patterns with gaussian random phase ones, we show that the non-gaussian signatures of the string patterns are detectable by tests based on the moments of the distributions only for angular scales smaller than a few arcminutes and for maps based on the gradient of temperature fluctuations. However, we find that tests of the gaussianity of the moments fail when we include a reasonable amount of instrumental noise in a pattern. Signal to noise ratios of 3.3 or greater completely suppress a string pattern's non-gaussian features even at the highest resolutions. RP GILBERT, AM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,DIV THEORET ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Perivolaropoulos, Leandros/0000-0001-9330-2371 NR 34 TC 4 Z9 4 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 J9 ASTROPART PHYS JI Astropart Phys. PD MAY PY 1995 VL 3 IS 3 BP 283 EP 294 DI 10.1016/0927-6505(95)00003-Y PG 12 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA RA670 UT WOS:A1995RA67000007 ER PT J AU MAOZ, E GRINDLAY, JE AF MAOZ, E GRINDLAY, JE TI AN EXTENDED GALACTIC POPULATION OF LOW-LUMINOSITY X-RAY SOURCES (CVS) AND THE DIFFUSE-X-RAY BACKGROUND SO ASTROPHYSICAL JOURNAL LA English DT Article DE DIFFUSE RADIATION; GALAXIES, STELLAR CONTENT; GALAXY, HALO; NOVAE, CATACLYSMIC VARIABLES; X-RAYS, GALAXIES; X-RAYS, STARS ID MEDIUM-SENSITIVITY SURVEY; CATACLYSMIC VARIABLES; NEUTRON-STARS; ORIGIN; FLUCTUATIONS; EVOLUTION; GALAXIES; FAINT; PLANE; SATELLITE AB The incompatibility of the properties of the X-ray background (XRB) with AGNs contributing greater than or similar to 60% at energies of a few keV has often been interpreted as being due to a substantial contribution of a new population of yet unrecognized X-ray sources. The existence of such population has been recently suggested also by an analysis of very deep ROSAT observations which revealed a considerable excess of faint X-ray sources over that expected from QSO evolution models, and that the average spectrum of the resolved sources becomes harder with decreasing flux limit. These sources could be extragalactic in origin, but if they make a substantial contribution to the XRB then they must exhibit much weaker clustering than galaxies or QSOs in order to be consistent with the stringent constraints on source clustering imposed by autocorrelation analyses of the unresolved XRB. We investigate the possibility that the indicated new population of X-ray sources is Galactic in origin. Examining spherical halo and thick disk distributions, we derive the allowed properties of such populations which would resolve the discrepancy found in the number counts of faint sources and be consistent with observational constraints on the total background intensity, the XRB anisotropy, the number of unidentified bright sources, the Galaxy's total X-ray luminosity, and with the results of fluctuation analyses of the unresolved XRB. We find that a flattened Galactic halo (or a thick disk) distribution with a scale height of a few kpc is consistent with all the above requirements. The typical X-ray luminosity of the sources is approximate to 10(30-31) ergs s(-1) in the 0.5-2 keV band, the number density of sources in the solar vicinity is similar to 10(-4.5) pc(-3), their total number in the Galaxy is similar to 10(8.5), and their total contribution to the Galaxy's X-ray luminosity is similar to 10(39) ergs s(-1). We discuss the possible nature of these sources, including their being subdwarfs, LMXBs, massive black holes, and old neutron stars. We argue that the inferred X-ray and optical luminosities of the sources, the slope of their energy spectrum, and the derived local number density and spatial distribution are all consistent with their being intrinsically faint cataclysmic variables with low accretion rates. We suggest a few possibilities for the origin of such population, including an origin from disrupted globular clusters or dark clusters. We make predictions and suggest tests that could either confirm or rule out our proposal in the near future. RP MAOZ, E (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 74 TC 10 Z9 10 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 1995 VL 444 IS 1 BP 183 EP 192 DI 10.1086/175593 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QV080 UT WOS:A1995QV08000016 ER PT J AU NARAYAN, R YI, I AF NARAYAN, R YI, I TI ADVECTION-DOMINATED ACCRETION - SELF-SIMILARITY AND BIPOLAR OUTFLOWS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; HYDRODYNAMICS; ISM, JETS AND OUTFLOWS ID BOUNDARY-LAYERS; DISKS; INSTABILITY AB We consider axisymmetric viscous accretion flows where a fraction f of the viscously dissipated energy is stored in the accreting gas as entropy and a fraction 1 - f is radiated. Assuming alpha-viscosity we obtain a two-parameter family of self-similar solutions. Very few such exact self-consistent solutions are known for viscous differentially rotating flows. When the parameter f is small, that is, when there is very little advection, our solutions resemble standard thin accretion disks in many respects except that they have a hot tenuous corona above the disk. In the opposite advection-dominated limit, when f --> 1, the solutions approach nearly spherical accretion. The gas is almost at virial temperature and rotates at much below the Keplerian rate, and the flow is much more akin to Bondi accretion than to disk accretion. None of the solutions have funnels. We compare our exact self-similar solutions with approximate solutions which have been previously obtained using a height-integrated system of equations. We find that various dynamical variables such as the radial velocity, angular velocity, and sound speed estimated from the approximate solutions agree very well with the corresponding spherically averaged quantities in the exact solutions. We conclude that the height-integration approximation is an excellent one for a wide range of accretion conditions, including nearly spherical flows, provided the equations are interpreted as spherical averages. We find that the Bernoulli parameter is positive in all our solutions, especially close to the rotation axis. This effect is produced by viscous transport of energy from small to large radii and from the equator to the poles. In addition, all the solutions are convectively unstable, and the convection is especially important near the rotation axis. For both reasons, we suggest that a bipolar outflow will develop along the axis of these flows, fed by material from the surface layers of the equatorial inflow. RP NARAYAN, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 20 TC 537 Z9 545 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 1995 VL 444 IS 1 BP 231 EP 243 DI 10.1086/175599 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QV080 UT WOS:A1995QV08000022 ER PT J AU BELL, KR LIN, DNC HARTMANN, LW KENYON, SJ AF BELL, KR LIN, DNC HARTMANN, LW KENYON, SJ TI THE FU ORIONIS OUTBURST AS A THERMAL ACCRETION EVENT - OBSERVATIONAL CONSTRAINTS FOR PROTOSTELLAR DISK MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; STARS, EVOLUTION; STARS, PRE-MAIN-SEQUENCE STARS, VARIABLES, OTHER (FU ORIONIS) ID AURIGA MOLECULAR CLOUD; YOUNG STELLAR OBJECTS; Z-CANIS-MAJORIS; T-TAURI STARS; V1057 CYGNI; SOLAR NEBULA; EVOLUTION; MULTIPLICITY; VARIABLES; LIGHT AB The results of the time-dependent disk models developed in Bell and Lin are compared with observed properties of FU Orionis variables. Specific models are fit to the light curves of FU Ori, V1515 Cyg, and V1057 Cyg. The slow risetime of V1515 Cyg can be matched by a self-regulated outburst model. The rapid risetimes of FU Ori and V1057 Cyg can be fitted with the application of modest perturbations to the disk surface density. Model disks display spectral features characteristic of observed objects. The color evolution of V1057 Cyg is naturally explained if mass flux drops in the inner disk (tau < 1/4 AU) while remaining steady in the outer disk. The decrease in optical line width (rotational velocity) observed during the decay of V1057 Cyg may be accounted for by an outward-propagating ionization front. We predict that before final decay to the quiescent phase, short-wavelength line widths (lambda < 1.5 mu m) will again increase. It is suggested that FU Orionis outbursts primarily occur to systems during the embedded phase with ages less than several times 10(5) yr. C1 UNIV CALIF SANTA CRUZ,LICK OBSERV,SANTA CRUZ,CA 95064. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OI Kenyon, Scott/0000-0003-0214-609X NR 55 TC 87 Z9 87 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 1995 VL 444 IS 1 BP 376 EP 395 DI 10.1086/175612 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QV080 UT WOS:A1995QV08000035 ER PT J AU SASSELOV, D GOLDWIRTH, D AF SASSELOV, D GOLDWIRTH, D TI A NEW ESTIMATE OF THE UNCERTAINTIES IN THE PRIMORDIAL HELIUM ABUNDANCE - NEW BOUNDS ON OMEGA-BARYONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, OBSERVATIONS; H II REGIONS; RADIATIVE TRANSFER ID RECOMBINATION-LINE-INTENSITIES; MINIMAL ISOCURVATURE MODEL; HYDROGENIC IONS; HE-I; NUCLEOSYNTHESIS; NEBULAE AB We reexamine the systematic errors in the determination of the primordial helium abundance, Y-p. We find that the systematics are significantly larger than the statistical errors. The uncertainty in (the determination of) Y-p is thus larger than is currently claimed. Furthermore, all these systematics lead to an underestimate of Y-p. We argue that the true upper bound on Y-p could be as large as 0.255, which allows cosmological models with no nonbaryonic dark matter in which Omega(total)=Omega(baryons)=Omega(BBN)=0.2h(50)(2). C1 TEL AVIV UNIV,SACKLER FAC EXACT SCI,SCH PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL. RP SASSELOV, D (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 39 TC 36 Z9 36 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 1995 VL 444 IS 1 BP L5 EP L8 DI 10.1086/187846 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QV081 UT WOS:A1995QV08100002 ER PT J AU LEPP, S BUCH, V DALGARNO, A AF LEPP, S BUCH, V DALGARNO, A TI COLLISIONAL EXCITATION OF H-2-MOLECULES BY H-ATOMS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM, MOLECULES; MOLECULAR PROCESSES ID POTENTIAL-ENERGY SURFACE; INFRARED-EMISSION; SHOCKS AB Semiclassical trajectory calculations of the rate coefficients for rotational and vibrational energy transfer were carried out for collisions of hydrogen atoms with hydrogen molecules at a temperature of 1000 K, using three potential energy surfaces. For one surface the calculations were carried down to 200 K. The rate coefficients for reactive collisions are similar for all three surfaces. For nonreactive collisions, rate coefficients for pure rotational transitions in which j changes from 0 to 2 and from 1 to 3 change significantly from one surface to another but for higher angular momenta transitions the differences tend to disappear. The validity of the semiclassical calculations is assessed. C1 HEBREW UNIV JERUSALEM,DEPT PHYS CHEM,IL-91904 JERUSALEM,ISRAEL. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP LEPP, S (reprint author), UNIV NEVADA,DEPT PHYS,4505 MARYLAND PKWY,LAS VEGAS,NV 89154, USA. NR 15 TC 27 Z9 27 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 1995 VL 98 IS 1 BP 345 EP 349 DI 10.1086/192164 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU868 UT WOS:A1995QU86800013 ER PT J AU JOB, DA BONESS, DJ FRANCIS, JM AF JOB, DA BONESS, DJ FRANCIS, JM TI INDIVIDUAL VARIATION IN NURSING VOCALIZATIONS OF HAWAIIAN MONK SEAL PUPS, MONACHUS-SCHAUINSLANDI (PHOCIDAE, PINNIPEDIA), AND LACK OF MATERNAL RECOGNITION SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article ID TADARIDA-BRASILIENSIS-MEXICANA; FREE-TAILED BATS; VOCAL RECOGNITION; FOSTERING BEHAVIOR; FUR SEALS; MOTHERS AB Vocalizations of individual Hawaiian monk seal pups, Monachus schauinslandi, do not have unique attributes that enable females to recognize their own offspring. Despite low aggregation density during pupping, aggressive encounters are common between females with pups. Fostering is prevalent and may reflect confusion over the identity of pups following aggressive encounters between females. All pup vocalizations were simple in structure and contained true harmonics. The coefficients of variation revealed considerable variance in vocalization structure within pups. Controlling for age, multivariate analyses of variance revealed significant. differences among pups in vocalization attributes. Significant developmental changes occurred in vocalization structure for some pups but not for others. Discriminant function analysis suggested that it would be difficult for females to distinguish between the vocalizations of pups. The results of experiments conducted in the field showed that females did not discriminate between filial and alien pups by voice. In addition, females tended not to foster pups that had vocalizations similar to those of their own offspring. Thus, females seem to be unable to recognize their pups by voice. The apparent lack of vocal recognition of pups may contribute to the high frequency of fostering in this species. C1 UNIV MARYLAND,DEPT ANIM SCI,COLLEGE PK,MD 20742. RP JOB, DA (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008, USA. NR 49 TC 34 Z9 34 U1 1 U2 6 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA ON K1A 0R6, CANADA SN 0008-4301 J9 CAN J ZOOL JI Can. J. Zool.-Rev. Can. Zool. PD MAY PY 1995 VL 73 IS 5 BP 975 EP 983 DI 10.1139/z95-114 PG 9 WC Zoology SC Zoology GA RR091 UT WOS:A1995RR09100019 ER PT J AU KOLMAN, CJ BERMINGHAM, E COOKE, R WARD, RH ARIAS, TD GUIONNEAUSINCLAIR, F AF KOLMAN, CJ BERMINGHAM, E COOKE, R WARD, RH ARIAS, TD GUIONNEAUSINCLAIR, F TI REDUCED MTDNA DIVERSITY IN THE NGOBE AMERINDS OF PANAMA SO GENETICS LA English DT Article ID HUMAN MITOCHONDRIAL-DNA; POPULATIONS; DIFFERENTIATION; MICROEVOLUTION; SEQUENCES; LINEAGES AB Mitochondrial DNA (mtDNA) haplotype diversity was determined for 46 Ngobe Amerinds sampled widely across their geographic range in western Panama. The Ngobe data were compared with mtDNA control region I sequences from two additional Amerind groups located at the northern and southern extremes of Amerind distribution, the Nuu-Chah-Nulth of the Pacific Northwest and the Chilean Mapuche and from one Na-Dene group, the Haida of the Pacific Northwest. The Ngobe exhibit the lowest mtDNA control region sequence diversity yet reported for an Amerind group. Moreover, they carry only two of the four Amerind founding lineages first described by Wallace and coworkers. We posit that the Ngobe passed through a population bottleneck caused by ethnogenesis from a small founding population and/or European conquest and colonization. Dating of the Ngobe population expansion using the HARPENDING et al. approach to the analysis of pairwise genetic differences indicates a Ngobe expansion at roughly 6800 years before present (range: 1850-14,000 years before present), a date more consistent with a bottleneck at Chibcha ethnogenesis than a conquest-based event. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. UNIV UTAH,DEPT HUMAN GENET,SALT LAKE CITY,UT 84132. UNIV PANAMA,DEPT ANTROPOL,PANAMA CITY,PANAMA. UNIV PANAMA,COLEGIO FARM,PANAMA CITY,PANAMA. NR 46 TC 93 Z9 95 U1 0 U2 4 PU GENETICS PI BALTIMORE PA 428 EAST PRESTON ST, BALTIMORE, MD 21202 SN 0016-6731 J9 GENETICS JI Genetics PD MAY PY 1995 VL 140 IS 1 BP 275 EP 283 PG 9 WC Genetics & Heredity SC Genetics & Heredity GA QV521 UT WOS:A1995QV52100023 PM 7635293 ER PT J AU BATISTA, O KOLMAN, CJ BERMINGHAM, E AF BATISTA, O KOLMAN, CJ BERMINGHAM, E TI MITOCHONDRIAL-DNA DIVERSITY IN THE KUNA AMERINDS OF PANAMA SO HUMAN MOLECULAR GENETICS LA English DT Article ID DIFFERENTIATION; MICROEVOLUTION; POPULATIONS; LINEAGES AB Mitochondrial DNA (mtDNA) haplotype diversity was determined for 63 Chibcha-speaking Kuna Amerinds sampled widely across their geographic range in eastern Panama. The Kuna data were compared with mtDNA control region I sequences from two neighboring Chibchan groups, the Ngobe and the Huetar; two Amerind groups located at the northern and southern extremes of Amerind distribution, the Nuu-Chah-Nulth of the Pacific Northwest and the Chilean Mapuche; and with a single Na-Dene group, the Haida of the Pacific Northwest, The Kuna exhibited low levels of mitochondrial diversity as had been reported for the other two Chibchan groups and, furthermore, carried only two of the four Amerind founding lineages first reported by Schurr and coworkers (Am. J. Hum. Genet. 1990; 46: 613-623), We posit that speakers of modern Chibchan languages (henceforth referred to as the Chibcha) passed through a population bottleneck caused either by ethnogenesis from a small founding population and/or subsequent European conquest and colonization, Using the approach of Harpending al al. (Curr. Anthropol. 1993; 34: 483-496), we estimated a Chibchan population bottleneck and subsequent expansion approximately 10000 years before present, a date consistent with a bottleneck at the time of Chibchan ethnogenesis, The low mtDNA diversity of Kuna Amerinds, as opposed to the generally high levels of mtDNA variation detected in other Amerind groups, demonstrates the need for adequate sampling of cultural or racial groups when attempting to genetically characterize human populations. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. UNIV COSTA RICA,SAN JOSE,COSTA RICA. NR 43 TC 81 Z9 85 U1 0 U2 2 PU OXFORD UNIV PRESS UNITED KINGDOM PI OXFORD PA WALTON ST JOURNALS DEPT, OXFORD, ENGLAND OX2 6DP SN 0964-6906 J9 HUM MOL GENET JI Hum. Mol. Genet. PD MAY PY 1995 VL 4 IS 5 BP 921 EP 929 DI 10.1093/hmg/4.5.921 PG 9 WC Biochemistry & Molecular Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Genetics & Heredity GA QX780 UT WOS:A1995QX78000018 PM 7633453 ER PT J AU YENER, KA JETT, P ADRIAENS, A AF YENER, KA JETT, P ADRIAENS, A TI SILVER AND COPPER ARTIFACTS FROM ANCIENT ANATOLIA SO JOM-JOURNAL OF THE MINERALS METALS & MATERIALS SOCIETY LA English DT Article C1 SMITHSONIAN INST,FREER GALLERY ART,WASHINGTON,DC 20560. SMITHSONIAN INST,ARTHUR M SACKLER GALLERY,WASHINGTON,DC 20560. UNIV ANTWERP,B-2020 ANTWERP,BELGIUM. RP YENER, KA (reprint author), UNIV CHICAGO,ORIENTAL INST,1155 E 58TH ST,CHICAGO,IL 60637, USA. RI Adriaens, Annemie/F-2520-2013 OI Adriaens, Annemie/0000-0003-4034-1881 NR 19 TC 1 Z9 1 U1 0 U2 1 PU MINERALS METALS MATERIALS SOC PI WARRENDALE PA 420 COMMONWEALTH DR, WARRENDALE, PA 15086 SN 1047-4838 J9 JOM-J MIN MET MAT S JI JOM-J. Miner. Met. Mater. Soc. PD MAY PY 1995 VL 47 IS 5 BP 70 EP 72 PG 3 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing SC Materials Science; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing GA QY351 UT WOS:A1995QY35100015 ER PT J AU COTE, R JAMIESON, MJ AF COTE, R JAMIESON, MJ TI COMPARISON OF PHASE-SHIFT CALCULATIONS BY ASYMPTOTIC FIT AND QUADRATURE IN ULTRA-LOW TEMPERATURE SCATTERING SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Note ID STATES C1 UNIV GLASGOW,DEPT COMP SCI,GLASGOW G61 1BD,LANARK,SCOTLAND. RP COTE, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 9 TC 11 Z9 11 U1 1 U2 2 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 SN 0021-9991 J9 J COMPUT PHYS JI J. Comput. Phys. PD MAY PY 1995 VL 118 IS 2 BP 388 EP 391 DI 10.1006/jcph.1995.1108 PG 4 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA QV550 UT WOS:A1995QV55000018 ER EF