FN Thomson Reuters Web of Science™ VR 1.0 PT J AU MIKOLAJEWSKA, J KENYON, SJ AF MIKOLAJEWSKA, J KENYON, SJ TI ON THE NOVA-LIKE ERUPTIONS OF SYMBIOTIC BINARIES SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ACCRETION, ACCRETION DISKS; BINARIES, SYMBIOTIC; STARS, EVOLUTION; STARS, INDIVIDUAL, R-AQR ID ACCRETING WHITE-DWARFS; HYDROGEN SHELL FLASHES; STAR RX PUPPIS; IUE OBSERVATIONS; VISCOUS DISKS; MASS-LOSS; CH CYGNI; AQUARII; EVOLUTION; PERIOD AB We discuss three popular explanations for the nova-like eruptions observed in symbiotic binary stars and compare model predictions with recent observations. Most outbursts occur when unstable hydrogen shell burning causes a hot white dwarf to expand to a radius of 1-100 R.. This model predicts a long-duration, constant-luminosity phase following visual maximum, and observations of the symbiotic novae and several steady-burning sources confirm this feature of thermonuclear runaway calculations. At least two symbiotics erupt when the accretion rate from a circum-stellar disc onto a solar-type central star increases by 1-2 orders of magnitude. Simple accretion models emit approximately 50 per cent of the gravitational energy in the disc and the remainder in a hot boundary layer between the disc and central star. Observations of CI Cyg and AX Per support this picture for accretion rates below approximately 10(-4) M. yr-1, but boundary layer emission vanishes for higher accretion rates. Finally, we associate observations of extra reddening and the appearance of high-ionization emission lines in R Aqr with an increase in the Mira mass-loss rate initiated, perhaps, by a helium shell flash above the Mira's degenerate core. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MIKOLAJEWSKA, J (reprint author), NICHOLAS COPERNICUS UNIV,INST ASTRON,UL CHOPINA 12-18,PL-87100 TORUN,POLAND. OI Kenyon, Scott/0000-0003-0214-609X NR 85 TC 75 Z9 76 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 MAY 15 PY 1992 VL 256 IS 2 BP 177 EP 185 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HU177 UT WOS:A1992HU17700001 ER PT J AU ARNAUD, M HUGHES, JP FORMAN, W JONES, C LACHIEZEREY, M YAMASHITA, K HATSUKADE, I AF ARNAUD, M HUGHES, JP FORMAN, W JONES, C LACHIEZEREY, M YAMASHITA, K HATSUKADE, I TI A2163 - AN EXCEPTIONALLY HOT CLUSTER OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE DARK MATTER; GALAXIES-CLUSTERING; X-RAYS-GALAXIES ID X-RAY OBSERVATIONS; COMA CLUSTER; EVOLUTION; EMISSION; OPHIUCHUS; MICROWAVE; CATALOG; SPECTRA; PLASMAS; ORIGIN AB We measured the X-ray spectrum of the distant galaxy cluster A2163 in the energy range 1-18 keV with the Ginga satellite. A combined analysis of these data with data previously obtained with the Einstein Observatory is presented. The mean temperature and X-ray luminosity we derive are exceptionally high compared to other clusters: kT = 12.9 keV, L(X) (2-10 keV) = 3.5 x 10(45) ergs s-1 for z = 0.15, as are the gas mass (6.7 x 10(14) M.) and binding mass (25 x 10(14) M.). The very existence of such a cluster can provide interesting constraints on the relative distribution of "visible" mass and dark matter, an important parameter in cold dark matter models for formation of structure in the universe. C1 CENS,SERV ASTROPHYS,F-91191 GIF SUR YVETTE,FRANCE. INST SPACE & ASTRONAUT SCI,SAGAMIHARA,KANAGAWA 229,JAPAN. MIYAZAKI UNIV,FAC ENGN,MIYAZAKI 88920,JAPAN. RP ARNAUD, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 37 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 MAY 10 PY 1992 VL 390 IS 2 BP 345 EP 349 DI 10.1086/171285 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HR232 UT WOS:A1992HR23200005 ER PT J AU STURTEVANT, WC AF STURTEVANT, WC TI ATLAS OF WORLD CULTURES - A GEOGRAPHICAL GUIDE TO ETHNOGRAPHIC LITERATURE - PRICE,DH SO AMERICAN ETHNOLOGIST LA English DT Book Review RP STURTEVANT, WC (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 SN 0094-0496 J9 AM ETHNOL JI Am. Ethnol. PD MAY PY 1992 VL 19 IS 2 BP 388 EP 389 DI 10.1525/ae.1992.19.2.02a00240 PG 2 WC Anthropology SC Anthropology GA HT816 UT WOS:A1992HT81600025 ER PT J AU BURCH, ES AF BURCH, ES TI OIL AGE ESKIMOS - JORGENSON,JG SO AMERICAN ETHNOLOGIST LA English DT Book Review RP BURCH, ES (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 SN 0094-0496 J9 AM ETHNOL JI Am. Ethnol. PD MAY PY 1992 VL 19 IS 2 BP 398 EP 399 PG 2 WC Anthropology SC Anthropology GA HT816 UT WOS:A1992HT81600036 ER PT J AU GUNTER, AC AF GUNTER, AC TI TREASURES FROM MESOPOTAMIA SO ARCHAEOLOGY LA English DT Article C1 SMITHSONIAN INST,ARTHUR M SACKLER GALLERY,WASHINGTON,DC 20560. SMITHSONIAN INST,FREER GALLERY ART,WASHINGTON,DC 20560. NR 0 TC 0 Z9 0 U1 0 U2 1 PU ARCHAEOLOGICAL INST PI NEW YORK PA 135 WILLIAM ST, NEW YORK, NY 10038-3805 SN 0003-8113 J9 ARCHAEOLOGY JI Archaeology PD MAY-JUN PY 1992 VL 45 IS 3 BP 48 EP 51 PG 4 WC Archaeology SC Archaeology GA KC616 UT WOS:A1992KC61600019 ER PT J AU PHILLIPS, MM WELLS, LA SUNTZEFF, NB HAMUY, M LEIBUNDGUT, B KIRSHNER, RP FOLTZ, CB AF PHILLIPS, MM WELLS, LA SUNTZEFF, NB HAMUY, M LEIBUNDGUT, B KIRSHNER, RP FOLTZ, CB TI SN-1991T - FURTHER EVIDENCE OF THE HETEROGENEOUS NATURE OF TYPE-IA SUPERNOVAE SO ASTRONOMICAL JOURNAL LA English DT Article ID ABSOLUTE-MAGNITUDE; SPECTROSCOPY; PHOTOMETRY; SPECTRUM; MODELS; 1986G; NOVA AB Optical spectra of SN 1991T obtained approximately one week before B maximum showed no evidence of the Si, Ca, and S absorption lines which normally dominate the spectra of type Ia supernovae at early phases. Nevertheless, within two weeks after maximum, the spectrum of SN 1991T had evolved to resemble closely that of other type Ia events. These observations suggest that the abundances of Si, Ca, and S in the outer ejecta of SN 1991T were unusually low. The B and V light curves of SN 1991T resembled those of other type Ia supernovae, but the slope of the initial decline following maximum was less steep than normal in both colors. In spite of these spectroscopic and photometric peculiarities, the absolute magnitude of SN 1991T at B maximum was apparently similar to that of a typical type Ia event. Thus, although the data suggest that SN 1991T was a type Ia supernova with peculiar surface abundances, in most other ways it seems to have been a completely normal type Ia explosion. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. MULTIPLE MIRROR TELESCOPE OBSERV,TUCSON,AZ 85721. RP PHILLIPS, MM (reprint author), ASSOC UNIV RES ASTRON INC,NATL OPT ASTRON OBSERV,CERRO TOLOLO INTER AMER OBSERV,CASILLA 603,LA SERERA,CHILE. RI Hamuy, Mario/G-7541-2016 NR 58 TC 227 Z9 229 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 1992 VL 103 IS 5 BP 1632 EP 1637 DI 10.1086/116177 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HR195 UT WOS:A1992HR19500022 ER PT J AU WHITNEY, BA CLAYTON, GC SCHULTELADBECK, RE MEADE, MR AF WHITNEY, BA CLAYTON, GC SCHULTELADBECK, RE MEADE, MR TI SPECTROPOLARIMETRY OF V854-CENTAURI AT MINIMUM LIGHT - CLUES TO THE GEOMETRY OF THE DUST AND EMISSION-LINE REGION SO ASTRONOMICAL JOURNAL LA English DT Article ID R-CORONAE-BOREALIS; STARS AB We have observed the RCB star V854 Cen during a very deep decline (DELTA-m = 8.2) at the AAT. The continuum polarization is very high, ranging from 14% at 4200 angstrom to about 4% at 6500 angstrom. The polarization decreases across the emission lines but the polarized flux remains constant. This indicates that the emission lines are unpolarized, so the emission probably arises in a region unobscured by dust. In such a deep minimum, the visible continuum flux is probably almost entirely scattered light, which explains its high polarization. The scattered flux may arise in the same clouds contributing to the observed IR flux if the albedo is low and the grains forward throwing. The emission-line spectrum itself is very unusual for an RCB star in decline, with strong C2 bands and Balmer lines. C1 UNIV COLORADO,CTR ASTROPHYS & SPACE ASTRON,BOULDER,CO 80309. UNIV WISCONSIN,SPACE ASTRON LAB,MADISON,WI 53706. RP WHITNEY, BA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 29 TC 37 Z9 37 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 MAY PY 1992 VL 103 IS 5 BP 1652 EP 1657 DI 10.1086/116180 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HR195 UT WOS:A1992HR19500025 ER PT J AU MARCAIDE, JM ALBERDI, A BARTEL, N CLARK, TA COREY, BE ELOSEGUI, P GORENSTEIN, MV GUIRADO, JC KARDASHEV, N POPOV, M PRESTON, R RATNER, MI RIOJA, MJ ROGERS, AEE SHAPIRO, II AF MARCAIDE, JM ALBERDI, A BARTEL, N CLARK, TA COREY, BE ELOSEGUI, P GORENSTEIN, MV GUIRADO, JC KARDASHEV, N POPOV, M PRESTON, R RATNER, MI RIOJA, MJ ROGERS, AEE SHAPIRO, II TI POSITION AND MORPHOLOGY OF THE COMPACT NONTHERMAL RADIO-SOURCE AT THE GALACTIC-CENTER SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE RADIO SOURCES, SGRA-ASTERISK; GALAXY, CENTER OF; INTERFEROMETRY, VLBI; ASTROMETRY ID SCATTERING; DISK AB We have determined with VLBI the position of the compact nonthermal radio source at the Galactic Center, commonly referred to as SgrA*, in the J2000.0 reference frame of extragalactic radio sources. We have also determined the size of SgrA* at 1.3, 3.6 and 13 cm wavelengths and found that the apparent size of the source increases proportionally to the observing wavelength squared, as expected from source size broadening by interstellar scattering and as reported previously by other authors (e.g. Davies et al. 1976; Marcaide et al. 1985; Lo et al. 1985; Jauncey et al. 1989). We have also established an upper limit of about 8 mJy at 3.6 cm wavelength for any ultracompact component. The actual size of the source is less than 15 AU. Fourier analysis of our very sensitive 3.6 cm observations of this source shows no significant variations of correlated flux density on time scales from 12 to 700 s. C1 MAX PLANCK INST RADIOASTRON, W-5300 BONN 1, GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NASA, GODDARD SPACE FLIGHT CTR, GREENBELT, MD 20771 USA. HAYSTACK OBSERV, WESTFORD, MA 01886 USA. MOSCOW SPACE RES INST, MOSCOW, USSR. JET PROP LAB, PASADENA, CA 91109 USA. RP MARCAIDE, JM (reprint author), CSIC, INST ASTROFIS ANDALUCIA, APARTADO 3004, E-18080 GRANADA, SPAIN. RI Kardashev, Nikolai/O-6441-2015 NR 24 TC 19 Z9 19 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 MAY PY 1992 VL 258 IS 2 BP 295 EP 301 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HV952 UT WOS:A1992HV95200016 ER PT J AU MAUROGORDATO, S SCHAEFFER, R DACOSTA, LN AF MAUROGORDATO, S SCHAEFFER, R DACOSTA, LN TI THE LARGE-SCALE GALAXY DISTRIBUTION IN THE SOUTHERN SKY REDSHIFT SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, OBSERVATIONS; GALAXIES, CLUSTERING; LARGE-SCALE STRUCTURE OF UNIVERSE ID INVARIANT MATTER DISTRIBUTION; POINT CORRELATION-FUNCTIONS; LUMINOSITY SEGREGATION; UNIVERSE; CATALOG; PROBABILITY; THERMODYNAMICS; FLUCTUATIONS; STATISTICS; CLUSTERS AB The recent SSRS (Southern Sky Redshift Survey) data are used to discuss the structure of the universe as viewed from the distribution of galaxies at scales ranging from 1 h-1 Mpc up to approximately 20 h-1 Mpc. In addition to the two-body correlation function, the J3 integral and galaxy counts in clustered regimes that describe the clustering especially in the dense parts, we focus also on the statistical indicators that best describe the under-dense regions: statistics of voids and counts in cells. We determine the typical size of voids and its dependence on the galaxy density. By considering samples of various depths (40, 60, and 80 h-1 Mpc), we carefully examine the variations of these statistical indicators. We find that the density decrease for the deeper samples is solely due to the variations of the galaxy diameter limit, and that all indicators, when corrected for their obvious density dependence, show only quite small variations. They, however, are systematic and can be attributed to variations of the correlation length due to diameter (luminosity) segregation. We find a density-dependent but depth-independent, limit for the size of the voids that for a sample with 10(-2) h-1 Mpc-3 galaxies have a diameter smaller than 20 h-1 Mpc at the 99% confidence limit. We also find strong evidence that the galaxy distribution obeys scaling laws in both the dense and underdense regions, that relate the observed distribution at different scales and densities over the entire range considered. The physical process that led to the galaxy clustering may thus be expected to have been the same at all the scales we have examined here. C1 CENS,SERV PHYS THEOR SACLAY,CEA,DIRECT SCI MATIERE LAB,F-91191 GIF SUR YVETTE,FRANCE. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MAUROGORDATO, S (reprint author), OBSERV MEUDON,DAEC,F-92195 MEUDON,FRANCE. NR 51 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 MAY 1 PY 1992 VL 390 IS 1 BP 17 EP 33 DI 10.1086/171255 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HP595 UT WOS:A1992HP59500003 ER PT J AU KOO, BC HEILES, C REACH, WT AF KOO, BC HEILES, C REACH, WT TI GALACTIC WORMS .1. CATALOG OF WORM CANDIDATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE CATALOGS; H-II REGIONS; ISM, BUBBLES; RADIO CONTINUUM, INTERSTELLAR; RADIO LINES, ATOMIC ID H-II REGIONS; INFRARED-EMISSION; MILKY-WAY; INTERSTELLAR GRAINS; GALAXY; DISK; DENSITY; IRAS; EXPLOSIONS; CLOUDS AB We have found and cataloged 118 isolated structures that appear both in H I and in infrared (60 and 100-mu-m). In the inner Galaxy, these correspond to the "H I worms" detected by Heiles. The worms are thought to be the walls surrounding superbubbles which have broken through the thin gaseous disk inside the solar circle. Among 118 structures, 52 are possibly associated with H II regions. The structures associated with H II regions have a higher probability for association with superbubbles. Upon analysis of the catalog, we found that (1) the 100-mu-m emissivity, I100/N(H I), increases systematically toward the Galactic interior, which is consistent with the increase of the general interstellar radiation field, (2) the 100-mu-m emissivity of the structures associated with H II regions is larger than that of the structures without associated H II regions, and (3) the 60-100-mu-m ratio is large, 0.28 +/- 0.03, which may indicate that the grains associated with atomic gas have a relatively large population of small grains. Among 118 structures, 35 appear in the 408 MHz continuum. About 70% of the 35 structures are possibly associated with H II regions. The infrared and the radio continuum properties suggest that the 408 MHz continuum emission in those structures is very likely thermal. The thermal emission probably originates from the gas ionized by photons from stars located in the same general region that produce the H II region. Some individual objects are briefly described. We discuss implications of our results on the ionization of gas far from the Galactic plane. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP KOO, BC (reprint author), UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720, USA. RI Reach, William/C-4710-2008 NR 56 TC 84 Z9 84 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 1992 VL 390 IS 1 BP 108 EP 132 DI 10.1086/171264 PN 1 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HP595 UT WOS:A1992HP59500012 ER PT J AU TEREBEY, S VOGEL, SN MYERS, PC AF TEREBEY, S VOGEL, SN MYERS, PC TI PROBING THE CIRCUMSTELLAR ENVIRONMENTS OF VERY YOUNG LOW-MASS STARS USING WATER MASERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; MASERS; RADIO CONTINUUM, STARS; STARS, FORMATION; STARS, MASS LOSS ID DENSE CORES; IRAS SOURCES; DARK CLOUDS; H2O MASERS; MOLECULAR CLOUD; BIPOLAR OUTFLOW; RESOLUTION; PROTOSTARS; EVOLUTION; L1551 AB We have used the VLA to search nearby very young low-mass stars for water maser emission. The sample consists of 26 low-luminosity IRAS sources embedded in dense molecular cores, a class of sources suspected to be newly forming low-mass stars on the order of a few hundred thousand years old. Three sources were detected: IRAS 16293 - 2422 in L1689, 05417 + 0907 in B35, and 16244 - 2432 in L1681B. The maser detection rate of 10% for the IRAS-dense cores is comparable to rates found in surveys of similar but typically higher luminosity sources. High spatial resolution maps show the region of maser emission is generally confined to an area smaller than approximately 0.5" (approximately 100 AU) near the star, and the velocities of individual components span intervals ranging from 20 to 40 km s-1. The maser velocities are too large to be due to gravitational motions in at least two of the sources, implying that the masers are associated with the winds from the young low-mass stars. Using the positions of the masers as probes of the wind's spatial structure provides a way to trace the collimation of the wind very close to the young star. Comparing the high spatial resolution maser data to lower resolution CO data shows no evidence for higher collimation close to the star-the stellar wind cavity appears to have similar collimation at 10(15) cm as at 10(17)-10(18) cm. C1 CALTECH,CTR INFRARED PROC & ANAL 10022,JET PROPULS LAB,PASADENA,CA 91125. UNIV MARYLAND,ASTRON PROGRAM,COLLEGE PK,MD 20742. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP TEREBEY, S (reprint author), CALTECH,CANADIAN INST THEORET ASTROPHYS,PASADENA,CA 91125, USA. NR 47 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 1992 VL 390 IS 1 BP 181 EP 190 DI 10.1086/171269 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HP595 UT WOS:A1992HP59500017 ER PT J AU ELVIS, M PLUMMER, D SCHACHTER, J FABBIANO, G AF ELVIS, M PLUMMER, D SCHACHTER, J FABBIANO, G TI THE EINSTEIN SLEW SURVEY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE BL LACERTAE OBJECTS; GENERAL; CATALOGS; QUASARS; GENERAL; X-RAYS; GENERAL; X-RAYS; STARS; SURVEYS ID MEDIUM-SENSITIVITY SURVEY; BRIGHT QUASAR SURVEY; X-RAY-SPECTRA; N-LOG-S; CATALOG; CLUSTERS; COMPILATION; GALAXIES; OBJECTS; SAMPLE AB A catalog of 819 sources detected in the Einstein IPC Slew Survey of the X-ray sky is presented; 313 of the sources were not previously known as X-ray sources. Typical count rates are 0.1 IPC count s-1, roughly equivalent to a flux of 3 x 10(-12) ergs CM-2 s-1. The sources have positional uncertainties of 1.'2 (90% confidence) radius, based on a subset of 452 sources identified with previously known pointlike X-ray sources (i.e. extent less than 3'). Identifications based on a number of existing catalogs of X-ray and optical objects are proposed for 637 of the sources, 78% of the survey, (within a 3' error radius) including 133 identifications of new X-ray sources. A public identification data base for the Slew Survey sources will be maintained at CfA, and contributions to this data base are invited. RP ELVIS, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 54 TC 191 Z9 192 U1 1 U2 1 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 1992 VL 80 IS 1 BP 257 EP 303 DI 10.1086/191665 PG 47 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HR035 UT WOS:A1992HR03500006 ER PT J AU ESCALANTE, V VICTOR, GA AF ESCALANTE, V VICTOR, GA TI PHOTOIONIZATION OF EXCITED-STATES OF NEUTRAL ATOMIC CARBON AND SINGLY IONIZED NITROGEN SO ATOMIC DATA AND NUCLEAR DATA TABLES LA English DT Article C1 HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOLEC PHYS, CAMBRIDGE, MA 02138 USA. RP NATL AUTONOMOUS UNIV MEXICO, INST ASTRON, AP POSTAL 70264, CIUDAD UNIV MEXICO, MEXICO CITY 04510, DF, MEXICO. NR 10 TC 3 Z9 4 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0092-640X EI 1090-2090 J9 ATOM DATA NUCL DATA JI Atom. Data Nucl. Data Tables PD MAY PY 1992 VL 51 IS 1 BP 1 EP 57 DI 10.1016/0092-640X(92)90014-9 PG 57 WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Physics GA HU005 UT WOS:A1992HU00500001 ER PT J AU DONOGHUE, AM JOHNSTON, LA MUNSON, L BROWN, JL WILDT, DE AF DONOGHUE, AM JOHNSTON, LA MUNSON, L BROWN, JL WILDT, DE TI INFLUENCE OF GONADOTROPIN TREATMENT INTERVAL ON FOLLICULAR MATURATION, INVITRO FERTILIZATION, CIRCULATING STEROID CONCENTRATIONS, AND SUBSEQUENT LUTEAL FUNCTION IN THE DOMESTIC CAT SO BIOLOGY OF REPRODUCTION LA English DT Article ID OVARIAN ACTIVITY; SEXUAL-BEHAVIOR; OOCYTES; PHASE; PROGESTERONE; ASPIRATION; CYCLICITY; PREGNANCY; ESTRADIOL; HORMONES AB The impact of the eCG-hCG interval on in vitro fertilization (IVF), endogenous hormonal patterns, and luteal integrity was studied in the domestic cat. Adult cats with inactive ovaries were given eCG (i.m.) and then hCG (i.m.) 80, 84, 88, 92, or 96 h later. Oocytes were aspirated 25-27 h after hCG and co-cultured with swim-up-processed cat spermatozoa. Blood samples were collected daily from 2 days before eCG treatment (Day -2) through Day 14, and sera were analyzed for estradiol-17-beta and progesterone. The mean number of oocytes recovered from the 80-92-h groups (range, 17.2 +/- 2.1 to 21.1 +/- 3.0) did not differ (p > 0.05); however, oocyte number was reduced (p < 0.05) in the 96-h group (10.3 +/- 2.1). The proportion of all oocytes classified as mature was greater (p < 0.05) when hCG was given 80, 84, or 88 h compared to 92 or 96 h after eCG. Delaying hCG treatment until 96 h caused more than 25% of all oocytes to degenerate, which was a greater rate (p < 0.05) than in all other groups. The IVF rate at 80 (57%), 84 (56.5%), 88 (65.0%), and 92 (52.5%) h was greater (p < 0.05) than that observed at 96 h (33.6%). Circulating estradiol-17-beta concentrations began to rise above nadir within 24 h of eCG injection in all interval groups. On the basis of areas under the curve, cats in the 80- and 84-h treatments produced more (p < 0.05) estradiol-17-beta than other groups. Circulating progesterone rose above nadir within the first 24 h of follicular aspiration, and there were no marked temporal differences among groups. Mean CL number on Day 14 ranged from 11.8 in the 96-h group to 20.3 in the 84-h group, but was not different (p > 0.05) because of wide variation among individual animals. Mean luteal weight per ovary was higher (p < 0.05) in the 80-92-h intervals (range, 0.13 +/- 0.01 to 0.21 +/- 0.14 g/ovary) than in the 96-h group (0.07 +/- 0.01 g/ovary), resulting in greater overall progesterone content per ovary (p < 0.05). However, neither progesterone concentration per unit mass of luteal tissue nor luteal histology differed (p > 0.05) among interval groups. Although cat oocytes normally reside within Graafian follicles for unpredictable intervals awaiting copulation, these oocytes are sensitive to the timing of the hormonal stimulus that triggers final maturation, but only if the interval between the FSH-like and LH-like stimulus exceeds 88 h. The effect is expressed by variation in the number and maturity of oocytes recovered and by as yet undefined alterations that influence fertilizability in vitro but not CL composition or function. C1 UNIFORMED SERV UNIV HLTH SCI,BETHESDA,MD 20814. NCI,VIRAL CARCINOGENESIS LAB,FREDERICK,MD 21701. UNIV TENNESSEE,COLL VET MED,KNOXVILLE,TN 37901. RP DONOGHUE, AM (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ANIM HLTH,WASHINGTON,DC 20008, USA. FU NICHD NIH HHS [HD 23853] NR 42 TC 45 Z9 47 U1 1 U2 6 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD MAY PY 1992 VL 46 IS 5 BP 972 EP 980 DI 10.1095/biolreprod46.5.972 PG 9 WC Reproductive Biology SC Reproductive Biology GA HP390 UT WOS:A1992HP39000028 PM 1591354 ER PT J AU JAMIESON, MJ FRIEDMAN, RS AF JAMIESON, MJ FRIEDMAN, RS TI ERROR ESTIMATION IN MOLECULAR VIBRATIONAL EIGENENERGIES CALCULATED BY THE HARTREE AND NUMEROV METHODS SO COMPUTER PHYSICS COMMUNICATIONS LA English DT Article ID SCHRODINGER-EQUATION AB Errors in the eigenenergies of some molecular vibrations are estimated for the Hartree and Numerov integration schemes and it is shown how the estimates can be used to determine suitable step sizes. The global truncation errors of the eigenenergies are demonstrated to be of orders two and four, respectively, in the step size. Some numerical comparisons are made. C1 UNIV GLASGOW,DEPT COMP SCI,GLASGOW G12 8QQ,SCOTLAND. HARVARD UNIV,DEPT CHEM,CAMBRIDGE,MA 02138. UNIV MINNESOTA,DEPT CHEM,MINNEAPOLIS,MN 55455. RP JAMIESON, MJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 12 TC 3 Z9 3 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0010-4655 J9 COMPUT PHYS COMMUN JI Comput. Phys. Commun. PD MAY PY 1992 VL 70 IS 1 BP 53 EP 58 DI 10.1016/0010-4655(92)90090-L PG 6 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA HT370 UT WOS:A1992HT37000005 ER PT J AU WARKENTIN, IG JAMES, PC OLIPHANT, LW AF WARKENTIN, IG JAMES, PC OLIPHANT, LW TI ASSORTATIVE MATING IN URBAN-BREEDING MERLINS SO CONDOR LA English DT Article DE MERLIN; FALCO-COLUMBARIUS; URBAN; ASSORTATIVE MATING; BREEDING; AGE; SASKATCHEWAN ID RED-WINGED BLACKBIRDS; MATE CHOICE; FALCO-COLUMBARIUS; TERRITORY QUALITY; FEMALE CHOICE; AGE; BIRDS; DISPERSAL; SELECTION; SPARROWHAWKS AB We examined assortative mating behavior in 149 pairs of Merlins (Falco columbarius) breeding in Saskatoon, Saskatchewan, Canada from 1985 through 1990. Yearlings paired with yearlings and adults (2-plus years old) paired with adults more frequently than expected. Among adult pairs, however, there was no significant assortment by age. The productivity of pairs which included a yearling member was significantly lower than that of pairs with two adult birds. Similarly, pairs with two adults hatched their young on average nine days earlier than pairs with at least one yearling. There was no significant assortment of pairs based on body size with the exception of tail length. Along with differences in the timing of breeding activities, one other possible proximate mechanism promoting the distinction between adults and yearlings when choosing a mate was the difference in plumage between adult and yearling males. C1 SASKATCHEWAN MUSEUM NAT HIST,REGINA S4P 3V7,SASKATCHEWAN,CANADA. UNIV SASKATCHEWAN,DEPT VET ANAT,SASKATOON S7N 0W0,SASKATCHEWAN,CANADA. RP WARKENTIN, IG (reprint author), SMITHSONIAN INST,DEPT ZOOL RES,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 33 TC 22 Z9 22 U1 1 U2 7 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 MAY PY 1992 VL 94 IS 2 BP 418 EP 426 DI 10.2307/1369214 PG 9 WC Ornithology SC Zoology GA HV531 UT WOS:A1992HV53100010 ER PT J AU WINKER, K RAPPOLE, JH AF WINKER, K RAPPOLE, JH TI THE AUTUMN PASSAGE OF YELLOW-BELLIED FLYCATCHERS IN SOUTH TEXAS SO CONDOR LA English DT Note DE MIGRATION; TIMING; NONBREEDING TERRITORIALITY; POPULATION DYNAMICS; AGE STRUCTURE ID LEAST FLYCATCHERS; WOOD THRUSH; MIGRATIONS; POPULATION; VERACRUZ C1 CONSERVAT & RES CTR,NATL ZOOL PK,FRONT ROYAL,VA 22630. RP WINKER, K (reprint author), BELL MUSEUM NAT HIST,10 CHURCH ST SE,MINNEAPOLIS,MN 55455, USA. RI Winker, Kevin/M-2042-2014 OI Winker, Kevin/0000-0002-8985-8104 NR 17 TC 4 Z9 4 U1 1 U2 3 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 MAY PY 1992 VL 94 IS 2 BP 526 EP 529 DI 10.2307/1369225 PG 4 WC Ornithology SC Zoology GA HV531 UT WOS:A1992HV53100021 ER PT J AU DUBOIS, A HEYER, WR AF DUBOIS, A HEYER, WR TI LEPTODACTYLUS-LABIALIS, THE VALID NAME FOR THE AMERICAN WHITE-LIPPED FROG (AMPHIBIA, LEPTODACTYLIDAE) SO COPEIA LA English DT Note C1 SMITHSONIAN INST, DEPT VERTEBRATE ZOOL, WASHINGTON, DC 20560 USA. RP DUBOIS, A (reprint author), MUSEUM NATL HIST NAT, REPTILES & AMPHIBIENS LAB, 25 RUE CUVIER, F-75005 PARIS, FRANCE. NR 4 TC 2 Z9 4 U1 0 U2 2 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD MAY 1 PY 1992 IS 2 BP 584 EP 585 PG 2 WC Zoology SC Zoology GA HT728 UT WOS:A1992HT72800038 ER PT J AU EPSTEIN, M AF EPSTEIN, M TI DYAR PETS - SLUG CATERPILLARS IN MOTION SO ENTOMOLOGICAL NEWS LA English DT Editorial Material RP EPSTEIN, M (reprint author), SMITHSONIAN INST,DEPT ENTOMOL,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 SN 0013-872X J9 ENTOMOL NEWS JI Entomol. News PD MAY-JUN PY 1992 VL 103 IS 3 BP 89 EP 89 PG 1 WC Entomology SC Entomology GA HZ371 UT WOS:A1992HZ37100007 ER PT J AU GREENBERG, R AF GREENBERG, R TI DIFFERENCES IN NEOPHOBIA BETWEEN NAIVE SONG AND SWAMP SPARROWS SO ETHOLOGY LA English DT Article ID ECOLOGICAL PLASTICITY; FEEDING NEOPHOBIA; WARBLERS; RATS; EXPERIENCE; RESPONSES; FOOD AB I measured feeding neophobia in song (Melospiza melodia) and swamp (M. georgiana) sparrows. The experiment had a counter-balanced design with each species divided into two rearing groups and each exposed to a different set of six objects. I tested sparrows at two months of age by measuring their latency to feed at cups placed at familiar and novel objects. These tests were repeated at six months using an additional four novel objects. In comparison with song sparrows, juvenile swamp sparrows had a significantly and consistently lower latency to feed at novel objects. I found this difference in older birds as well. Feeding latencies at familiar objects were statistically indistinguishable between species. These results suggest that song sparrows are more neophobic than swamp sparrows. I obtained opposite results from similar experiments conducted in the field and using wild-caught birds in captivity. Greater neophobia in wild swamp sparrows may be a consequence of differential experience between the two species in nature. Differences found between hand-raised song and swamp sparrows is one of the first demonstrations of interspecific differences in neophobia under similar and controlled rearing conditions. A possible adaptive explanation is that, typically, juvenile swamp sparrows are reared in a simpler, more predictable and hence safer environment and may not require the protection of an aversion to novelty. RP GREENBERG, R (reprint author), NATL ZOOL PK,SMITHSONIAN MIGRATORY BIRD CTR,WASHINGTON,DC 20008, USA. NR 21 TC 16 Z9 16 U1 2 U2 17 PU BLACKWELL WISSENSCHAFTS-VERLAG GMBH PI BERLIN PA KURFURSTENDAMM 57, D-10707 BERLIN, GERMANY SN 0179-1613 J9 ETHOLOGY JI Ethology PD MAY PY 1992 VL 91 IS 1 BP 17 EP 24 PG 8 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA HY369 UT WOS:A1992HY36900002 ER PT J AU WEATHERFORD, E AF WEATHERFORD, E TI 'STARTING FIRE WITH GUNPOWDER' + NATIVE-AMERICAN INDIAN FILMS AND DOCUMENTARIES SO FILM COMMENT LA English DT Article RP WEATHERFORD, E (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER INDIAN,WASHINGTON,DC 20560, USA. NR 6 TC 1 Z9 1 U1 0 U2 0 PU FILM SOC LINCOLN CENTER PI NEW YORK PA 70 LINCOLN CENTER PLAZA, NEW YORK, NY 10023-6595 SN 0015-119X J9 FILM COMMENT JI Film Comment PD MAY-JUN PY 1992 VL 28 IS 3 BP 64 EP 67 PG 4 WC Film, Radio, Television SC Film, Radio & Television GA HT458 UT WOS:A1992HT45800016 ER PT J AU ROZANOV, VV TIMOFEEV, YM POLYAKOV, AV BURROWS, J CHANCE, K AF ROZANOV, VV TIMOFEEV, YM POLYAKOV, AV BURROWS, J CHANCE, K TI ON THE POSSIBILITIES OF PRECISION-MEASUREMENTS OF O3 AND NO2 FROM SPACE BY SOLAR-RADIATION ABSORPTION-SPECTRA SO IZVESTIYA AKADEMII NAUK FIZIKA ATMOSFERY I OKEANA LA Russian DT Article AB Possibilities are considered of application of a new calss of multispectrum apparatus (SCIAMACHY, the Scanning Imaging Absorption Spectrometer) for high precision measurements of O3 and NO2 vertical profiles in UV and visible ranges. It is shown that application of imaging spectrometer gives possibility to retrieve O3 vertical profile in height range 20-65 km with potential accuracy of 0.1-0.3%, and NO2 vertical profile in height range 22-38 km with accuracy of about 5%. C1 MAX PLANCK INST CHEM,W-6500 MAINZ,GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP ROZANOV, VV (reprint author), AA ZHDANOV STATE UNIV,LENINGRAD B-164,USSR. RI Timofeev, Yuriy/K-1618-2013; Polyakov, Alexander/I-7509-2013 OI Timofeev, Yuriy/0000-0003-2771-9931; Polyakov, Alexander/0000-0002-7406-8986 NR 8 TC 2 Z9 2 U1 0 U2 2 PU MEZHDUNARODNAYA KNIGA PI MOSCOW PA 39 DIMITROVA UL., 113095 MOSCOW, RUSSIA SN 0002-3515 J9 IZV AN FIZ ATMOS OK+ JI Izv. Akad. Nauk. Fiz. Atmos. Okean. Biol. PD MAY PY 1992 VL 28 IS 5 BP 500 EP 505 PG 6 WC Meteorology & Atmospheric Sciences; Oceanography SC Meteorology & Atmospheric Sciences; Oceanography GA HZ991 UT WOS:A1992HZ99100006 ER PT J AU ALBERTS, AC SHARP, TR WERNER, DI WELDON, PJ AF ALBERTS, AC SHARP, TR WERNER, DI WELDON, PJ TI SEASONAL-VARIATION OF LIPIDS IN FEMORAL GLAND SECRETIONS OF MALE GREEN IGUANAS (IGUANA-IGUANA) SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE FEMORAL GLANDS; LIPIDS; FATTY ACIDS; STEROLS; PHEROMONES; IGUANA-IGUANA ID LIZARD AB Femoral gland secretions were collected from 21 captive adult male green iguanas (Iguana iguana) in Orotina, Costa Rica, and San Diego, California, during the breeding (November) and nonbreeding (March) seasons. Lipids were extracted with methylene chloride, weighed, separated by thin-layer chromatography, and analyzed by gas chromatography-mass spectrometry. Free and esterified C-14-C26 fatty acids, 5-beta-cholestan-3-alpha-ol (epicoprostanol), cholest-5-en-3-beta-ol (cholesterol), cholest-5-en-24-methyl-3-beta-ol (campesterol), cholesta-5,22-dien-24b-ethyl-3-beta-ol (stigmasterol), cholesta-8,24(5-alpha)-dien-4,4,14-alpha-trimethyl-3-beta-ol (lanosterol), cholest-5-en-24-ethyl-3-beta-ol (beta-sitosterol), and two uncharacterized sterols were indicated. More lipids were recovered from femoral gland secretions obtained during the breeding than the nonbreeding months, indicating that secretion deposits may be more detectable during the mating season. C1 TEXAS A&M UNIV SYST,DEPT CHEM,COLLEGE STN,TX 77843. FDN PRO IGUANA VERDE,SAN JOSE,COSTA RICA. TEXAS A&M UNIV SYST,DEPT BIOL,COLLEGE STN,TX 77843. SMITHSONIAN INST,NATL ZOOL PK,DEPT HERPETOL,WASHINGTON,DC 20008. RP ALBERTS, AC (reprint author), ZOOL SOC SAN DIEGO,CTR REPROD ENDANGERED SPECIES,POB 551,SAN DIEGO,CA 92112, USA. NR 30 TC 44 Z9 45 U1 1 U2 15 PU PLENUM PUBL CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 SN 0098-0331 J9 J CHEM ECOL JI J. Chem. Ecol. PD MAY PY 1992 VL 18 IS 5 BP 703 EP 712 DI 10.1007/BF00994608 PG 10 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA HR480 UT WOS:A1992HR48000003 PM 24253964 ER PT J AU SUN, Y DALGARNO, A AF SUN, Y DALGARNO, A TI RADIATIVE ASSOCIATION OF N-ATOMS AND O-ATOMS AT LOW-TEMPERATURES SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Note ID SINGLE ROTATIONAL LEVELS; FLUORESCENCE LIFETIMES AB The rate coefficients for the radiative association of N(4S) and O(3P) atoms are calculated for temperatures between 1 K and 2000 K. Below 200 K the effects of the interaction between the B2-PI and C2-PI states have to be included. Experimental spectroscopic data are analyzed to determine the mixing of the states and to infer the radiative and predissociation lifetimes for the quasi-bound rotational levels through which the radiative association occurs at low temperatures. At 20 K the rate coefficient is 6.5 x 10(-17) cm3 s-1 , and at 200 K it is 2.3 x 10(-17) cm3 s-1. RP SUN, Y (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 7 TC 5 Z9 5 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES JI J. Geophys. Res-Space Phys. PD MAY 1 PY 1992 VL 97 IS A5 BP 6537 EP 6539 DI 10.1029/92JA00498 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HT743 UT WOS:A1992HT74300028 ER PT J AU MCCORMICKGOODHART, MH AF MCCORMICKGOODHART, MH TI AN ANALYSIS OF IMAGE DETERIORATION IN WET-PLATE NEGATIVES FROM THE BRADY,MATHEW STUDIOS SO JOURNAL OF IMAGING SCIENCE AND TECHNOLOGY LA English DT Article AB The deterioration of collodion wet-plate negatives made in the Mathew Brady Studios during the 1860s was investigated. The most seriously degraded plates were found to have saponified varnish coatings. Carboxylic acid metal salts in the varnish layer were determined by Fourier transform infrared spectroscopy. Subsequent identification of the metal ion as sodium by energy dispersive x-ray spectroscopy led to an investigation of the glass composition. Glass composition was measured by electron microprobe analysis, using wavelength-dispersive x-ray technique; the saponified varnish plates had glass substrates of the same composition, characterized by high sodium content. RP MCCORMICKGOODHART, MH (reprint author), SMITHSONIAN INST,CONSERVAT ANAL LAB,WASHINGTON,DC 20560, USA. NR 24 TC 0 Z9 0 U1 0 U2 2 PU I S & T - SOC IMAGING SCIENCE TECHNOLOGY PI SPRINGFIELD PA 7003 KILWORTH LANE, SPRINGFIELD, VA 22151 SN 8750-9237 J9 J IMAGING SCI TECHN JI J. Imaging Sci. Technol. PD MAY-JUN PY 1992 VL 36 IS 3 BP 297 EP 305 PG 9 WC Imaging Science & Photographic Technology SC Imaging Science & Photographic Technology GA HZ237 UT WOS:A1992HZ23700017 ER PT J AU HOLZENBEIN, S MARCHINTON, RL AF HOLZENBEIN, S MARCHINTON, RL TI SPATIAL INTEGRATION OF MATURING-MALE WHITE-TAILED DEER INTO THE ADULT-POPULATION SO JOURNAL OF MAMMALOGY LA English DT Article DE ODOCOILEUS; MALE DISPERSAL; RADIOTELEMETRY ID HOME-RANGE; PERMUTATION PROCEDURES; DISPERSAL; MOVEMENTS; MORTALITY; BEHAVIOR AB We monitored range-use patterns of 15 male white-tailed deer (Odocoileus virginianus) orphaned as fawns (<12 months) and 19 males maturing with their mothers. Survivors were radiotracked until they were greater-than-or-equal-to 30-months old. Some males did not change their natal range, whereas others extended it, dispersed from it, or made occasional excursions. Dispersals could be classified as gradual short-distance or abrupt long-distance movements. Orphaned males maintained greater affinity for their natal ranges than did non-orphans, but had seasonal ranges that were larger on average until 18 months of age. Common use of range between non-orphans and their mothers ceased as males matured and all but one dispersed. The multiple-response permutation procedure successfully was used for the analysis of range fidelity over time or between individuals as an alternative to range-overlap estimates. The results support the hypothesis that dispersal evolved as a means to reduce the chance of inbreeding; the inclusive fitness of mothers may benefit most from dispersal of their male offspring, leading to a situation in which mothers force their male offspring to leave. C1 UNIV GEORGIA,SCH FOREST RESOURCES,ATHENS,GA 30602. SMITHSONIAN INST,CTR CONSERVAT & RES,NATL ZOOL PK,FRONT ROYAL,VA 22630. NR 61 TC 41 Z9 42 U1 0 U2 5 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 MAY PY 1992 VL 73 IS 2 BP 326 EP 334 DI 10.2307/1382065 PG 9 WC Zoology SC Zoology GA HW965 UT WOS:A1992HW96500011 ER PT J AU COOKSY, AL WATSON, JKG GOTTLIEB, CA THADDEUS, P AF COOKSY, AL WATSON, JKG GOTTLIEB, CA THADDEUS, P TI THE MILLIMETER-WAVE SPECTRA OF THE HCCCO AND DCCCO RADICALS SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article ID MICROWAVE-SPECTRUM; SEMIRIGID BENDER; TOP MOLECULES; GROUND-STATE; PROPADIENONE; GEOMETRY; HCNO; HO2; HCO C1 HARVARD UNIV,DEPT CHEM,CAMBRIDGE,MA 02138. NATL RES COUNCIL CANADA,HERZBERG INST ASTROPHYS,OTTAWA K1A 0R6,ONTARIO,CANADA. HARVARD UNIV,DIV APPL SCI,CAMBRIDGE,MA 02138. RP COOKSY, AL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 35 TC 19 Z9 20 U1 2 U2 3 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD MAY-JUN PY 1992 VL 153 IS 1-2 BP 610 EP 626 DI 10.1016/0022-2852(92)90497-C PG 17 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA HT478 UT WOS:A1992HT47800046 ER PT J AU COLE, KS SHAPIRO, DY AF COLE, KS SHAPIRO, DY TI GONADAL STRUCTURE AND POPULATION CHARACTERISTICS OF THE PROTOGYNOUS GOBY CORYPHOPTERUS-GLAUCOFRAENUM SO MARINE BIOLOGY LA English DT Article ID CORAL-REEF FISH; SEX-CHANGE; SOCIAL-CONTROL; MARINE GOBY; HERMAPHRODITISM; MORPHOLOGY; TELEOSTEI; NICHOLSI; LABRIDAE; PISCES AB Protogynous hermaphroditism has been reported in two gobiid species within the genus Coryphopterus, including C. nicholsi from the temperate northeastern Pacific and C. personatus from the Carribbean. In a third species from the Caribbean, C. glaucofraenum, experimental groups were established and gonad structure of experimental individuals (collected off the southwest coast of Puerto Rico between February 1985 and June 1987) was subsequently examined histologically to determine the sexual pattern. Protogyny was confirmed in C. glaucofraenum. Sex change was either initiated or completed, typically by the largest female. in all-female groups held for 10 to 40 d. Ovarian, transitional, and testis structure were similar to that of C. nicholsi and C. personatus. No preformed testicular tissue was evident in the ovary proper and ovarian features were not retained in the sex-changed testis beyond the newly transformed stage. Secretory accessory gonadal Structures associated with the testis and which develop at the time of sex change arose from precursive tissue masses associated with the ventral portion of the ovarian wall in the region of the common genital sinus. The rapid development and onset of function in these structures, generally preceding that of the associated developing testis, suggest that they may play an important role in sex change events and in advertising new male status. Based on observed similarities of ovarian. transitional and secondary testis structure in three protogynous Coryphopterus species, including one species isolated since the last closing of the American landbridge, it is probable that protogyny is an ancestral condition in this genus. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. UNIV PUERTO RICO,DEPT MARINE SCI,MAYAGUEZ,PR 00709. NR 38 TC 25 Z9 25 U1 1 U2 3 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD MAY PY 1992 VL 113 IS 1 BP 1 EP 9 DI 10.1007/BF00367632 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA HW275 UT WOS:A1992HW27500001 ER PT J AU AVISE, JC BOWEN, BW LAMB, T MEYLAN, AB BERMINGHAM, E AF AVISE, JC BOWEN, BW LAMB, T MEYLAN, AB BERMINGHAM, E TI MITOCHONDRIAL-DNA EVOLUTION AT A TURTLES PACE - EVIDENCE FOR LOW GENETIC-VARIABILITY AND REDUCED MICROEVOLUTIONARY RATE IN THE TESTUDINES SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE EVOLUTIONARY RATES; TURTLES; MITOCHONDRIAL DNA ID NUCLEOTIDE SUBSTITUTION; HYBRIDIZATION EVIDENCE; HAWAIIAN DROSOPHILA; MOLECULAR EVOLUTION; SEQUENCE EVOLUTION; NUCLEAR-DNA; POPULATIONS; CLOCK; TEMPO; MODE AB Evidence is compiled suggesting a slowdown in mean microevolutionary rate for turtle mitochondrial DNA (mtDNA). Within each of six species or species complexes of Testudines, representing six genera and three taxonomic families, sequence divergence estimates derived from restriction assays are consistently lower than expectations based on either (a) the dates of particular geographic barriers with which significant mtDNA genetic clades appear associated or (b) the magnitudes of sequence divergence between mtDNA clades in nonturtle species that otherwise exhibit striking phylogeographic concordance with the genetic partitions in turtles. Magnitudes of the inferred rate slowdowns average eightfold relative to the "conventional" mtDNA clock calibration of 2%/Myr sequence divergence between higher animal lineages. Reasons for the postulated deceleration remain unknown, but two intriguing correlates are (a) the exceptionally long generation length of most turtles and (b) turtles' low metabolic rate. Both factors have been suspected of influencing evolutionary rates in the DNA sequences of some other vertebrate groups. Uncertainties about the dates of cladogenetic events in these Testudines leave room for alternatives to the slowdown interpretation, but consistency in the direction of the inferred pattern, across several turtle species and evolutionary settings, suggests the need for caution in acceptance of a universal mtDNA-clock calibration for higher animals. C1 E CAROLINA UNIV,DEPT BIOL,GREENVILLE,NC 27834. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP AVISE, JC (reprint author), UNIV GEORGIA,DEPT GENET,ATHENS,GA 30602, USA. NR 79 TC 232 Z9 238 U1 3 U2 26 PU SOC MOLECULAR BIOLOGY EVOLUTION PI LAWRENCE PA PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0737-4038 J9 MOL BIOL EVOL JI Mol. Biol. Evol. PD MAY PY 1992 VL 9 IS 3 BP 457 EP 473 PG 17 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA HP202 UT WOS:A1992HP20200007 PM 1584014 ER PT J AU BAND, YB AF BAND, YB TI ADIABATIC APPROXIMATION FOR THE DENSITY-MATRIX SO PHYSICAL REVIEW A LA English DT Article ID STIMULATED RAMAN-SCATTERING; POPULATION TRANSFER; MULTILEVEL SYSTEMS; VIBRATIONAL LEVELS; RADIATION REACTION; FREQUENCY-SHIFTS; INVERSION; PULSES; VAPOR AB An adiabatic approximation for the Liouville density-matrix equation which includes decay terms is developed. The adiabatic approximation employs the eigenvectors of the non-normal Liouville operator. The approximation is valid when there exists a complete set of eigenvectors of the non-normal Liouville operator (i.e., the eigenvectors span the density-matrix space), the time rate of change of the Liouville operator is small, and an auxiliary matrix is nonsingular. Numerical examples are presented involving efficient population transfer in a molecule by stimulated Raman scattering, with the intermediate level of the molecule decaying on a time scale that is fast compared with the pulse durations of the pump and Stokes fields. The adiabatic density-matrix approximation can be simply used to determine the density matrix for atomic or molecular systems interacting with cw electromagnetic fields when spontaneous emission or other decay mechanisms prevail. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOLEC PHYS, CAMBRIDGE, MA 02138 USA. RP BEN GURION UNIV NEGEV, DEPT CHEM, IL-84105 BEER SHEVA, ISRAEL. NR 29 TC 15 Z9 15 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD MAY 1 PY 1992 VL 45 IS 9 BP 6643 EP 6651 DI 10.1103/PhysRevA.45.6643 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA HT733 UT WOS:A1992HT73300058 ER PT J AU GOLDWIRTH, DS PIRAN, T AF GOLDWIRTH, DS PIRAN, T TI INITIAL CONDITIONS FOR INFLATION SO PHYSICS REPORTS-REVIEW SECTION OF PHYSICS LETTERS LA English DT Review ID HOMOGENEOUS COSMOLOGICAL MODELS; SUPERHEAVY MAGNETIC MONOPOLES; SPONTANEOUS SYMMETRY-BREAKING; 1ST-ORDER PHASE-TRANSITION; COLEMAN-WEINBERG THEORY; GRAND UNIFIED THEORIES; MASSIVE SCALAR FIELD; CHAOTIC INFLATION; UNIVERSE SCENARIO; ANISOTROPIC COSMOLOGIES AB Inflation has attracted cosmologists because of its potential to free the standard big bang model from its worst flaw. the need for special initial conditions and, in particular, the requirement of initial acausal homogeneity. Naturally one must check whether inflation itself depends critically on initial conditions. Several "no hair" theorems and perturbation calculations have indicated that inflation is stable, and that it will take place when the initial conditions are perturbed. This has led to the belief that inflation will start in any generic universe. On the other hand, since most studies of inflation were carried out in a FRW background. inflation has been criticized and it was suggested that. like the big bang model, it depends heavily on an unnatural homogeneous initial state. Great progress has been achieved in the last few years in understanding which conditions are indeed necessary for inflation to begin. In this paper we review the various conditions required for the onset of both "chaotic" and "new" inflation. We review the various studies of the effects of the scalar field kinetic term, the cosmological "no hair" conjecture. the possible roles of curvature and anisotropy, and the influence of inhomogeneities. We describe the essential conditions for the onset of inflation for all these cases. We show that "chaotic" inflation is not very sensitive to the initial conditions. It requires that the average value of the scalar field be larger than a few m(pl) over a region of several initial horizon radii; short-wavelength gradients on top of a high average field will generally not prevent inflation. "New" inflation is much more dependent on the initial conditions and, unless the potential is extremely flat. it requires that after the "new" inflation phase transition the scalar field must be localized at rest on the top of its potential at the origin. While our main objective is to classify the different initial conditions required for inflation, we also discuss some of the physical significance of these conditions. For example, we address the issue of whether the conditions that we find necessary for "chaotic" inflation prevail in the post quantum era early universe. These prerequisites could have far-reaching implications for inflationary models and for quantum cosmology and particle physics. C1 HEBREW UNIV JERUSALEM,RACAH INST PHYS,IL-91904 JERUSALEM,ISRAEL. RP GOLDWIRTH, DS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 191 TC 131 Z9 131 U1 0 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-1573 J9 PHYS REP JI Phys. Rep.-Rev. Sec. Phys. Lett. PD MAY PY 1992 VL 214 IS 4 BP 223 EP 292 DI 10.1016/0370-1573(92)90073-9 PG 70 WC Physics, Multidisciplinary SC Physics GA JE224 UT WOS:A1992JE22400001 ER PT J AU ZDERO, C BOHLMANN, F KING, RM AF ZDERO, C BOHLMANN, F KING, RM TI ENT-LABDANES, MANOYLOXIDE AND HELIPTEROL DERIVATIVES FROM CHRYSOCEPHALUM-AMBIGUUM SO PHYTOCHEMISTRY LA English DT Article DE CHRYSOCEPHALUM-AMBIGUUM; COMPOSITAE; DITERPENES; ENT-LABDANES; ENT-MANOYLOXIDE DERIVATIVES; MONOCYCLIC DITERPENES ID SESQUITERPENE LACTONES; CONSTITUENTS AB The aerial parts of Chrysocephalum ambiguum afforded, in addition to two known diterpenes, 28 new ones, 22 ent-labdanes, four ent-manoyloxide derivatives and two monocyclic diterpenes derived from helipterol. The structures were elucidated by high field H-1 NMR spectroscopy. C1 SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560. RP ZDERO, C (reprint author), TECH UNIV BERLIN,INST ORGAN CHEM,W-1000 BERLIN 12,GERMANY. NR 15 TC 15 Z9 15 U1 0 U2 3 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 MAY PY 1992 VL 31 IS 5 BP 1631 EP 1638 DI 10.1016/0031-9422(92)83119-J PG 8 WC Biochemistry & Molecular Biology; Plant Sciences SC Biochemistry & Molecular Biology; Plant Sciences GA HT906 UT WOS:A1992HT90600035 ER PT J AU ZDERO, C BOHLMANN, F KING, RM AF ZDERO, C BOHLMANN, F KING, RM TI CLERODANE AND LABDANE DERIVATIVES FROM OLEARIA-TERETIFOLIA SO PHYTOCHEMISTRY LA English DT Article DE OLEARIA-TERETIFOLIA; COMPOSITAE; ASTEREAE; DITERPENES; ENT-CLERODANES; ENT-LABDANES; ACETYLENIC COMPOUNDS; PHENYLPROPANE DERIVATIVE ID DITERPENOIDS; TERPENE; ACID AB The aerial parts of Olearia teretifolia afforded, in addition to two known diterpenes, 39 new ones, 20 ent-clerodanes and 19 ent-labdanes. Furthermore, a new enediynediene and coniferyl acetate were present. The structures were elucidated by high field NMR techniques. Chemotaxonomic aspects are discussed briefly. C1 SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560. RP ZDERO, C (reprint author), TECH UNIV BERLIN,INST ORGAN CHEM,W-1000 BERLIN 12,GERMANY. NR 15 TC 9 Z9 9 U1 0 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 MAY PY 1992 VL 31 IS 5 BP 1703 EP 1711 DI 10.1016/0031-9422(92)83132-I PG 9 WC Biochemistry & Molecular Biology; Plant Sciences SC Biochemistry & Molecular Biology; Plant Sciences GA HT906 UT WOS:A1992HT90600048 ER PT J AU SOKER, N AF SOKER, N TI PLANETARY-NEBULAE SO SCIENTIFIC AMERICAN LA English DT Article RP SOKER, N (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 5 TC 1 Z9 1 U1 1 U2 3 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 MAY PY 1992 VL 266 IS 5 BP 78 EP 85 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA HQ759 UT WOS:A1992HQ75900013 ER PT J AU BREMER, B ERIKSSON, O AF BREMER, B ERIKSSON, O TI ECOLOGICAL SPECIES CONCEPTS - A REPLY SO TAXON LA English DT Editorial Material ID COEXISTENCE; COMMUNITIES; PLANTS; NICHE C1 UNIV UPPSALA,DEPT SYSTEMAT BOT,S-75121 UPPSALA,SWEDEN. UNIV STOCKHOLM,DEPT BOT,S-10691 STOCKHOLM,SWEDEN. RP BREMER, B (reprint author), SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560, USA. NR 19 TC 0 Z9 0 U1 2 U2 5 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 MAY PY 1992 VL 41 IS 2 BP 307 EP 309 DI 10.2307/1222334 PG 3 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA HV749 UT WOS:A1992HV74900008 ER PT J AU FOSBERG, FR AF FOSBERG, FR TI AN ESSAY ON LECTOTYPIFICATION SO TAXON LA English DT Article AB Lectotypification is a serious matter and aspects of the current Code do not make things easier, suggesting the need for amendments. RP FOSBERG, FR (reprint author), SMITHSONIAN INST,DEPT BOT,NHB 166,WASHINGTON,DC 20560, USA. NR 0 TC 2 Z9 2 U1 0 U2 1 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 MAY PY 1992 VL 41 IS 2 BP 321 EP 323 DI 10.2307/1222339 PG 3 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA HV749 UT WOS:A1992HV74900013 ER PT J AU KOLBE, E LANGANKE, K KREWALD, S THIELEMANN, FK AF KOLBE, E LANGANKE, K KREWALD, S THIELEMANN, FK TI INELASTIC NEUTRINO SCATTERING ON C-12 AND O-16 ABOVE THE PARTICLE-EMISSION THRESHOLD SO NUCLEAR PHYSICS A LA English DT Article ID II SUPERNOVAE; NUCLEI; DECAY; MODEL AB Recently a new formalism has been developed to described nuclear electromagnetic response within the continuum RPA theory. This model is extended in order to calculate cross sections for weak interactions in nuclei, in particular for inelastic neutrino scattering. The results of a numerical analysis are presented for C-12 and O-16. We consider neutrino spectra like those generated in muon decay (relevant for terrestrial experiments) or in a supernova explosion. For the latter case we calculate neutral current cross sections for various neutrino-induced particle reactions on C-12 and O-16, relevant for the nu-nucleosynthesis. C1 UNIV MUNSTER,INST THEORET PHYS 1,WILHEM KLEMM STR 9,W-4400 MUNSTER,GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. FORSCHUNGSZENTRUM JULICH,INST KERNPHYS,W-5170 JULICH,GERMANY. OI Krewald, Siegfried/0000-0002-8596-8429 NR 43 TC 83 Z9 83 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0375-9474 J9 NUCL PHYS A JI Nucl. Phys. A PD APR 27 PY 1992 VL 540 IS 3-4 BP 599 EP 620 DI 10.1016/0375-9474(92)90175-J PG 22 WC Physics, Nuclear SC Physics GA HZ335 UT WOS:A1992HZ33500009 ER PT J AU SIEBERT, L AF SIEBERT, L TI VOLCANO HAZARDS - THREATS FROM DEBRIS AVALANCHES SO NATURE LA English DT Editorial Material ID ST-AUGUSTINE VOLCANO; ALASKA RP SIEBERT, L (reprint author), SMITHSONIAN INST,GLOBAL VOLCANISM PROGRAM,WASHINGTON,DC 20560, USA. NR 9 TC 41 Z9 42 U1 0 U2 6 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD APR 23 PY 1992 VL 356 IS 6371 BP 658 EP 659 DI 10.1038/356658a0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA HQ146 UT WOS:A1992HQ14600028 ER PT J AU DAVID, LP BLUMENTHAL, GR AF DAVID, LP BLUMENTHAL, GR TI THE EFFICIENCY OF GALAXY FORMATION IN CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE DARK MATTER; GALAXIES CLUSTERING; GALAXIES FORMATION; INTERGALACTIC MEDIUM ID COLD DARK MATTER; LARGE-SCALE STRUCTURE; POOR CLUSTERS; CD GALAXIES; EINSTEIN; MECHANISMS AB We examine whether the observed decrease in the efficiency of galaxy formation between poor and rich X-ray clusters is consistent with galaxy formation scenarios involving hierarchical clustering, such as cold dark matter (CDM). To calculate the efficiency of galaxy formation we adopt the common biased galaxy formation scenario in which galaxies form only at peaks in the primordial distribution of density fluctuations that exceed some critical density threshold. The efficiency of galaxy formation in a cluster can then be defined as the fractional mass within a cluster contained within galaxy peaks exceeding this threshold. The distribution of cluster and galaxy scale overdensities is described as a bivariate Gaussian random field. For relatively flat primordial spectra, such as the CDM power spectrum between galaxy and cluster mass scales, there is a significant amount of statistical correlation between the two length scales. The probability that a random galaxy scale peak exceeds the biasing threshold depends strongly on the mass and amplitude of any background protocluster fluctuation. A greater statistical correlation is present between galaxy and poor cluster masses than between galaxy and rich cluster masses due to the closer proximity in filter length. This is the fundamental reason why galaxy formation is more efficient in poor clusters than in rich clusters. We find that the observed trend in the efficiency of galaxy formation and the observed values can be reproduced within the context of CDM biased galaxy formation scenarios or other scenarios involving flat spectra if X-ray luminous clusters are typically 2-3 sigma objects. This is consistent with the observed number density of X-ray clusters and their virial properties only if the biasing parameter b is close to unity. C1 UNIV CALIF SANTA CRUZ,LICK OBSERV,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064. RP DAVID, LP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 29 TC 18 Z9 18 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 APR 20 PY 1992 VL 389 IS 2 BP 510 EP 516 DI 10.1086/171227 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HP119 UT WOS:A1992HP11900006 ER PT J AU BENZ, W HILLS, JG AF BENZ, W HILLS, JG TI 3-DIMENSIONAL HYDRODYNAMICAL SIMULATIONS OF COLLIDING STARS .3. COLLISIONS AND TIDAL CAPTURES OF UNEQUAL-MASS MAIN-SEQUENCE STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE CELESTIAL MECHANICS, STELLAR DYNAMICS; GLOBULAR CLUSTERS GENERAL; HYDRODYNAMICS; METHODS NUMERICAL ID STELLAR COLLISIONS; GLOBULAR CLUSTERS; BINARIES; SYSTEMS AB We used a three-dimensional smooth-particle hydrodynamics (SPH) code with 7000 particles to simulate 30 collisions between lower main-sequence (MS) stars whose masses differ by a factor of 5. We also simulated encounters with point-mass intruders to understand better how the finite radius of the intruder affects the dynamics. The two MS stars become gravitationally bound in a physical collision if their relative velocity, V, at infinity is less than a critical (dissipation) velocity, V(d). We find that V(d) decreases from 1000 km s-1 in a head-on collision to 150 km s-1 in a grazing one. If the less massive star is replaced by a point mass (e.g., a white dwarf), V(d) remains the same for grazing collisions and tidal encounters, but it drops to approximately 600 km s-1 in head-on collisions. If V > V(d), the lower mass ms star, which is the denser of the two, passes through the more massive MS star and escapes without becoming gravitationally bound to it. In collisions between two main-sequence stars, V(d) increases with V due to increased shock dissipation. In collisions between a point mass and a main-sequence star, V(d) decreases as V increases. The only dissipation in these cases is by gravitationally induced oscillations that decrease in importance as V increases. If the two MS stars coalesce in a physical collision, the denser (lower mass) MS star settles to the center of the other one. The violent mixing of the more massive star during the encounter and the settling of the low-mass star to its center should reset the nuclear clock of the coalesced star, so it contracts to the (helium-rich) MS. The fraction of the stellar mass lost in these collisions is much less than that lost in collisions between stars of equal mass and density. In particular, grazing collisions do not produce the large mass loss and accretion disks that characterize collisions between equal-mass stars. We find that tidal captures of binary stars in globular clusters can only occur in encounters in which the closest approach of the two stars to their center of mass is less than 2.0 times the sum of their radii. Coalescence of two MS stars in a globular cluster is more probable than their forming a binary by tidal capture. Tidal capture is not possible if the impact velocity at infinity exceeds 150 km s-1. Even at zero impact velocity, the coalesced star acquires a kick velocity of up to 4.5 km s-1 by asymmetric jetting during the collision. This velocity is not enough to eject the coalesced star from a globular cluster, but it largely compensates for the dynamical cooling resulting from the coalescence of the two stars. The coalescence of stars in globular clusters does not speed up the dynamical collapse of the core of the cluster. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CALIF LOS ALAMOS SCI LAB,DIV THEORET,LOS ALAMOS,NM 87545. NR 17 TC 67 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 APR 20 PY 1992 VL 389 IS 2 BP 546 EP 557 DI 10.1086/171230 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HP119 UT WOS:A1992HP11900009 ER PT J AU BALL, R ARENS, JF JERNIGAN, JG KETO, E MEIXNER, MM AF BALL, R ARENS, JF JERNIGAN, JG KETO, E MEIXNER, MM TI THERMAL DUST IMAGING - THE ONSET OF ASYMMETRY IN THE ULTRACOMPACT H-II REGION G5.89-0.39 SO ASTROPHYSICAL JOURNAL LA English DT Article DE DUST, EXTINCTION; H-II REGIONS; INFRARED INTERSTELLAR CONTINUUM; ISM INDIVIDUAL (G5.89-0.39); STARS FORMATION ID ACTIVE STAR FORMATION; INFRARED-EMISSION BANDS; H2O MASERS; MOLECULAR CLOUDS; IRAS SOURCES; OBJECTS; 10-MU-M; OUTFLOW; 20-MU-M; BUBBLES AB We have obtained images of the compact radio and infrared nebula G5.89-0.39 with the Berkeley/IGPP mid-infrared array camera. The images have a resolution of 1."1 and cover five wavelength bands between 8 and 13-mu-m. On the basis of the structure and spectral energy distribution, we concur with previously published assertions that G5.89-0.39 is an ultracompact H II region. The infrared emission is extended over 6" x 4".5, very similar to the object's size in published high-resolution radio continuum maps. The mid-infrared nebula is arcuate in shape, taking the form of a partial shell open to the south, unlike the radio images where the shell is complete. At our shortest wavelength the structure is sharp-edged as in the radio maps, but diffuse emission is seen at the longest wavelength. A deep silicate absorption band is the principal feature of the spectrum of the object at these wavelengths. The ratio of the 12.5 to the 8.5-mu-m surface brightness indicates a gradual cooling of the dust toward the western side of the infrared nebula, and a more abrupt temperature drop at the inner boundary of a zone of cool, diffuse emission in the southeast. The radio and infrared structure of G5.89-0.39 can be understood in the context of a previously published model in which the O star is surrounded by a dust-free cavity that is in turn embedded in a dusty molecular cloud. The ionization front is trapped in the swept-up material that lines the boundary of this cavity, and the mid-infrared emission arises from warm dust in the same location. The new element which our infrared data add to this picture is a clear indication of how the source deviates from spherical symmetry. The intensities and temperatures of the dust are well fitted by a simple model that places the star off-center in the radio shell, implying that the expansion of the ionization front has been anisotropic. Correlations between specific features in the radio and mid-infrared images suggest that the expansion has been shaped by density variations in the molecular medium surrounding the star and that, as a consequence, G5.89-0.39 may be undergoing a rapid transition from a state of approximate spherical symmetry to one of fairly irregular morphology. C1 UNIV CALIF LAWRENCE LIVERMORE NATL LAB,INST GEOPHYS & PLANETARY PHYS,LIVERMORE,CA 94550. UNIV CALIF BERKELEY,SPACE SCI LAB,BERKELEY,CA 94720. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. HARVARD SMITHSONIAN CTR ASTROPHYS,SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. NR 32 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 APR 20 PY 1992 VL 389 IS 2 BP 616 EP 627 DI 10.1086/171234 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HP119 UT WOS:A1992HP11900013 ER PT J AU SOKER, N AF SOKER, N TI JET FORMATION IN THE TRANSITION FROM THE ASYMPTOTIC GIANT BRANCH TO PLANETARY-NEBULAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE BINARIES GENERAL; ISM JETS AND OUTFLOWS; PLANETARY NEBULAE GENERAL ID DOUBLE-CORE EVOLUTION; COMMON ENVELOPE EVOLUTION; RED GIANT; CATACLYSMIC BINARIES; STELLAR EVOLUTION; MASS-LOSS; STARS; SEQUENCES; COMPANION AB We demonstrate the feasibility of a scenario by which a star in a common envelope blows a collimated wind as it evolves from the asymptotic giant branch (AGB) to the central star of a planetary nebula. The collimated flow turns into jets along the symmetry axis. These jets then form in their leading front the ansae- two opposite bright knots along the major axis which are observed in many elliptical planetary nebulae. An essential ingredient in the proposed scenario is that the evolving AGB star is in a common envelope with a low-mass companion. The low-mass companion, which orbits close to the giant core, spins up the envelope efficiently at late stages of the evolution. We calculate the surface shape of the rotating envelope by assuming a simple angular momentum distribution. The deformed surface of the rotating envelope is assumed to blow a substantial fraction of the wind along the rotation axis. The proposed scenario leads to two types of jets and ansae. One type is slow, approximately 50 km s-1, and relatively heavy-a total mass of less-than-or-similar-to 10(-3) M.. The second type, which can continue to be active during the planetary nebula stage, is fast, 100-300 km s-1, and light approximately 10(-4) M.. RP SOKER, N (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 40 TC 65 Z9 65 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 APR 20 PY 1992 VL 389 IS 2 BP 628 EP 634 DI 10.1086/171235 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HP119 UT WOS:A1992HP11900014 ER PT J AU PIRAN, T AF PIRAN, T TI THE IMPLICATIONS OF THE COMPTON (GRO) OBSERVATIONS FOR COSMOLOGICAL GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, OBSERVATIONS; GAMMA RAYS, BURSTS ID CYCLOTRON AB The BATSE observations (Fishman et al.; Meegan et al.) have shown that the angular distribution of gamma-ray sources in the sky is isotropic and that [V/V(max)] = 0.35. We show that these observations are consistent with a cosmological distribution of sources. In fact the observed distribution of V/V(max) values is the one toward which a cosmological distribution converges. If there is even a weak cosmological time dependence of the event rate, then the bursts originate at modest z values (z(max) almost-equal-to 1). For flat cosmological models, this requires 10(50) ergs or less. The energy and the observed event rate are in full agreement with the binary neutron star merger model. C1 HEBREW UNIV JERUSALEM,RACAH INST PHYS,JERUSALEM,ISRAEL. RP PIRAN, T (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02133, USA. NR 26 TC 169 Z9 171 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 APR 20 PY 1992 VL 389 IS 2 BP L45 EP L48 DI 10.1086/186345 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HP121 UT WOS:A1992HP12100002 ER PT J AU HUCHRA, JP AF HUCHRA, JP TI THE HUBBLE CONSTANT SO SCIENCE LA English DT Article ID EXTRAGALACTIC DISTANCE SCALE; TULLY-FISHER RELATION; ABSOLUTE MAGNITUDE RELATION; VELOCITY-WIDTH RELATION; COLD DARK MATTER; TO-LIGHT RATIOS; ELLIPTICAL GALAXIES; COSMOLOGICAL CONSTANT; VIRGO CLUSTER; HERCULES SUPERCLUSTER AB The Hubble constant is the constant of proportionality between recession velocity and distance in the expanding universe. It is a fundamental property of cosmology that sets both the scale and the expansion age of the universe. It is determined by measurement of galaxy radial velocities and distances. Although there has been considerable progress in the development of new techniques for the measurements of galaxy distances, both calibration uncertainties and debates over systematic errors remain. Current determinations still range over nearly a factor of 2; the higher values favored by most local measurements are not consistent with many theories of the origin of large-scale structure and stellar evolution. RP HUCHRA, JP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 95 TC 30 Z9 30 U1 0 U2 2 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD APR 17 PY 1992 VL 256 IS 5055 BP 321 EP 325 DI 10.1126/science.256.5055.321 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA HP032 UT WOS:A1992HP03200024 PM 17743107 ER PT J AU COLINVAUX, P AF COLINVAUX, P TI DIVERSITY AND THE TROPICAL RAIN-FOREST - TERBORGH,J SO NATURE LA English DT Book Review RP COLINVAUX, P (reprint author), SMITHSONIAN TROP RES INST,POB 2072,BALBOA,PANAMA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD APR 16 PY 1992 VL 356 IS 6370 BP 625 EP 626 DI 10.1038/356625a0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA HP031 UT WOS:A1992HP03100058 ER PT J AU SMETTE, A SURDEJ, J SHAVER, PA FOLTZ, CB CHAFFEE, FH WEYMANN, RJ WILLIAMS, RE MAGAIN, P AF SMETTE, A SURDEJ, J SHAVER, PA FOLTZ, CB CHAFFEE, FH WEYMANN, RJ WILLIAMS, RE MAGAIN, P TI A SPECTROSCOPIC STUDY OF UM-673-A AND UM-673-B - ON THE SIZE OF LYMAN-ALPHA CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GRAVITATIONAL LENSING; QUASARS ABSORPTION LINES; QUASARS INDIVIDUAL (UM-673) ID + 561 A,B; ABSORPTION REDSHIFTS; GALAXY; SYSTEMS; SPECTRA; FOREST; LINES; EVOLUTION; ORIGIN; Z=0.39 AB We present a study of the Ly-alpha forest spectra (2 angstrom resolution) obtained for the A and B images of the gravitationally lensed high-redshift quasar UM 673. We also present higher resolution data of the brightest (A) image. In the 2 angstrom resolution spectra, all the absorption lines detected at 5-sigma in the spectrum of the fainter B image are present in the A image; however, we find two anticoincidences, i.e., two lines in A which do not have a counterpart in B at more than a 3-sigma confidence level. Given the fact that corresponding Ly-alpha lines in the spectra of A and B have their equivalent widths well correlated, this proves that both light beams actually cross the same clouds. Most of the velocity differences between corresponding lines are compatible with 0 km s-1 within the error bars, with a standard deviation of 17 km s-1. As the comoving linear separation increases from virtually Oh50(-1) kpc (H-0 = 50h50 km s-1 Mpc-1, q0 = 0) at the redshift of the QSO to 2h50(-1) kpc, we derive a best value of 12h50(-1) kpc for the 2-sigma lower limit and of 160h50(-1) kpc for the 2-sigma upper limit of the diameter of spherical Ly-alpha clouds in the redshift range 2.1-2.7, by means of Monte Carlo simulations. However, if we interpret the two anticoincidences as due to a Mg II doublet at z = 0.4261, we find in this case a best value of 23h50(-1) kpc to the 2-sigma lower limit of the Ly-alpha cloud diameter, but we cannot derive any upper limit. For the two major heavy-element systems detected in the spectrum of UM 673, we do not find any significant difference between the corresponding lines in the two spectra, indicating that these systems do not show dramatic variations over scales of 0.8h50(-1) and 2.1h(50)-1 kpc, respectively. C1 UNIV LIEGE,INST ASTROPHYS,B-4000 COINTE OUGREE,BELGIUM. UNIV CAMBRIDGE,INST ASTRON,CAMBRIDGE CB3 0HA,ENGLAND. CERRO TOLOLO INTERAMER OBSERV,LA SERENA,CHILE. SMITHSONIAN INST,MULTIPLE MIRROR TELESCOPE OBSERV,TUCSON,AZ 85721. CARNEGIE INST WASHINGTON OBSERV,PASADENA,CA 91101. RP SMETTE, A (reprint author), EUROPEAN SO OBSERV,KARL SCHWARZSCHILD STR 2,W-8046 GARCHING,GERMANY. NR 31 TC 124 Z9 125 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 APR 10 PY 1992 VL 389 IS 1 BP 39 EP 62 DI 10.1086/171187 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HM689 UT WOS:A1992HM68900004 ER PT J AU KETO, E BALL, R ARENS, J JERNIGAN, G MEIXNER, M AF KETO, E BALL, R ARENS, J JERNIGAN, G MEIXNER, M TI SUBARCSECOND MIDINFRARED IMAGING OF THE NUCLEI OF THE INFRARED BRIGHT GALAXIES NGC-1614 AND NGC-7469 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES INDIVIDUAL (NGC-1614, NGC-7469); GALAXIES NUCLEI; INFRARED GALAXIES; STARS FORMATION ID STAR FORMATION; APERTURE SYNTHESIS; GALACTIC NUCLEI; PHOTOMETRY; EMISSION; 10-MU-M AB We report on the first subarcsecond resolution mid-IR images of the nuclei of two galaxies from the IRAS bright sample, NGC 1614 and NGC 7469. Our results show that the starburst galaxy NGC 1614 contains a double structure in the nuclear region. Most of the flux, 78% of 650 +/- 50 mJy, is emitted in two unresolved regions of 0.6" FWHM (190 pc at 64 Mpc) of nearly equal strength separated by 0.6" (200 pc). Most of the remaining flux is derived from a small arm 1" in length (310 pc). The Seyfert I galaxy NGC 7469 shows an elongated structure, 1.4" x 0.7" (450 x 220 pc at 66 Mpc). C1 UNIV HAWAII,NASA,INFRARED TELESCOPE FACIL,HONOLULU,HI 96822. UNIV CALIF LAWRENCE LIVERMORE NATL LAB,INST GEOPHYS & PLANETARY PHYS,LIVERMORE,CA 94550. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94760. RP KETO, E (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 23 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 APR 10 PY 1992 VL 389 IS 1 BP 223 EP 226 DI 10.1086/171199 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HM689 UT WOS:A1992HM68900016 ER PT J AU REISENFELD, DB RAYMOND, JC YOUNG, AR KOHL, JL AF REISENFELD, DB RAYMOND, JC YOUNG, AR KOHL, JL TI ON THE DENSITY AND FIELD SENSITIVITIES OF DIELECTRONIC RECOMBINATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC PROCESSES; LINE, FORMATION; STARS, CORONAE; SUN, MAGNETIC FIELDS; SUN, TRANSITION REGION; SUN, UV RADIATION ID SOLAR TRANSITION REGION; DISTORTED-WAVE CALCULATIONS; ELECTRIC-FIELDS; ENERGY-BALANCE; LOOPS; IONS; ENHANCEMENT; SPECTRUM; FLARE AB Dielectronic recombination dominates the recombination rates of most ions in coronal plasmas at their temperatures of peak concentration. Because dielectronic recombination goes by way of high nl doubly excited levels, it is susceptible to collisional excitation and ionization, leading to a decreased rate. On the other hand, theoretical studies show that Stark mixing of the nl levels by a modest electric field enhances the dielectronic recombination rate severalfold. A companion paper presents a calculation of the combined effects of plasma microfields and collisional processes on the dielectronic recombination rates of carbon ions. Here, we compute the ionization balance as a function of density. We find that the new results require increased emission measures to match the C IV emission line intensities observed in the Sun and in late-type stars. They also make it more difficult to interpret the overall EUV emission line spectrum of the Sun. C1 CALTECH,NORMAN BRIDGE LAB PHYS 16133,PASADENA,CA 91125. RP REISENFELD, DB (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Reisenfeld, Daniel/F-7614-2015 NR 44 TC 6 Z9 6 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 APR 10 PY 1992 VL 389 IS 1 BP L37 EP L40 DI 10.1086/186343 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HM690 UT WOS:A1992HM69000010 ER PT J AU BERTSCHE, KJ WEDEL, WR AF BERTSCHE, KJ WEDEL, WR TI RADIOCARBON ANALYSIS OF IRON ARCHAEOLOGICAL ARTIFACTS SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 UNIV CALIF LAWRENCE LIVERMORE NATL LAB,LIVERMORE,CA 94550. SMITHSONIAN INST,DEPT ANTHROPOL,WASHINGTON,DC 20560. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD APR 5 PY 1992 VL 203 BP 16 EP NUCL PN 2 PG 0 WC Chemistry, Multidisciplinary SC Chemistry GA HK162 UT WOS:A1992HK16201240 ER PT J AU VAITHIYANATHAN, P JORDAN, TE CORRELL, DL AF VAITHIYANATHAN, P JORDAN, TE CORRELL, DL TI PHOSPHORUS DIAGENESIS IN THE RHODE RIVER ESTUARY SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 UNIV QUEBEC,INRS EAU,ST FOY G1V 4C7,QUEBEC,CANADA. SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD APR 5 PY 1992 VL 203 BP 130 EP ENVR PN 1 PG 0 WC Chemistry, Multidisciplinary SC Chemistry GA HK161 UT WOS:A1992HK16102063 ER PT J AU LELLINGER, DB AF LELLINGER, DB TI CORRECT PUBLICATION DATE OF SODIRO CRYPTOGAMAE VASCULARES QUITENSES SO AMERICAN FERN JOURNAL LA English DT Note RP LELLINGER, DB (reprint author), SMITHSONIAN INST,US NATL HERBARIUM,NHB-166,WASHINGTON,DC 20560, USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU AMER FERN SOC INC PI WASHINGTON PA C/O DAVID B LELLINGER, SMITHSONIAN INST, BOTANY DEPT, WASHINGTON, DC 20560 SN 0002-8444 J9 AM FERN J JI Am. Fern J. PD APR-JUN PY 1992 VL 82 IS 2 BP 86 EP 86 DI 10.2307/1547389 PG 1 WC Plant Sciences SC Plant Sciences GA JE393 UT WOS:A1992JE39300012 ER PT J AU YENER, KA AF YENER, KA TI GOLTEPE EXCAVATIONS, 1991 - AN EARLY BRONZE-AGE TIN-PROCESSING SITE IN THE TAURUS MOUNTAINS SO AMERICAN JOURNAL OF ARCHAEOLOGY LA English DT Meeting Abstract C1 SMITHSONIAN INST,WASHINGTON,DC 20560. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARCHAEOLOGICAL INST PI NEW YORK PA 135 WILLIAM ST, NEW YORK, NY 10038-3805 SN 0002-9114 J9 AM J ARCHAEOL JI Am. J. Archaeol. PD APR PY 1992 VL 96 IS 2 BP 341 EP 342 PG 2 WC Archaeology SC Archaeology GA HQ216 UT WOS:A1992HQ21600045 ER PT J AU PENA, JT VANDIVER, P AF PENA, JT VANDIVER, P TI CONTINUITY OR DISCONTINUITY IN CENTRAL ITALIAN GLAZED POTTERY MANUFACTURE - NEW EVIDENCE FROM THE PALATINE HILL IN ROME SO AMERICAN JOURNAL OF ARCHAEOLOGY LA English DT Meeting Abstract C1 SUNY ALBANY,ALBANY,NY 12222. SMITHSONIAN INST,WASHINGTON,DC 20560. NR 0 TC 0 Z9 0 U1 0 U2 2 PU ARCHAEOLOGICAL INST PI NEW YORK PA 135 WILLIAM ST, NEW YORK, NY 10038-3805 SN 0002-9114 J9 AM J ARCHAEOL JI Am. J. Archaeol. PD APR PY 1992 VL 96 IS 2 BP 365 EP 366 PG 2 WC Archaeology SC Archaeology GA HQ216 UT WOS:A1992HQ21600134 ER PT J AU SPIRA, TP SNOW, AA WHIGHAM, DF LEAK, J AF SPIRA, TP SNOW, AA WHIGHAM, DF LEAK, J TI FLOWER VISITATION, POLLEN DEPOSITION, AND POLLEN-TUBE COMPETITION IN HIBISCUS-MOSCHEUTOS (MALVACEAE) SO AMERICAN JOURNAL OF BOTANY LA English DT Article ID ZEA-MAYS; MESSENGER-RNAS; DIVERSITY; GROWTH; SHOOTS AB The potential influence of pollen-tube competition on offspring "quality" has received considerable attention in recent years. Yet the prevalence of pollen competition in natural populations is largely unknown because few investigators have actually measured rates of pollen deposition on stigmas. In this study, we assess the potential for pollen-tube competition in natural populations of the self-compatible, pollinator-dependent herbaceous perennial, Hibiscus moscheutos. Individual flowers averaged two to four visits per 15 min by potential pollinators (Ptilothrix and Bombus), and about 34% of these visits involved contact with a stigma. The median number of pollen grains deposited on virgin stigmas per contact visit was 70 grains (values ranged from 0 to 889), and flowers averaged about four contact visits per hour. Approximately 360 pollen grains must reach stigmas for full seed set to occur in a typical flower (an average ovary has 139 ovules, and 2.6 pollen grains are required per seed). Within 2 and 3 hr exposure to pollinators, 65% and 97% of the flowers received excess pollen (> 360 grains) and median stigmatic pollen loads exceeded the number of ovules by a factor of 4.O and 5.4, respectively. Based on 3 yr observations, it is concluded that pollen competition may frequently occur in this species. C1 SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. OHIO STATE UNIV,DEPT PLANT BIOL,COLUMBUS,OH 43210. RP SPIRA, TP (reprint author), GEORGIA SO UNIV,DEPT BIOL,STATESBORO,GA 30460, USA. OI Whigham, Dennis/0000-0003-1488-820X NR 25 TC 56 Z9 69 U1 0 U2 11 PU BOTANICAL SOC AMER INC PI COLUMBUS PA OHIO STATE UNIV-DEPT BOTANY 1735 NEIL AVE, COLUMBUS, OH 43210 SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD APR PY 1992 VL 79 IS 4 BP 428 EP 433 DI 10.2307/2445155 PG 6 WC Plant Sciences SC Plant Sciences GA HQ215 UT WOS:A1992HQ21500008 ER PT J AU MATTHEWS, NL AF MATTHEWS, NL TI LAW AND GOVERNMENT UNDER THE TUDORS - ESSAYS PRESENTED TO ELTON,GEOFFREY, REGIUS PROFESSOR OF MODERN-HISTORY IN THE UNIVERSITY-OF-CAMBRIDGE ON THE OCCASION OF HIS RETIREMENT - CROSS,C, LOADES,D, SCARISBRICK,JJ SO AMERICAN JOURNAL OF LEGAL HISTORY LA English DT Book Review RP MATTHEWS, NL (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU TEMPLE UNIV SCHOOL LAW PI PHILADELPHIA PA 1719 NORTH BROAD STREET, PHILADELPHIA, PA 19122 SN 0002-9319 J9 AM J LEGAL HIST JI Am. J. Legal Hist. PD APR PY 1992 VL 36 IS 2 BP 210 EP 212 DI 10.2307/845862 PG 3 WC Law SC Government & Law GA HQ527 UT WOS:A1992HQ52700009 ER PT J AU TAYLOR, LE AF TAYLOR, LE TI FOR DEMOCRACY, WORKERS AND GOD - LABOR SONG POEMS AND LABOR PROTEST, 1865-95 - HALKER,CD SO AMERICAN STUDIES INTERNATIONAL LA English DT Book Review RP TAYLOR, LE (reprint author), SMITHSONIAN INST,CTR FOLKLIFE PROGRAMS CULTURAL STUDIES,WASHINGTON,DC 20560, USA. NR 1 TC 1 Z9 1 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 APR PY 1992 VL 30 IS 1 BP 121 EP 121 PG 1 WC History SC History GA HP913 UT WOS:A1992HP91300020 ER PT J AU GARCIA, MR GRINDLAY, JE BAILYN, CD PIPHER, JL SHURE, MA WOODWARD, CE AF GARCIA, MR GRINDLAY, JE BAILYN, CD PIPHER, JL SHURE, MA WOODWARD, CE TI THE INFRARED COUNTERPART OF GX-13+1 SO ASTRONOMICAL JOURNAL LA English DT Article ID X-RAY SOURCES; X-1; VARIABILITY; SCATTERING; CYGNUS-X-3; EMISSION; BINARIES; SEARCH; HALOS; STAR AB We have discovered a bright (K = 12) infrared source which is likely the counterpart to the bright galactic bulge x-ray source GX 13 + 1. Observations with the MMT infrared photometer and the Rochester infrared Array camera at the IRTF allow determination of the source position to approximately 0.7 arcsec, allow the infrared colors to be measured, and shows no variability on a 1 yr timescale. We consider four possible sources for the infrared emission, and conclude that it is most likely due to a K giant secondary. Future observations should allow more definite discrimination between the various possibilities. The discovery of a late-type giant secondary in GX 13 + 1 is contrary to the expectation that low-mass x-ray binaries (LMXB) which show quasiperiodic oscillations (QPO) have giant companions, while those which do not show QPO (like GX 13 + 1) have dwarf secondaries. The relation between the size of the scattered x-ray halo and the A(V) inferred from the infrared observations is compared to that found in other x-ray sources. C1 YALE UNIV,DEPT ASTRON,NEW HAVEN,CT 06511. UNIV ROCHESTER,DEPT PHYS & ASTRON,ROCHESTER,NY 14627. UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822. UNIV WYOMING,WYOMING INFRARED OBSERV,LARAMIE,WY 82071. UNIV HAWAII,NASA,INFRARED TELESCOPE FACIL,HONOLULU,HI 96822. RP GARCIA, MR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 44 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 APR PY 1992 VL 103 IS 4 BP 1325 EP 1329 DI 10.1086/116145 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HK359 UT WOS:A1992HK35900024 ER PT J AU BLUMENTHAL, GR DACOSTA, LN GOLDWIRTH, DS LECAR, M PIRAN, T AF BLUMENTHAL, GR DACOSTA, LN GOLDWIRTH, DS LECAR, M PIRAN, T TI THE LARGEST POSSIBLE VOIDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMIC MICROWAVE BACKGROUND; GALAXIES CLUSTERING; LARGE-SCALE STRUCTURE OF UNIVERSE ID EINSTEIN-DESITTER UNIVERSE; REDSHIFT SURVEY; MATTER; GALAXIES AB Observational constraints on the isotropy of the microwave background on angular scales greater than 1-degrees seriously limit the possible fluctuations in the gravitational potential in the universe because of the Sachs-Wolfe effect. Consequently, they also provide a limit on the initial density inhomogeneities in the universe. We use these limits to show that the typical voids in the mass distribution in an OMEGA = 1 universe have limiting diameter D < 80h-1 Mpc and that, for Gaussian initial fluctuations, there should be at most one void in the whole Hubble volume with a diameter D > 130h-1 Mpc. Consequently, the observation of voids in the galaxy distribution larger than the above limit would imply that either (1) gravitational instabilities do not produce the observed structure on large scales, (2) variations in the galaxy distribution can be much more extreme than in the mass distribution (that is, light does not trace mass), or (3) the universe has a density parameter OMEGA not-equal 1. If the current upper limits on the cosmic microwave background isotropy were reduced by a factor of 4, our upper limit would come into conflict with the currently observed sizes of voids, and one would have to invoke one of the above alternatives. C1 CONSELHO NACL PESQUISAS,OBSERV NACL,BR-22290 RIO DE JANEIRO,RJ,BRAZIL. UNIV CALIF SANTA CRUZ,LICK OBSERV,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064. HEBREW UNIV JERUSALEM,RACAH INST PHYS,IL-91904 JERUSALEM,ISRAEL. RP BLUMENTHAL, GR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 37 TC 66 Z9 66 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 APR 1 PY 1992 VL 388 IS 2 BP 234 EP 241 DI 10.1086/171147 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HM051 UT WOS:A1992HM05100002 ER PT J AU BOTHUN, GD SCHOMMER, RA WILLIAMS, TB MOULD, JR HUCHRA, JP AF BOTHUN, GD SCHOMMER, RA WILLIAMS, TB MOULD, JR HUCHRA, JP TI PECULIAR VELOCITIES OF FIELD SPIRAL GALAXIES NEAR AND BEYOND THE GREAT ATTRACTOR SO ASTROPHYSICAL JOURNAL LA English DT Article DE CELESTIAL MECHANICS, STELLAR DYNAMICS; GALAXIES DISTANCES AND REDSHIFTS ID ELLIPTICAL GALAXIES; LOCAL SUPERCLUSTER; DISTANCE SCALE; WIDTH RELATION; CLUSTERS; MOTION; ANISOTROPY; PHOTOMETRY; CENTAURUS; VIRGO AB We measure peculiar velocities for a sample of 48 late-type spiral galaxies which are located in the general vicinity of the Great Attractor (GA). Relative distances are derived using the I-band Tully-Fisher relation. We confirm the existence of positive velocity residuals, with amplitude 500-2000 km s-1 in the Hydra-Centaurus region, for galaxies located at kinematic distances of 20-30 Mpc. Beyond 45 Mpc, we have a very weak signal of negative velocity residuals whose amplitude is very sensitive to the form of the Malmquist correction. However, positive velocity residuals can be detected in galaxies with distances as large as 80 Mpc. We test the origin of these motions by the use of a nonlinear spherical infall model which predicts the position of the caustic surface as a function of distance from the GA. We also use all available velocities to search for the caustics in redshift space. We explicitly incorporate distance errors into the models and adopt a Malmquist correction which is appropriate for a highly clustered distribution. Comparison of the data with the model yields the following results: (1) we cannot identify a symmetric infall pattern centered on the GA, (2) a bulk flow "infall" pattern, centered on a kinematic distance of 4350 km s-1, provides the best means of correcting the observed velocity so as to produce a Tully-Fisher relation with the least amount of scatter, and (3) galaxies in the vicinity of OCA 3574 appear to participate in a small-scale infall pattern. The overall behavior of the data shows that we have not yet obtained a sample over a sufficiently large volume to isolate the true source of the observed peculiar velocities. The possibility of large peculiar motions on the scale of 10,000 km s-1 remains viable. However, the morphology in redshift space of the Centaurus Cluster, coupled with the large observed peculiar velocities in this region, strongly suggests that this structure is a main contributor to the observed flow. C1 CERRO TOLOLO INTERAMER OBSERV,NATL OPT ASTRON OBSERV,LA SERENA 1353,CHILE. RUTGERS STATE UNIV,DEPT PHYS & ASTRON,PISCATAWAY,NJ 08855. PALOMAR OBSERV,PASADENA,CA 91125. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP BOTHUN, GD (reprint author), UNIV OREGON,DEPT DIABET RES & TRAINING,EUGENE,OR 97403, USA. NR 48 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 APR 1 PY 1992 VL 388 IS 2 BP 253 EP 267 DI 10.1086/171149 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HM051 UT WOS:A1992HM05100004 ER PT J AU CHRISTODOULOU, DM NARAYAN, R AF CHRISTODOULOU, DM NARAYAN, R TI THE STABILITY OF ACCRETION TORI .4. FISSION AND FRAGMENTATION OF SLENDER, SELF-GRAVITATING ANNULI SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; HYDRODYNAMICS; INSTABILITIES; STARS FORMATION ID DIFFERENTIALLY ROTATING-DISKS; NON-LINEAR EVOLUTION; T-TAURI STARS; DYNAMICAL STABILITY; ANGULAR-MOMENTUM; NONAXISYMMETRIC INSTABILITIES; VERSATILE METHOD; BLACK-HOLE; RINGS; POLYTROPES AB We present results on the dynamical evolution of two-dimensional, geometrically slender, differentially rotating, self-gravitating annuli orbiting around a central mass. These are idealized models of thick (pressure supported) accretion disks. The initial axisymmetric equilibrium models we have studied are compressible with polytropic index n = 1 and have constant specific angular momentum. The linear growth rates of the different modes are calculated through a solution of the linearized fluid equations. Some model evolutions have also been carried into the nonlinear regime using a two-dimensional, Eulerian hydro code that is second-order accurate in both space and time. We find good agreement between the results from linear analysis and the linear regime of the hydro code, which strongly validates both approaches. Three kinds of unstable modes are known to operate in these annuli, the P, I, and J modes. In the nonlinear regime, we confirm the well-documented result that the P-mode causes a breakup of the slender annulus into "planets" that do not separate completely but eventually merge to form a new, roughly axisymmetric configuration. No mechanism has been previously identified for the I-mode. We show that this mode is due to a fission instability similar to the one discussed in the context of classical instabilities of rotating, self-gravitating, ellipsoidal, fluid masses. Under the action of an I-mode with azimuthal wavenumber m = 2, the circular annulus initially deforms into an elliptical shape (triangular, square shape for m = 3, 4, etc.) and later separates into symmetrical clumps that move out to a larger radius. If the central star is allowed to move in response to the developing nonaxisymmetry of the annulus, then power is shifted predominantly to the I-mode with m = 1. In this case, the annulus breaks up into one major clump with debris, forming a binary system with the original central star. The J-mode has been previously identified with the Jeans mechanism of instability. We confirm this interpretation. In the nonlinear regime, the behavior of this mode is analogous to the fragmentation process that is discussed in the context of collapsing clouds. We find that the mode generates severe clumpiness in the annulus, ultimately causing it to break up into multiple blobs. The fragments interact through tidal torques, and several of them fall to the center where they merge into a single object. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 66 TC 27 Z9 27 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 APR 1 PY 1992 VL 388 IS 2 BP 451 EP 466 DI 10.1086/171166 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HM051 UT WOS:A1992HM05100021 ER PT J AU HEANEY, PJ POST, JE EVANS, HT AF HEANEY, PJ POST, JE EVANS, HT TI THE CRYSTAL-STRUCTURE OF BANNISTERITE SO CLAYS AND CLAY MINERALS LA English DT Article DE BANNISTERITE; INTERLAYER CATIONS; LAYER STRUCTURE; MODULATED STRUCTURE; X-RAY STRUCTURE REFINEMENT ID LAYER SILICATES AB The crystal structure of bannisterite, a modulated, mica-like mineral species, of general composition Ca0.5(K,Na)0.5(Mn,Fe,Mg,Zn)10(Si,Al)16O38(OH)8.nH2O, has been solved and refined for specimens from Franklin Furnace, New Jersey (FF), and Broken Hill, Australia (BH). The crystals are monoclinic in space group A2/a, with (for FF) a = 22.265(1) angstrom, b = 16.368(1) angstrom, c = 24.668(2) angstrom, beta = 94.285(5)-degrees; and (for BH) a = 22.286(1) angstrom, b = 16.386(1) angstrom, c = 24.575(2) angstrom, beta = 94.355(7)-degrees; Z = 8. Refinement with anisotropic thermal factors reached R(W) = 0.034 (FF) and 0.039 (BH). Like stilpnomelane and ganophyllite, bannisterite has a modified 2:1 trioctahedral layer structure in which some of the tetrahedra are inverted towards the interlayer region and linked to inverted tetrahedra in the opposite layer. The octahedral sheet is strongly corrugated along b. The tetrahedral sheet consists of 5-, 6-, and 7-fold rings. and bond distance calculations indicate that Al is concentrated into two of the four inverted tetrahedra. The interlayer Ca, K, and H2O species are highly disordered, as indicated by anomalously large temperature factors and partial occupancies. Localized differences in the Al/Si arrangements in the inverted tetrahedra induce disorder among the interlayer cations. C1 SMITHSONIAN INST, DEPT MINERAL SCI, WASHINGTON, DC 20560 USA. US GEOL SURVEY, RESTON, VA 22092 USA. NR 21 TC 9 Z9 10 U1 1 U2 2 PU CLAY MINERALS SOC PI CHANTILLY PA 3635 CONCORDE PKWY, STE 500, CHANTILLY, VA 20151-1125 USA SN 0009-8604 EI 1552-8367 J9 CLAY CLAY MINER JI Clay Clay Min. PD APR PY 1992 VL 40 IS 2 BP 129 EP 144 DI 10.1346/CCMN.1992.0400201 PG 16 WC Chemistry, Physical; Geosciences, Multidisciplinary; Mineralogy; Soil Science SC Chemistry; Geology; Mineralogy; Agriculture GA HW847 UT WOS:A1992HW84700001 ER PT J AU TAUXE, L DEINO, AD BEHRENSMEYER, AK POTTS, R AF TAUXE, L DEINO, AD BEHRENSMEYER, AK POTTS, R TI PINNING DOWN THE BRUNHES MATUYAMA AND UPPER JARAMILLO BOUNDARIES - A RECONCILIATION OF ORBITAL AND ISOTOPIC TIME SCALES SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article ID SOUTHERN KENYA RIFT; REVERSAL; GEOCHRONOLOGY; OLORGESAILIE; BP AB Until recently, the temporal calibration of the Plio/Pleistocene portion of the geomagnetic reversal time scale (GRTS) was based exclusively on K-Ar isotopic ages of volcanic rocks. The so-called "chronogram technique" estimates the age that minimizes discrepancies between a given age assignment for a reversal boundary and the population of dates of known polarity. The most widely quoted date, 0.73 Ma, for the Brunhes/Matuyama boundary was derived in such a manner [1]. Radioactive decay is not the only source of temporal information in the geologic record, however. Variations in several of the orbital parameters of the Earth (e.g. precession, obliquity, eccentricity) can be calculated for the last several million years and the climatic response approximated. A recent analysis of the so-called "astronomical technique" on oxygen isotopic data from deep-sea sediments suggested an age of 0.78 Ma for the Brunhes/Matuyama boundary [2], some 50,000 years older than the chronogram estimate. We reconcile the two estimates for the age of the last reversal by first presenting new magnetostratigraphic data tied to high-quality Ar-40/Ar-39 dates. Our date for the upper Jaramillo boundary is 0.992 +/- 0.039 Ma, considerably older than the estimate of 0.91 Ma in the standard (chronogram-based) time scale [3]. Furthermore, an age of 0.746 +/- 0.009 Ma was obtained for sediments immediately overlying the Brunhes/Matuyama boundary. These data are consistent with the astronomical estimates of 0.78 Ma and 0.99 Ma for the Brunhes/Matuyama and upper Jaramillo boundaries, respectively. Finally, we present a new method for estimating the uncertainties of ages calculated using the chronogram technique that employs a simple bootstrap resampling scheme. The 95% confidence region for the chronogram estimate of the Brunhes/Matuyama boundary, using an updated compilation of date/polarity pairs, spans from 0.73 to 0.78 Ma. We find, therefore, that the discrepancies between the isotopic data set and the astronomical calibration of the Brunhes/Matuyama boundary disappear when appropriate uncertainties are applied for the most recent compilation of isotopic data. C1 INST HUMAN ORIGINS,BERKELEY,CA 94709. SMITHSONIAN INST,WASHINGTON,DC 20560. RP TAUXE, L (reprint author), UNIV CALIF SAN DIEGO,SCRIPPS INST OCEANOG,LA JOLLA,CA 92093, USA. NR 32 TC 79 Z9 79 U1 0 U2 4 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 APR PY 1992 VL 109 IS 3-4 BP 561 EP 572 DI 10.1016/0012-821X(92)90114-B PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA HU460 UT WOS:A1992HU46000024 ER PT J AU PETERSEN, CW WARNER, RR COHEN, S HESS, HC SEWELL, AT AF PETERSEN, CW WARNER, RR COHEN, S HESS, HC SEWELL, AT TI VARIABLE PELAGIC FERTILIZATION SUCCESS - IMPLICATIONS FOR MATE CHOICE AND SPATIAL PATTERNS OF MATING SO ECOLOGY LA English DT Article DE CARIBBEAN; EXTERNAL FERTILIZATION; LABRIDAE; MATE CHOICE; SPAWNING; SPERM COMPETITION; SPERM DEPLETION; THALASSOMA ID CORAL-REEF FISH; SERRANUS-FASCIATUS; SITE DETERMINATION; CONSEQUENCES; THALASSOMA; BEHAVIOR; SYSTEM; SIZE AB Fertilization success was measured in the bluehead wrasse, Thalassoma bifasciatum, a tropical reef fish with external fertilization of pelagic eggs. This species exhibits intraspecific variation in its spawning behavior; females either spawn with single males (pair spawning) or spawn with a group of at least three and often > 20 males (group spawning). Fertilization success averaged almost-equal-to 75% and did not differ between pair and group spawning, despite an estimated 80-fold increase in sperm release in group spawns. There was also no evidence that pair-spawning males suffered sperm depletion over the course of the spawning period. Thalassoma bifasciatum occurs in a variety of habitats and is exposed to varying levels of water turbulence. Fertilization success varied among days, and decreased with rougher water conditions. Within a reef, the calmer spawning sites behind the reef relative to the current had higher fertilization success than those along the side of the reef. These data suggest that while the type of spawning occurring at the site does not affect selection for fertilization success, females may gain fertilizations by selecting particular locations or periods of calmer water conditions to spawn. This is an alternative hypothesis to explain temporal and spatial patterns of mating. We provide detailed methods on how to accurately obtain data on fertilization success. Our technique can be used to study natural spawning in a wide variety of reef fishes and other marine organisms with pelagic eggs, external fertilization, and predictable spawning. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. UNIV WASHINGTON,FRIDAY HARBOR LABS,FRIDAY HARBOR,WA 98250. UNIV CALIF SANTA BARBARA,DEPT BIOL SCI,SANTA BARBARA,CA 93106. UNIV WASHINGTON,DEPT ZOOL,SEATTLE,WA 98195. RI Warner, Robert/M-5342-2013 OI Warner, Robert/0000-0002-3299-5685 NR 39 TC 95 Z9 95 U1 0 U2 5 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE, NW, STE 400, WASHINGTON, DC 20036 SN 0012-9658 J9 ECOLOGY JI Ecology PD APR PY 1992 VL 73 IS 2 BP 391 EP 401 DI 10.2307/1940747 PG 11 WC Ecology SC Environmental Sciences & Ecology GA HK464 UT WOS:A1992HK46400001 ER PT J AU FINCKE, OM AF FINCKE, OM TI CONSEQUENCES OF LARVAL ECOLOGY FOR TERRITORIALITY AND REPRODUCTIVE SUCCESS OF A NEOTROPICAL DAMSELFLY SO ECOLOGY LA English DT Article DE LARVAE; NEOTROPICAL; ODONATE; OVIPOSITION; PSEUDOSTIGMATIDAE; REPRODUCTIVE SUCCESS; TERRITORIALITY; TREE HOLE ID LIFETIME MATING SUCCESS; HAGENI WALSH ODONATA; SEXUAL SELECTION; OVIPOSITION PREFERENCE; EVOLUTION; SIZE; DIMORPHISM; COENAGRIONIDAE; CALOPTERYGIDAE; LIBELLULIDAE AB Male territorial behavior and female oviposition behavior of Megaloprepus coerulatus, a damselfly that develops in water-filled tree holes, is interpreted in light of its larval ecology. Sexual selection favors large males because they win more territorial contests than do smaller males, and females mate only in the vicinity of defended tree holes (i.e., passive female choice). Small males behave as territory holders until displaced, and/or act as subordinate satellites at large territories. Females are more predictably found in forest light gaps, even though they oviposit in both gap and understory tree holes. Males defended only 14% of the sites used by ovipositing females. Large tree holes are relatively rare, but support a greater number of emerging adults per season and produce larger adults than tree holes containing less-than-or-equal-to 1 L of water, which rarely produce more than one individual per season. By defending only large tree holes in gap areas, a male increases his chances of mating, and of producing multiple offspring and reproductively successful sons. Results from a field experiment suggest that both mate acquisition and procurement of superior larval habitats have been selective pressures in the evolution of male territory choice. Because even large holes are inadequate to support a female's entire clutch, and the presence of conspecific and heterospecific odonate larvae makes offspring survival uncertain, selection favors a female that partitions her clutch among multiple tree holes. C1 SMITHSONIAN TROP RES INST,MIAMI,FL 34002. RP FINCKE, OM (reprint author), UNIV OKLAHOMA,DEPT ZOOL,NORMAN,OK 73019, USA. NR 53 TC 41 Z9 46 U1 0 U2 9 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE, NW, STE 400, WASHINGTON, DC 20036 SN 0012-9658 J9 ECOLOGY JI Ecology PD APR PY 1992 VL 73 IS 2 BP 449 EP 462 DI 10.2307/1940752 PG 14 WC Ecology SC Environmental Sciences & Ecology GA HK464 UT WOS:A1992HK46400006 ER PT J AU DINERSTEIN, E AF DINERSTEIN, E TI EFFECTS OF RHINOCEROS-UNICORNIS ON RIVERINE FOREST STRUCTURE IN LOWLAND NEPAL SO ECOLOGY LA English DT Note C1 SMITHSONIAN NEPAL TERAI ECOL PROJECT,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630. NR 18 TC 5 Z9 6 U1 0 U2 3 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE, NW, STE 400, WASHINGTON, DC 20036 SN 0012-9658 J9 ECOLOGY JI Ecology PD APR PY 1992 VL 73 IS 2 BP 701 EP 704 DI 10.2307/1940778 PG 4 WC Ecology SC Environmental Sciences & Ecology GA HK464 UT WOS:A1992HK46400032 ER PT J AU HICKMOTT, DD SORENSEN, SS ROGERS, PSZ AF HICKMOTT, DD SORENSEN, SS ROGERS, PSZ TI METASOMATISM IN A SUBDUCTION COMPLEX - CONSTRAINTS FROM MICROANALYSIS OF TRACE-ELEMENTS IN MINERALS FROM GARNET AMPHIBOLITE FROM THE CATALINA SCHIST SO GEOLOGY LA English DT Article ID SOUTHERN-CALIFORNIA; FRANCISCAN-COMPLEX; HIGH-PRESSURE; ARC BASALTS; MAGMAS; GENESIS; ZONE; TERRANE; MANTLE; ROCKS AB Trace element abundances and zoning were measured in minerals from a metasomatized garnet-amphibolite block from the Catalina Schist, using both ion and proton microprobes. Zoisite strongly concentrates light rare earth elements (REEs), Sr, Y, and Pb; amphibole concentrates Ni and Zn; garnet concentrates Y and heavy REEs; and titanite concentrates Nb. Major and trace elements in the garnets are zoned. Garnets in the core of the block display an overgrowth enriched in Mn, Y, and heavy REE, on a Y- and heavy-REE-poor core. Zirconium values remain relatively constant. The element enrichments in the garnet overgrowth suggest mobility of REEs at either a hand-sample or regional scale at subduction-zone pressure-temperature conditions. Metamorphic fluids may selectively transport heavy REEs relative to some high field strength elements in some convergent-margin settings. The distribution of Sr and Pb within subduction zones may reflect the dehydration and melting behavior of epidote-group minerals. C1 SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560. RP HICKMOTT, DD (reprint author), UNIV CALIF LOS ALAMOS SCI LAB,EES-1,MS-D462,LOS ALAMOS,NM 87545, USA. RI Hickmott, Donald/C-2886-2011 NR 29 TC 32 Z9 32 U1 2 U2 9 PU GEOLOGICAL SOC AMERICA PI BOULDER PA PO BOX 9140 3300 PENROSE PLACE, BOULDER, CO 80301 SN 0091-7613 J9 GEOLOGY JI Geology PD APR PY 1992 VL 20 IS 4 BP 347 EP 350 DI 10.1130/0091-7613(1992)020<0347:MIASCC>2.3.CO;2 PG 4 WC Geology SC Geology GA HL911 UT WOS:A1992HL91100015 ER PT J AU LECAR, M FRANKLIN, F SOPER, P AF LECAR, M FRANKLIN, F SOPER, P TI ON THE ORIGINAL DISTRIBUTION OF THE ASTEROIDS .4. NUMERICAL EXPERIMENTS IN THE OUTER ASTEROID BELT SO ICARUS LA English DT Article ID SOLAR-SYSTEM; JUPITER; ORBITS; SATURN; MOTION RP LECAR, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 16 TC 20 Z9 20 U1 0 U2 0 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD APR PY 1992 VL 96 IS 2 BP 234 EP 250 DI 10.1016/0019-1035(92)90078-L PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HU441 UT WOS:A1992HU44100011 ER PT J AU SUN, Y DALGARNO, A AF SUN, Y DALGARNO, A TI COLLISIONAL EXCITATION OF METASTABLE O(1D) ATOMS SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID RYDBERG; STATES; O-2 AB The excitation of ground state O(3P) atoms into the metastable O(1D) state by collision with O(3P) atoms occurs predominantly via the lowest (3)PI(g) states of O2. Experimental data on the decay products of the (3)PI(g) Rydberg state are used in a scattering calculation to predict the cross sections and rate coefficients for the excitation and quenching of O(1D) atoms in collision with O(3P) atoms. At 1000 K, the quenching rate coefficient is 6.9 x 10(-12) cm3 s-1. The excitation cross section reaches a maximum of 7.2 x 10(-18) cm2 at a relative energy of 3.8 eV. RP SUN, Y (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 14 TC 16 Z9 16 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 APR 1 PY 1992 VL 96 IS 7 BP 5017 EP 5019 DI 10.1063/1.462744 PG 3 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA HL099 UT WOS:A1992HL09900021 ER PT J AU VAITHIYANATHAN, P CORRELL, DL AF VAITHIYANATHAN, P CORRELL, DL TI THE RHODE RIVER WATERSHED - PHOSPHORUS DISTRIBUTION AND EXPORT IN FOREST AND AGRICULTURAL SOILS SO JOURNAL OF ENVIRONMENTAL QUALITY LA English DT Article ID GRASSLAND SOILS; LAND-USE; CULTIVATION; AVAILABILITY; FRACTIONS; PHOSPHATE; RAINFALL; DYNAMICS; NITRATE; EROSION AB To evaluate the effects of land use on P transport and transformation in the Atlantic coastal plain, we examined the distribution and fractionation of P in forested and agricultural soils of the Rhode River watershed and their export rates. Nearly 70% of P in forest soils was bound in organic forms. Fractionation studies reveal that cultivation and fertilizer P application increased total and inorganic P content and decreased organic P content of the soils. About half of the increase in the inorganic P content of the agricultural soils is due to the mineralization of organic P during cultivation and the rest is probably due to fertilizer P application. The inorganic phosphates in the forest and agricultural soils are chiefly associated with Fe either as iron phosphates or as phosphates adsorbed on the iron oxide surfaces. The agricultural watershed had a higher P export (46.3 g P ha-1 wk-1) compared to the forested watershed (5.% g P ha-1 wk-1). Particulate P dominated the P export from both watersheds. Variations in the P flux from the watersheds was correlated to changes in water discharge. The discharge pattern of organic and inorganic P forms from the watersheds are highly related to their soil P composition. C1 SMITHSONIAN ENVIRONM RES CTR,POB 28,EDGEWATER,MD 21037. NR 46 TC 65 Z9 70 U1 2 U2 9 PU AMER SOC AGRONOMY PI MADISON PA 677 S SEGOE RD, MADISON, WI 53711 SN 0047-2425 J9 J ENVIRON QUAL JI J. Environ. Qual. PD APR-JUN PY 1992 VL 21 IS 2 BP 280 EP 288 PG 9 WC Environmental Sciences SC Environmental Sciences & Ecology GA HU312 UT WOS:A1992HU31200020 ER PT J AU FLINT, OS AF FLINT, OS TI HYDROPSYCHE-FRANCLEMONTI, A NEW SPECIES OF THE SCALARIS GROUP FROM EASTERN NORTH-AMERICA (TRICHOPTERA, HYDROPSYCHIDAE) SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Article AB The new hydropsychid caddisfly, Hydropsyche franclemonti, is described, illustrated and its distribution plotted (Connecticut, New York, North and South Carolina, Virginia and Quebec). It is differentiated from its closest relatives in the scalaris group, H. rossi and H. mississippiensis, and their distributional patterns are discussed. RP FLINT, OS (reprint author), SMITHSONIAN INST,DEPT ENTOMOL,WASHINGTON,DC 20560, USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 SN 0028-7199 J9 J NEW YORK ENTOMOL S JI J. N.Y. Entomol. Soc. PD APR PY 1992 VL 100 IS 2 BP 320 EP 324 PG 5 WC Entomology SC Entomology GA HQ231 UT WOS:A1992HQ23100011 ER PT J AU BUSH, MB AF BUSH, MB TI A SIMPLE YET EFFICIENT POLLEN TRAP FOR USE IN VEGETATION STUDIES SO JOURNAL OF VEGETATION SCIENCE LA English DT Article RP BUSH, MB (reprint author), SMITHSONIAN TROP RES INST,0948 UNIT,APO AA 34002-0948,POB 2072,BALBOA,PANAMA. NR 0 TC 17 Z9 18 U1 0 U2 3 PU OPULUS PRESS UPPSALA AB PI KNIVSTA PA APELSINVAGEN 47, S 741 00 KNIVSTA, SWEDEN SN 1100-9233 J9 J VEG SCI JI J. Veg. Sci. PD APR PY 1992 VL 3 IS 2 BP 275 EP 276 DI 10.2307/3235691 PG 2 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA HX617 UT WOS:A1992HX61700018 ER PT J AU GALLEGOS, CL AF GALLEGOS, CL TI PHYTOPLANKTON PHOTOSYNTHESIS, PRODUCTIVITY, AND SPECIES COMPOSITION IN A EUTROPHIC ESTUARY - COMPARISON OF BLOOM AND NON-BLOOM ASSEMBLAGES SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article ID SPECTRAL ABSORPTION-COEFFICIENTS; MARINE-PHYTOPLANKTON; PHYSICAL VARIABILITY; CELL-SIZE; GROWTH; LIGHT; IRRADIANCE; PARAMETERS; COASTAL; SEA AB During 2 periods in the late spring and early summer 1989, blooms in the Rhode River, Maryland, USA, were triggered by nutrient inputs from local and remote watersheds. Parameters of the photosynthesis-irradiance relationship increased in May when the bloom was dominated by Thalassiosira pseudonana, and decreased in June when the bloom was dominated by large dinoflagellates. Relative variability of quantum efficiency was as great as that of chlorophyll-specific absorption coefficient. Light-saturated photosynthesis rates were predictable based on species counts and previously published size-dependent, nutrient-saturated growth rates for diatoms and dinoflagellates. Dinoflagellate blooms occur in years of high hydrologic nutrient input, but, due to the reduced photosynthetic efficiency of the dinoflagellate blooms, carbon fixation in the system varies proportionately less than biomass. RP GALLEGOS, CL (reprint author), SMITHSONIAN ENVIRONM RES CTR, POB 28, EDGEWATER, MD 21037 USA. OI Gallegos, Charles/0000-0001-5112-0166 NR 46 TC 45 Z9 45 U1 1 U2 2 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD APR PY 1992 VL 81 IS 3 BP 257 EP 267 DI 10.3354/meps081257 PG 11 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA HV529 UT WOS:A1992HV52900005 ER PT J AU RALLS, K SINIFF, DB DOROFF, A MERCURE, A AF RALLS, K SINIFF, DB DOROFF, A MERCURE, A TI MOVEMENTS OF SEA OTTERS RELOCATED ALONG THE CALIFORNIA COAST SO MARINE MAMMAL SCIENCE LA English DT Note C1 UNIV MINNESOTA,DEPT ECOL EVOLUT & BEHAV,MINNEAPOLIS,MN 55455. US FISH & WILDLIFE SERV,ANCHORAGE,AK 99503. RP RALLS, K (reprint author), SMITHSONIAN INST,NATL 200L PK,WASHINGTON,DC 20008, USA. NR 9 TC 9 Z9 9 U1 1 U2 4 PU SOC MARINE MAMMALOGY PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 SN 0824-0469 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD APR PY 1992 VL 8 IS 2 BP 178 EP 184 DI 10.1111/j.1748-7692.1992.tb00380.x PG 7 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA HR283 UT WOS:A1992HR28300012 ER PT J AU RAWLINGS, JMC HARTQUIST, TW MENTEN, KM WILLIAMS, DA AF RAWLINGS, JMC HARTQUIST, TW MENTEN, KM WILLIAMS, DA TI DIRECT DIAGNOSIS OF INFALL IN COLLAPSING PROTOSTARS .1. THE THEORETICAL IDENTIFICATION OF MOLECULAR-SPECIES WITH BROAD VELOCITY DISTRIBUTIONS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article ID DENSE INTERSTELLAR CLOUDS; SOLAR-TYPE STARS; SPHERICAL-SYMMETRY; DARK CLOUDS; GRAINS; CHEMISTRY; EVOLUTION; AMMONIA; MODELS; CORES AB We have developed chemical models, including depletion on to grains, for the collapsing envelopes of protostars. Our primary goal has been to identify molecular species having broad velocity distributions, so that observations of their line profiles can be employed to diagnose the dynamics of protostar formation, and to yield information on the collapse age and depletion rate. Previously obtained data for NH3 emission lines, from a number of dark cores with embedded protostars, have shown no clear evidence for systematic collapse. Results from our model indicate that the collapse initiates very soon after the formation of an isothermal pressure-balanced sphere. The collapse is preceded by a period of exceptional quiescence. We demonstrate here that as depletion reduces the fractional abundance of NH3 in the accelerating gas of an infalling envelope and prevents the formation of broad wings on NH3 emission lines, the fractional abundances of some other species initially increase as the heavy elements become depleted, leading those species to have emission lines broader than those of NH3. CH is an observable species which, for a large variety of conditions, possesses a fairly constant or increasing fractional abundance in collapsing envelope gas in which depletion is occurring. High angular resolution observations of CH would be very desirable, but would require appropriate instrumentation on an array, or perhaps the Arecibo telescope. When the water abundance is sufficiently high in the outer envelope, so that many molecular ions are removed primarily in reactions with it rather than by dissociative recombination, the abundances of HCO+, N2H+ and H2S rise when collapse and depletion occur. Millimetre lines from these species can be observed with single-dish telescopes at higher angular resolution than can NH3, resulting in their lines having broader wings in spatially resolved sources than those of NH3, even when their abundances relative to NH3 do not increase substantially in the infall. HCO is a particularly interesting species, because its abundance ratio relative to HCO+ increases with growing density if the fractional abundance of gas-phase heavy metals remains constant. Also, HCO line emission can be observed with high angular resolution. C1 UNIV OXFORD,DEPT PHYS ASTROPHYS,NUCL PHYS LAB,OXFORD OX1 3RH,ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV MANCHESTER,INST SCI & TECHNOL,DEPT MATH,MANCHESTER M60 1QD,LANCS,ENGLAND. RP RAWLINGS, JMC (reprint author), MAX PLANCK INST PHYS & ASTROPHYS,W-8046 GARCHING,GERMANY. NR 30 TC 160 Z9 160 U1 0 U2 16 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 APR 1 PY 1992 VL 255 IS 3 BP 471 EP 485 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HL902 UT WOS:A1992HL90200014 ER PT J AU WRIGHT, SJ MACHADO, JL MULKEY, SS SMITH, AP AF WRIGHT, SJ MACHADO, JL MULKEY, SS SMITH, AP TI DROUGHT ACCLIMATION AMONG TROPICAL FOREST SHRUBS (PSYCHOTRIA, RUBIACEAE) SO OECOLOGIA LA English DT Article DE DRY SEASON; IRRIGATION; OSMOTIC ADJUSTMENT; PHENOLOGY; PRESSURE-VOLUME CURVES ID TISSUE WATER RELATIONS; REVISION; EVERGREEN; PANAMA AB Mechanisms of dry-season drought resistance were evaluated for five evergreen shrubs (Psychotria, Rubiaceae) which occur syntopically in tropical moist forest in central Panama. Rooting depths, leaf conductance, tissue osmotic potentials and elasticity, and the timing of leaf production were evaluated. From wet to dry season, tissue osmotic potentials declined and moduli of elasticity increased in four and five species, respectively. Irrigation only affected osmotic adjustment by P. furcata. The other seasonal changes in leaf tissue properties represented ontogenetic change. Nevertheless, they made an important contribution to dry-season turgor maintenance. Small between-year differences in dry season rainfall had large effects on plant water status. In 1986, 51 mm of rain fell between 1 January and 31 March, and pre-dawn turgor potentials averaged < 0.1 MPa for all five Psychotria species in March (Wright 1991). In 1989, 111 mm of rain fell in the same period, pre-dawn turgor potentials averaged from 0.75 to 1.0 MPa for three of the species in April, and only P. chagrensis lost turgor. The relation between leaf production and drought differed among species. P. limonensis was buffered against drought by the lowest dry-season conductances and the deepest roots (averaging 244% deeper than its congeners) and was the only species to produce large numbers of leaves in the dry season. P. chagrensis was most susceptible to drought, and leaf production ceased as turgor loss developed. For the other species, water stress during severe dry seasons may select against dry-season leaf production. C1 UNIV VERMONT,PROCTOR MAPLE RES CTR,UNDERHILL CTR,VT 05490. UNIV MISSOURI,DEPT BIOL,ST LOUIS,MO 63121. RP WRIGHT, SJ (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 31 TC 37 Z9 41 U1 1 U2 10 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0029-8549 J9 OECOLOGIA JI Oecologia PD APR PY 1992 VL 89 IS 4 BP 457 EP 463 PG 7 WC Ecology SC Environmental Sciences & Ecology GA HL791 UT WOS:A1992HL79100001 PM 28311873 ER PT J AU SMITH, LD AF SMITH, LD TI THE IMPACT OF LIMB AUTOTOMY ON MATE COMPETITION IN BLUE CRABS CALLINECTES-SAPIDUS RATHBUN SO OECOLOGIA LA English DT Article DE AUTOTOMY; BLUE CRABS; MATE COMPETITION; PAIRING PRECEDENCE; BODY SIZE ID SEXUAL SELECTION; HOMARUS-AMERICANUS; AGONISTIC BEHAVIOR; MATING SUCCESS; TAIL AUTOTOMY; SIZE; REGENERATION; SALAMANDER; STRATEGIES; DIMORPHISM AB This study is the first to demonstrate experimentally that autotomy (self-amputation of a body part) adversely affects competition for mates. Experiments were conducted using blue crabs Callinectes sapidus Rathbun to examine the consequences of limb loss and pairing precedence on mate acquisition by males. Two adult males of equivalent size were introduced sequentially into pools containing a sexually-receptive female and observed after 24 h and 48 h. One male in each pair was left intact, while the other experienced: (1) no autotomy, (2) autotomy of one cheliped, or (3) autotomy of both chelipeds, one walking leg, and one swimming leg. In the absence of a competitor (first 24 h), both intact and injured males established precopulatory embraces with females. Intact males were highly successful (84-95%) in defending females from intact or injured intruders in the second 24 h period. Both autotomy treatments, however, significantly reduced the ability of males to defend females from intact intruders. Females in experiments suffered greater frequency of limb loss than did males. In the field, paired blue crabs showed significantly higher incidence of limb loss than unpaired crabs. Limb loss frequency increases with body size, and field observations indicated that larger males may be more successful than smaller males in obtaining females. Both experimental manipulations and field studies provide strong evidence for mate competition in this ecologically and commercially important portunid species. C1 UNIV MARYLAND,DEPT ZOOL,COLLEGE PK,MD 20742. SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. NR 67 TC 50 Z9 53 U1 0 U2 11 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0029-8549 J9 OECOLOGIA JI Oecologia PD APR PY 1992 VL 89 IS 4 BP 494 EP 501 PG 8 WC Ecology SC Environmental Sciences & Ecology GA HL791 UT WOS:A1992HL79100007 PM 28311879 ER PT J AU SCOTT, TC SHERTZER, J MOORE, RA AF SCOTT, TC SHERTZER, J MOORE, RA TI ACCURATE FINITE-ELEMENT SOLUTIONS OF THE 2-BODY DIRAC-EQUATION SO PHYSICAL REVIEW A LA English DT Article AB A general analysis of the two-body Dirac equation is presented for the case of equal masses interacting via a static Coulomb potential. Radial equations are derived and their analytical structure is discussed. Standard analytical and perturbative methods have failed to provide solutions to the radial equations due to the presence of the singularity on the negative radial axis at roughly the distance of the classical electron radius. The exact radial equations are solved using finite-element analysis, and the low-lying bound states are obtained to an accuracy of one part in 10(18). The effect of the singularity is clearly seen in the structure of the finite-element radial components. C1 GUELPH WATERLOO PROGRAM GRAD WORK PHYS,WATERLOO N2L 3G1,ONTARIO,CANADA. COLL HOLY CROSS,DEPT PHYS,WORCESTER,MA 01610. RP SCOTT, TC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 19 TC 17 Z9 17 U1 0 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 APR 1 PY 1992 VL 45 IS 7 BP 4393 EP 4398 DI 10.1103/PhysRevA.45.4393 PN A PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA HN474 UT WOS:A1992HN47400027 ER PT J AU ALEXANDER, BA AF ALEXANDER, BA TI A CLADISTIC-ANALYSIS OF THE SUBFAMILY PHILANTHINAE (HYMENOPTERA, SPHECIDAE) SO SYSTEMATIC ENTOMOLOGY LA English DT Article AB The Philanthinae, as treated here, contains the eight valid genera Aphilanthops Patton, Cerceris Latreille, Clypeadon Patton, Eucerceris Cresson, Philanthinus Beaumont, Philanthus Fabricius, Pseudoscolia Radoszkowski and Trachypus Klug. Listropygia Bohart is synonymized with Clypeadon, syn.n. The genera Eremiasphecium Kohl and Odontosphex Arnold are removed from the Philanthinae and regarded as genera incertae sedis within Sphecidae. Analysis of the genera of this redefined subfamily Philanthinae finds two major clades whose monophyly is strongly supported: (Philanthinus + (Philanthus + Trachypus)) [= Tribe Philanthini] and (Pseudoscolia + (Cerceris + Eucerceris)) [= Tribe Cercerini]. There is some evidence for the monophyly of Clypeadon + Aphilanthops [= Tribe Aphilanthopini]. Cerceris and Philanthus are inferred to be paraphyletic with respect to Eucerceris and Trachypus, respectively. Philanthinus is removed from the tribe Aphilanthopini and placed in the tribe Philanthini, and the monotypic tribe Pseudoscoliini is synonymized with Cercerini. C1 SMITHSONIAN INST,WASHINGTON,DC 20560. RP ALEXANDER, BA (reprint author), UNIV KANSAS,SNOW ENTOMOL MUSEUM,SNOW HALL,LAWRENCE,KS 66045, USA. NR 29 TC 14 Z9 15 U1 0 U2 5 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0307-6970 J9 SYST ENTOMOL JI Syst. Entomol. PD APR PY 1992 VL 17 IS 2 BP 91 EP 108 DI 10.1111/j.1365-3113.1992.tb00324.x PG 18 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA HK897 UT WOS:A1992HK89700001 ER PT J AU RUMM, JC AF RUMM, JC TI KEEPING WATCH - A HISTORY OF AMERICAN TIME - OMALLEY,M SO TECHNOLOGY AND CULTURE LA English DT Book Review RP RUMM, JC (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 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD APR PY 1992 VL 33 IS 2 BP 366 EP 367 DI 10.2307/3105876 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA JE101 UT WOS:A1992JE10100020 ER PT J AU WHITE, JH AF WHITE, JH TI THE NORTH-CAROLINA RAILROAD, 1849-1871, AND THE MODERNIZATION OF NORTH-CAROLINA - TRELEASE,AW SO TECHNOLOGY AND CULTURE LA English DT Book Review RP WHITE, JH (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 APR PY 1992 VL 33 IS 2 BP 378 EP 378 DI 10.2307/3105884 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA JE101 UT WOS:A1992JE10100028 ER PT J AU PERIVOLAROPOULOS, L AF PERIVOLAROPOULOS, L TI LARGE-SCALE STRUCTURE BY GLOBAL MONOPOLES AND COLD DARK MATTER SO MODERN PHYSICS LETTERS A LA English DT Article AB A cosmological model in which the primordial perturbations are provided by global monopoles and in which the dark matter is cold has several interesting features. The model is normalized by choosing its single parameter within the bounds obtained from gravitational wave constraints and by demanding coherent velocity flows of about 600 km/sec on scales of 50 h-1 Mpc. Using this normalization, the model predicts the existence of dominant structures with mass 2 x 10(16) M. on a scale 35 h-1 Mpc, i.e., larger than the horizon at t(eq). The magnitude of the predicted mass function in the galactic mass range is in good agreement with the observed Schechter function. RP PERIVOLAROPOULOS, L (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,DIV THEORET ASTROPHYS,MS-51,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Perivolaropoulos, Leandros/0000-0001-9330-2371 NR 0 TC 2 Z9 2 U1 0 U2 0 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 MAR 28 PY 1992 VL 7 IS 10 BP 903 EP 910 DI 10.1142/S0217732392003542 PG 8 WC Physics, Nuclear; Physics, Particles & Fields; Physics, Mathematical SC Physics GA HP192 UT WOS:A1992HP19200010 ER PT J AU GABUZDA, DC CAWTHORNE, TV ROBERTS, DH WARDLE, JFC AF GABUZDA, DC CAWTHORNE, TV ROBERTS, DH WARDLE, JFC TI A SURVEY OF THE MILLIARCSECOND POLARIZATION PROPERTIES OF BL LACERTAE OBJECTS AT 5 GHZ SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL LACERTAE OBJECTS, GENERAL; GALAXIES, JETS; GRAVITATIONAL LENSING; POLARIZATION; RADIO CONTINUUM, GALAXIES ID SPECTRUM RADIO-SOURCES; LINEAR-POLARIZATION; LAC OBJECTS; RESOLUTION; OJ-287; MAPS; VLBI; AO-0235+164; ARTIFACTS; EMISSION AB Milliarcsecond resolution total intensity and linear polarization maps at 5 GHz are presented for 11 BL Lacertae objects, 10 of which have never before been mapped with polarization sensitivity and six of which have never before been mapped using VLBI. There are now 18 BL Lacertae objects for which information about the polarization of the emission on VLBI scales is available. In every BL Lacertae object in which we have detected polarization structure (0454 + 844, 0735 + 178, OJ287, 0954 + 658, 1219 + 285, 1538 + 149, 1803 + 784, 1823 + 568, and BL Lac), the polarization position angle in the knots is nearly parallel to the VLBI structural axis. In contrast, the direction of polarization in the cores of these sources appears to be random. One likely explanation for the preferred polarization direction in the jets is that plane perpendicular shock waves are common in these sources; the origin of the absence of preferred polarization direction in the core components is not clear. These results strengthen our earlier conclusion that it cannot be the case that a significant number of BL Lacertae objects are gravitationally microlensed images of more distant quasars, since the characteristic VLBI polarization structures observed in these two types of object are very different. C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. BRANDEIS UNIV,DEPT PHYS,WALTHAM,MA 02254. RP GABUZDA, DC (reprint author), UNIV CALGARY,DEPT PHYS & ASTRON,CANADIAN NETWORK SPACE RES,2500 UNIV DR NW,CALGARY T2N 1N4,ALBERTA,CANADA. NR 52 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 MAR 20 PY 1992 VL 388 IS 1 BP 40 EP 54 DI 10.1086/171128 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HK566 UT WOS:A1992HK56600006 ER PT J AU DAVID, LP JONES, C FORMAN, W AF DAVID, LP JONES, C FORMAN, W TI X-RAY-PROPERTIES OF BRIGHT FAR-INFRARED GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, STELLAR CONTENT; INFRARED, GALAXIES; X-RAYS, GALAXIES ID SPIRAL GALAXIES; EMISSION; M82; SPECTRA; NUCLEUS; NGC-253; NGC-1068; QUASARS; SAMPLE; WIND AB We have searched the Einstein data base for observations of galaxies in the IRAS Bright Galaxy Sample. Of the 324 galaxies in this sample, 81 were observed with the Imaging Proportional Counter, and 51 were detected at greater than a 3-sigma confidence level. A strong correlation exists between the far-infrared and X-ray luminosities among the normal and starburst (NSB) galaxies with, L(X) is-proportional-to L(fir)0.90-1.01 (90% confidence limits). The X-ray luminosity of the 10 Seyfert galaxies in this sample is a factor of approximately 10 greater than the NSB galaxies with the same far-infrared luminosity. The relation between the X-ray and blue luminosity of the NSB galaxies is also consistent with a linear relation. L(X) is-proportional-to L(B)1.03-1.18 (90% confidence limits) but exhibits increasing scatter with increasing L(B). In fact, the residuals in L(X) around the best-fit relation are strongly correlated with the ratio L(fir)/L(B), which is a measure of the current star formation rate. These correlations in the NSB sample can be understood through a two-component model for the X-ray emission from spirals. One component consists of relatively old objects (Type I supernovae and low-mass X-ray binaries) and is proportional to L(B), while the second component comprises young objects (Type II supernovae, O stars, and high-mass X-ray binaries) and is proportional to the far-infrared luminosity from active regions of star formation. The first component dominates in more quiescent galaxies, while the second component dominates in starburst galaxies. We find that the efficiency of X-ray production through star formation is nearly independent of the star formation rate with 10(47.5) ergs of energy (between 0.5 and 4.5 keV) produced for each solar mass consumed into stars. On energetic grounds alone, we find that the integrated emission from individual Type II supernova remnants and O star atmospheres can only account for approximately 10% and 30% of the total observed X-ray luminosity from starburst galaxies. The observed X-ray luminosity of starbursts can be accounted for by high-mass X-ray binaries if approximately 4% of the newly formed O stars reside in such systems or by gas collectively heated by supernovae. Our results also show that the X-ray emission from bright far-infrared galaxies can make a significant contribution to the observed X-ray background. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP DAVID, LP (reprint author), SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 48 TC 162 Z9 162 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 MAR 20 PY 1992 VL 388 IS 1 BP 82 EP 92 DI 10.1086/171131 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HK566 UT WOS:A1992HK56600009 ER PT J AU SEIDENSTICKER, J AF SEIDENSTICKER, J TI THE NATURAL-HISTORY OF THE WILD CATS - KITCHENER,A SO SCIENCE LA English DT Book Review RP SEIDENSTICKER, J (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 1 TC 0 Z9 0 U1 1 U2 6 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD MAR 20 PY 1992 VL 255 IS 5051 BP 1588 EP 1589 DI 10.1126/science.255.5051.1588 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA HJ809 UT WOS:A1992HJ80900051 PM 17820176 ER PT J AU KUTZELNIGG, W MORGAN, JD AF KUTZELNIGG, W MORGAN, JD TI RATES OF CONVERGENCE OF THE PARTIAL-WAVE EXPANSIONS OF ATOMIC CORRELATION ENERGIES SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID GAUSSIAN-TYPE GEMINALS; PAIR FUNCTIONS; PERTURBATION-THEORY; BASIS-SET; SYSTEMS; 1/Z AB The coefficients of the leading terms of the partial-wave expansion of atomic correlation energies in powers of (l + 1/2)-1 are derived for the second- and third-order perturbed energies in the 1/Z expansion for all possible states of two-electron atoms, and for second-order Moller-Plesset (many-body perturbation) theory for arbitrary n-electron atoms. The expressions for these coefficients given in Table I involve simple integrals over the zeroth-order wave functions (for the third order energies first-order wave functions are also involved). The leading term of E(2) goes as (l + 1/2)-4 for natural parity singlet states, as (l + 1/2)-6 for triplet states, and as (l + 1/2)-8 for unnatural parity singlet states. There are no odd powers of (l + 1/2)-1 present in E(2), and the coefficient of the (l + 1/2)-6 term for natural parity singlet states of two-electron systems in the 1/Z expansion is generally -5/4 times the coefficient of the (l + 1/2)-4 term. In E(3) there are terms that go as odd powers of (l + 1/2)-1; the leading term is expressible in terms of the zeroth-order wave function and goes as (l + 1/2)-5 for natural parity singlet states, as (l + 1/2)-7 for triplet states, and as (l + 1/2)-9 for unnatural parity singlet states. Numerical values of the coefficients for E(2) in two-electron atoms are given in Table II. The relation of our results to those obtained by Hill for variational calculations on the He ground state is discussed and generalizations of Hill's formulas are conjectured. The unexpected results for unnatural parity singlet states are traced back to the behavior of their wave functions at the point of coalescence of two electrons. In terms of the relative coordinate of the two electrons they represent d waves, in contrast to s waves for natural parity singlet states and p waves for triplet states of either parity. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOLEC PHYS, CAMBRIDGE, MA 02138 USA. HARVARD UNIV, DEPT CHEM, CAMBRIDGE, MA 02138 USA. HARVARD UNIV, DEPT PHYS, CAMBRIDGE, MA 02138 USA. UNIV DELAWARE, DEPT PHYS & ASTRON, NEWARK, DE 19716 USA. RP KUTZELNIGG, W (reprint author), RUHR UNIV BOCHUM, LEHRSTUHL THEORET CHEM, W-4630 BOCHUM, GERMANY. NR 38 TC 345 Z9 346 U1 1 U2 22 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD MAR 15 PY 1992 VL 96 IS 6 BP 4484 EP 4508 DI 10.1063/1.462811 PG 25 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA HK019 UT WOS:A1992HK01900047 ER PT J AU GRAVES, GR BRAUN, MJ AF GRAVES, GR BRAUN, MJ TI MUSEUMS - STOREHOUSES OF DNA SO SCIENCE LA English DT Letter RP GRAVES, GR (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,WASHINGTON,DC 20560, USA. NR 4 TC 13 Z9 14 U1 1 U2 1 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD MAR 13 PY 1992 VL 255 IS 5050 BP 1335 EP 1336 DI 10.1126/science.255.5050.1335-d PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA HH744 UT WOS:A1992HH74400006 PM 1542783 ER PT J AU VEGAPEREZ, LA BOWMAN, TE AF VEGAPEREZ, LA BOWMAN, TE TI DESCRIPTION OF THE PELAGIC COPEPOD, CTENOCALANUS-HERONAE VEGA-PEREZ AND BOWMAN, FROM OFF SAO-PAULO, BRAZIL (CALANOIDA, CLAUSOCALANIDAE) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Ctenocalanus heronae is described from Atlantic waters of the Ubatuba region, Sao Paulo state, Brazil. It is distinguished by its short antennae 1, the form of the genital segment, and the number and form of the ctenospines on leg 4. C1 SMITHSONIAN INST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560. RP VEGAPEREZ, LA (reprint author), UNIV SAO PAULO,INST OCEANOG,CIDADE UNIV BUTANTA,CAIXA POSTAL 9075,BR-05508 SAO PAULO,BRAZIL. NR 19 TC 3 Z9 3 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 MAR 12 PY 1992 VL 105 IS 1 BP 97 EP 101 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA HW186 UT WOS:A1992HW18600014 ER PT J AU DUPREE, AK SASSELOV, DD LESTER, JB AF DUPREE, AK SASSELOV, DD LESTER, JB TI DISCOVERY OF A FAST WIND FROM A FIELD POPULATION-II GIANT STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE GLOBULAR CLUSTERS, GENERAL; STARS, CHROMOSPHERES; STARS, GIANT; STARS, INDIVIDUAL (HD-6833); STARS, MASS LOSS; STARS, POPULATION-II ID CLUSTER RED GIANTS; MASS-LOSS; CHROMOSPHERIC LINE; GLOBULAR-CLUSTERS; SPECTRUM; PROFILES; HELIUM AB The He I lambda-10830 absorption in the metal-deficient field giant star HD 6833, extends to at least -90 km s-1, a value that is comparable to, or exceeds the escape velocity from the photosphere of the star. This spectrum provides strong observational evidence for mass loss. Because this field giant is a surrogate for red giants in globular clusters, and a velocity of 90 km s-1 is larger than the central escape velocity from most globular clusters, this observation suggests that material lost from globular cluster stars may easily escape from the cluster, and thus resolve the dilemma of the missing interstellar medium in globular clusters. C1 UNIV TORONTO,ERINDALE COLL,DEPT ASTRON,MISSISSAUGA L5L 1C6,ONTARIO,CANADA. RP DUPREE, AK (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 39 TC 42 Z9 42 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 MAR 10 PY 1992 VL 387 IS 2 BP L85 EP L88 DI 10.1086/186311 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HF939 UT WOS:A1992HF93900008 ER PT J AU LATHAM, DW STEFANIK, RP MAZEH, T AF LATHAM, DW STEFANIK, RP MAZEH, T TI SPECTROSCOPIC SEARCHES FOR LOW-MASS COMPANIONS OF STARS SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 40TH CONGRESS OF THE INTERNATIONAL ASTRONAUTICAL FEDERATION CY OCT 07-13, 1989 CL MALAGA, SPAIN SP INT ASTRONAUT FEDERAT AB For several years we have monitored the radial velocities of hundreds of late-type stars. The typical precision for a single measurement can be better than 500 m s-1. Five main samples of stars have been observed extensively; two-dozen nearby early M dwarfs together with an equal number of comparison stars, 250 stars in a magnitude-limited sample at the north Galactic pole, a dozen radial-velocity standard stars, 100 stars in the old open cluster M 67, and 1500 dwarfs in a survey of proper-motion stars. In this paper we present low-amplitude orbital solutions for some of the stars in these samples. Perhaps our best case is the solar-type star HD 114762, which undergoes periodic variations in radial velocity which we attribute to orbital motion due to an unseen companion. The rather short period of 84 days places the companion in an orbit similar to that of Mercury around the sun, while the rather low velocity amplitude of about 600 m s-1 implies that the mass of the companion may be as low as 0.011 solar masses, or 11 Jupiter masses. RP LATHAM, DW (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 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 MAR-APR PY 1992 VL 26 IS 3-4 BP 145 EP 149 DI 10.1016/0094-5765(92)90086-X PG 5 WC Engineering, Aerospace SC Engineering GA JF917 UT WOS:A1992JF91700004 ER PT J AU SINGLETON, T AF SINGLETON, T TI THE OLD VILLAGE AND THE GREAT HOUSE - AN ARCHAEOLOGICAL AND HISTORICAL EXAMINATION OF DRAX-HALL-PLANTATION, ST-ANNS BAY, JAMAICA - ARMSTRONG,DV SO AMERICAN ANTHROPOLOGIST LA English DT Book Review RP SINGLETON, T (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 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 MAR PY 1992 VL 94 IS 1 BP 206 EP 207 DI 10.1525/aa.1992.94.1.02a00460 PG 2 WC Anthropology SC Anthropology GA HJ260 UT WOS:A1992HJ26000050 ER PT J AU HOOVER, CA AF HOOVER, CA TI THE PIANO IN AMERICA, 1890-1940 - ROELL,CH SO AMERICAN MUSIC LA English DT Book Review RP HOOVER, CA (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV ILLINOIS PRESS PI CHAMPAIGN PA 1325 S OAK ST, CHAMPAIGN, IL 61820 SN 0734-4392 J9 AM MUSIC JI Am. Music PD SPR PY 1992 VL 10 IS 1 BP 100 EP 102 DI 10.2307/3052149 PG 3 WC Music SC Music GA JL752 UT WOS:A1992JL75200010 ER PT J AU HOOVER, CA AF HOOVER, CA TI STEINWAY - RATCLIFFE,RV SO AMERICAN MUSIC LA English DT Book Review RP HOOVER, CA (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV ILLINOIS PRESS PI CHAMPAIGN PA 1325 S OAK ST, CHAMPAIGN, IL 61820 SN 0734-4392 J9 AM MUSIC JI Am. Music PD SPR PY 1992 VL 10 IS 1 BP 100 EP 102 DI 10.2307/3052149 PG 3 WC Music SC Music GA JL752 UT WOS:A1992JL75200009 ER PT J AU JOHNSON, PJ AF JOHNSON, PJ TI OJIBWAY MUSIC FROM MINNESOTA - A CENTURY OF SONG FOR VOICE AND DRUM + VENNUM,T - MINNESOTA-HISTORICAL-SOCIETY-C-003 SO AMERICAN MUSIC LA English DT Record Review RP JOHNSON, PJ (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV ILLINOIS PRESS PI CHAMPAIGN PA 1325 S OAK ST, CHAMPAIGN, IL 61820 SN 0734-4392 J9 AM MUSIC JI Am. Music PD SPR PY 1992 VL 10 IS 1 BP 103 EP 106 DI 10.2307/3052150 PG 4 WC Music SC Music GA JL752 UT WOS:A1992JL75200011 ER PT J AU JOHNSON, PJ AF JOHNSON, PJ TI NORWEGIAN-AMERICAN MUSIC FROM MINNESOTA - OLD-TIME AND TRADITIONAL FAVORITES + NUSBAUM,P - MINNESOTA-HISTORICAL-SOCIETY-C-002 SO AMERICAN MUSIC LA English DT Record Review RP JOHNSON, PJ (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV ILLINOIS PRESS PI CHAMPAIGN PA 1325 S OAK ST, CHAMPAIGN, IL 61820 SN 0734-4392 J9 AM MUSIC JI Am. Music PD SPR PY 1992 VL 10 IS 1 BP 103 EP 106 DI 10.2307/3052150 PG 4 WC Music SC Music GA JL752 UT WOS:A1992JL75200012 ER PT J AU BENEDICT, GF HIGDON, JL TOLLESTRUP, EV HAHN, JM HARVEY, PM AF BENEDICT, GF HIGDON, JL TOLLESTRUP, EV HAHN, JM HARVEY, PM TI NGC-4314 .1. VISIBLE AND SHORT-WAVELENGTH INFRARED SURFACE PHOTOMETRY OF THE NUCLEUS AND BAR SO ASTRONOMICAL JOURNAL LA English DT Article ID SPIRAL GALAXY NGC-1097; STAR FORMATION; STANDARD STARS; MOLECULAR RING; CENTRAL REGION; DYNAMICS; EMISSION; GAS; LUMINOSITY; KINEMATICS AB We present BVI (TI CCD) and JHK (University of Texas IR Camera) surface photometry of NGC 4314, an SB (rs)ap anemic spiral with a nuclear ring containing recent star formation. The shortwave IR (SWIR) frames reveal a nuclear bar of length 2 arcsec at P.A. = 0-degrees. The nuclear ring and associated dust have been detected in all SWIR color indices. We have detected a nuclear spiral in the visible and SWIR just exterior to the ring. We find extremely low amplitude spiral-shaped deficits in the stellar distribution in the SWIR in this same region. We attribute these to dust, since CO is detectable at or near these locations. Average minor-axis profiles show this galaxy to have a nuclear bulge obeying the de Vaucouleurs r1/4 law for values of 2 < r < 7 arcsec. Away from the dust lanes and patches, the bar is shown to have an exponential cross section. We find that the extinction characteristics of a dusty region in the bar are similar to those of dust in our Galaxy. We have determined extinction and scattering characteristics of dust near the sites of recent star formation in the nuclear ring. Because of scattering, the I - J color index best maps dust near the nuclear ring. Unsharp masking techniques reveal structure all along the bar. The dust lanes associated with the bar terminate well before the ends of the bar and appear to turn back toward the galaxy center. We argue that some of the structure in the bar can be explained as resonance phenomena. We also interpret multiple peaks within previously published CO spectra as gas streaming along the dust lanes in the bar. Shocks at the intersection points of the gas in the bar dust lanes and the gas in the rotating inner ring are a likely explantation for the ring of star formation. We discuss several mechanisms capable of forming and maintaining the nuclear spiral found just outside the nuclear ring. No one mechanism compellingly explains this spiral. C1 UNIV TEXAS,DEPT ASTRON,AUSTIN,TX 78712. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV NOTRE DAME,DEPT PHYS,NOTRE DAME,IN 46556. RP BENEDICT, GF (reprint author), UNIV TEXAS,MCDONALD OBSERV,AUSTIN,TX 78712, USA. NR 71 TC 29 Z9 29 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 MAR PY 1992 VL 103 IS 3 BP 757 EP & DI 10.1086/116099 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HE673 UT WOS:A1992HE67300006 ER PT J AU CALDWELL, N ARMANDROFF, TE SEITZER, P DACOSTA, GS AF CALDWELL, N ARMANDROFF, TE SEITZER, P DACOSTA, GS TI THE DWARF SPHEROIDAL COMPANIONS TO M31 - SURFACE-BRIGHTNESS PROFILES SO ASTRONOMICAL JOURNAL LA English DT Article ID ELLIPTICAL GALAXIES; STELLAR POPULATIONS; GLOBULAR-CLUSTERS; NONLUMINOUS MATTER; GIANT BRANCH; PHOTOMETRY; FORNAX; VIRGO; SPECTROSCOPY; PARAMETERS AB We present CCD images and surface photometry for the three dwarf spheroidal companions to M31. The derived light profiles are the most accurate to date for galaxies of this type and serve to define the faint end of the surface-brightness-luminosity relation for early type dwarfs. We also compute new structural parameters for a subset of the Galactic dwarf spheroidals, which indicate, when compared to the M31 dwarfs, that both sets of dwarf galaxies are similar. A B - V color is measured for And I and found to be in accord with that expected from the metallicity derived by Mould and Kristian from their color-magnitude diagram study. However, to a high degree of accuracy, we rule out their claim of a color gradient in this galaxy. The metallicity-luminosity relation for E galaxies is investigated using these and other new data. The results suggest that a change in slope occurs between the dwarfs (Z approximately L0.4) and the more luminous E galaxies (Z approximately L0.6). Furthermore, our results, together with other available data, confirm earlier suggestions that the correlation between central surface brightness and luminosity for dE galaxies breaks down for central surface brightnesses fainter than approximately 24th V mag per square arcsec; below this limit dE galaxies are found over a wide range of luminosities. C1 SMITHSONIAN INST,FI WHIPPLE OBSERV,AMADO,AZ 85645. UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. ANGLO AUSTRALIAN OBSERV,EPPING,NSW 2121,AUSTRALIA. NR 59 TC 103 Z9 103 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 MAR PY 1992 VL 103 IS 3 BP 840 EP & DI 10.1086/116105 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HE673 UT WOS:A1992HE67300012 ER PT J AU ZSOLDOS, E SASSELOV, DD AF ZSOLDOS, E SASSELOV, DD TI THE PULSATIONS OF YELLOW SEMIREGULAR VARIABLES .1. DOUBLE-MODE BEHAVIOR OF UU-HERCULIS SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE VARIABLE; STARS, OSCILLATIONS OF; UU HER ID SEMI-REGULAR VARIABLES; RV-TAURI; FOURIER-ANALYSIS; STELLAR MODELS; STARS; HD-161796 AB Long series of visual and photoelectric observations of UU Her since 1908 has been analysed. It is shown that UU Her is a double-mode semiregular variable, the two excited modes of pulsation are probably the fundamental and the first overtone. A simple model is presented to explain the amplitude variations observed in both modes. The model which assumes pure sinusoidal amplitude variation is quite successful in explaining the power spectrum of the variable. The question of the mass of UU Her is also discussed. It is argued that no observation of the star so far points unambiguously to its having a low mass. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP ZSOLDOS, E (reprint author), KONKOLY OBSERV BUDAPEST, POB 67, H-1525 BUDAPEST, HUNGARY. NR 55 TC 10 Z9 10 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 MAR PY 1992 VL 256 IS 1 BP 107 EP 112 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HH020 UT WOS:A1992HH02000017 ER PT J AU BODO, G FERRARI, A MASSAGLIA, S ROSSI, P SHIBATA, K UCHIDA, Y AF BODO, G FERRARI, A MASSAGLIA, S ROSSI, P SHIBATA, K UCHIDA, Y TI NONLINEAR EVOLUTION OF SYNCHROTRON THERMAL INSTABILITIES SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE MAGNETOHYDRODYNAMICS; RADIATION MECHANISMS, SYNCHROTRON RADIATION; PLASMAS; GALAXIES, JETS OF ID COOLING FLOWS; RADIO-SOURCES; MAGNETIC-FIELDS; CYGNUS-A; FILAMENTS; M87; JET AB We present a time-dependent, non-linear study of thermal instability in a magnetized plasma whose relativistic component supports the pressure and undergoes synchrotron losses while the thermal matter provides the inertia of the medium. We follow the temporal evolution of the instability in the non-linear regime by means of a one-dimensional, finite-difference MHD numerical code employing either free or periodic boundary conditions. We find that, in a plasma subject to constant heating, after an initial phase in which the instability growth rate follows the linear model, the instability reaches a quasi equilibrium state on timescales of the order of several synchrotron timescales. An essential condition for this instability to be efficient is that the plasma is out of equipartition with the relativistic particle energy exceeding the magnetic field energy. The mechanism considered can interpret the formation of filaments of enhanced emission observed, at high resolution, in lobes and jets of several extragalactic radio sources. C1 UNIV TURIN, IST FIS GEN, VIA P GIURIA 1, I-10125 TURIN, ITALY. UNIV TURIN, IST FIS MATEMAT, I-10123 TURIN, ITALY. UNIV TOKYO, DEPT ASTRON, BUNKYO KU, TOKYO 113, JAPAN. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RI Bodo, Gianluigi/F-9223-2012 OI Bodo, Gianluigi/0000-0002-9265-4081 NR 25 TC 10 Z9 10 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 MAR PY 1992 VL 256 IS 2 BP 689 EP 700 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HL037 UT WOS:A1992HL03700047 ER PT J AU KENT, SM AF KENT, SM TI GALACTIC STRUCTURE FROM THE SPACELAB INFRARED TELESCOPE .3. A DYNAMIC-MODEL FOR THE MILKY-WAY BULGE SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXY KINEMATICS AND DYNAMICS ID MASSIVE BLACK-HOLE; SPIRAL GALAXIES; SPHERICAL GALAXIES; ELLIPTIC GALAXIES; ROTATION CURVE; NUCLEAR BULGE; DARK-MATTER; M GIANTS; KINEMATICS; DISK AB The Milky Way bulge is modeled as an oblate isotropic rotator with constant M/L ratio. A model with M/L2.2-mu-m) = 1 successfully reproduces a variety of stellar velocity dispersion measurements for 2 < R < 1200 pc. An observed increase in the stellar velocity dispersion inside 2 pc requires either that there be an additional central mass of order 3 x 10(6) M. or that the stellar motions become anisotropic there. The model has insufficient mass to reproduce the observed peak in the H I and CO rotation curve of 250 km s-1 at 300 pc; it is argued that the peak arises from noncircular gas motions and does not reflect the true mass of the bulge. C1 FERMI NATL ACCELERATOR LAB,BATAVIA,IL 60510. RP KENT, SM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MAIL STOP 20,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 64 TC 193 Z9 193 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 MAR 1 PY 1992 VL 387 IS 1 BP 181 EP 188 DI 10.1086/171070 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HF369 UT WOS:A1992HF36900016 ER PT J AU PRATAP, P SNYDER, LE BATRLA, W AF PRATAP, P SNYDER, LE BATRLA, W TI ARE THE NGC-7538 FORMALDEHYDE MASERS REALLY UNUSUAL SO ASTROPHYSICAL JOURNAL LA English DT Article DE H-II REGIONS; ISM INDIVIDUAL (NGC-7538); ISM MOLECULES; MASERS ID VLA OBSERVATIONS; H2CO MASER; EMISSION; AMMONIA; LINE AB The molecular cloud around NGC 7358 IRS 1 has been studied in order to understand the excitation conditions for the unusual H2CO masers. Maps in the J = 1 --> 0 transition of (CO)-C-13 indicate densities with a lower bound of approximately 2 x 10(3) cm-3 or more in the cloud around the H II region. The results from the study of various molecular transitions indicate that the conditions required by the Boland & de Jong model for the excitation of the H2CO maser are not very stringent or unique. The maser can be excited by a compact H II region which is optically thin at millimeter wavelengths. The H-2 density in the region should be approximately 10(4) cm-3 and the masing gas should be between 0.011 and 0.017 pc from the center of the H II region to produce the observed brightness temperature for the maser. C1 UNIV ILLINOIS,DEPT ASTRON,URBANA,IL 61801. FACHHSCH COBURG,ABT MUNCHBERG,W-8660 MUNCHBERG,GERMANY. RP PRATAP, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 20 TC 18 Z9 18 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 MAR 1 PY 1992 VL 387 IS 1 BP 241 EP 247 DI 10.1086/171075 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HF369 UT WOS:A1992HF36900021 ER PT J AU HUMMER, DG RYBICKI, GB AF HUMMER, DG RYBICKI, GB TI THE SOBOLEV APPROXIMATION FOR LINE FORMATION WITH PARTIAL FREQUENCY REDISTRIBUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE LINE FORMATION; RADIATIVE TRANSFER ID ESCAPE PROBABILITY; P METHOD; SCATTERING; RADIATION; FLOWS AB The formation of a spectral line in a uniformly expanding infinite medium is investigated in the Sobolev approximation with particular attention to the various mechanisms for frequency redistribution. Numerical and analytic solutions of the transfer equation are presented for a number of redistribution functions and their approximations, including type I and type II partial redistribution, coherent scattering and complete redistribution, and the Fokker-Planck and uncorrelated approximation to the R(II) function. The solutions for the mean intensity are shown to depend very much on the type of redistribution mechanism, while for the frequency-weighted mean intensity JBAR, which enters the rate equations, this dependence is weak. This implies that use of Sobolev escape probabilities based on complete redistribution can be an adequate approximation for many calculations for which only the radiative excitation rates are needed. However, it is shown that the criteria for applicability of Sobolev theory may be difficult to meet when transfer occurs primarily in the Voigt wings, especially for complete redistribution. C1 UNIV COLORADO,JOINT INST LAB ASTROPHYS,BOULDER,CO 80309. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 32 TC 15 Z9 15 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 MAR 1 PY 1992 VL 387 IS 1 BP 248 EP 257 DI 10.1086/171076 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HF369 UT WOS:A1992HF36900022 ER PT J AU HERANT, M BENZ, W AF HERANT, M BENZ, W TI POSTEXPLOSION HYDRODYNAMICS OF SN-1987A SO ASTROPHYSICAL JOURNAL LA English DT Article DE HYDRODYNAMICS; STARS INDIVIDUAL (SN-1987A); STARS INTERIORS; SUPERNOVAE GENERAL ID SUPERNOVA 1987A; CRAB-NEBULA; LIGHT-CURVE; X-RAY; LINE-PROFILES; LATE BEHAVIOR; SN 1987A; EMISSION; INSTABILITY; FILAMENTS AB We present a comprehensive study of the postexplosion hydrodynamics of the ejecta of SN 1987A, encompassing the Rayleigh-Taylor instabilities at the shell interfaces and the dynamical effects of the energy input due to the radioactive decay of N-56 and Co-56. In an attempt to explain the observed high-velocity wings of the iron line of SN 1987A, we investigate the dependence of the hydrodynamical behavior on progenitor structure, initial perturbations, explosion energy, and dimensionality of the numerical simulation. We show that none of these factors leads to the required high-velocity tail of iron, although we are able to reproduce the line core adequately. This failure points toward early instabilities which would premix the nickel outward during, or shortly after, the explosion itself, and therefore enable the nickel to participate in the subsequent round of Rayleigh-Taylor instabilities. By artificially premixing nickel in our initial model, we find that this early mixing has to affect the inner 1.5 M . of the ejecta to reproduce the high-velocity wings at a time of 90 days. We speculate that the high-entropy bubble associated with the delayed mechanism is responsible for this premixing by driving convective motions early in the explosion. C1 UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85724. RP HERANT, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 48 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 MAR 1 PY 1992 VL 387 IS 1 BP 294 EP 308 DI 10.1086/171081 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HF369 UT WOS:A1992HF36900027 ER PT J AU KETO, E BALL, R ARENS, J JERNIGAN, G MEIXNER, M AF KETO, E BALL, R ARENS, J JERNIGAN, G MEIXNER, M TI MIDINFRARED IMAGING OF MARKARIAN-231 AND ARP-220 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, NUCLEI ID BRIGHT GALAXY SAMPLE; CO EMISSION; RESOLUTION AB High angular resolution observations of Arp 220 and Mrk 231 provide images of the nuclei and show that the source of the strong mid-IR emission is confined to regions less than about 0".5 or 400 pc in diameter in Mrk 231 and less than 1".5 x 0".9 or 320 x 530 pc in Arp 220. If much of the far-IR emission also derives from such a small region, the implied radiation densities are quite high, equivalent to one O star pc-3. Although in normal galaxies the near-IR traces an older population of evolved, cool stars, such high radiation densities in the IR bright galaxies suggest the possibility that the spatial correlation observed between the near-IR, mid-IR, and radio may hold because emission in all three bands is associated with hot interstellar gas and dust. C1 UNIV HAWAII,NASA,INFRARED TELESCOPE FACIL,HONOLULU,HI 96822. UNIV CALIF BERKELEY,SPACE SCI LAB,BERKELEY,CA 94720. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. UNIV CALIF LAWRENCE LIVERMORE NATL LAB,INST GEOPHYS & PLANETARY PHYS,LIVERMORE,CA 94550. RP KETO, E (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 23 TC 15 Z9 15 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 MAR 1 PY 1992 VL 387 IS 1 BP L17 EP L19 DI 10.1086/186295 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HF370 UT WOS:A1992HF37000004 ER PT J AU MILONE, EF STAGG, CR KURUCZ, RL AF MILONE, EF STAGG, CR KURUCZ, RL TI THE ECLIPSING BINARY AI PHOENICIS - NEW RESULTS BASED ON AN IMPROVED LIGHT-CURVE ANALYSIS PROGRAM SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE BINARIES, ECLIPSING; STARS, ATMOSPHERES; STARS, INDIVIDUAL (AI PHOENICIS) ID STAR AB The 24.6 day eclipsing binary AI Phe contains two sharp-lined stars of comparable luminosity which undergo total eclipse, and yet are well separated. Radial velocity, photometric, and ultraviolet observations of this star have been remodeled using our improved version of the Wilson-Devinney code on the University of Calgary's Cyber 205 and Myrias SPS-2 computers. This version now has a new atmospheres option which makes use of Kurucz' model atmospheres to approximate the surface fluxes of the two stars. With the option, light curve fitting is now demonstrably improved for optical wavelengths. Rough empirical corrections result in still further improvement, with smaller discrepancies in U and u than are found using either the blackbody approximation or the previously used (Carbon-Gingerich) atmospheres option. For a specified temperature, wavelength, and log g, interpolation is performed within a table of values representing the ratio of blackbody to stellar atmosphere flux. The model atmosphere option simulates fluxes in Stromgren uvby or Johnson UBV bandpasses, as well as in other band-passes with widths DELTA-log-lambda = 0.1 in the range 0.316 to 3.550-mu-m, and DELTA-log-lambda = 0.05 in the UV (at 10 specified wavelengths from 0.100 to 0.282-mu-m). The limb darkening of the hotter component in the far UV as it undergoes total eclipse is also investigated and compared with Kurucz models. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MILONE, EF (reprint author), UNIV CALGARY,DEPT PHYS & ASTRON,ROTHNEY ASTROPHYS OBSERV,2500 UNIV DR NW,CALGARY T2N 1N4,ALBERTA,CANADA. NR 21 TC 52 Z9 53 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 MAR PY 1992 VL 79 IS 1 BP 123 EP 137 DI 10.1086/191647 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HE442 UT WOS:A1992HE44200006 ER PT J AU ZEH, DW ZEH, JA AF ZEH, DW ZEH, JA TI DISPERSAL-GENERATED SEXUAL SELECTION IN A BEETLE-RIDING PSEUDOSCORPION SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article ID NATURAL-SELECTION; BODY SIZE; DIMORPHISM; EVOLUTION; INSECTS; PROTANDRY; CONSEQUENCES; MAINTENANCE; STRATEGIES; CHARACTERS AB After several generations within a decaying tree (Ficus spp.), populations of the pseudoscorpion Cordylochernes scorpioides disperse by climbing under the elytra of harlequin beetles (Acrocinus longimanus) eclosing from the tree. Because the beetles then fly to newly-decaying Ficus for mating and oviposition, they act as effective dispersal agents. Field experiments and observations indicate that this dispersal mode has been exploited by males who compete to remain on a beetle as a strategic site for inseminating females dispersing on it and on other beetles. Whereas beetles just eclosed from old trees carried large, female-biased groups of dispersing pseudoscorpions, beetles captured after their maiden flight generally carried a single large male. Multivariate morphometric analyses indicated that these beetle-riding males were much larger than individuals randomly sampled from trees, with fighting traits exhibiting the greatest potential for selection (highest "phoretic" differentials). In females, sexual receptivity was significantly higher at the beginning of dispersal than at the end, suggesting that mating occurs on beetles. Field experiments confirmed that on-beetle insemination does take place and that small males are displaced from the "subelytral space" by larger rivals. By contrast, laboratory experiments suggest that large male size may not confer high mating success under the low-density conditions which characterize populations within trees. Thus, in addition to indicating a novel role for dispersal in the evolution of exaggerated male traits, this study suggests that oscillating sexual selection may be important in the maintenance of the extreme phenotypic variation exhibited by males of this species. RP ZEH, DW (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO AA 34002-0948,BALBOA,PANAMA. NR 57 TC 27 Z9 28 U1 0 U2 10 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 MAR PY 1992 VL 30 IS 2 BP 135 EP 142 PG 8 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA HH184 UT WOS:A1992HH18400008 ER PT J AU ZEH, DW ZEH, JA TAVAKILIAN, G AF ZEH, DW ZEH, JA TAVAKILIAN, G TI SEXUAL SELECTION AND SEXUAL DIMORPHISM IN THE HARLEQUIN BEETLE ACROCINUS-LONGIMANUS SO BIOTROPICA LA English DT Article ID NATURAL-SELECTION; CHARACTERS; EVOLUTION; SYSTEMS AB To investigate the causes of striking sexual dimorphism in the harlequin beetle (Acrocinus longimanus), we carried out a study of the behavior and morphology of two widely separated populations (in French Guiana and Panama). Males of this species possess greatly elongated forelegs which exhibit strong positive allometry with body size (elytra length). Males use their forelegs in fights with other males and in guarding females and oviposition sites. Field data on fighting and mating success suggest that sexual selection favors large size in males. However, the direct targets of selection were masked by high correlation between traits of the elytra, forelegs, and antennae. Sexual selection appears to be driven by intense male competition to monopolize suitable sites for egg deposition. Female harlequin beetles are highly selective in choosing only recently dead or dying trees for oviposition (Moraceae and Apocynaceae). Despite marked geographic variation in coloration, host trees, and climate, the two populations did not differ in mean size and extent of sexual dimorphism. We suggest that sexual selection in this species is sufficiently intense to override any effects of differing ecological factors. C1 ORSTOM,F-97323 CAYENNE,FRENCH GUIANA. RP ZEH, DW (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO AA 34002-0948,BALBOA,PANAMA. NR 37 TC 26 Z9 28 U1 1 U2 19 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 MAR PY 1992 VL 24 IS 1 BP 86 EP 96 DI 10.2307/2388476 PG 11 WC Ecology SC Environmental Sciences & Ecology GA HL369 UT WOS:A1992HL36900009 ER PT J AU COURTNEY, GW SMITH, IM AF COURTNEY, GW SMITH, IM TI 1ST RECORD OF LARVAL WATER MITES (ACARI, LEBERTIOIDEA, SPERCHONTIDAE) PARASITIC ON MOUNTAIN MIDGES (DIPTERA, DEUTEROPHLEBIIDAE) SO CANADIAN ENTOMOLOGIST LA English DT Note ID PARASITENGONA; ASSOCIATIONS C1 AGR CANADA,CTR LAND & BIOL RESOURCES RES,DIV BIOL RES,OTTAWA K1A 0C6,ONTARIO,CANADA. RP COURTNEY, GW (reprint author), SMITHSONIAN INST,DEPT ENTOMOL,NHB 169,WASHINGTON,DC 20560, USA. NR 11 TC 2 Z9 2 U1 0 U2 2 PU ENTOMOL SOC CANADA PI OTTAWA PA 393 WINSTON AVE, OTTAWA ON K2A 1Y8, CANADA SN 0008-347X J9 CAN ENTOMOL JI Can. Entomol. PD MAR-APR PY 1992 VL 124 IS 2 BP 421 EP 423 PG 3 WC Entomology SC Entomology GA HQ323 UT WOS:A1992HQ32300019 ER PT J AU ANSELL, HG ROBERTS, AC DUNN, PJ BIRCH, WD ANSELL, VE GRICE, JD AF ANSELL, HG ROBERTS, AC DUNN, PJ BIRCH, WD ANSELL, VE GRICE, JD TI FERRILOTHARMEYERITE, A NEW CA-ZN-FE3+ HYDROXYL ARSENATE FROM TSUMEB, NAMIBIA SO CANADIAN MINERALOGIST LA English DT Article DE FERRILOTHARMEYERITE; CALCIUM ZINC FERRIC IRON HYDROXYL ARSENATE; NEW MINERAL SPECIES; X-RAY DATA; CHEMICAL COMPOSITION; TSUMEB MINE; NAMIBIA ID LOTHARMEYERITE; KIPUSHITE AB Ferrilotharmeyerite occurs at the Tsumeb mine, Tsumeb, Namibia, as multiple subhedral crystallites and as tabular to wedge-or lozenge-shaped crystals associated with tennantite, scorodite, conichalcite, schneiderhohnite and beudantite. The mineral is monoclinic, space group C2, Cm or C2/m (diffraction aspect C*/*), with refined unit-cell parameters a 8.997(7), b 6.236(2), c 7.390(3) angstrom, beta 115.74(4)-degrees, V 373.5(5) angstrom 3, a:b:c 1.443:1:1.185, Z = 2. The strongest seven lines of the X-ray powder-diffraction pattern [d in angstrom (I)(hkl)] are: 4.95(70)(110), 3.398(100)(202BAR), 3.175(100)(112BAR), 2.938(100)(201), 2.823(70)(021), 2.702(70)(311BAR), 2.544(100)(221BAR). The crystallites are transparent to translucent, medium to brownish yellow with an adamantine to greasy lustre and a pale yellow streak. The mineral is brittle, with an uneven fracture and a good {001} cleavage. D(meas.) 4.25(5), D(calc.) 4.25 and 4.38 g/cm3 for two empirical formulas. Optically, the mineral is biaxial positive, with alpha 1.811(5), beta 1.844(5), gamma 1.88(1), 2V(meas.) 85(5)-degrees, 2V(calc.) 89-degrees, X approximately parallel-to a, Y parallel-to b. Pleochroism is strong: X olive green, Y pale green, Z colorless. Absorption is X > Y >> Z. Inclined dispersion of the optic axes is distinct, r > nu. The ideal chemical formula is Ca(Zn,Cu)(Fe3+,Zn)(AsO3OH)2(OH)3, derived from electron-microprobe analyses, water determination and microchemical tests. Ferrilotharmeyerite is the ferric iron analogue of lotharmeyerite, and is named to reflect this relationship. C1 SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560. MUSEUM VICTORIA,DEPT MINERAL & PETROL,MELBOURNE,VIC 3000,AUSTRALIA. CANADIAN MUSEUM NAT,MINERAL SCI SECT,OTTAWA K1P 6P4,ONTARIO,CANADA. RP ANSELL, HG (reprint author), GEOL SURVEY CANADA,601 BOOTH ST,OTTAWA K1A 0E8,ONTARIO,CANADA. NR 5 TC 1 Z9 1 U1 1 U2 2 PU MINERALOGICAL ASSOC CANADA PI NEPEAN PA CITYVIEW 78087, NEPEAN ON K2G 5W2, CANADA SN 0008-4476 J9 CAN MINERAL JI Can. Mineral. PD MAR PY 1992 VL 30 BP 225 EP 227 PN 1 PG 3 WC Mineralogy SC Mineralogy GA HU932 UT WOS:A1992HU93200017 ER PT J AU Whipple, FL AF Whipple, Fred L. TI THE ACTIVITIES OF COMETS RELATED TO THEIR AGING AND ORIGIN SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY LA English DT Article DE Comets; aging of comets; activity of comets ID SHORT-PERIOD COMETS; PLANETESIMALS; CLOUD AB Two indices have been developed for the purpose of comparing the natures of various classes of comets. The first is the Activity Index (AI), measuring the inherent magnitude increase in brightness from great solar distances to maximum near perihelion. The second, or Volatility Index (VI), measures the variation in magnitude near perihelion. Tentative determinations of these two indices are derived from observations by Max Beyer over more than 30 years for long-period (L-P) and short-period (S-P) comets near perihelion and from other homogeneous sources. AI determinations are made for 32 long-period (L-P) comets and for 14 short-period (S-P). The range of values of AI is of the order of 3 to 10 magnitudes with a median about 6. An expected strong correlation with perihelion distance q, is found to vary as similar to q(-2.3). Residuals from a least-square solution (Delta AI) are used for comparing comets of different orbital classes, the standard deviation of a single value of Delta AI is only +/- 1(m).1 for L-P comets and +/- 1(m).2 for S-P comets. Among the L-P cornets, 19 of period P larger than 104 years yield = 0(m).27 +/- 0(m).25 compared to 0(m).39 +/- 0(m).26 for 13 of period between 10(2) years and 10(4) years. This denies any fading with aging among the L-P comets. Also no systematic change with period occurs for the VI index, leading to the same conclusions. Weak correlations are found with the Gas/Dust ratio of comets. No correlations are found between the two indices, nor of either index with near-perihelion magnitudes or orbital inclination. The various data are consistent with a uniform origin for all types of comets, the nuclei being homogeneous on the large scale but quite diverse on a small scale (the order of a fraction of kilometer in extent). Small comets thus may sublimate away entirely, leaving no solid core, while huge comets may develop a less volatile core by radioactive heating and possibly become inactive like asteroids after many S-P revolutions about the Sun. When relatively new, huge comets may be quite active at great solar distances because of volatiles from the core that have refrozen in the outer layers. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Whipple, FL (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 33 TC 6 Z9 6 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-2958 J9 CELEST MECH DYN ASTR JI Celest. Mech. Dyn. Astron. PD MAR PY 1992 VL 54 IS 1-3 BP 1 EP 11 DI 10.1007/BF00049540 PG 11 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA V05NB UT WOS:000207131600002 ER PT J AU CHOPTUIK, MW GOLDWIRTH, DS PIRAN, T AF CHOPTUIK, MW GOLDWIRTH, DS PIRAN, T TI A DIRECT COMPARISON OF 2 CODES IN NUMERICAL RELATIVITY SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID EINSTEIN-SCALAR EQUATIONS; GRAVITATIONAL COLLAPSE; GENERALIZED SOLUTIONS; SYSTEMS; FIELD AB We discuss a detailed numerical comparison of the results of two codes which treat the same model problem in numerical relativity. The model consists of a single, massless scalar field minimally coupled to the gravitational field with a further restriction to spherical symmetry. The comparison was complicated by the fact that the codes were based on different formalisms, used different coordinate systems and employed different numerical solution techniques. After briefly reviewing the model and our basic solution methods we describe in detail the additional numerical analysis which enabled us to directly (event-by-event) compare our solutions. We also describe some new algorithms which use Richardson extrapolation to significantly increase the accuracy of one of the codes at a given resolution. Using the basic methodology of convergence testing, and with the aid of high-accuracy (better than 0.001%) numerical results (also generated using extrapolation techniques), we find clear evidence that both codes are convergent even in the regime where the field interactions are significantly non-linear and highly time-dependent. We suggest that techniques such as those described in this paper will be very useful for testing codes which solve more general problems in numerical relativity. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. HEBREW UNIV JERUSALEM,RACAH INST PHYS,IL-91904 JERUSALEM,ISRAEL. RP CHOPTUIK, MW (reprint author), CANADIAN INST THEORET ASTROPHYS,60 ST GEORGE ST,TORONTO M5S 1A1,ONTARIO,CANADA. NR 22 TC 11 Z9 11 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TECHNO HOUSE, REDCLIFFE WAY, BRISTOL, ENGLAND BS1 6NX SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD MAR PY 1992 VL 9 IS 3 BP 721 EP 750 DI 10.1088/0264-9381/9/3/013 PG 30 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA HJ138 UT WOS:A1992HJ13800013 ER PT J AU FERRARI, FD AF FERRARI, FD TI THE ANTENNAL EXOPOD OF NOODTORTHOPSYLLUS AND THE NEXT EVOLUTIONARY SYNTHESIS (COPEPODA) SO CRUSTACEANA LA English DT Article RP FERRARI, FD (reprint author), SMITHSONIAN INST,SMITHSONIAN OCEANOG SORTING CTR,WASHINGTON,DC 20560, USA. NR 26 TC 1 Z9 1 U1 0 U2 0 PU E J BRILL PI LEIDEN PA PO BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X J9 CRUSTACEANA JI Crustaceana PD MAR PY 1992 VL 62 BP 128 EP 132 DI 10.1163/156854092X00686 PN 2 PG 5 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA HQ959 UT WOS:A1992HQ95900003 ER PT J AU CRIST, RH OBERHOLSER, K MCGARRITY, J CRIST, DR JOHNSON, JK BRITTSAN, JM AF CRIST, RH OBERHOLSER, K MCGARRITY, J CRIST, DR JOHNSON, JK BRITTSAN, JM TI INTERACTION OF METALS AND PROTONS WITH ALGAE .3. MARINE-ALGAE, WITH EMPHASIS ON LEAD AND ALUMINUM SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article AB The proton uptake rate for intact cells of marine algae is 20 times faster than for freshwater (FW) species, partly due to a higher Na content, but also possibly due to differences in cell wall porosity. Metal displacement by protons on acidification (pH change from 7 to 1) shows two inflection ranges, one at ca. pH 5 due to the presence of carboxylate anions and the other at pH ca. 1.5 for sulfate groups. Cladophora, Rhizoclonium, and Polysiphonia each have the two inflection ranges, while Enteromorpha and freshwater Vaucheria (FW) each have only one, for sulfate and carboxylate, respectively. Sulfate analysis of Cladophora indicates a sulfate polymer content of ca. 8.2%, which is comparable to that estimated from metal release. Adsorption of Pb and Al on Rhizoclonium under acidic conditions (metals present as ions) releases H, Ca, and Mg ions from the algae, while adsorption of Pb and Cd at pH 10 and Al at pH 5, where these metal ions are present in very low concentration in equilibrium with solid hydroxide, also releases OH from the hydroxides. C1 GEORGETOWN UNIV,DEPT CHEM,WASHINGTON,DC 20057. SMITHSONIAN INST,MARINE SYST LAB,WASHINGTON,DC 20560. MESSIAH COLL,GRANTHAM,PA 17027. NR 17 TC 99 Z9 108 U1 2 U2 8 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD MAR PY 1992 VL 26 IS 3 BP 496 EP 502 DI 10.1021/es00027a007 PG 7 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA HG158 UT WOS:A1992HG15800014 ER PT J AU WASHBURN, WE AF WASHBURN, WE TI WHO WAS WHO IN NATIVE-AMERICAN HISTORY - INDIANS AND NON-INDIANS FROM EARLY CONTACTS THROUGH 1900 - WALDMAN,C SO ETHNOHISTORY 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 DUKE UNIV PRESS PI DURHAM PA BOX 90660, DURHAM, NC 27708-0660 SN 0014-1801 J9 ETHNOHISTORY JI Ethnohistory PD SPR PY 1992 VL 39 IS 2 BP 202 EP 203 DI 10.2307/482405 PG 2 WC Anthropology; History SC Anthropology; History GA JF493 UT WOS:A1992JF49300020 ER PT J AU STEWART, MM RAND, AS AF STEWART, MM RAND, AS TI DIEL VARIATION IN THE USE OF AGGRESSIVE CALLS BY THE FROG ELEUTHERODACTYLUS-COQUI SO HERPETOLOGICA LA English DT Article DE ANURA; ELEUTHERODACTYLUS-COQUI; AGGRESSIVE CALLS; DAWN-DUSK VOCALIZATION; BEHAVIOR ID NEOTROPICAL TREEFROG; HYLA-EBRACCATA; TERRITORIALITY; BEHAVIOR AB Males of Eleutherodactylus coqui, the Puerto Rican coqui, use multinote aggressive calls extensively at dawn and dusk and sporadically during the day. In April, most aggressive calls counted in a population were heard between 0545-0630 h and between 1800-1845 h. More aggressive calls were given per time period in the morning (maximum of 345/15 min period) than in the evening (maximum of 87/15 min period). Aggressive calls are used most frequently at times when frogs move into or out of diurnal retreats. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP STEWART, MM (reprint author), SUNY ALBANY,DEPT BIOL SCI,ALBANY,NY 12222, USA. NR 30 TC 16 Z9 17 U1 0 U2 0 PU HERPETOLOGISTS LEAGUE PI JOHNSON CITY PA EAST TENNESSEE STATE UNIV, DEPT BIOLOGICAL SCIENCES, BOX 70726, JOHNSON CITY, TN 37614-0726 SN 0018-0831 J9 HERPETOLOGICA JI Herpetologica PD MAR PY 1992 VL 48 IS 1 BP 49 EP 56 PG 8 WC Zoology SC Zoology GA HH080 UT WOS:A1992HH08000004 ER PT J AU MATTISON, EM AF MATTISON, EM TI PHYSICS OF SYSTEMATIC FREQUENCY VARIATIONS IN HYDROGEN MASERS SO IEEE TRANSACTIONS ON ULTRASONICS FERROELECTRICS AND FREQUENCY CONTROL LA English DT Article AB The frequency stability of hydrogen masers for intervals longer than 10(4) s is currently limited by systematic processes. The paper discusses the physics of frequency-determining mechanisms internal to the maser that are susceptible to systematic variations, and the connections between these internal mechanisms and external environmental factors. From estimates of the magnitudes of systematic effects, it is found that the primary internal mechanisms limiting long-term maser frequency stability are cavity pulling, at the level of parts in 10(15) per day, and wall shift variations, at the level of parts in 10(16) to parts in 10(15) per day. Strategies for reducing systematic frequency variations are discussed. RP MATTISON, EM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 24 TC 2 Z9 2 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 0885-3010 J9 IEEE T ULTRASON FERR JI IEEE Trans. Ultrason. Ferroelectr. Freq. Control PD MAR PY 1992 VL 39 IS 2 BP 250 EP 255 DI 10.1109/58.139121 PG 6 WC Acoustics; Engineering, Electrical & Electronic SC Acoustics; Engineering GA HV423 UT WOS:A1992HV42300012 PM 18263143 ER PT J AU KIDWELL, PA AF KIDWELL, PA TI REVOLUTION IN MEASUREMENT - WESTERN-EUROPEAN WEIGHTS AND MEASURES SINCE THE AGE OF SCIENCE - ZUPKO,RE SO ISIS LA English DT Book Review RP KIDWELL, PA (reprint author), SMITHSONIAN INST,NAT 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 0021-1753 J9 ISIS JI Isis PD MAR PY 1992 VL 83 IS 1 BP 111 EP 111 DI 10.1086/356034 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA HL978 UT WOS:A1992HL97800014 ER PT J AU PISANO, DA AF PISANO, DA TI THE ELECTRONIC SWEATSHOP - HOW COMPUTERS ARE TRANSFORMING THE OFFICE OF THE FUTURE INTO THE FACTORY OF THE PAST - GARSON,B SO ISIS LA English DT Book Review RP PISANO, DA (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 CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD MAR PY 1992 VL 83 IS 1 BP 168 EP 170 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA HL978 UT WOS:A1992HL97800076 ER PT J AU ROTHENBERG, M AF ROTHENBERG, M TI GUIDE TO HISTORICAL RESOURCES IN THE ATMOSPHERIC SCIENCES - ARCHIVES, MANUSCRIPTS, AND SPECIAL COLLECTIONS IN THE WASHINGTON, DC, AREA - FLEMING,JR SO ISIS LA English DT Book Review RP ROTHENBERG, M (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0021-1753 J9 ISIS JI Isis PD MAR PY 1992 VL 83 IS 1 BP 183 EP 184 DI 10.1086/356108 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA HL978 UT WOS:A1992HL97800094 ER PT J AU WOODS, BA AF WOODS, BA TI RACE AND HISTORY - SELECTED ESSAYS, 1938-1988 - FRANKLIN,JH SO JOURNAL OF AMERICAN ETHNIC HISTORY LA English DT Book Review C1 SMITHSONIAN INST,NATL MUSEUM AM HIST,WASHINGTON,DC 20560. RP WOODS, BA (reprint author), SMITHSONIAN INST,ASSOC STUDY AFROAMER LIFE & HIST,WASHINGTON,DC 20560, USA. NR 1 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 0278-5927 J9 J AM ETHNIC HIST JI J. Am. Ethn. Hist. PD SPR PY 1992 VL 11 IS 3 BP 75 EP 80 PG 6 WC Ethnic Studies; History SC Ethnic Studies; History GA HR891 UT WOS:A1992HR89100007 ER PT J AU CONNORS, A AF CONNORS, A TI IMAGES OF PENANCE, IMAGES OF MERCY - SANTOS AND CEREMONIES OF THE HISPANIC SOUTHWEST SO JOURNAL OF AMERICAN FOLKLORE LA English DT Art Exhibit Review RP CONNORS, A (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER ART,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 SN 0021-8715 J9 J AM FOLKLORE JI J. Am. Folk. PD SPR PY 1992 VL 105 IS 416 BP 230 EP 233 DI 10.2307/541091 PG 4 WC Folklore SC Arts & Humanities - Other Topics GA HR505 UT WOS:A1992HR50500009 ER PT J AU SMITH, RW AF SMITH, RW TI VIEWING THE EARTH - THE SOCIAL CONSTRUCTION OF THE LANDSAT SATELLITE SYSTEM - MACK,PE SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review RP SMITH, RW (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGANIZATION AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47408 SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD MAR PY 1992 VL 78 IS 4 BP 1528 EP 1528 DI 10.2307/2079494 PG 1 WC History SC History GA HL053 UT WOS:A1992HL05300161 ER PT J AU MCELROY, D MORAN, P BERMINGHAM, E KORNFIELD, I AF MCELROY, D MORAN, P BERMINGHAM, E KORNFIELD, I TI REAP - AN INTEGRATED ENVIRONMENT FOR THE MANIPULATION AND PHYLOGENETIC ANALYSIS OF RESTRICTION DATA SO JOURNAL OF HEREDITY LA English DT Note ID NUCLEOTIDE SUBSTITUTIONS; ENDONUCLEASES; NUMBER C1 UNIV MAINE,CTR MARINE STUDIES,ORONO,ME 04469. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP MCELROY, D (reprint author), UNIV MAINE,MIGRATORY FISH RES INST,DEPT ZOOL,217 MURRAY HALL,ORONO,ME 04469, USA. NR 11 TC 379 Z9 394 U1 2 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 SN 0022-1503 J9 J HERED JI J. Hered. PD MAR-APR PY 1992 VL 83 IS 2 BP 157 EP 158 PG 2 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA HR241 UT WOS:A1992HR24100018 PM 1349617 ER PT J AU ELDRIDGE, BF HARBACH, RE AF ELDRIDGE, BF HARBACH, RE TI CONSERVATION OF THE NAMES CULEX-STIGMATOSOMA AND CULEX-THRIAMBUS SO JOURNAL OF THE AMERICAN MOSQUITO CONTROL ASSOCIATION LA English DT Note AB As a result of action by the International Commission on Zoological Nomenclature, the name Culex peus Speiser is suppressed and never to be used as a valid name, and the names Culex stigmatosoma Dyar and Culex thriambus Dyar are conserved for the western banded foul-water mosquito and the related southwestern U.S. species, respectively. C1 SMITHSONIAN INST,MUSEUM SUPPORT CTR,WALTER REED BIOSYST UNIT,WASHINGTON,DC 20560. RP ELDRIDGE, BF (reprint author), UNIV CALIF DAVIS,DEPT ENTOMOL,DAVIS,CA 95616, USA. NR 10 TC 5 Z9 5 U1 0 U2 0 PU AMER MOSQUITO CONTROL ASSN INC PI LAKE CHARLES PA 707-A EAST PRIEN LAKE ROAD, PO BOX 5416, LAKE CHARLES, LA 70606-5416 SN 8756-971X J9 J AM MOSQUITO CONTR JI J. Am. Mosq. Control Assoc. PD MAR PY 1992 VL 8 IS 1 BP 104 EP 105 PG 2 WC Entomology SC Entomology GA HM114 UT WOS:A1992HM11400024 PM 1583481 ER PT J AU COOKE, R AF COOKE, R TI PREHISTORIC NEARSHORE AND LITTORAL FISHING IN THE EASTERN TROPICAL PACIFIC, AN ICHTHYOLOGICAL EVALUATION SO JOURNAL OF WORLD PREHISTORY LA English DT Article DE FISHING; PREHISTORIC SUBSISTENCE; TROPICAL PACIFIC; ESTUARIES; CENTRAL AND SOUTH AMERICA ID COASTAL LAGOON SYSTEM; COSTA-RICA; COMMUNITY STRUCTURE; SPECIES COMPOSITION; AUSTRALIAN ESTUARY; CENTRAL-AMERICA; DISCARDED FISH; BY-CATCH; NICOYA; GULF RP COOKE, R (reprint author), SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 177 TC 10 Z9 12 U1 0 U2 1 PU PLENUM PUBL CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 SN 0892-7537 J9 J WORLD PREHIST JI J. World Prehist. PD MAR PY 1992 VL 6 IS 1 BP 1 EP 49 DI 10.1007/BF00997584 PG 49 WC Anthropology; Archaeology SC Anthropology; Archaeology GA HF306 UT WOS:A1992HF30600001 ER PT J AU TELL, LA CITINO, SB AF TELL, LA CITINO, SB TI HEMATOLOGIC AND SERUM CHEMISTRY REFERENCE INTERVALS FOR CUBAN AMAZON PARROTS (AMAZONA-LEUCOCEPHALA-LEUCOCEPHALA) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE PARROT; AMAZONA-LEUCOCEPHALA-LEUCOCEPHALA; HEMATOLOGY; SERUM CHEMISTRY AB Blood samples from 37 Cuban Amazon parrots (Amazona leucocephala leucocephala) were evaluated to determine hematologic and serum biochemical reference intervals. Hematologic and serum chemistry values were not significantly different (P > 0.05) between males and females. Value ranges for Cuban Amazon parrots were comparable to those published for other Amazona species. C1 MIAMI METRO ZOO,MIAMI,FL 33177. RP TELL, LA (reprint author), SMITHSONIAN INST,DEPT ANIM HLTH,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 8 TC 10 Z9 10 U1 0 U2 2 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD MAR PY 1992 VL 23 IS 1 BP 62 EP 64 PG 3 WC Veterinary Sciences SC Veterinary Sciences GA HR897 UT WOS:A1992HR89700006 ER PT J AU FLEISCHER, RC MURPHY, MT AF FLEISCHER, RC MURPHY, MT TI RELATIONSHIPS AMONG ALLOZYME HETEROZYGOSITY, MORPHOLOGY AND LIPID-LEVELS IN HOUSE SPARROWS DURING WINTER SO JOURNAL OF ZOOLOGY LA English DT Article ID MULTIPLE-LOCUS HETEROZYGOSITY; PASSER-DOMESTICUS; BODY SIZE; PHYSIOLOGICAL ENERGETICS; NATURAL-POPULATIONS; SEASONAL-CHANGES; PREDATION RISK; GROWTH-RATE; BIRDS; TEMPERATURE AB House sparrows (Passer domesticus) were collected during cold (43 individuals) and warm (31 individuals) periods in February 1982 from farms near Lawrence, Kansas. Fat scores (from flank, rump and furcula) and body mass were measured from the carcasses, which were then reduced to skeletons. Heterozygosity was determined by electrophoresis of three polymorphic allozymes. Pectoral lipid content was determined by petroleum ether extraction. Principal component (PC) analysis was conducted on 14 skeletal measurements. Summed fat score, body mass and pectoral lipid content served as dependent variables in three multiple regressions. Sex, period (cold versus warm), number of heterozygous loci (0-3), and scores of PC1, PC2 and PC3 were independent variables. Each of the dependent variables was also included as an independent variable in regressions in which they were not the dependent variable. Pectoral lipid content was significantly related only to the number of heterozygous loci (R2 = 0.18, P = 0.008). Summed fat score differed between sexes and periods (P = 0.012 and 0.001, respectively) when body mass was included in the regression (P < 0.001). Body mass was related to summed fat score as above, and also to body size (PC1, P < 0.0001) and period (P = 0.014). Females exhibited a positive regression between body size and summed fat score (P = 0.007). Body size (PC1) was greater for both sexes in the sample from the warm period (P = 0.022), suggesting that selection for increased body size may have occurred. Increased metabolic efficiency of heterozygous enzymes or individuals is suggested as an explanation for the observed relationship between heterozygosity and intramuscular lipid level. C1 HARTWICK COLL,DEPT BIOL,ONEONTA,NY 13820. RP FLEISCHER, RC (reprint author), SMITHSONIAN INST,DEPT ZOOL RES,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 45 TC 4 Z9 4 U1 0 U2 0 PU OXFORD UNIV PRESS UNITED KINGDOM PI OXFORD PA WALTON ST JOURNALS DEPT, OXFORD, ENGLAND OX2 6DP SN 0952-8369 J9 J ZOOL JI J. Zool. PD MAR PY 1992 VL 226 BP 409 EP 419 PN 3 PG 11 WC Zoology SC Zoology GA HK700 UT WOS:A1992HK70000005 ER PT J AU LESSIOS, HA AF LESSIOS, HA TI TESTING ELECTROPHORETIC DATA FOR AGREEMENT WITH HARDY-WEINBERG EXPECTATIONS SO MARINE BIOLOGY LA English DT Article ID ASEXUAL REPRODUCTION; GEOGRAPHIC-VARIATION; GENETIC-STRUCTURE; POPULATIONS; FREQUENCIES; EQUILIBRIUM; POLYMORPHISM; SCALE; CHI2 AB Electrophoretic data from marine organisms are routinely tested for conformity to expectations of the Hardy-Weinberg rule, but the statistical procedures used and the interpretation of their results are often flawed. This paper summarizes literature on statistical testing for Hardy-Weinberg equilibrium and suggests an analytical strategy based on carrying out computationally simple goodness-of-fit chi-2 tests (with pooling and correction factors for continuity if necessary) when appropriate, and resorting to computationally tedious, exact tests when necessary. It recommends adjustments of significance levels to avoid the large Type-I error that may result from multiple tests for Hardy-Weinberg equilibrium, one for each locus and each population. It points out the obvious but common error of interpreting non-significant tests as evidence of conformity to Hardy-Weinberg expectations, and makes suggestions as to how tests that produce significance can be used to reach conclusions of biological relevance. RP SMITHSONIAN TROP RES INST, POB 2072, BALBOA, PANAMA. NR 73 TC 206 Z9 212 U1 0 U2 7 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD MAR PY 1992 VL 112 IS 3 BP 517 EP 523 DI 10.1007/BF00356299 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA HJ522 UT WOS:A1992HJ52200021 ER PT J AU MARVIN, UB AF MARVIN, UB TI THE METEORITE OF ENSISHEIM - 1492 TO 1992 SO METEORITICS LA English DT Review AB On November 7, 1492, a 127-kg stony meteorite fell at Ensisheim in Alsace after a fireball explosion that was heard for a distance of 150 km over the upper Rhineland. Today, a 56-kg specimen of the stone, an LL6 chondrite with large patches of fusion crust, remains on display in the Hotel de Ville at Ensisheim. This was the earliest witnessed meteorite fall in the West from which pieces are preserved. Initially, the stone's survival depended on the presence of a magistrate at Ensisheim who forbade the removal of pieces, which had begun apace as soon as a crowd gathered and pulled the stone out of a 1-m hole in a wheat field. He ordered the stone brought into the city to await the arrival of King Maximilian, son of the Holy Roman Emperor Friedrich III, who was approaching with his army. In nearby Basel, broadsheets were printed within weeks bearing the story in Latin and German verses by the eminent poet, Sebastian Brant, who turned the sheets into propaganda tracts by claiming the stone as a portent of victory and admonishing Maximilian to make war on the French without delay. Maximilian declared the stone to be a sign of divine favor and ordered it to be preserved in the Ensisheim parish church. The stone grew in fame when Maximilian won his impending battle with the French, but strange new elements entered the story as it was repeated over the years in books and chronicles. Through centuries of battle and political changes, the stone remained in the church until 1793 when French revolutionaries transferred it to a new National Museum in Colmar. There, many pieces were taken for chemical analyses during the birth of the meteoritics at the turn of the 19th century. In 1803 the stone was returned to the Ensisheim church where it outlasted the structure itself which collapsed in 1854. This paper traces the history of the stone itself and people's responses to it through the 500 years since the fall at Ensisheim. C1 HARVARD UNIV,DEPT EARTH & PLANETARY SCI,CAMBRIDGE,MA 02138. RP MARVIN, UB (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 104 TC 22 Z9 22 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 MAR PY 1992 VL 27 IS 1 BP 28 EP 72 PG 45 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA HN056 UT WOS:A1992HN05600006 ER PT J AU ANDREWS, JC HOWARD, JG BAVISTER, BD WILDT, DE AF ANDREWS, JC HOWARD, JG BAVISTER, BD WILDT, DE TI SPERM CAPACITATION IN THE DOMESTIC CAT (FELIS-CATUS) AND LEOPARD CAT (FELIS-BENGALENSIS) AS STUDIED WITH A SALT-STORED ZONA-PELLUCIDA PENETRATION ASSAY SO MOLECULAR REPRODUCTION AND DEVELOPMENT LA English DT Article DE PROTEIN-FREE MEDIUM; BSA; INVITRO SPERM PENETRATION ID INVITRO FERTILIZATION; HAMSTER SPERMATOZOA; FOLLICULAR OOCYTES; PLASMA-MEMBRANE; SERUM-ALBUMIN; EGGS; MATURATION; MECHANISM; MOTILITY; PROTEIN AB The ability of domestic cat or leopard cat spermatozoa to penetrate zonae pellucidae (ZP) of salt-stored, domestic cat oocytes was examined as an assay for sperm capacitation. Ovarian oocytes were recovered after ovariectomy and matured in vitro for 18-36 h. Following removal of cumulus cells, the oocytes were used fresh, or stored (4-degrees-C, 0.5-24 weeks) in a HEPES-buffered hypertonic salt solution. Electroejaculated, washed sperm (2-4 x 10(6) sperm/ml) were preincubated for 1.0 h (38-degrees-C, 5% CO2 in air) and then co-incubated (2 x 10(5) sperm/ml) with fresh or stored oocytes for 6.0 h. Gametes were incubated in a protein-free, modified Tyrode's solution (TLP-PVA) or in the same medium containing 4.0 mg/ml bovine serum albumin (BSA; TALP-PVA). Treatments were compared for percentage ZP penetration (defined as sperm heads reaching more than halfway through the ZP) as an index of sperm capacitation. In both the domestic cat and leopard cat, there was no difference (P > 0.05) in sperm penetration of fresh ZP (domestic cat, 42.5 +/- 5.4%; leopard cat, 38.6 +/- 2.8%) or stored ZP (domestic cat, 32.4 +/-4.2%; leopard cat, 27.6 +/- 2.3%). Sperm incubated in protein-free medium (TLP-PVA) were less capable (P < 0.05) of ZP penetration (domestic cat, 14.6 +/- 5.9%; leopard cat, 7.9 +/- 3.0%) than sperm incubated in medium TALP-PVA containing BSA (domestic cat, 60.3 +/- 5.9%; leopard cat, 58.4 +/- 3.0%). These data indicate that (1) albumin facilitates capacitation and ZP penetrating ability of cat spermatozoa; (2) domestic cat ZP appear to lack a block to heterospecific penetration by "foreign' (leopard cat) sperm; and (3) penetration of stored domestic cat ZP can be used as an index of sperm capacitation in the domestic cat and the leopard cat. C1 SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20560. RP ANDREWS, JC (reprint author), UNIV WISCONSIN,DEPT VET SCI,1655 LINDEN DR,MADISON,WI 53706, USA. FU NCRR NIH HHS [RR00045]; NICHD NIH HHS [HD23853] NR 45 TC 46 Z9 47 U1 1 U2 5 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 1040-452X J9 MOL REPROD DEV JI Mol. Reprod. Dev. PD MAR PY 1992 VL 31 IS 3 BP 200 EP 207 DI 10.1002/mrd.1080310307 PG 8 WC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology SC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology GA HF782 UT WOS:A1992HF78200006 PM 1554505 ER PT J AU DOERING, ZD AF DOERING, ZD TI ENVIRONMENTAL EXHIBITS AT THE SMITHSONIAN SO MUSEUM NEWS LA English DT Article RP DOERING, ZD (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD MAR-APR PY 1992 VL 71 IS 2 BP 50 EP 52 PG 3 WC Art SC Art GA HG952 UT WOS:A1992HG95200016 ER PT J AU RAVENHILL, PL AF RAVENHILL, PL TI WHAT MUSEUMS FOR AFRICA SO MUSEUM NEWS LA English DT Article RP RAVENHILL, PL (reprint author), SMITHSONIAN INST,NAT MUSEUM AFRICAN ART,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD MAR-APR PY 1992 VL 71 IS 2 BP 78 EP & PG 0 WC Art SC Art GA HG952 UT WOS:A1992HG95200020 ER PT J AU LORNELL, K AF LORNELL, K TI ROCKABILLY - A BIBLIOGRAPHIC RESOURCE GUIDE - COOPER,BL, HANEY,WS SO NOTES LA English DT Book Review RP LORNELL, K (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU MUSIC LIBRARY ASSN PI CATON PA BUSINESS OFFICE PO BOX 487, CATON, MA 02021 SN 0027-4380 J9 NOTES JI Notes PD MAR PY 1992 VL 48 IS 3 BP 911 EP 912 DI 10.2307/941731 PG 2 WC Music SC Music GA HH185 UT WOS:A1992HH18500052 ER PT J AU MANN, RW GOMEZ, G AF MANN, RW GOMEZ, G TI UNEXPECTED FINDING OF A STAPES PROSTHESIS SO OTOLARYNGOLOGY-HEAD AND NECK SURGERY LA English DT Letter RP MANN, RW (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MOSBY-YEAR BOOK INC PI ST LOUIS PA 11830 WESTLINE INDUSTRIAL DR, ST LOUIS, MO 63146-3318 SN 0194-5998 J9 OTOLARYNG HEAD NECK JI Otolaryngol. Head Neck Surg. PD MAR PY 1992 VL 106 IS 3 BP 317 EP 317 PG 1 WC Otorhinolaryngology; Surgery SC Otorhinolaryngology; Surgery GA HJ155 UT WOS:A1992HJ15500028 PM 1589229 ER PT J AU CALAMAI, AG HAN, XF PARKINSON, WH AF CALAMAI, AG HAN, XF PARKINSON, WH TI RADIATIVE LIFETIME OF THE 3S3P(3)(5S2(0)) METASTABLE LEVEL OF P+ SO PHYSICAL REVIEW A LA English DT Article ID TRANSITION-PROBABILITY; ISOELECTRONIC SEQUENCE; INTERCOMBINATION LINE; OSCILLATOR-STRENGTHS; INTERSYSTEM LINE; SILICON SEQUENCE; ION TRAP; SI-III; SPECTRUM; IDENTIFICATION AB The radiative lifetime of the 3s3p3(5S2o) metastable level of P+ has been measured by counting, for equal time intervals, the approximately 221-nm photons emitted when the metastable ions decay to the 3s(2)3p2(3P2,1) levels of P+. This is the first lifetime measurement of the 3s3p3(5S2o) level belonging to a low-charge-state ion in the SiI isoelectronic sequence. Although forbidden to decay by the LS selection rule DELTA-S = 0, the 5S2o level decays via intercombination electric dipole transitions by spin-orbit mixing with other levels of the 3s3p3 configuration. A metastable P+ ion population was produced inside a cylindrical radio-frequency ion trap by electron bombardment of PH3 vapor at pressures ranging from 5 x 10(-8) to 40 x 10(-8) Torr. The trap, operated with potential-well depths ranging from 12 to 20 eV, consists of two circular, wire-mesh end caps and a cylindrical, wire-mesh ring electrode with physical dimensions r0 = z0 = 1.67 cm. Some of the light emitted by the decaying 5S2o population was focused onto a 19-nm-bandwidth interference filter in front of a photomultiplier tube operated in single-photon counting mode. The mean lifetime was obtained from the decay-rate parameter of a nonlinear least-squares fit of a single exponential plus a constant background to the decay counts. Our result for the radiative lifetime of 3s3p3(5S2o) metastable level of P+ is 167 +/- 12-mu-s. RP CALAMAI, AG (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 40 TC 29 Z9 29 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 MAR 1 PY 1992 VL 45 IS 5 BP 2716 EP 2722 DI 10.1103/PhysRevA.45.2716 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA HH617 UT WOS:A1992HH61700013 ER PT J AU GUBERMAN, SL DALGARNO, A AF GUBERMAN, SL DALGARNO, A TI DIPOLE-MOMENTS AND TRANSITION-PROBABILITIES OF THE I 3-PI-G-B 3-SIGMA-U(+),C 3-PI-U-A 3-SIGMA-G(+), AND I 3-PI-G-C 3-PI-U SYSTEMS OF MOLECULAR-HYDROGEN SO PHYSICAL REVIEW A LA English DT Article ID DISSOCIATIVE DECAY; ELECTRON-IMPACT; H-2; SPECTROSCOPY; SPECTRUM; EMISSION; STATES; H2; LIFETIMES; ENERGIES AB Ab initio calculations using the Born-Oppenheimer approximation are described of the dipole moments of the i (3)PI(g)-b (3)SIGMA(u)+, c (3)PI(u)-a (3)SIGMA(g)+, and i (3)PI(g)-c (3)PI(u) transitions of molecular hydrogen. Tables are provided of the dipole transition probabilities and Franck-Condon factors. Franck-Condon factors are presented for transitions originating in the lowest vibrational level of the ground X (1)SIGMA(g)+ state. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP GUBERMAN, SL (reprint author), INST SCI RES,33 BEDFORD ST,LEXINGTON,MA 02173, USA. NR 37 TC 21 Z9 21 U1 0 U2 5 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 MAR 1 PY 1992 VL 45 IS 5 BP 2784 EP 2789 DI 10.1103/PhysRevA.45.2784 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA HH617 UT WOS:A1992HH61700023 ER PT J AU JAKUPOVIC, J GANZER, U PRITSCHOW, P LEHMANN, L BOHLMANN, F KING, RM AF JAKUPOVIC, J GANZER, U PRITSCHOW, P LEHMANN, L BOHLMANN, F KING, RM TI SESQUITERPENE LACTONES AND OTHER CONSTITUENTS FROM URSINIA SPECIES SO PHYTOCHEMISTRY LA English DT Article DE URSINIA SP; COMPOSITAE; SESQUITERPENE LACTONES; GERMACRANOLIDES; GUAIANOLIDES; REARRANGED EUDESMANOLIDE, GUAIANE, EUDESMANE AND EREMOPHILANE DERIVATIVES; FULVENES; FARNESOL DERIVATIVES; FUROSESQUITERPENE ID OCCURRING TERPENE DERIVATIVES; ANTHEMOIDES L POIRET; JASONIA-MONTANA; GUAIANOLIDES; FURANOSESQUITERPENES; GERMACRANOLIDE; EUDESMANOLIDES; GLAUCOLIDES AB From 12 Ursinia species, in addition to known compounds, 31 new sesquiterpene lactones, 10 being germacranolides, 19 guaianolides, one eudesmanolide and a rearranged one, were isolated. Furthermore, seven sesquiterpene acids and methyl esters, including two fulvenes and a rearranged eudesmane, a nerolidol and seven farnesol derivatives, a furosesquiterpene derived from dehydrolasiospermane, three eudesmane and three eremophilane derivatives as well as a triynene were present. The structures were elucidated by high field NMR techniques. The chemistry supports the placement of the genus in the tribe Anthemideae, probably as a subtribe, together with related South African genera. C1 SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560. RP JAKUPOVIC, J (reprint author), TECH UNIV BERLIN,INST ORGAN CHEM,W-1000 BERLIN 12,GERMANY. NR 52 TC 28 Z9 30 U1 0 U2 2 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 MAR PY 1992 VL 31 IS 3 BP 863 EP 880 PG 18 WC Biochemistry & Molecular Biology; Plant Sciences SC Biochemistry & Molecular Biology; Plant Sciences GA HG872 UT WOS:A1992HG87200029 ER PT J AU STORM, J CARNEY, BW LATHAM, DW AF STORM, J CARNEY, BW LATHAM, DW TI K-BAND LIGHT CURVES FOR RR LYRAE STARS IN THE GLOBULAR CLUSTER-M5 AND GLOBULAR CLUSTER-M92 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID PHOTOMETRY; DISTANCES AB K-band photometry for the RR Lyrae stars V1 and V3 in the extremely metal-poor globular cluster M92 (NGC 6341) and V8 and V28 in the intermediate-metallicity cluster M5 (NGC 5904) have been acquired during the 1987-1990 observing seasons, for use in a Baade-Wesselink analysis. A single-channel photometer as well as IR imagers have been used for the data acquisition and the results from the different systems show good agreement. The reduction procedure for these data and the resulting light curves, good to better than 0.02 mag, based on 340, 541, 284, and 212 measurements for M92-V1, M92-V3, M5-V8, and M5-V28, respectively, are presented. Preliminary distance estimates for the clusters using the [M(K)] -log P relation for the RR Lyr stars leads to values of (m - M)0 = 14.36 for M92 and (m - M)0 = 14.24 for M5. C1 COPENHAGEN UNIV OBSERV,DK-1350 COPENHAGEN K,DENMARK. ASSOC UNIV RES ASTRON INC,KITT PEAK NATL OBSERV,TUCSON,AZ 85726. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP STORM, J (reprint author), UNIV N CAROLINA,DEPT PHYS & ASTRON,CB 3255,PHILLIPS HALL,CHAPEL HILL,NC 27599, USA. NR 14 TC 12 Z9 12 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 MAR PY 1992 VL 104 IS 673 BP 159 EP 167 DI 10.1086/132973 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HK944 UT WOS:A1992HK94400001 ER PT J AU STORM, J CARNEY, BW LATHAM, DW DAVIS, RJ LAIRD, JB AF STORM, J CARNEY, BW LATHAM, DW DAVIS, RJ LAIRD, JB TI RADIAL-VELOCITY CURVES FOR RR LYRAE STARS IN THE GLOBULAR CLUSTER-M5 AND CLUSTER-M92 OBTAINED USING SYNTHETIC SPECTRA CROSS-CORRELATION TEMPLATES SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID BAADE-WESSELINK METHOD; HORIZONTAL-BRANCH; GALAXY AB Radial-velocity curves are presented for the RR Lyrae stars V1 and V3 in the low-metallicity globular cluster M92 (NGC 6341) and V8 and V28 in the intermediate-metallicity globular cluster M5 (NGC 5904) based on between 50 and 90 observations per star. The radial velocities were derived by cross-correlating spectra obtained with the Multiple Mirror Telescope echelle spectrograph with synthetic templates calculated using Kurucz's model atmospheres (ATLAS8) and synthetic spectrum (SYNTHE) codes. The synthetic templates provide a better match to the observed spectra than the available observed templates, especially for the metal-poor stars, resulting in high-precision radial velocities good to a few km s-1 in most cases. We find systemic velocities of -125.4, -122.6, +48.7, and +53.6 km s-1 for M92-V1, M92-V3, M5-V8, and M5-V28, respectively, in good agreement with previous determinations of cluster mean velocities. C1 COPENHAGEN UNIV OBSERV,DK-1350 COPENHAGEN K,DENMARK. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. BOWLING GREEN STATE UNIV,DEPT PHYS & ASTRON,BOWLING GREEN,OH 43403. RP STORM, J (reprint author), UNIV N CAROLINA,DEPT PHYS ASTRON,CB 3255,PHILLIPS HALL,CHAPEL HILL,NC 27599, USA. NR 27 TC 10 Z9 10 U1 0 U2 1 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 MAR PY 1992 VL 104 IS 673 BP 168 EP 178 DI 10.1086/132974 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HK944 UT WOS:A1992HK94400002 ER PT J AU KURUCZ, RL AF KURUCZ, RL TI ATOMIC AND MOLECULAR-DATA FOR OPACITY CALCULATIONS SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article; Proceedings Paper CT WORKSHOP ON ASTROPHYSICAL OPACITIES CY JUL 15-19, 1991 CL IBM VENEZUELA SCI CTR, CARACAS, VENEZUELA SP IBM VENEZUELA, FDN POLAR, VENEZUELAN CONICIT HO IBM VENEZUELA SCI CTR DE ATOMIC PROCESSES; MOLECULAR PROCESSES; TRANSITION PROBABILITIES ID SPECTRA AB I am attempting to produce line lists for all atoms and diatomic molecules that are important in stars. I collect all published data on spectrum analysis and oscillator strengths. I compute the energy levels, wavelengths, gf values, and damping constants that are not available from the literature. Line lists have been computed for diatomic molecules H-2, CH, NH, OH, MgH, SiH, CN, C2, CO, SiO, and TiO, and for the iron group atoms Ca I-IX to Ni I-IX. These lists total 58 million lines. These calculations are being revised as new laboratory data become available. The work is being extended to other diatomic molecules, to lighter and heavier elements, and to higher stages of ionization. RP KURUCZ, RL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 13 TC 202 Z9 202 U1 0 U2 4 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD MAR PY 1992 VL 23 SI SI BP 45 EP 48 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HV967 UT WOS:A1992HV96700004 ER PT J AU KURUCZ, RL AF KURUCZ, RL TI FINDING THE MISSING SOLAR ULTRAVIOLET OPACITY SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article; Proceedings Paper CT WORKSHOP ON ASTROPHYSICAL OPACITIES CY JUL 15-19, 1991 CL IBM VENEZUELA SCI CTR, CARACAS, VENEZUELA SP IBM VENEZUELA, FDN POLAR, VENEZUELAN CONICIT HO IBM VENEZUELA SCI CTR DE ATOMIC PROCESSES; MOLECULAR PROCESSES; OPACITIES AB I have computed new opacities for model stellar atmospheres and envelopes using a large grant of Cray computer time at the San Diego Supercomputer Center. The opacities include 58,000,000 atomic and diatomic molecular lines. Twelve-step distribution functions are tabulated for 56 temperatures in the range from 2000 K to 200000 K, for 21 log pressures from -2 to 8, for 1212 wavelength intervals from 10 to 10000 nm, for microturbulent velocities 0, 1, 2, 4, and 8 km/s, for scaled solar abundances [+1.0], [+0.5], [+0.3], [+0.2], [+0.1], [0.0], [-0.1], [-0.2], [-0.3], [-0.5], [-1.0], [-1.5], [-2.0], [-2.5], [-3.0], [-3.5], [-4.0], [-4.5], [-5.0], and [+0.0, no He] (log abundance of elements heavier than helium relative to solar). Rosseland means are also tabulated for each case. The final files for each two 6250 bpi VAX backup tapes. I am now distributing tape copies. I hope to have CD-ROMs available in the near future. A solar photospheric model computed with the new opacities matches the observed energy distribution. RP KURUCZ, RL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 20 TC 175 Z9 175 U1 0 U2 1 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD MAR PY 1992 VL 23 SI SI BP 181 EP 186 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HV967 UT WOS:A1992HV96700020 ER PT J AU KURUCZ, RL AF KURUCZ, RL TI REMAINING LINE OPACITY PROBLEMS FOR THE SOLAR SPECTRUM SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article DE ATOMIC PROCESSES; MOLECULAR PROCESSES; TRANSITION PROBABILITIES; SUN - SPECTRA AB We need high-resolution, high-signal-to-noise spectra of the sun with complete spectral coverage. The solar spectrum provides the insolation that controls the atmospheric chemistry of the earth and of all the solar system bodies. It is important for stellar astrophysics as the "standard" stellar spectrum because it can be observed better than that of any other star. It is important for understanding the sun, for it allows us to study the conditions and motions at its surface. It is an important high-temperature laboratory source for atomic and molecular spectroscopy. To interpret the spectrum we require accurate energy levels, accurate wavelengths, accurate gf values, accurate damping constants. We require hyperfine splitting, isotopic splitting, and Zeeman splitting. We require completeness in order to deconvolve blends. We need every level below the lowest ionization or dissociation energy. For molecules that is every vibrational and rotational level. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 14 TC 47 Z9 47 U1 0 U2 1 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD MAR PY 1992 VL 23 SI SI BP 187 EP 194 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HV967 UT WOS:A1992HV96700021 ER PT J AU ADAMS, RM AF ADAMS, RM TI SMITHSONIAN HORIZONS SO SMITHSONIAN LA English DT Article RP ADAMS, RM (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD MAR PY 1992 VL 22 IS 12 BP 10 EP 10 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA HF844 UT WOS:A1992HF84400001 ER PT J AU FELLEY, JD DANIELS, GL AF FELLEY, JD DANIELS, GL TI LIFE-HISTORY OF THE SAILFIN MOLLY (POECILIA-LATIPINNA) IN 2 DEGRADED WATERWAYS OF SOUTHWESTERN LOUISIANA SO SOUTHWESTERN NATURALIST LA English DT Article AB Contraband Bayou and Bayou d'Inde are two highly degraded waterways draining into the Calcasieu Estuary of southwestern Louisiana. Both bayous are affected by municipal wastes, and Bayou d'Inde receives additional effluents from a large petrochemical complex. Fish-kills occur frequently in both bayous, and the fish faunas of both are highly depauperate compared to those of more pristine waterways. Bayou d'Inde has many fewer species than Contraband Bayou. Poecilia latipinna is abundant in both waterways. We investigated the life history of P. latipinna to determine whether the added stresses present in Bayou d'Inde would be reflected in this population. There were no significant differences in population sizes, sizes of individuals, or fecundity of females. Poecilia latipinna in these two bayous had life-history trends similar to those of Gambusia affinis in southwestern Louisiana. Both species showed fast growth early in the year, and females reproducing in the summer and fall of the year in which they were born produced significantly fewer propagules than did females that over-wintered. RP FELLEY, JD (reprint author), SMITHSONIAN INST,OFF INFORMAT RESOURCE MANAGEMENT,ROOM 2310,AI BLDG,WASHINGTON,DC 20560, USA. NR 0 TC 2 Z9 2 U1 1 U2 3 PU SOUTHWESTERN ASSN NATURALISTS PI SAN MARCOS PA SOUTHWEST TEXAS STATE UNIV, DEPT BIOLOGY, 601 UNIVERSITY DR, SAN MARCOS, TX 78666 SN 0038-4909 J9 SOUTHWEST NAT JI Southw. Natural. PD MAR PY 1992 VL 37 IS 1 BP 16 EP 21 DI 10.2307/3672141 PG 6 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA HQ393 UT WOS:A1992HQ39300003 ER PT J AU WALTMAN, JR BEISSINGER, SR AF WALTMAN, JR BEISSINGER, SR TI BREEDING-BEHAVIOR OF THE GREEN-RUMPED PARROTLET SO WILSON BULLETIN LA English DT Article ID BIOLOGY; GROWTH; EGGS AB We studied the breeding behavior of Green-rumped Parrotlets (Forpus passerinus) using nest boxes in the Ilanos of Venezuela. Aggressive and courtship displays, and nest prospecting behavior are described. Females occupied nest boxes for about 80% of daylight hours from shortly before egg laying through hatching (30-40 days), and did all incubating and brooding. Males spent nearly 80% of the time away from the nest, presumably foraging for their mates and chicks. Clutch sizes of females were correlated positively with the rate at which they were fed by males during egg laying, Clutches hatched asynchronously, and nestling growth and development was slow. Females stopped brooding when oldest chicks were one to two weeks of age to join their mates in feeding young, though the youngest chicks were at most a few days old. Food delivery rates by parents to young were related positively to brood size after all eggs had hatched. Most pairs (91%) remained mated throughout the breeding season. Mate replacement between years was more common (greater-than-or-equal-to 31%). More than half of the females that nested in the first part of the breeding season attempted second nests. Intervals between nesting attempts (xBAR = 22 days) were correlated positively with the number of young fledging from first nests. Over three-quarters of the pairs that remained together and renested used the same nest box, even though intruders constantly attempted to obtain nest sites. Results are discussed in relation to the division of parental care and the high degree of pair cohesion exhibited by parrots. C1 YALE UNIV,SCH FORESTRY & ENVIRONM STUDIES,NEW HAVEN,CT 06511. SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. RI Beissinger, Steven/F-3809-2012 NR 37 TC 61 Z9 62 U1 1 U2 7 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 MAR PY 1992 VL 104 IS 1 BP 65 EP 84 PG 20 WC Ornithology SC Zoology GA HJ931 UT WOS:A1992HJ93100006 ER PT J AU STUWE, M SCRIBNER, KT ALKON, PU AF STUWE, M SCRIBNER, KT ALKON, PU TI A COMPARISON OF GENETIC DIVERSITY IN NUBIAN IBEX (CAPRA-IBEX-NUBIANA) AND ALPINE IBEX (CAPRA-I-IBEX) SO ZEITSCHRIFT FUR SAUGETIERKUNDE-INTERNATIONAL JOURNAL OF MAMMALIAN BIOLOGY LA English DT Note ID VARIABILITY C1 BEN GURION UNIV NEGEV,JACOB BLAUSTEIN INST DESERT RES,IL-84990 SEDE BOQER,ISRAEL. UNIV GEORGIA,DEPT ZOOL,ATHENS,GA 30602. RP STUWE, M (reprint author), SMITHSONIAN INST,NATL ZOOL PK,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630, USA. NR 17 TC 7 Z9 7 U1 1 U2 3 PU GUSTAV FISCHER VERLAG PI JENA PA VILLENGANG 2, D-07745 JENA, GERMANY SN 0044-3468 J9 Z SAUGETIERKD JI Z. Saugetierkd.-Int. J. Mamm. Biol. PD MAR PY 1992 VL 57 IS 2 BP 120 EP 123 PG 4 WC Zoology SC Zoology GA HN551 UT WOS:A1992HN55100010 ER PT J AU LUPFER, C AF LUPFER, C TI A THIN BLUE LINE SO APPLIED OPTICS LA English DT Editorial Material RP LUPFER, C (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 SN 0003-6935 J9 APPL OPTICS JI Appl. Optics PD FEB 20 PY 1992 VL 31 IS 6 BP 694 EP 695 PG 2 WC Optics SC Optics GA HD626 UT WOS:A1992HD62600001 ER PT J AU LUPFER, C AF LUPFER, C TI SEEING MORE SO APPLIED OPTICS LA English DT Editorial Material RP LUPFER, C (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 SN 0003-6935 J9 APPL OPTICS JI Appl. Optics PD FEB 20 PY 1992 VL 31 IS 6 BP 695 EP 696 PG 2 WC Optics SC Optics GA HD626 UT WOS:A1992HD62600002 ER PT J AU JONES, RV CARNEY, BW STORM, J LATHAM, DW AF JONES, RV CARNEY, BW STORM, J LATHAM, DW TI THE BAADE-WESSELINK METHOD AND THE DISTANCES TO RR LYRAE STARS .7. THE FIELD STARS SW ANDROMEDAE AND DX DELPHINI AND A COMPARISON OF RECENT BAADE-WESSELINK ANALYSES SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, FUNDAMENTAL PARAMETERS; STARS, INDIVIDUAL (DX DEL, SW AND); STARS, OSCILLATIONS; STARS, VARIABLES, OTHER ID OOSTERHOFF PERIOD GROUPS; GLOBULAR-CLUSTER SYSTEM; HORIZONTAL-BRANCH STARS; ABSOLUTE MAGNITUDES; VY SERPENTIS; MODEL ATMOSPHERES; METAL ABUNDANCES; LUMINOSITY SCALE; STANDARD STARS; X-ARIETIS AB We present new BVK photometry and radial velocities from high-resolution spectroscopy for the metal-rich ([Fe/H] = -0.2) ab-type RR Lyrae star SW Andromedae. We utilize these data, along with previously published optical data, to derive the distance and absolute magnitudes of this star using the infrared surface brightness version of the Baade-Wesselink method. We also analyze the metal-rich ([Fe/H] = -0.2) RR Lyrae variable DX Delphini using the same technique and previously published data. We obtain = 1.10 mag, = 1.10 mag, and = + 0.10 mag for SW And, and = 0.68 mag, = 0.69 mag, and = -0.35 mag for DX Del. We compare these results, and the values we derived in previous papers in this series, with the results from three other recent applications of the Baade-Wesselink method, and find that they agree to within 0.10 mag when the appropriate phase intervals are considered. Excluding the highly reddened and highly evolved stars, we derive = 0.16[Fe/H] + 1.02, = 0.21[Fe/H] + 1.04, = -2.33 log P - 0.88, using weighted least-squares fitting for 18 stars. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP JONES, RV (reprint author), UNIV N CAROLINA,DEPT PHYS & ASTRON,CB 3255,PHILLIPS HALL,CHAPEL HILL,NC 27599, USA. NR 65 TC 111 Z9 111 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 FEB 20 PY 1992 VL 386 IS 2 BP 646 EP 662 DI 10.1086/171046 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HC827 UT WOS:A1992HC82700022 ER PT J AU BAND, YB JULIENNE, PS AF BAND, YB JULIENNE, PS TI COMPLETE ALIGNMENT AND ORIENTATION OF ATOMS AND MOLECULES BY STIMULATED RAMAN-SCATTERING WITH TEMPORALLY SHIFTED LASERS SO JOURNAL OF CHEMICAL PHYSICS LA English DT Note ID VIBRATIONAL LEVELS C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. NATL INST STAND & TECHNOL,DIV MOLEC SPECT,GAITHERSBURG,MD 20899. RP BAND, YB (reprint author), BEN GURION UNIV NEGEV,DEPT CHEM,IL-84105 BEER SHEVA,ISRAEL. RI Julienne, Paul/E-9378-2012 OI Julienne, Paul/0000-0002-5494-1442 NR 11 TC 32 Z9 32 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 FEB 15 PY 1992 VL 96 IS 4 BP 3339 EP 3341 DI 10.1063/1.461929 PG 3 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA HE743 UT WOS:A1992HE74300097 ER PT J AU HODGES, HM AF HODGES, HM TI PARTICLE ABUNDANCES IN OUR UNIVERSE - DETERMINISTIC, OR RANDOMLY DETERMINED VIA QUANTUM COSMOLOGY OR INFLATIONARY QUANTUM FLUCTUATIONS SO PHYSICAL REVIEW D LA English DT Article ID SUPERHEAVY MAGNETIC MONOPOLES; SCALAR-FIELD; EXPANDING UNIVERSE; THERMAL PRODUCTION; PHASE-TRANSITIONS; BARYON ASYMMETRY; INVISIBLE AXION; CP CONSERVATION; COSMIC STRINGS; PERTURBATIONS AB There is a rather large class of particle species that may never achieve a thermal abundance after inflation. The abundance, relative to photons, of these particles (if stable), or the stable decay products from these particles, or the abundances of thermal relics diluted by an entropy-producing decay of such a particle, may not be possible to uniquely predict, even with full knowledge of the fundamental physics. Quantum cosmology, or inflationary quantum fluctuations, enables random processes to manifest themselves on very large scales, well beyond our horizon. Particle abundances that are not completely fixed by thermodynamics may be linked to these random processes, and significant large-scale variations in particle abundances may be realized without the exceedingly tiny probabilities that are associated with purely thermal processes. It is known that certain axion models may not yield a unique prediction for the axion abundance. After reviewing and further analyzing the axion case, we explore other models of particle species in which the element of chance may play a nontrivial role in determining the relic abundance. It appears that any relic abundance can be significantly affected by random processes, depending upon the details of the particle physics. Specific examples studied in this paper include baryons, monopoles, other possible supermassive relics, gravitons, scalar field relics, and shadow matter. Also examined is the entropy-producing decay of a nonthermal relic, which may adjust the densities of all other frozen-out relics (e.g., supersymmetric relics), relative to the photon abundance, by a random amount. Simple models are provided in which the probability distributions of relic abundances relative to photons are explicitly calculated, and the possibility of obtaining a wide variety of abundances with modest changes in the probability is demonstrated. Typically, the probability distributions of abundances have simple power-law dependence on the abundance. The broad nature of some of the distributions indicates that "anthropic selection effects" may be important for interpreting how our Universe fits into the full range of possible universes. In several cases, there are even regimes in which the likelihood of a relic abundance occurring in any logarithmic interval of abundances is nearly constant. Contrary to previous expectations, it is also found that the energy density associated with a "shadow world," with symmetric microphysics, may naturally be similar to the energy density in our world after a period of inflation. The similarity between the baryonic and dark-matter energy densities might naturally be explained if shadow baryons account for the missing mass. Implications for particle searches, the axion in particular, are also discussed. RP HODGES, HM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 79 TC 3 Z9 3 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 FEB 15 PY 1992 VL 45 IS 4 BP 1113 EP 1129 DI 10.1103/PhysRevD.45.1113 PG 17 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA HE352 UT WOS:A1992HE35200014 ER PT J AU SOKER, N AF SOKER, N TI EXCITATION OF PRESSURE MODES IN COMMON ENVELOPES SO ASTROPHYSICAL JOURNAL LA English DT Article DE BINARIES, GENERAL; STARS, INDIVIDUAL (SN-1987A); STARS, MASS LOSS; STARS, OSCILLATIONS ID DOUBLE-CORE EVOLUTION; STAR-PLANET SYSTEMS; CATACLYSMIC BINARIES; MASS-LOSS; NEBULAE; PROGENITORS; WAVES AB We study the excitation of oscillatory modes by a low-mass star orbiting inside a common envelope with a more massive star. We treat adiabatic high spherical harmonic degree (l >> 1) modes propagating outward in the envelope. The dominant oscillatory modes are those for which the spherical harmonic order is large m approximately l, and thus the amplitudes are large close to the equatorial plane and small closer to the poles. A secondary of mass approximately 1% of the primary mass excites modes with relative surface amplitudes of a few x 10%. Even a Jupiter-like brown dwarf when it is very deep in the envelope of an asymptotic giant branch star can cause perturbations of relative surface amplitudes of approximately 10% near the equatorial plane. If mass loss is influenced by oscillation then this mechanism can lead to higher mass loss in the equatorial plane. In case of an asymptotic giant branch primary this might lead to the formation of an elliptical planetary nebulae. Oscillation excitation by a low-mass secondary might also be relevant to the formation of the ring around SN 1987A. RP SOKER, N (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 34 TC 20 Z9 20 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 FEB 10 PY 1992 VL 386 IS 1 BP 190 EP 196 DI 10.1086/171004 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HC501 UT WOS:A1992HC50100020 ER PT J AU CALVET, N HARTMANN, L HEWETT, R AF CALVET, N HARTMANN, L HEWETT, R TI WINDS FROM T-TAURI STARS .2. BALMER LINE-PROFILES FOR INNER DISK WINDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE LINE, FORMATION; LINE, PROFILES; STARS, EMISSION-LINE, BE; STARS, MASS-LOSS; STARS, PRE-MAIN-SEQUENCE ID WAVE-DRIVEN WINDS; ACCRETION DISKS; RADIAL-VELOCITIES; COOL STARS; EMISSION; MODELS; ENVELOPES; ROTATION; FLOWS AB Balmer line profiles have been calculated using escape probability methods for T Tauri wind models with non-spherically symmetric geometry. The wind is assumed to originate in the inner regions of an accretion disk surrounding the T Tauri star, and flows outward in a "cone" geometry. We consider two types of wind models, both with monotonically increasing expansion velocities as a function of radial distance. For flows with large turbulent velocities, such as the high-frequency Alfven wave-driven wind models, the effect of cone geometry is to increase the blue wing emission, and to move the absorption reversal close to line center. This type of model can provide good agreement with observed H-alpha line profiles of some T Tauri stars. However, even in cone geometry turbulent wind models still tend to produce too much blueshifted absorption in H-beta and H-gamma. We have also calculated line profiles for a wind model rotating with the same angular velocity as the inner disk. The Balmer lines of this model are significantly broader than observed in most objects, suggesting that the observed emission lines do not arise in a region rotating at Keplerian velocity. Both turbulent and rotating wind models have difficulties explaining the centrally peaked emission line profiles often observed. Thus, the wind models considered here do not provide very satisfactory explanations of the Balmer line profiles of many T Tauri stars. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP CALVET, N (reprint author), CTR INVEST ASTRON,AP POSTAL 264,MERIDA 5101A,VENEZUELA. NR 40 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 FEB 10 PY 1992 VL 386 IS 1 BP 229 EP 238 DI 10.1086/171009 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HC501 UT WOS:A1992HC50100025 ER PT J AU CALVET, N HARTMANN, L AF CALVET, N HARTMANN, L TI BALMER LINE-PROFILES FOR INFALLING T-TAURI ENVELOPES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; LINE, PROFILES; STARS, EMISSION-LINE, BE; STARS, PRE-MAIN-SEQUENCE ID MAIN-SEQUENCE STARS; MAGNETIC NEUTRON STARS; X-RAY SOURCES; RADIAL-VELOCITIES; ACCRETION DISKS; FORBIDDEN-LINE; WINDS; MASS; MAGNETOSPHERE; EVOLUTION AB We consider the possibility that the Balmer emission lines of T Tauri stars arise in infalling envelopes rather than winds. Line profiles for the upper Balmer lines are presented for models with cone geometry, intended to simulate the basic features of magnetospheric accretion from a circumstellar disk. An escape probability treatment is used to determine line source functions in nonspherically symmetric geometry. We find that thermalization effects can produce nearly symmetric H-alpha line profiles at the same time the higher Balmer series lines exhibit inverse P Cygni profiles. The infall models produce centrally peaked emission line wings, in good agreement with observations of many T Tauri stars. Furthermore, if it is assumed that the flow follows a dipole pattern, infall models can produce narrow central absorption reversals that are slightly blueshifted when viewed from certain angles. We suggest that the Balmer emission of many T Tauri stars may be produced in an infalling envelope, with blueshifted absorption contributed by an overlying wind. Some of the observed narrow absorption components with small blueshifts may also arise in the accretion column. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP CALVET, N (reprint author), CTR INVEST ASTRON,AP POSTAL 264,MERIDA 5101A,VENEZUELA. NR 53 TC 107 Z9 107 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 FEB 10 PY 1992 VL 386 IS 1 BP 239 EP 247 DI 10.1086/171010 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HC501 UT WOS:A1992HC50100026 ER PT J AU CANNIZZO, JK KENYON, SJ AF CANNIZZO, JK KENYON, SJ TI THE SECONDARY OUTBURST MAXIMUM OF T-CORONAE BOREALIS - IMPLICATIONS FOR THE PHYSICS OF ACCRETION DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; BINARIES, SYMBIOTIC; STARS, INDIVIDUAL (T-CORONAE BOREALIS) ID SYMBIOTIC STARS; RECURRENT NOVAE; VISCOUS DISKS; EVOLUTION; DWARF AB We examine Webbink's hypothesis that the accretion of a torus of matter onto a main-sequence star caused secondary maxima during the 1866 and 1946 eruptions of the recurrent nova T CrB. Our simple one-dimensional hydrodynamical calculations show that the accretion disk viscosity must increase with time to produce light curves resembling observations. We adopt a model in which the viscosity parameter-alpha increases from a seed value-alpha(i) to a final value-alpha(f) via the relation alpha(t) = alpha(f)/[1 + (alpha(f)/alpha(i)) exp (-t/tau)]. The observed light curve requires alpha(i) = 10(-3) and alpha(f) = 3 if the initial torus mass is 10(-4) M. and the viscous growth time, tau, is the orbital time at the initial radius of the torus. Our model implies that the physical mechanism responsible for producing the viscous dissipation in the accretion disk has a fast growth rate and saturates to an alpha of order unity. Balbus & Hawley identify a MHD instability with the same growth rate and saturation viscosity required by our phenomenological model. The good agreement between parameters estimated from observations and those derived from a physical viscosity mechanism suggests that this instability is a promising source for the accretion disk viscosity. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 32 TC 11 Z9 11 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 FEB 10 PY 1992 VL 386 IS 1 BP L17 EP L21 DI 10.1086/186282 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HC502 UT WOS:A1992HC50200005 ER PT J AU COOKSY, AL WATSON, JKG GOTTLIEB, CA THADDEUS, P AF COOKSY, AL WATSON, JKG GOTTLIEB, CA THADDEUS, P TI THE ROTATIONAL SPECTRUM OF THE CARBON CHAIN RADICAL HCCCO SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, MOLECULES; MOLECULAR DATA; MOLECULAR PROCESSES ID MICROWAVE-SPECTRUM; WAVE SPECTRUM; GROUND-STATE; PROPADIENONE; MOLECULES; HO2 AB The bent chain radical HCCCO has been identified from laboratory measurement of 248 rotational transitions between 81 and 400 GHz. Because two molecules with the same heavy atom backbone, CCCO and HCCCHO, have already been observed in TMC-1, HCCCO is a good candidate for detection in molecular clouds and circumstellar envelopes. Rotational transition frequencies for the K(a)= 0 manifold are tabulated, as well as precise values for the rotational, centrifugal distortion, and spin-rotation constants, which allow calculation of the entire rotational spectrum into the far-IR. C1 HARVARD UNIV,DEPT CHEM,CAMBRIDGE,MA 02138. HARVARD UNIV,DIV APPL SCI,CAMBRIDGE,MA 02138. NATL RES COUNCIL CANADA,HERZBERG INST ASTROPHYS,OTTAWA K1A 0R6,ONTARIO,CANADA. RP COOKSY, AL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 18 TC 13 Z9 13 U1 1 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 FEB 10 PY 1992 VL 386 IS 1 BP L27 EP L30 DI 10.1086/186284 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HC502 UT WOS:A1992HC50200007 ER PT J AU SHIGEYAMA, T NOMOTO, K YAMAOKA, H THIELEMANN, FK AF SHIGEYAMA, T NOMOTO, K YAMAOKA, H THIELEMANN, FK TI POSSIBLE MODELS FOR THE TYPE-IA SUPERNOVA-1990N SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, DISTANCES AND REDSHIFTS; NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES; STARS, INDIVIDUAL (SN-1990N); SUPERNOVAE, INDIVIDUAL (SN-1990N); WHITE DWARFS ID WHITE-DWARF MODELS; CARBON-DEFLAGRATION SUPERNOVA; NEUTRON STAR; LIGHT-CURVE; EXPLOSIVE NUCLEOSYNTHESIS; DEGENERATE DWARF; EVOLUTION; BINARIES; NOVAE; MASS AB Possible interpretations of new spectral and photometric features of Type Ia supernova 1990N with carbon deflagration/detonation models are presented. To explain the presence of Si and Ca at high expansion velocities in SN 1990N, we suggest four possible models, among which is a carbon detonation in a white dwarf with a mass approximately 1 M.. The slow rise of the light curve of SN 1990N can be reproduced by both the deflagration and detonation models if the optical opacity is somewhat larger than that previously adopted. Implications for the Hubble constant are discussed. C1 UNIV TOKYO,FAC SCI,DEPT ASTRON,TOKYO 113,JAPAN. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP SHIGEYAMA, T (reprint author), MAX PLANCK INST ASTROPHYS,W-8046 GARCHING,GERMANY. RI Nomoto, Ken'ichi/A-4393-2011; SHIGEYAMA, TOSHIKAZU/G-4894-2014 NR 53 TC 62 Z9 62 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 FEB 10 PY 1992 VL 386 IS 1 BP L13 EP L16 DI 10.1086/186281 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HC502 UT WOS:A1992HC50200004 ER PT J AU BABB, JF SHERTZER, J AF BABB, JF SHERTZER, J TI ACCURATE NONRELATIVISTIC EXPECTATION VALUES FOR H2+ SO CHEMICAL PHYSICS LETTERS LA English DT Article AB Two separate approaches (a perturbation theory which extends the Born-Oppenheimer approximation of molecular physics and finite element analysis of the three body Coulomb problem) are used to solve the nonrelativistic Schrodinger equation for the hydrogen molecular ion ground state. For both approaches, expectation values are calculated for the bond length, the rotational constant, the permanent quadrupole moment, the Fermi contact parameter, and other operators. These results are compared with "nonadiabatic" variational results, where available. C1 COLL HOLY CROSS,WORCESTER,MA 01610. 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 12 TC 20 Z9 20 U1 0 U2 6 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 FEB 7 PY 1992 VL 189 IS 3 BP 287 EP 290 DI 10.1016/0009-2614(92)85141-V PG 4 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA HD950 UT WOS:A1992HD95000018 ER PT J AU LIGHTMAN, A GINGERICH, O AF LIGHTMAN, A GINGERICH, O TI WHEN DO ANOMALIES BEGIN SO SCIENCE LA English DT Article AB An anomaly in science is an observed fact that is difficult to explain in terms of the existing conceptual framework. Anomalies often point to the inadequacy of the current theory and herald a new one. It is argued here that certain scientific anomalies are recognized as anomalies only after they are given compelling explanations within a new conceptual framework. Before this recognition, the peculiar facts are taken as givens or are ignored in the old framework. Such a "retrorecognition" phenomenon reveals not only a significant feature of the process of scientific discovery but also an important aspect of human psychology. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. MIT,DEPT PHYS,CAMBRIDGE,MA 02139. RP LIGHTMAN, A (reprint author), MIT,PROGRAM WRITING & HUMANIST STUDIES,CAMBRIDGE,MA 02139, USA. NR 18 TC 31 Z9 31 U1 2 U2 3 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD FEB 7 PY 1992 VL 255 IS 5045 BP 690 EP 695 DI 10.1126/science.255.5045.690 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA HC506 UT WOS:A1992HC50600031 PM 17756947 ER PT J AU HO, PTP AF HO, PTP TI MILKY-WAY - WILL THE REAL GALACTIC-CENTER PLEASE STAND UP SO NATURE LA English DT Editorial Material ID BROAD HELIUM; GALAXY RP HO, PTP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 14 TC 0 Z9 1 U1 0 U2 0 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD FEB 6 PY 1992 VL 355 IS 6360 BP 495 EP 496 DI 10.1038/355495a0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA HC526 UT WOS:A1992HC52600022 ER PT J AU CREEL, S CREEL, N WILDT, DE MONFORT, SL AF CREEL, S CREEL, N WILDT, DE MONFORT, SL TI BEHAVIORAL AND ENDOCRINE MECHANISMS OF REPRODUCTIVE SUPPRESSION IN SERENGETI DWARF MONGOOSES SO ANIMAL BEHAVIOUR LA English DT Article ID NAKED MOLE-RATS; OVARIAN CYCLICITY; MARMOSET MONKEYS; PROGESTERONE; FERTILITY; EXCRETION; MAMMALS; CYCLE C1 TANZANIA NATL PARKS,SERENGETI WILDLIFE RES CTR,ARUSHA,TANZANIA. SMITHSONIAN INST,NATL ZOOL PK,CTR CONSERVAT & RES,ENDOCRINE RES LAB,FRONT ROYAL,VA 22630. PURDUE UNIV,DEPT BIOL SCI,W LAFAYETTE,IN 47907. NR 43 TC 127 Z9 130 U1 7 U2 36 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD FEB PY 1992 VL 43 IS 2 BP 231 EP 245 DI 10.1016/S0003-3472(05)80219-2 PG 15 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA HF461 UT WOS:A1992HF46100005 ER PT J AU SAYRE, EV YENER, KA JOEL, EC BARNES, IL AF SAYRE, EV YENER, KA JOEL, EC BARNES, IL TI STATISTICAL EVALUATION OF THE PRESENTLY ACCUMULATED LEAD ISOTOPE DATA FROM ANATOLIA AND SURROUNDING REGIONS SO ARCHAEOMETRY LA English DT Article DE AEGEAN; ANATOLIA; CHALCOLITHIC; BRONZE AGE; IRON AGE; LEAD ISOTOPE ANALYSIS; MULTIVARIATE STATISTICS; COPPER; LEAD; ORES; PROVENANCE ID BRONZE-AGE AB Several hundred new stable lead isotope ratio determinations of ore and slag specimens from ancient mining sites throughout Anatolia and of samples of artefacts of the Chalcolithic, Bronze Age and Early Iron Age from museum collections in Turkey and the United States have been combined with the accumulated published isotope determinations of such specimens from throughout the eastern Mediterranean and Aegean regions to form a data base of nearly 1000 analyses. It is the purpose of this paper to evaluate the practical effectiveness of using this now extensive data base to discriminate between the many sources of metals throughout this region and to propose methods to enhance this discrimination. By using the full three-dimensional isotopic data in multivariate statistical treatments and by separating isotopically resolvable source groups within some of the source areas and isolating statistically outlying specimens from them, it has been possible to characterize some ore sources more precisely and compactly and thereby achieve better resolution between ore sources. It has also been possible to isolate isotopically compatible artefact groups which possibly relate to ore sources that, as yet, have not been well defined by isotopic analysis. C1 NATL INST STAND & TECHNOL,GAITHERSBURG,MD. RP SAYRE, EV (reprint author), SMITHSONIAN INST,CTR MUSEUM SUPPORT,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560, USA. NR 62 TC 45 Z9 45 U1 1 U2 2 PU OXFORD UNIV PI OXFORD PA RES LAB ARCHAEOL HIST ART 6 KEBLE RD, OXFORD, ENGLAND OX1 3QJ SN 0003-813X J9 ARCHAEOMETRY JI Archaeometry PD FEB PY 1992 VL 34 BP 73 EP 105 DI 10.1111/j.1475-4754.1992.tb00479.x PN 1 PG 33 WC Archaeology; Chemistry, Analytical; Chemistry, Inorganic & Nuclear; Geosciences, Multidisciplinary SC Archaeology; Chemistry; Geology GA KE658 UT WOS:A1992KE65800009 ER PT J AU CEDERBLOOM, SE MOSS, MJ COHN, HN LUGGER, PM BAILYN, CD GRINDLAY, JE MCCLURE, RD AF CEDERBLOOM, SE MOSS, MJ COHN, HN LUGGER, PM BAILYN, CD GRINDLAY, JE MCCLURE, RD TI FURTHER EVIDENCE FOR A COLOR GRADIENT IN M15 SO ASTRONOMICAL JOURNAL LA English DT Article ID GLOBULAR-CLUSTER NGC-5466; X-RAY SOURCES; PHOTOGRAPHIC PHOTOMETRY; BLUE STRAGGLERS; VARIABLES; CORE; MASS AB Using data obtained at the Canada-France-Hawaii Telescope (CFHT) in subarcsecond seeing (0.5"-0.6" FWHM), we construct color maps in B - V and H-alpha - R of the central regions of the globular cluster M15. Comparison in B - V of the region within 6.6" (0.31 pc) of the cluster center with a coadded sample taken from the surrounding region demonstrates a color gradient, in the sense that the central region is bluer than the surrounding region at a high level of statistical significance. This is in agreement with the previous finding of a U - B color gradient in M15 by Bailyn et al. [AJ, 98, 882 (1989)] based on a color map with lower angular resolution. Analysis of the H-alpha - R color map indicates that the central region is "H-alpha-deficient," i.e., has a stronger H-alpha-absorption line on average than the coadded region. This result argues against the possibility that the excess blue light from the central region is due to cataclysmic variables. Instead, two possible causes of the color gradient are (1) it may be due to a centrally concentrated population of faint blue stars, possibly resulting from binary-single star interactions, and (2) it may result from a central deficit of low-mass main-sequence stars. C1 NATL RES COUNCIL CANADA,DOMINION ASTROPHYS OBSERV,VICTORIA V8X 4M6,BC,CANADA. INDIANA UNIV,DEPT ASTRON,BLOOMINGTON,IN 47405. YALE UNIV,DEPT ASTRON,NEW HAVEN,CT 06511. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 35 TC 22 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 FEB PY 1992 VL 103 IS 2 BP 480 EP & DI 10.1086/116076 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HB494 UT WOS:A1992HB49400012 ER PT J AU MIKOLAJEWSKA, J KENYON, SJ AF MIKOLAJEWSKA, J KENYON, SJ TI ON THE NATURE OF THE SYMBIOTIC BINARY AX PERSEI SO ASTRONOMICAL JOURNAL LA English DT Article ID ACCRETION DISK MODELS; ORBITAL PERIOD CHANGES; T-TAURI STARS; SPECTROSCOPIC ORBITS; FORBIDDEN LINES; BF-CYGNI; SYSTEMS; VARIABLES AB We present photometric and spectroscopic observations of the symbiotic binary AX Persei. This system contains a red giant that fills its tidal lobe and transfers material into an accretion disk surrounding a low-mass main-sequence star. The stellar masses- M(g) is similar to 1 M. for the red giant and M(h) is similar to 0.4 M. for the companion-suggest AX Per is poised to enter a common envelope phase of evolution. The disk luminosity increases from L(disk) is similar to 100 L. in quiescence to L(disk) is similar to 5700 L. in outburst for a distance of d = 2.5 kpc. Except for visual maximum, high ionization permitted emission lines-such as He II-imply an EUV luminosity comparable to the disk luminosity. High-energy photons emitted by a hot boundary layer between the disk and central star ionize a surrounding nebula to produce this permitted line emission. High ionization forbidden lines, such as [Fe VII], form in an extended, shock-excited region well out of the binary's orbital plane and may be associated with mass loss from the disk. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MIKOLAJEWSKA, J (reprint author), NICHOLAS COPERNICUS UNIV,INST ASTRON,UL CHOPINA 12-18,PL-87100 TORUN,POLAND. OI Kenyon, Scott/0000-0003-0214-609X NR 91 TC 63 Z9 63 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 FEB PY 1992 VL 103 IS 2 BP 579 EP 592 DI 10.1086/116085 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HB494 UT WOS:A1992HB49400021 ER PT J AU ARNAUD, M ROTHENFLUG, R BOULADE, O VIGROUX, L VANGIONIFLAM, E AF ARNAUD, M ROTHENFLUG, R BOULADE, O VIGROUX, L VANGIONIFLAM, E TI SOME CONSTRAINTS ON THE ORIGIN OF THE IRON ENRICHED INTRA-CLUSTER MEDIUM SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE CLUSTERS, OF GALAXIES; INTERGALACTIC MEDIUM; GALAXIES, EVOLUTION OF; X-RAYS, GENERAL ID BIMODAL STAR FORMATION; NEARBY ABELL CLUSTERS; X-RAY OBSERVATIONS; RICH CLUSTERS; ELLIPTICAL GALAXIES; CHEMICAL EVOLUTION; PERSEUS CLUSTER; HOT PLASMA; HYDROSTATIC NUCLEOSYNTHESIS; POPULATION SYNTHESIS AB We study the correlations between gas mass, iron mass and optical luminosity in clusters of galaxies. The gas mass in the intracluster medium (ICM) is highly correlated with the luminosity from ellipticals and lenticulars. The iron mass is directly proportional to it. No correlation is observed with the luminosity from spirals. Therefore we conclude that only ellipticals and lenticulars have participated in the enrichment of the ICM. Using typical mass to light ratio, we show that the gas mass is equal to 2-5 times the stellar mass present in these galaxies and we confirm that the gas mass over stellar mass ratio increases with the cluster richness. This probably means that most of the ICM is primordial in origin and that the galaxy formation (at least for ellipticals) has been less efficient in more massive clusters. The iron mass over stellar mass ratio reaches approximately 2 10(-3). We emphasize that this ratio is the physical meaningful quantity for the study of the ICM enrichment. It is indeed linked to a fundamental quantity in chemical evolution models, namely the iron mass that a given population of stars can produce: the iron yield. In clusters this ratio is more than an order of magnitude greater than in our galaxy. This constraint challenges any chemical evolution model. Whatever the model, we show that it is impossible to produce such a quantity of iron by stellar mass with a standard iron yield. We discuss other possibilities and suggest that a bimodal star formation in the cluster galaxies could better reproduce the observational constraints. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. INST ASTROPHYS, F-75014 PARIS, FRANCE. RP ARNAUD, M (reprint author), CENS, SERV ASTROPHYS, F-91191 GIF SUR YVETTE, FRANCE. NR 90 TC 243 Z9 243 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 FEB PY 1992 VL 254 IS 1-2 BP 49 EP 64 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HC817 UT WOS:A1992HC81700019 ER PT J AU PRESS, WH RYBICKI, GB HEWITT, JN AF PRESS, WH RYBICKI, GB HEWITT, JN TI THE TIME-DELAY OF GRAVITATIONAL LENS 0957+561 .1. METHODOLOGY AND ANALYSIS OF OPTICAL PHOTOMETRIC DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, OBSERVATIONS; GRAVITATIONAL LENSING; METHODS, NUMERICAL; QUASARS, INDIVIDUAL (0957+561) ID EXTRAGALACTIC OBJECTS; VARIABILITY AB When a data set's underlying covariance function (autocorrelation) can be estimated, one can construct from the data set a global chi(2) statistic that takes into account the expected statistical relationship between all pairs of points. Incorporating a projection operator, the statistic is independent of the underlying process' mean and total variance, which are poorly determined (or ill-defined) for low-frequency divergent signals. Minimizing this chi(2) gives (1) an optimal reconstruction of the underlying signal, (2) standard errors on that reconstruction, and (3) an optimal determination of additional model parameters, such as the time delay and magnitude differences of two different sets of observations. Applying this methodology to the gravitational lens 0957 + 561, and using previously published optical data, we obtain the value 536(-12)+14 days (95% confidence interval) for the delay, consistent with the less precise radio value of Lehar et al., but inconsistent with previous optical determinations, including those using the same optical data. We find that the existence of a time delay is highly significant (1% level). Monte Carlo simulations demonstrate the effect of seasonal and monthly windowing on the optical data, and show why previous analyses are likely to have given erroneous results. C1 MIT,DEPT PHYS,CAMBRIDGE,MA 02139. RP PRESS, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 31 TC 123 Z9 123 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1992 VL 385 IS 2 BP 404 EP 415 DI 10.1086/170951 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HB576 UT WOS:A1992HB57600003 ER PT J AU PRESS, WH RYBICKI, GB HEWITT, JN AF PRESS, WH RYBICKI, GB HEWITT, JN TI THE TIME-DELAY OF GRAVITATIONAL LENS 0957+561 .2. ANALYSIS OF RADIO DATA AND COMBINED OPTICAL-RADIO ANALYSIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, OBSERVATIONS; GRAVITATIONAL LENSING; METHODS, NUMERICAL; QUASARS, INDIVIDUAL (0957+561) AB The method for determining the time delay of gravitational lens 0957 + 561, which we previously applied to published optical data, is here extended and applied to the radio data of Lehar et al. The radio data are relatively free of the windowing effects of seasonal observing. For the radio data alone, our analysis gives the result tau(AB) = 548(-16)+19 days (95% C.L.). Combined analysis of the optical and radio data yield tau(AB) = 540 +/- 12 days (95% C.L.). We have also fitted for a linear drift between the two components (possibly an indication of microlensing). The radio data are consistent with zero drift (as expected theoretically), while the optical data show a small but marginally significant drift at the 2.4 sigma-level. C1 MIT,DEPT PHYS,CAMBRIDGE,MA 02139. RP PRESS, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 7 TC 72 Z9 73 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 FEB 1 PY 1992 VL 385 IS 2 BP 416 EP 420 DI 10.1086/170952 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HB576 UT WOS:A1992HB57600004 ER PT J AU KENT, SM MINK, D FAZIO, G KOCH, D MELNICK, G TARDIFF, A MAXSON, C AF KENT, SM MINK, D FAZIO, G KOCH, D MELNICK, G TARDIFF, A MAXSON, C TI GALACTIC STRUCTURE FROM THE SPACELAB INFRARED TELESCOPE .1. 2.4 MICRON MAP SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE GALAXIES, PHOTOMETRY; GALAXY, STRUCTURE; INFRARED, INTERSTELLAR, CONTINUUM ID GALAXY; REGION AB The Infrared Telescope (IRT), flown aboard the Space Shuttle as part of the Spacelab-2 mission, scanned a large fraction of the sky at 2.4-mu-m with a resolution of approximately 1-degrees. We present a calibrated map of the Galactic plane in the region -20-degrees < l < 120-degrees and -30-degrees < b < 30-degrees. The photometry is accurate to a surface brightness of mu(K) = 20.0 mag arcsec-2 . Aside from uncertainties in the magnitude zero-point, the data agree quite well with previous maps derived from balloon experiments, except that some systematic differences at high Galactic longitudes are evident. These data will permit more extensive modeling of the 2.4-mu-m emissivity in the Milky Way than has been possible previously. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 16 TC 13 Z9 13 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 FEB PY 1992 VL 78 IS 2 BP 403 EP 408 DI 10.1086/191633 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HB067 UT WOS:A1992HB06700004 ER PT J AU WELDON, PJ BRINKMEIER, WG FORTUNATO, H AF WELDON, PJ BRINKMEIER, WG FORTUNATO, H TI GULAR PUMPING RESPONSES BY JUVENILE AMERICAN ALLIGATORS (ALLIGATOR-MISSISSIPPIENSIS) TO MEAT SCENTS SO CHEMICAL SENSES LA English DT Note AB Juvenile American alligators exhibited variable rates of gular pumping to the scents of different meats, indicating that they distinguish among foods by airborne chemical cues. A chloroform extract of beef elicited more gular pumps than did chloroform alone, demonstrating that alligators detect meat-derived lipids by olfaction. C1 SMITHSONIAN TROP RES INST,APO,MIAMI,FL 34002. TEXAS A&M UNIV SYST,DEPT BIOL,COLLEGE STN,TX 77843. RP WELDON, PJ (reprint author), SMITHSONIAN INST,DEPT HERPETOL,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 7 TC 5 Z9 6 U1 1 U2 4 PU OXFORD UNIV PRESS UNITED KINGDOM PI OXFORD PA WALTON ST JOURNALS DEPT, OXFORD, ENGLAND OX2 6DP SN 0379-864X J9 CHEM SENSES JI Chem. Senses PD FEB PY 1992 VL 17 IS 1 BP 79 EP 83 DI 10.1093/chemse/17.1.79 PG 5 WC Behavioral Sciences; Food Science & Technology; Neurosciences; Physiology SC Behavioral Sciences; Food Science & Technology; Neurosciences & Neurology; Physiology GA HJ811 UT WOS:A1992HJ81100008 ER PT J AU ERWIN, DH AF ERWIN, DH TI INVERTEBRATE PALEONTOLOGY SO GEOTIMES LA English DT Article RP ERWIN, DH (reprint author), SMITHSONIAN INST,DEPT PALEOBIOL NHB121,WASHINGTON,DC 20560, USA. RI Erwin, Douglas/A-9668-2009 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOLOGICAL INST PI ALEXANDRIA PA 4220 KING ST, ALEXANDRIA, VA 22302-1507 SN 0016-8556 J9 GEOTIMES JI Geotimes PD FEB PY 1992 VL 37 IS 2 BP 31 EP 32 PG 2 WC Geosciences, Multidisciplinary SC Geology GA HC764 UT WOS:A1992HC76400023 ER PT J AU CORT, LA LEFFERTS, HL AF CORT, LA LEFFERTS, HL TI GUANGDONG CERAMICS FROM BUTUAN AND OTHER PHILIPPINE SITES - BROWN,RM SO JOURNAL OF ASIAN STUDIES LA English DT Book Review C1 DREW UNIV,MADISON,NJ 07940. RP CORT, LA (reprint author), SMITHSONIAN INST,FREER & SACKLER GALLERIES,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ASSN ASIAN STUDIES INC PI ANN ARBOR PA UNIV MICH 1 LANE HALL, ANN ARBOR, MI 48109 SN 0021-9118 J9 J ASIAN STUD JI J. Asian Stud. PD FEB PY 1992 VL 51 IS 1 BP 206 EP 207 DI 10.2307/2058409 PG 2 WC Area Studies; Asian Studies SC Area Studies; Asian Studies GA HL111 UT WOS:A1992HL11100073 ER PT J AU GARCIAGARZA, ME RODRIGUEZALMAREZ, GA BOWMAN, TE AF GARCIAGARZA, ME RODRIGUEZALMAREZ, GA BOWMAN, TE TI DISTRIBUTION OF THE POSSUM SHRIMP TAPHROMYSIS-LOUISIANAE (MYSIDACEA), INCLUDING NEW FAR INLAND RECORDS SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article AB The distribution of Taphromysis louisianae, including some previously unreported records, is mapped. This species ranges from the Florida panhandle to the northern end of the Texas Laguna Madre in fresh or brackish waters. A disjunct population has been reported from Veracruz, Mexico. Three new and far inland records are reported from the Tennessee River, Jackson County, Alabama, from the Poteau River, Le Flore County, Oklahoma, and from the Salado River, Tamaulipas, Mexico. C1 SMITHSONIAN INST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560. RP GARCIAGARZA, ME (reprint author), UNIV AUTONOMO NUEVO LEON,FAC CIENCIAS BIOL,ARTROPODOS LAB,APARTADO POSTAL 2981,MONTERREY 6400,NUEVO LEON,MEXICO. NR 9 TC 3 Z9 3 U1 0 U2 2 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 FEB PY 1992 VL 12 IS 1 BP 101 EP 103 DI 10.2307/1548724 PG 3 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA HC680 UT WOS:A1992HC68000012 ER PT J AU MCSHEA, WJ GILLES, AB AF MCSHEA, WJ GILLES, AB TI A COMPARISON OF TRAPS AND FLUORESCENT POWDER TO DESCRIBE FORAGING FOR MAST BY PEROMYSCUS-LEUCOPUS SO JOURNAL OF MAMMALOGY LA English DT Article DE PEROMYSCUS; FORAGING; FLUORESCENT DYES; TRAPPING SUCCESS ID CENTRAL TEXAS; HABITAT; PECTORALIS; MAMMALS AB The ability to quantify the foraging movements of white-footed mice (Peromyscus leucopus) using livetraps or fluorescent powder was compared. No significant shifts in the location of trap captures were detectable before, during, and after the mast-fall within the study area. Fluorescent powder trails revealed a significant shift into oak microhabitats during the mast fall and increased ground foraging during the same period. There was no significant difference in the foraging behavior of males and females. Results indicate fluorescent powder allows more sensitive monitoring of microhabitat shifts than livetrapping. RP MCSHEA, WJ (reprint author), CONSERVAT & RES CTR,DEPT CONSERVAT,NATL ZOOL PK,FRONT ROYAL,VA 22630, USA. NR 25 TC 27 Z9 28 U1 1 U2 6 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 FEB PY 1992 VL 73 IS 1 BP 218 EP 222 DI 10.2307/1381886 PG 5 WC Zoology SC Zoology GA HQ612 UT WOS:A1992HQ61200025 ER PT J AU FAUST, MA AF FAUST, MA TI OBSERVATIONS ON THE MORPHOLOGY AND SEXUAL REPRODUCTION OF COOLIA-MONOTIS (DINOPHYCEAE) SO JOURNAL OF PHYCOLOGY LA English DT Article DE ASEXUAL REPRODUCTION; BENTHIC AND EPIPHYTIC DINOFLAGELLATES; CYST; DAPI; DINOPHYCEAE; FLUORESCENCE MICROSCOPY; LIFE CYCLE; LIGHT MICROSCOPY; MANGROVE HABITAT; MORPHOLOGY; OSTREOPSIDACEAE; PYRROPHYTA; SCANNING ELECTRON MICROSCOPY, SEXUAL REPRODUCTION ID DINOFLAGELLATE GAMBIERDISCUS-TOXICUS; GYRODINIUM-UNCATENUM AB The surface morphology of the dinoflagellate Coolia monotis Meunier was compared with the surface morphology of Ostreopsis. The apical pore of C. monotis is similar in architecture to that of Ostreopsis but considerably longer (12-mu-m) than in O. heptagona (8-9-mu-m) and O. ovata (6-7-mu-m). A ventral pore in C. monotis is located on the right ventral margin between apical plate 1' and precingular plate 6" and is similar in appearance and location to the ventral pore of O. ovata. The longitudinal flagellum (20-mu-m) in C. monotis is longer than in O. ovata (12-mu-m). Although Coolia and Ostreopsis appear to be distinctly different and should remain as two separate genera, they appear to be related. Cells of C. monotis divided by binary fission. Doubling time was 3-4 days in the logarithmic phase of growth at 23-degrees-C, 12:12 h L:D, 30-90-mu-E.m-2.s-1, and a salinity of 36 parts per thousand. Cultures reached cell densities of 2.5 x 10(3) cells.L-1 after 15 days of growth. The sexual process in C. monotis occurred in Erdschreiber's medium when Danish soil extract was substituted with mangrove sediment extract under the culture conditions described above. Gamete fusion produced large biflagellated planozygotes (70-75-mu-m diam). Planozygote maturation involved cytoplasmic reorganization, loss of motility, development of a spherical shape (80-90-mu-m diam), and two to three orange accumulation bodies. The cells at this stage appeared to be thin-walled cysts. Further development included reorganization of cyst contents, emergence of non-motile gametes, and development of chloroplasts, sulcus, and girdle. The nucleus of the newly formed cells occupied 50% or more of the total cell volume. Meiosis occurred in the cyst, but nuclear cyclosis was not observed. Four daughter cells were produced within 36-48 h, and motile gametes developed. The gametes exhibited sexuality for 2 months and completed the sexual life cycle by going through a thin-walled cyst stage. RP FAUST, MA (reprint author), SMITHSONIAN INST,CTR MUSEUM SUPPORT,DEPT BOT,4201 SILVER HILL RD,SUITLAND,MD 20746, USA. NR 43 TC 39 Z9 41 U1 0 U2 7 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 FEB PY 1992 VL 28 IS 1 BP 94 EP 104 PG 11 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA HE700 UT WOS:A1992HE70000014 ER PT J AU TINE, S AIELLO, S BELLENI, A PESTELLINI, CC AF TINE, S AIELLO, S BELLENI, A PESTELLINI, CC TI A SOLUTION TO THE PROBLEM OF RADIATION TRANSFER IN INHOMOGENEOUS-MEDIA USING THE SHM SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article ID SPACE-DEPENDENT ALBEDO; PLANE-PARALLEL MEDIUM; DARK CLOUDS; SCATTERING AB We extend the spherical harmonics method (SHM) to solve the radiative transfer equation for the case of radially-varying extinction and scattering coefficients. The formalism is first introduced and discussed. Some numerical results of astrophysical importance are then presented. C1 UNIV FLORENCE,DIPARTIMENTO ASTRON & SCI SPAZIO,I-50121 FLORENCE,ITALY. UNIV FLORENCE,DIPARTIMENTO INGN CIVILE,I-50121 FLORENCE,ITALY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OI Cecchi Pestellini, Cesare/0000-0001-7480-0324 NR 19 TC 8 Z9 8 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD FEB PY 1992 VL 47 IS 2 BP 95 EP 102 DI 10.1016/0022-4073(92)90067-E PG 8 WC Optics; Spectroscopy SC Optics; Spectroscopy GA HD750 UT WOS:A1992HD75000003 ER PT J AU POST, RC AF POST, RC TI AMERICAN NARROW GAUGE RAILROADS - HILTON,GW SO PACIFIC HISTORICAL REVIEW 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 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 FEB PY 1992 VL 61 IS 1 BP 135 EP 137 PG 3 WC History SC History GA HH611 UT WOS:A1992HH61100019 ER PT J AU SADEGHPOUR, HR GREENE, CH CAVAGNERO, M AF SADEGHPOUR, HR GREENE, CH CAVAGNERO, M TI EXTENSIVE EIGENCHANNEL R-MATRIX STUDY OF THE H- PHOTODETACHMENT SPECTRUM SO PHYSICAL REVIEW A LA English DT Article ID DOUBLY-EXCITED-STATES; QUANTUM-DEFECT THEORY; HYDROGENIC THRESHOLDS; MOLECULAR DESCRIPTION; ELECTRON-HYDROGEN; 2-ELECTRON ATOMS; CROSS-SECTION; RESONANCES; ION; CLASSIFICATION AB We combine an eigenchannel R-matrix calculation with an analytic description of electron motion in a dipole field to predict photodetachment cross sections of the hydrogen negative ion, including resonant structures up to the n = 4 hydrogenic threshold. Partial cross sections for the production of hydrogen-atom fragments in states with specific principal quantum numbers n are also presented for comparison with a recent experiment. An analysis of the delay-time matrix indicates that the autodetaching Feshbach resonances decay primarily into the nearest energetically accessible continuum channel, an observation which is not at all apparent from the calculated and observed partial cross sections, but has been anticipated in previous theoretical work. We find, for instance, that the n = 4{upsilon = 0} m = 4A = + resonant state below the H(n = 4) threshold decays 73% of the time to the 3{0}+ photodetachment channel. C1 UNIV COLORADO,DEPT PHYS,BOULDER,CO 80309. UNIV COLORADO,JOINT INST LAB ASTROPHYS,BOULDER,CO 80309. UNIV KENTUCKY,DEPT PHYS & ASTRON,LEXINGTON,KY 40506. RP SADEGHPOUR, HR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Greene, Chris/C-3821-2011 OI Greene, Chris/0000-0002-2096-6385 NR 49 TC 87 Z9 87 U1 0 U2 5 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 FEB 1 PY 1992 VL 45 IS 3 BP 1587 EP 1595 DI 10.1103/PhysRevA.45.1587 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA HC995 UT WOS:A1992HC99500042 ER PT J AU YOSHINO, K ESMOND, JR CHEUNG, ASC FREEMAN, DE PARKINSON, WH AF YOSHINO, K ESMOND, JR CHEUNG, ASC FREEMAN, DE PARKINSON, WH TI HIGH-RESOLUTION ABSORPTION CROSS-SECTIONS IN THE TRANSMISSION WINDOW REGION OF THE SCHUMANN-RUNGE BANDS AND HERZBERG CONTINUUM OF O-2 SO PLANETARY AND SPACE SCIENCE LA English DT Article ID MOLECULAR-OXYGEN PHOTODISSOCIATION; OSCILLATOR-STRENGTHS; AERONOMIC PROBLEMS; NM; RATES; STATE AB The absorption cross sections of the Schumann-Runge bands in the window region between the rotational lines have been measured in the wavelength region 180-195 nm. The measurements have been done with many different pressures of oxygen, 2.5-760 torr, so that the pressure-dependent absorption can be separated from the main cross sections. The published cross sections [Yoshino et al., Planet. Space Sci. 31, 339 (1983)] in the window region are superseded by the present cross sections. The combined cross sections are presented graphically here and are available at wavenumber intervals of approximately 0.1 cm-1 as numerical compilations stored on magnetic tape, from the National Space Science Data Center, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, U.S.A. The Herzberg continuum cross sections are derived after subtracting calculated contributions from the Schumann Runge bands and are significantly smaller than any previous measurements. RP YOSHINO, K (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 24 TC 61 Z9 62 U1 0 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD FEB-MAR PY 1992 VL 40 IS 2-3 BP 185 EP 192 DI 10.1016/0032-0633(92)90056-T PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HL073 UT WOS:A1992HL07300002 ER PT J AU DALGARNO, A BABB, JF SUN, Y AF DALGARNO, A BABB, JF SUN, Y TI RADIATIVE ASSOCIATION IN PLANETARY-ATMOSPHERES SO PLANETARY AND SPACE SCIENCE LA English DT Article ID TEMPERATURE-DEPENDENCE; CHARGE-TRANSFER; NITRIC-OXIDE; PREDISSOCIATION; ABSORPTION; BANDS; NO; COLLISIONS; NIGHTGLOW; CONTINUUM AB A summary account is presented of radiative association processes that may be significant in producing continuum emission in the atmospheres of the planets. The importance of the radiative association of N and O and of NO + O has been established by the presence in the airglow of the emission spectra. The possible contributions of O + O, O + O2 and O+ + O are discussed. The radiative association of He+ and H may be an important source of HeH+ in the Jovian ionospheres. RP DALGARNO, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Babb, James/0000-0002-3883-9501 NR 44 TC 15 Z9 15 U1 1 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD FEB-MAR PY 1992 VL 40 IS 2-3 BP 243 EP 246 DI 10.1016/0032-0633(92)90062-S PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HL073 UT WOS:A1992HL07300008 ER PT J AU ADAMS, RM AF ADAMS, RM TI SMITHSONIAN HORIZONS SO SMITHSONIAN LA English DT Editorial Material RP ADAMS, RM (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD FEB PY 1992 VL 22 IS 11 BP 8 EP 8 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA HB018 UT WOS:A1992HB01800001 ER PT J AU WEEKES, TC AF WEEKES, TC TI TEV RADIATION FROM GALACTIC SOURCES SO SPACE SCIENCE REVIEWS LA English DT Review ID ENERGY GAMMA-RAYS; NEUTRAL PARTICLES; VELA X-1; COS-B; MOLECULAR CLOUDS; 1ST OBSERVATION; CRAB-NEBULA; CYG X-3; X-RAY; CYGNUS-X-3 AB The detection of the Crab Nebula as a steady source of TeV gamma rays puts the field of Very High Energy Gamma-Ray Astronomy on a firm observational basis and permits a critical re-assessment of the claims for the detection of a multitude of episodic binary sources. A new generation of detectors in the TeV and PeV energy regions is coming on-line; together with the telescopes of the Gamma-Ray Observatory these instruments will present a new perspective on one of the last frontiers of astronomy. RP WEEKES, TC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,AMADO,AZ 85645, USA. NR 162 TC 71 Z9 71 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1992 VL 59 IS 3-4 BP 315 EP 364 PG 50 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HE173 UT WOS:A1992HE17300002 ER PT J AU NAVEAU, V AF NAVEAU, V TI A FEW WORDS ON TRAINING SO TRAINING & DEVELOPMENT LA English DT Letter RP NAVEAU, V (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC TRAINING DEVELOPMENT PI ALEXANDRIA PA 1640 KING ST, BOX 1443, ALEXANDRIA, VA 22313-2043 SN 1055-9760 J9 TRAINING DEV JI Train. Dev. PD FEB PY 1992 VL 46 IS 2 BP 4 EP 4 PG 1 WC Business SC Business & Economics GA HC875 UT WOS:A1992HC87500002 ER PT J AU MILLER, S TENNYSON, J LEPP, S DALGARNO, A AF MILLER, S TENNYSON, J LEPP, S DALGARNO, A TI IDENTIFICATION OF FEATURES DUE TO H-3+ IN THE INFRARED-SPECTRUM OF SUPERNOVA 1987A SO NATURE LA English DT Article ID FUNDAMENTAL-BAND; JUPITER; MOLECULES; CLOUDS AB THE molecular ion H-3(+) occupies a central position in theoretical models of interstellar chemistry 1,2. It forms readily in hydrogen-rich interstellar gas clouds when ionized H-2 reacts with neutral H-2. The H-3(+) ion can then donate a proton to oxygen, carbon and other heavy atoms. From this beginning nearly 100 different interstellar molecules are formed, such as the reactive hydroxyl radical OH, neutral CO, ethanol, the linear polyacetylenes HC(x)N and cyclic species such as cyclopropenylidene, C3H3. But in spite of a decade of searching 3,4, H-3(+) has eluded detection except in the hydrogen-rich atmosphere of Jupiter 5. Here we present evidence for the presence of H-3(+) in the envelope of supernova 1987 A, where it is produced by an unusual chemistry in which excited hydrogen atoms are the main source of molecule formation. Infrared spectra of SN1987A (ref. 6) in the first few hundred days after the explosion contain two previously unidentified peaks which we attribute to H-3(+). Chemical modelling produces quantities of H-3(+) consistent with the observed peak intensities, and also predicts significant amounts of HeH+, which may be responsible for some weaker features in the spectra. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP UNIV LONDON UNIV COLL, DEPT PHYS & ASTRON, GOWER ST, LONDON WC1E 6BT, ENGLAND. RI Tennyson, Jonathan/I-2222-2012 OI Tennyson, Jonathan/0000-0002-4994-5238 NR 16 TC 83 Z9 82 U1 0 U2 1 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 JAN 30 PY 1992 VL 355 IS 6359 BP 420 EP 422 DI 10.1038/355420a0 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA HB530 UT WOS:A1992HB53000058 ER PT J AU HEANEY, PJ POST, JE AF HEANEY, PJ POST, JE TI THE WIDESPREAD DISTRIBUTION OF A NOVEL SILICA POLYMORPH IN MICROCRYSTALLINE QUARTZ VARIETIES SO SCIENCE LA English DT Article ID LENGTH-SLOW CHALCEDONY; DIFFRACTION AB An x-ray examination of more than 150 specimens of fine-grained quartz varieties from around the world has revealed that more than 10% and as much as 80% of the silica in many samples is actually moganite, a little-known silica polymorph. Rietveld refinements of 50 powder x-ray diffraction patterns produced by fibrous quartz (agate, chalcedony) and nonfibrous quartz (chert, flint) indicate that the concentrations of moganite within each subgroup are widely distributed. The large amount of moganite (> 30%) found in cherts from arid, alkaline environments may resurrect length-slow silica as an indicator of evaporitic regimes, and the absence of moganite in weathered and hydrothermally altered silica samples may be a useful measure of fluid-rock interaction. C1 SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560. NR 22 TC 110 Z9 112 U1 2 U2 14 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD JAN 24 PY 1992 VL 255 IS 5043 BP 441 EP 443 DI 10.1126/science.255.5043.441 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA HA590 UT WOS:A1992HA59000032 PM 17842895 ER PT J AU DONAHUE, M STOCKE, JT GIOIA, IM AF DONAHUE, M STOCKE, JT GIOIA, IM TI DISTANT COOLING FLOWS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COOLING FLOWS; GALAXIES; CLUSTERING; X-RAYS; GALAXIES ID MEDIUM-SENSITIVITY SURVEY; X-RAY SPECTROSCOPY; EMISSION-LINE GAS; RADIATIVE ACCRETION; LUMINOSITY FUNCTIONS; CLUSTER GALAXIES; STAR FORMATION; EINSTEIN; EVOLUTION; REDSHIFT AB Luminous, extended H-alpha emission has been detected in 14 distant X-ray-selected clusters of galaxies (0.07 < z < 0.37). Eleven of these detections are from a complete flux-limited sample (f(x) greater-than-or-equal-to 8 x 10(-13) ergs cm-2 s-1, delta greater-than-or-equal-to -20-degrees) of 23 clusters extracted from the Einstein Extended Medium-Sensitivity Survey (EMSS). The H-alpha detections indicate the presence of cool gas embedded within hotter, X-ray-emitting cluster gas, a signature of a massive cooling flow. We draw several conclusions about the distant cooling flows revealed by their H-alpha emission. The X-ray and optical properties of these distant cooling flows are similar to cooling flows found nearby (z < 0.1). If extended H-alpha emission is an unbiased indicator of a cooling flow (i.e., the relationship between the presence of a cooling flow and detectable H-alpha emission does not change with redshift), then the fraction of X-ray-emitting clusters that possess massive cooling flows has decreased by a factor of about 2 since z approximately 0.3. The EMSS is rich in distant cooling flow clusters, not because of a selection effect as previously suggested but because cooling flow clusters comprised a large percentage of X-ray-emitting clusters in the past. There is limited evidence that the cosmological evolution of cooling flow clusters may be different from the non-cooling flow clusters. Also, accounting for the expected differences in the spatial extent of the X-ray emission of cooling flow and non-cooling flow clusters does not alter the conclusion of Gioia et al. that X-ray-luminous clusters have increased in number and/or luminosity since z approximately 0.3. One candidate luminous blue arc has been discovered in the course of this study. C1 UNIV COLORADO,CTR ASTROPHYS & SPACE ASTRON,BOULDER,CO 80309. UNIV COLORADO,DEPT ASTROPHYS PLANETARY & ATMOSPHER SCI,BOULDER,CO 80309. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CNR,INST RADIOASTRON,I-40126 BOLOGNA,ITALY. RI Donahue, Megan/B-5361-2012; Gioia, Isabella/B-6982-2012; OI Gioia, Isabella/0000-0003-3127-498X; Donahue, Megan/0000-0002-2808-0853 NR 58 TC 78 Z9 78 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 JAN 20 PY 1992 VL 385 IS 1 BP 49 EP & DI 10.1086/170914 PN 1 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GZ903 UT WOS:A1992GZ90300005 ER PT J AU JOHNSTON, KJ GAUME, R STOLOVY, S WILSON, TL WALMSLEY, CM MENTEN, KM AF JOHNSTON, KJ GAUME, R STOLOVY, S WILSON, TL WALMSLEY, CM MENTEN, KM TI THE DISTRIBUTION OF THE 62-61 AND 52-51 E-TYPE METHANOL MASERS IN OMC-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, KINEMATICS AND DYNAMICS; ISM, MOLECULES; ISM, STRUCTURE; MASERS ID ORION-KL; CO OUTFLOW; KINEMATICS; NEBULA; REGION; TRANSITIONS; EMISSION; AMMONIA; MAPS AB The 6(2)-6(1) and 5(2)-5(1) E transitions of CH3OH have been mapped toward the Orion-KL region with an angular resolution of 3" and a frequency resolution of 12 kHz (= 0.15 km s-1). There are at least 16 masers of flux density greater than 3 Jy. These are distributed in a 40" long crescent shaped region, extending from NW to SE around the "hot core." The radial velocities and positions of some of these masers agree with a peak of the 8(0)-7(1) A transition of CH3OH, near 95 GHz. The most intense 6(2)-6(1) E maser is unresolved; the flux density of 103 Jy and size of less than 1".1 give a brightness temperature of greater than 10(5) K. The FWHP line widths, including the instrumental resolution, range from less than 0.15 km s-1 (unresolved) to 1 km s-1. What have been previously cataloged as spatially extended individual masers are most likely blends of maser components with slightly different radial velocities. The E-type masers in Orion appear to cluster on scale sizes of less than 3". From a multiline analysis and our limits to maser source sizes, the column densities in the regions with the most intense lines are greater than 2 x 10(22) cm-2. The spatial distribution and the observed velocities suggest that the methanol masers arise from high column density gas-adjacent to the Hot Core. The masers may be located very near the interface of the high-velocity outflow and the surrounding dense gas. C1 MAX PLANCK INST RADIOASTRON,W-5300 BONN 1,GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP JOHNSTON, KJ (reprint author), USN,RES LAB,CTR ADV SPACE SENSING,CODE 4200,WASHINGTON,DC 20375, USA. NR 30 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 JAN 20 PY 1992 VL 385 IS 1 BP 232 EP 239 DI 10.1086/170930 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GZ903 UT WOS:A1992GZ90300021 ER PT J AU JAFFE, DT GRAF, UU HARRIS, AI STUTZKI, J LEPP, SH AF JAFFE, DT GRAF, UU HARRIS, AI STUTZKI, J LEPP, SH TI DETECTION OF HCO+ J=9-]8 LINE EMISSION TOWARD ORION IRC2 - MOLECULAR-IONS IN HOT DENSE GAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE LINE, IDENTIFICATION; ISM, INDIVIDUAL (ORION IRC2); ISM, MOLECULES ID HIGH-VELOCITY HCO+; INTERSTELLAR CLOUDS; ROTATIONAL-EXCITATION; SHOCK CHEMISTRY; PHASE CHEMISTRY; 1ST DETECTION; GHZ LINE; ABUNDANCES; COLLISIONS; IONIZATION AB We have detected the HCO+ J = 9 --> 8 802.458 GHz transition toward IRc2 in Orion. The line width implies that the emission originates in the low-velocity flow/doughnut most likely 10" or less from IRc2. If the line is optically thin, the density in the line-forming region is 10(7) cm-3 or higher. If the HCO+ line arises in the same approximately 10" x 20" source as other lines with similar width, the total column density of HCO+ is 3 x 10(14) cm-2 or higher, implying a line-of-sight averaged abundance 2 x 10(-9) or more. This abundance is significantly greater than would be expected in a high-density region. Equilibrium chemical models predict an abundance more than an order of magnitude lower than observed. Enhancement of HCO+ by local ultraviolet and X-ray fields is probably also insufficient to explain the observations. Time-dependent enhancement of the HCO+ abundance in shocks may offer an explanation, if initial conditions are appropriate, but published models are not relevant to the conditions immediately around IRc2. Under some circumstances, mechanisms which lower the electron abundance may also be able to raise the HCO+ abundance to the observed value. C1 MAX PLANCK INST PHYS & ASTROPHYS, INST EXTRATERR PHYS, W-8046 GARCHING, GERMANY. UNIV COLOGNE, INST PHYS 1, W-5000 COLOGNE 41, GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP UNIV TEXAS, DEPT ASTRON, RL MOORE HALL, AUSTIN, TX 78712 USA. NR 44 TC 7 Z9 7 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 JAN 20 PY 1992 VL 385 IS 1 BP 240 EP 243 DI 10.1086/170931 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GZ903 UT WOS:A1992GZ90300022 ER PT J AU MUNDY, LG WOOTTEN, A WILKING, BA BLAKE, GA SARGENT, AI AF MUNDY, LG WOOTTEN, A WILKING, BA BLAKE, GA SARGENT, AI TI IRAS-16293-2422 - A VERY YOUNG BINARY-SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; INFRARED, STARS; STARS, INDIVIDUAL (IRAS-16293-2422); STARS, PRE-MAIN-SEQUENCE ID SPECTRAL ENERGY-DISTRIBUTIONS; OPHIUCHI INFRARED CLUSTER; MAIN-SEQUENCE BINARIES; LOW-MASS STARS; RHO-OPHIUCHI; IRAS 16293-2422; MOLECULAR CLOUDS; STELLAR OBJECTS; T-TAURI; OUTFLOW AB We present 4".5 x 2".5 resolution millimeter wavelength observations of the young far-infrared source IRAS 16293-2422 which resolve the continuum emission into two sources, MM 1 and MM 2. These sources coincide with known radio continuum sources and may constitute a very young binary system with a projected separation of 840 AU. Flux measurements from 18 cm to 25-mu-m show that the majority of the millimeter wavelength emission arises from dust within 300 AU of the individual central objects. The total dynamical mass of 1.1-1.3 M., coupled with our mass estimates for MM 1 and MM 2, suggests that the mass in circumstellar material is comparable to that of the central stellar cores. Since the stellar masses are constrained to be less-than-or-equal-to 0.5 M. each, it is likely that the bolometric luminosity of 30-40 L. is derived mainly from accretion of the observed circumstellar material. Maps of the J = 2, 3-1, 2 transition of SO obtained simultaneously show that this emission is centered on MM 1, with weaker emission in a clumpy distribution to the east and west. No SO emission is detected toward MM 2, indicating an upper limit to the fractional abundance which is a factor of 10 below that toward MM 1. We propose that the SO emission toward MM 1 is a result of the outflow activity associated with this source and that the outlying emission clumps trace regions of mild interaction between the outflow and the ambient cloud. C1 NATL RADIO ASTRON OBSERV,CHARLOTTESVILLE,VA 22903. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV MISSOURI,DEPT PHYS & ASTRON,ST LOUIS,MO 63121. CALTECH,DEPT GEOL & PLANETARY SCI,PASADENA,CA 91125. CALTECH,OWENS VALLEY RADIO OBSERV,PASADENA,CA 91125. RP MUNDY, LG (reprint author), UNIV MARYLAND,ASTRON PROGRAM,COLLEGE PK,MD 20742, USA. NR 54 TC 111 Z9 111 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 JAN 20 PY 1992 VL 385 IS 1 BP 306 EP 313 DI 10.1086/170939 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GZ903 UT WOS:A1992GZ90300030 ER PT J AU CARROLL, SM FARHI, E GUTH, AH AF CARROLL, SM FARHI, E GUTH, AH TI AN OBSTACLE TO BUILDING A TIME MACHINE SO PHYSICAL REVIEW LETTERS LA English DT Article ID 2+1 DIMENSIONAL GRAVITY; SPACE-TIME; SCATTERING AB Gott has shown that a spacetime with two infinite parallel cosmic strings passing each other with sufficient velocity contains closed timelike curves. We discuss an attempt to build such a time machine. Using the energy-momentum conservation laws in the equivalent (2 + 1)-dimensional theory, we explicitly construct the spacetime representing the decay of one gravitating particle into two. We find that there is never enough mass in an open universe to build the time machine from the products of decays of stationary particles. More generally, the Gott time machine cannot exist in any open (2 + 1)-dimensional universe for which the total momentum is timelike. C1 MIT,CTR THEORET PHYS,NUCL SCI LAB,CAMBRIDGE,MA 02139. MIT,DEPT PHYS,CAMBRIDGE,MA 02139. RP CARROLL, SM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 20 TC 39 Z9 39 U1 1 U2 6 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 JAN 20 PY 1992 VL 68 IS 3 BP 263 EP 266 DI 10.1103/PhysRevLett.68.263 PG 4 WC Physics, Multidisciplinary SC Physics GA GZ967 UT WOS:A1992GZ96700003 ER PT J AU KNOWLTON, N WEIL, E WEIGT, LA GUZMAN, HM AF KNOWLTON, N WEIL, E WEIGT, LA GUZMAN, HM TI SIBLING SPECIES IN MONTASTRAEA-ANNULARIS, CORAL BLEACHING, AND THE CORAL CLIMATE RECORD SO SCIENCE LA English DT Article ID REEF-CORALS; SCLERACTINIAN CORALS; GROWTH; FLORIDA; REPRODUCTION; PATTERNS; SOLANDER; DEPTH; ELLIS AB Measures of growth and skeletal isotopic ratios in the Caribbean coral Montastraea annularis are fundamental to many studies of paleoceanography, environmental degradation, and global climate change. This taxon is shown to consist of at least three sibling species in shallow waters. The two most commonly studied of these show highly significant differences in growth rate and oxygen isotopic ratios, parameters routinely used to estimate past climatic conditions; unusual coloration in the third may have confused research on coral bleaching. Interpretation or comparison of past and current studies can be jeopardized by ignoring these species boundaries. RP KNOWLTON, N (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. NR 35 TC 209 Z9 219 U1 0 U2 17 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD JAN 17 PY 1992 VL 255 IS 5042 BP 330 EP 333 DI 10.1126/science.255.5042.330 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA GZ695 UT WOS:A1992GZ69500042 PM 17779583 ER PT J AU GUTH, AH JAIN, B AF GUTH, AH JAIN, B TI DENSITY-FLUCTUATIONS IN EXTENDED INFLATION SO PHYSICAL REVIEW D LA English DT Article ID UNIVERSE; PERTURBATIONS; COSMOLOGIES; SCENARIO; GRAVITY AB We estimate the density perturbation spectrum delta-rho/rho in the extended inflationary model, in which the scalar curvature is coupled to a Brans-Dicke field. Through a conformal transformation and a redefinition of the Brans-Dicke field, the action of the theory is cast into a form with no coupling to the scalar curvature and a canonical kinetic term for the redefined field. Following Kolb, Salopek, and Turner, we calculate delta-rho/rho using the transformed action and the standard recipe developed for conventional inflation. This recipe is expected to give a valid order-of-magnitude estimate, but a precise calculation would require a more careful treatment of several aspects of the problem. The spectrum behaves as a positive power of the wavelength, a feature that might be useful in building models to account for the observed large-scale structure of the universe. Our result for the overall amplitude of density perturbations differs slightly from that of the previous authors, and the reasons for these differences are discussed. We also point out that the conformal transformation method can be applied to a wider class of generalized gravity theories. C1 MIT,DEPT PHYS,CAMBRIDGE,MA 02139. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP GUTH, AH (reprint author), MIT,CTR THEORET PHYS,NUCL SCI LAB,CAMBRIDGE,MA 02139, USA. NR 23 TC 31 Z9 31 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 JAN 15 PY 1992 VL 45 IS 2 BP 426 EP 432 DI 10.1103/PhysRevD.45.426 PG 7 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA HB215 UT WOS:A1992HB21500006 ER PT J AU SADEGHPOUR, HR AF SADEGHPOUR, HR TI RESONANT ELECTRON HYDROGEN-ATOM SCATTERING USING HYPERSPHERICAL COORDINATE METHOD SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Letter ID DOUBLY EXCITED-STATES; QUANTUM-DEFECT THEORY; INTERMEDIATE ENERGIES; ELASTIC-SCATTERING; EXCITATION; CLASSIFICATION; THRESHOLDS; CHANNELS; IMPACT AB The scattering of unpolarized electrons from hydrogen atoms is treated using the hyperspherical coordinate and the multichannel quantum defect approach with particular emphasis on the formation of quasi-stable resonant e--H complexes. Resonant positions and widths, formed below the H(n = 2), H(n = 3), and H(n = 4) thresholds, are calculated for symmetries 1,3S(e), 3P(o), and 1D(e). Resonant cross sections are also given for the singlet and triplet L = 0 partial waves. Good agreement is found with other more computationally intensive calculations. RP SADEGHPOUR, HR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 34 TC 15 Z9 15 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 JAN 14 PY 1992 VL 25 IS 1 BP L29 EP L35 DI 10.1088/0953-4075/25/1/006 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA HA952 UT WOS:A1992HA95200006 ER PT J AU RAMELLA, M GELLER, MJ HUCHRA, JP AF RAMELLA, M GELLER, MJ HUCHRA, JP TI THE DISTRIBUTION OF GALAXIES WITHIN THE GREAT WALL SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, OBSERVATIONS; GALAXIES, CLUSTERING; GALAXIES, DISTANCES AND REDSHIFTS ID LARGE-SCALE DISTRIBUTION; REDSHIFT SURVEY SLICES; LUMINOSITY FUNCTION; UNIVERSE AB We examine the galaxy distribution within the "Great Wall," the most striking feature in the first three "slices" of the CfA redshift survey extension. We extract the Great Wall from the sample and analyze it by counting galaxies in cells. We compute the "local" two-point correlation function within the Great Wall and estimate the local correlation length, s0GW. We obtain s0GW congruent-to 15 h-1 Mpc, approximately 3 times larger than the correlation length for the entire sample (de Lapparent et al.). The redshift distribution of galaxies in the pencil-beam survey by Broadhurst et al. shows peaks separated by large "voids," at least to a redshift z congruent-to 0.3. The peaks might represent the intersections of their approximately 5 h-1 Mpc pencil beams with structures similar to the Great Wall (Broadhurst et al.). Under this hypothesis, sampling of the Great Wall shows that l congruent-to 12 h-1 Mpc is the minimum projected beam size required to detect all the "walls" at redshifts between the peak of the selection function and the effective depth of the survey. (We use a Hubble constant H0 = 100 h km s-1 Mpc. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP RAMELLA, M (reprint author), OSSERV ASTRON TRIESTE,VIA GB TIEPOLO 11,I-34131 TRIESTE,ITALY. NR 15 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 JAN 10 PY 1992 VL 384 IS 2 BP 396 EP 403 DI 10.1086/170882 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GY758 UT WOS:A1992GY75800002 ER PT J AU POSTMAN, M HUCHRA, JP GELLER, MJ AF POSTMAN, M HUCHRA, JP GELLER, MJ TI THE DISTRIBUTION OF NEARBY RICH CLUSTERS OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERING; GALAXIES, DISTANCES AND REDSHIFTS ID X-RAY-CLUSTERS; ABELL CLUSTERS; VELOCITY DISPERSIONS; RADIAL-VELOCITIES; CATALOG; REDSHIFTS; SUPERCLUSTER; SCALE AB We have acquired redshifts for a complete sample of 351 Abell clusters with tenth-ranked galaxy magnitudes (m10) less than or equal to 16.5, including 115 entirely new cluster redshifts. The survey includes all such clusters which lie north of delta = -27-degrees-30' and is the largest magnitude-limited redshift survey of rich clusters to date. Analysis of the spatial distribution of these clusters reveals no clustering on scales larger than 75h-1 Mpc; we do not detect the large supercluster complexes reported by Tully. The correlation length is 20.0(+/- 4.3)h-1 Mpc, consistent with the results from other surveys. The frequency of voids with radii of order 60h-1 Mpc or less is consistent with the form and amplitude of the observed two-point correlation function. There is no significant difference between the clustering properties of RC = 0 and RC greater-than-or-equal-to 1 clusters. A percolation analysis yields 23 superclusters, 17 of which are new. The superclusters are not significantly elongated in the radial direction; large-scale peculiar motions are of order 1000 km s-1 or less. Dramatically new constraints on the large-scale cluster distribution will require surveys an order of magnitude larger. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP POSTMAN, M (reprint author), JOHNS HOPKINS UNIV,INST SPACE TELESCOPE SCI,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. OI Postman, Marc/0000-0002-9365-7989 NR 51 TC 187 Z9 187 U1 1 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 JAN 10 PY 1992 VL 384 IS 2 BP 404 EP 422 DI 10.1086/170883 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GY758 UT WOS:A1992GY75800003 ER PT J AU VIEGAS, SM DALPINO, EMD AF VIEGAS, SM DALPINO, EMD TI THE ORIGIN OF THE OPTICAL-EMISSION LINES ASSOCIATED WITH EXTRAGALACTIC RADIO-SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, JETS; LINE, FORMATION; RADIO CONTINUUM, GALAXIES; STARS, FORMATION ID ACTIVE GALACTIC NUCLEI; EMITTING GAS; CENTAURUS-A; IONIZED-GAS; GALAXIES; MODELS; REGION; ALIGNMENT; FILAMENTS; JET AB We investigate the observed extended emission-line regions (EELRs) associated with the jets and lobes of low-redshift extragalactic radio sources with moderate power (3C 227, 3C 277.3, 3C 305, Cen A [NGC 5128], NGC 7385, PKS 0349-27, PKS 2152-69, and Minkowski's Object). Using hybrid models which take into account the coupled effect of both the photoionization by a nonthermal radiation and the thermal collisions due to shocks, we calculated the line intensity ratio diagrams that best fit the observations. We found that the main energy sources of the EELR are: (1) a power-law radiation, with a flux at 1 Ryd F(H) congruent-to (10(8)-10(10)) cm-2 s-1 eV-1 and a spectral index alpha = 2.2-2.8 (equivalent to 1.2-1.8 for a flux given in units of ergs cm-2 s-1 eV-1), which probably originates at the central region of the galaxy, and (2) shocks with velocities v0 congruent-to 300-1000 km s-1 and preshock densities n0 congruent-to 5-100 cm-3, resulting from the interaction of the relativistic plasma flow with the ambient medium. In all cases investigated, a [N/O] underabundance by a factor 4 relative to the cosmic value is required in order to explain the observed [N II]/[O II] line ratios. The ability of radio jets to interact with the ambient medium and stimulate star formation has been suggested by a number of observational works and demonstrated by a number of authors. Considering both the estimated lifetimes of the radio sources and the stellar evolution time scales, the [N/O] underabundance could be explained by a burst of star formation where only the more massive stars (M greater-than-or-equal-to 8 M.) have already evolved. C1 EUROPEAN SO OBSERV,W-8046 GARCHING,GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP VIEGAS, SM (reprint author), UNIV SAO PAULO,INST ASTRON & GEOFIS,AV MIGUEL STEFANO 4200,BR-04301 SAO PAULO,BRAZIL. RI de Gouveia Dal Pino, Elisabete/H-9560-2013 OI de Gouveia Dal Pino, Elisabete/0000-0001-8058-4752 NR 52 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 JAN 10 PY 1992 VL 384 IS 2 BP 467 EP 473 DI 10.1086/170888 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GY758 UT WOS:A1992GY75800008 ER PT J AU RAYMOND, JC AF RAYMOND, JC TI MICROFLARE HEATING OF THE GALACTIC HALO SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXY, HALO; MHD; X-RAYS, GALAXIES ID X-RAY-EMISSION; INTERSTELLAR-MEDIUM; HYDROSTATIC EQUILIBRIUM; ULTRAVIOLET-RADIATION; EXTREME-ULTRAVIOLET; MAGNETIC-FIELDS; SHOCK-WAVES; GAS; CORONA; IONIZATION AB Recent estimates of the strength of the random component of the galactic magnetic field suggest that magnetic reconnection is probably important in heating the galactic halo. A microflare model of impulsive energy release has been proposed for the solar corona by Sturrock and collaborators. When the solar microflare model is scaled to a heating rate and pressure appropriate to the galactic halo, it predicts soft X-ray background emission, column densities of highly ionized species, and diffuse UV line emission in reasonable agreement with observed values. Column densities and surface brightnesses of low-ionization species are more ambiguously predicted by the model, but magnetic heating could contribute to them as well. RP RAYMOND, JC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 76 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 JAN 10 PY 1992 VL 384 IS 2 BP 502 EP 507 DI 10.1086/170892 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GY758 UT WOS:A1992GY75800012 ER PT J AU FULLER, GA MYERS, PC AF FULLER, GA MYERS, PC TI DENSE CORES IN DARK CLOUDS .7. LINE WIDTH-SIZE RELATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, KINEMATICS AND DYNAMICS; ISM, MOLECULES; RADIO LINES, MOLECULAR, INTERSTELLAR ID MOLECULAR CLOUDS; STAR FORMATION; GAS-DENSITY; MASS; TURBULENCE; OUTFLOWS; TAURUS AB Observations of 14 dense cores in lines of CS, (CO)-O-18 and NH3 are combined to examine the relations between the Doppler width of a line and the spatial extent of the map of line intensity. The line width increases with map size R as R(p). The deduced width DELTA-upsilon(TOT) of the velocity distribution of the molecule of mean mass has p = 0.20 +/- 0.04, and the deduced width DELTA-upsilon(NT) Of the nonthermal velocity distribution has p = 0.7 +/- 0.1. The values of p for eight cores with embedded stars and for six cores without embedded stars are statistically indistinguishable, but p is better determined for cores without stars. Thus the physical basis of the line width-size relations is part of the initial conditions for star formation, rather than a consequence of the star-core interaction. The cores appear close to virial equilibrium, consequently the variation of number density with distance r from the core density maximum is deduced. Expressed as a single power law, the number density varies as r(-q), with q = 1.6 +/- 0.1, and the nonthermal pressure varies as r(-s), with s = 0.2 +/- 0.1. If the nonthermal pressure is magnetic, the field strength increases with density as B is-proportional-to n0.05. The density variation within the cores is also deduced for a model where the thermal and nonthermal motions imply two corresponding power law components of density. C1 UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. UNIV CALIF BERKELEY,RADIO ASTRON LAB,BERKELEY,CA 94720. RP FULLER, GA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MAIL STOP 42,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 39 TC 164 Z9 164 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 JAN 10 PY 1992 VL 384 IS 2 BP 523 EP 527 DI 10.1086/170894 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GY758 UT WOS:A1992GY75800014 ER PT J AU TORRELLES, JM EIROA, C MAUERSBERGER, R ESTALELLA, R MIRANDA, LF ANGLADA, G AF TORRELLES, JM EIROA, C MAUERSBERGER, R ESTALELLA, R MIRANDA, LF ANGLADA, G TI THE MOLECULAR CORE IN THE AFGL-5157 REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (AFGL-5157); ISM, JETS AND OUTFLOWS; ISM, KINEMATICS AND DYNAMICS; ISM, MOLECULES; STARS, PRE-MAIN-SEQUENCE ID INTERSTELLAR CLOUDS; PLANETARY-NEBULAE; INFRARED SOURCES; OUTFLOWS; OBJECTS AB We present 40" resolution observations of the (1, 1) and (2, 2) ammonia transition lines toward the molecular core in the AFGL 5157 region. The observed high-density condensation has a size of 1'.3 x less-than-or-equal-to 0'.7. This structure has an orientation perpendicular to the axis of the bipolar molecular outflow previously observed in the region. The mass of the ammonia core is much larger than the mass of the bipolar molecular outflow. These results suggest that the observed elongated molecular condensation preceded, rather than followed, the outflow phenomenon phase, and that it can play an important role in the collimation processes at interstellar scales (approximately 0.1 pc). A rotational temperature T(R)(2, 2; 1, 1) congruent-to 17 K is obtained for the ammonia core, implying the presence of an internal heating source with a luminosity L greater-than-or-equal-to 5 x 10(2) (d/1800 pc)2 L. to keep that temperature. We have also carried out near-infrared observations (JHKL) and I, H-alpha, [S II], and red continuum CCD images. There are two reflection nebulae in the field of our images: one is NGC 1985, which coincides with AFGL 5157 (IRAS 05345 + 3157), and the other one is GM 39, which has a bipolar-like morphology and is probably excited by a pre-main-sequence star. Both nebulosities do not seem to be related to the powering source of the outflow. We failed to detect emission down to I = 23 mag at the peak of the ammonia condensation. There are also five small nebulosities, only detected with the emission-line filters, which probably are Herbig-Haro objects. Four of them are around the reflection nebula NGC 1985. The fifth is located near to a star in the field, at the southern border of the ammonia core. We suggest that some of these candidate HH objects, as well as a previously detected strong H2O maser in the region, could be excited by the same powering source as the molecular outflow. This powering source could be deeply embedded at the center of the ammonia core. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. OBSERV ASTRON MADRID IGN, E-28014 MADRID, SPAIN. MAX PLANCK INST RADIOASTRON, W-5300 BONN 1, GERMANY. UNIV BARCELONA, DEPT ASTRON & METEOROL, E-08028 BARCELONA, SPAIN. SOC CATALANA FIS, ASTROFIS LAB, BARCELONA, SPAIN. RP CSIC, INST ASTROFIS ANDALUCIA, AP CORREOS 3004, C-SANCHO PANZA S-N, E-18080 GRANADA, SPAIN. OI Torrelles, Jose Maria/0000-0002-6896-6085 NR 23 TC 17 Z9 18 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 JAN 10 PY 1992 VL 384 IS 2 BP 528 EP 535 DI 10.1086/170895 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GY758 UT WOS:A1992GY75800015 ER PT J AU BARSONY, M KENYON, SJ AF BARSONY, M KENYON, SJ TI ON THE ORIGIN OF SUBMILLIMETER EMISSION FROM YOUNG STARS IN TAURUS-AURIGA SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS FORMATION; STARS PRE-MAIN-SEQUENCE ID T-TAURI; MILLIMETER OBSERVATIONS; STELLAR OBJECTS; DENSE CORES; PHOTOMETRY; EVOLUTION; CLOUDS; DISK AB We present submillimeter photometry of embedded sources in the nearby Taurus-Auriga molecular cloud. We find that, for all sources in our sample, the submillimeter emission contributes 5% or less to the total source luminosity, confirming the relatively "low" luminosity (0.46 L. less-than-or-equal-to L. less-than-or-equal-to 4.2 L.) of this class of objects as previously pointed out by Kenyon and coworkers. From the observed 800-mu-m fluxes, beam-averaged values of the visual extinction are estimated to be in the range 40 < A(v) < 500. However, since all the objects in our sample have 2-mu-m detections, there must be cavities in the dust envelopes surrounding them. We find that the spectral energy distributions of the embedded sources longward of 300-mu-m are indistinguishable from those of the brightest, and presumably youngest, of the T Tauri stars, and, furthermore, are uncorrelated with source luminosity, IRAS flux, or near-infrared colors. Large submillimeter fluxes, however, do appear correlated with the presence of extended optical and/or near-infrared emission, reminiscent of the recently found correlation between high millimeter flux and the presence of well-developed outflows (Cabrit & Andre). This correlation suggests the possibility that dust envelope cavities may have been formed by as yet undetected molecular outflows in our embedded source sample. RP BARSONY, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 41 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 JAN 10 PY 1992 VL 384 IS 2 BP L53 EP L57 DI 10.1086/186260 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GY759 UT WOS:A1992GY75900006 ER PT J AU TORRELLES, JM GOMEZ, JF CURIEL, S EIROA, C RODRIGUEZ, LF HO, PTP AF TORRELLES, JM GOMEZ, JF CURIEL, S EIROA, C RODRIGUEZ, LF HO, PTP TI THE TRIPLE RADIO-CONTINUUM SOURCE IN SERPENS - ITS INTERACTION WITH THE AMBIENT MOLECULAR GAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM INDIVIDUAL OBJECTS (SERPENS REGION); ISM JETS AND OUTFLOWS; ISM MOLECULES; STARS PRE-MAIN-SEQUENCE ID HERBIG-HARO OBJECTS; STAR FORMATION; CLOUD; AMMONIA; S68 AB We present VLA D observations of the NH3(1, 1) and NH3(2, 2) lines toward the triple radio continuum source in the Serpens region. A nonthermal radio spectrum for the outer components of this triple radio source was suggested in 1989 by Rodriguez et al. These spectral ammonia line observations were made in the VLA 4IF mode. A sensitivity of 4 mJy per channel of 48.8 kHz of resolution (approximately 0.6 km s-1) was reached. This is the highest sensitivity for ammonia data obtained with the VLA. We find a perturbation of the molecular gas near the triple radio continuum source in terms of heating and broadening of the ammonia lines. These results convincingly support a Galactic nature for the triple radio source. The origin of the observed heating in the molecular gas is probably the luminosity of the central object. We propose that the line broadening observed along the direction of the proper motions of the outer components of the triple radio source may be driven by a shock associated with a wind from the central object. C1 OBSERV ASTRON MADRID,IGN,E-28014 MADRID,SPAIN. NATL AUTONOMOUS UNIV MEXICO,INST ASTRON,MEXICO CITY 04510,DF,MEXICO. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP TORRELLES, JM (reprint author), CSIC,INST ASTROFIS ANDALUCIA,APARTADO CORREOS 3004,C-SANCHO PANZA S-N,E-18080 GRANADA,SPAIN. RI Gomez, Jose Francisco/D-8392-2016 OI Gomez, Jose Francisco/0000-0002-7065-542X NR 18 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 JAN 10 PY 1992 VL 384 IS 2 BP L59 EP & DI 10.1086/186261 PN 2 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GY759 UT WOS:A1992GY75900007 ER PT J AU RAVENHILL, PL AF RAVENHILL, PL TI THE ART OF THE PERSONAL OBJECT SO AFRICAN ARTS LA English DT Article RP RAVENHILL, PL (reprint author), SMITHSONIAN INST,NAT MUSEUM AFRICAN ARTS,WASHINGTON,DC 20560, USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD JAN PY 1992 VL 25 IS 1 BP 70 EP 75 DI 10.2307/3337022 PG 6 WC Art SC Art GA HF367 UT WOS:A1992HF36700009 ER PT J AU REAVES, WW AF REAVES, WW TI 'HIS EXCELLENCY GENL WASHINGTON' - PEALE,CHARLES,WILLSON LONG-LOST MEZZOTINT DISCOVERED SO AMERICAN ART JOURNAL LA English DT Article RP REAVES, WW (reprint author), SMITHSONIAN INST,NATL PORTRAIT GALLERY,WASHINGTON,DC 20560, USA. NR 19 TC 0 Z9 0 U1 0 U2 0 PU KENNEDY GALLERIES INC PI NEW YORK PA ISRAEL SACK INC 40 W 57TH ST-5TH FLOOR, NEW YORK, NY 10019 SN 0002-7359 J9 AM ART J JI Am. Art J. PY 1992 VL 24 IS 1-2 BP 45 EP 59 PG 15 WC Art SC Art GA MR127 UT WOS:A1992MR12700002 ER PT J AU ROGERS, JD AF ROGERS, JD TI THE MISSISSIPPIAN EMERGENCE - SMITH,BD SO AMERICAN INDIAN CULTURE AND RESEARCH JOURNAL LA English DT Book Review RP ROGERS, JD (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU U C L A, AMER INDIAN STUDIES CENTER PI LOS ANGELES PA 3220 CAMPBELL HALL, BOX 951548, LOS ANGELES, CA 90095-1548 SN 0161-6463 J9 AM INDIAN CULT RES J JI Am. Indian Cult. Res. J. PY 1992 VL 16 IS 1 BP 219 EP 221 PG 3 WC History SC History GA KA192 UT WOS:A1992KA19200025 ER PT J AU HENRICKSON, RC AF HENRICKSON, RC TI THE HOLMES EXPEDITIONS TO LURISTAN - SCHMIDT,EF, VANLOON,MN, CURVERS,HH SO AMERICAN JOURNAL OF ARCHAEOLOGY LA English DT Book Review RP HENRICKSON, RC (reprint author), SMITHSONIAN INST,MUSEUM SUPPORT CTR,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ARCHAEOLOGICAL INST PI NEW YORK PA 135 WILLIAM ST, NEW YORK, NY 10038-3805 SN 0002-9114 J9 AM J ARCHAEOL JI Am. J. Archaeol. PD JAN PY 1992 VL 96 IS 1 BP 179 EP 180 DI 10.2307/505774 PG 2 WC Archaeology SC Archaeology GA HB249 UT WOS:A1992HB24900020 ER PT J AU CHEVERUD, JM DITTUS, WPJ AF CHEVERUD, JM DITTUS, WPJ TI PRIMATE POPULATION STUDIES AT POLONNARUWA .2. HERITABILITY OF BODY MEASUREMENTS IN A NATURAL-POPULATION OF TOQUE MACAQUES (MACACA-SINICA) SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE QUANTITATIVE GENETICS; PRIMATES; NATURAL POPULATION; ANTHROPOMETRICS ID QUANTITATIVE GENETICS; RHESUS MACAQUES; NONTRANSMISSIBLE COMPONENTS; ALEXANDERWOHL MENNONITES; ANTHROPOMETRIC VARIATION; CAYO-SANTIAGO; EVOLUTION; SELECTION; MULATTA; DENSITY AB The heritability of quantitative traits, or the proportion of phenotypic variation due to additive genetic or heritable effects, plays an important role in determining the evolutionary response to natural selection. Most quantitative genetic studies are performed in the laboratory, due to difficulty in obtaining genealogical data in natural populations. Genealogies are known, however, from a unique 20-year study of toque macaques (Macaca sinica) at Polonnaruwa, Sri Lanka. Heritability in this natural population was, therefore, estimated. Twenty-seven body measurements representing the lengths and widths of the head, trunk, extremities, and tail were collected from 270 individuals. The sample included 172 offspring-mother pairs from 39 different matrilineal families. Heritabilities were estimated using traditional mother-offspring regression and maximum likelihood methods which utilize all genealogical relationships in the sample. On the common assumption that environmental (including social) factors affecting morphology were randomly distributed across families, all but two of the traits (25 of 27) were significantly heritable, with an average heritability of 0.51 for the mother-offspring analysis and 0.56 for the maximum likelihood analysis. Heritability estimates obtained from the two analyses were very similar. We conclude that the Polonnaruwa macaques exhibit a comparatively moderate to high level of heritability for body form. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20560. INST FUNDAMENTAL STUDIES,KANDY,SRI LANKA. RP CHEVERUD, JM (reprint author), WASHINGTON UNIV,SCH MED,DEPT ANAT & NEUROBIOL,BOX 8108,660 S EUCLID AVE,ST LOUIS,MO 63110, USA. NR 32 TC 23 Z9 23 U1 1 U2 8 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PY 1992 VL 27 IS 2 BP 145 EP 156 DI 10.1002/ajp.1350270209 PG 12 WC Zoology SC Zoology GA HV701 UT WOS:A1992HV70100008 ER PT J AU RHINE, RJ NORTON, GW ROGERS, J WASSER, SK AF RHINE, RJ NORTON, GW ROGERS, J WASSER, SK TI SECONDARY SEX-RATIO AND MATERNAL DOMINANCE RANK AMONG WILD YELLOW BABOONS (PAPIO-CYNOCEPHALUS) OF MIKUMI-NATIONAL-PARK, TANZANIA SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE TRIVERS AND WILLARD; CERCOPITHECINE; RESOURCE COMPETITION ID LOCAL RESOURCE COMPETITION; MACAQUES MACACA-SYLVANUS; REPRODUCTIVE SUCCESS; JAPANESE MACAQUES; RHESUS MACAQUES; FEMALE BABOONS; SOCIAL RANK; LONG-TERM; ADJUSTMENT; FASCICULARIS AB The Trivers and Willard model predicts that offspring of dominant mothers will be biased toward males and offspring of subordinate mothers towards females, whereas a local-resource-competition hypothesis predicts the reverse. Available data bearing upon these alternative predictions are inconsistent. It has been suggested that the local-resource-competition hypothesis will predominate when resources are scarce, and the Trivers-Willard hypothesis when resources are abundant. The relationship between maternal dominance and secondary sex ratio for 214 offspring of 61 females was examined using four troops of wild yellow baboons living in Mikumi National Park, where the population was increasing in a resource-rich habitat. For all troops combined, no significant relationship was found between offspring sex ratio and maternal rank. The four troops separately showed inconsistent trends, and in no case did the relationship reach conventional levels of statistical significance. In contrast, the local-resource-competition hypothesis was supported by a study of yellow baboons done with one troop and 80 offspring in Amboseli National Park, where a massive population decline had occurred. The contrasting Amboseli and Mikumi results may be due to differences in resource-competition at the two study sites, or to stochastic variation. C1 UNIV CAMBRIDGE,DEPT ZOOL,CAMBRIDGE,ENGLAND. SW FDN BIOMED RES,DEPT GENET,SAN ANTONIO,TX 78284. SMITHSONIAN INST,CONSERVAT & RES CTR,FRONT ROYAL,VA. RP RHINE, RJ (reprint author), UNIV CALIF RIVERSIDE,DEPT PSYCHOL,RIVERSIDE,CA 92521, USA. NR 42 TC 24 Z9 24 U1 1 U2 5 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PY 1992 VL 27 IS 4 BP 261 EP 273 DI 10.1002/ajp.1350270404 PG 13 WC Zoology SC Zoology GA JF475 UT WOS:A1992JF47500003 ER PT J AU BAKER, AJ WOODS, F AF BAKER, AJ WOODS, F TI REPRODUCTION OF THE EMPEROR TAMARIN (SAGUINUS-IMPERATOR) IN CAPTIVITY, WITH COMPARISONS TO COTTON-TOP AND GOLDEN LION TAMARINS SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE CALLITRICHIDS; PARENTAL BEHAVIOR; INTERBIRTH INTERVAL ID CALLITHRIX-JACCHUS-JACCHUS; COMMON MARMOSET; MACACA-MULATTA; FERTILITY; LACTATION; OEDIPUS; COLONY; BEHAVIOR AB Little information has been published on the reproductive biology and behavior of the emperor tamarin (Saguinus imperator). We analyzed twelve years of data on emperor tamarins at the Los Angeles Zoo and made comparisons with data on cotton-top tamarins (Saguinus o. oedipus) and golden lion tamarins (Leontopithecus rosalia) from the same collection. Secondary sex ratios did not differ significantly from 50:50. Births were not strictly seasonal for any species. The number of infants reared had a significant effect on interbirth interval for all species, with shorter intervals when only one or no infants were reared, but females did sometimes conceive early in lactation. In emperor tamarin families, all fathers and most older siblings carried new infants, usually beginning within a few days after a birth. Previous exposure to younger siblings did not appear to be critical to the development of competent parental behavior by zooborn emperor tamarin females. C1 LOS ANGELES ZOO,LOS ANGELES,CA. RP BAKER, AJ (reprint author), SMITHSONIAN INST,DEPT ZOOL RES,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 37 TC 19 Z9 19 U1 3 U2 22 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PY 1992 VL 26 IS 1 BP 1 EP 10 DI 10.1002/ajp.1350260104 PG 10 WC Zoology SC Zoology GA HB480 UT WOS:A1992HB48000002 ER PT J AU FINCKE, OM AF FINCKE, OM TI INTERSPECIFIC COMPETITION FOR TREE HOLES - CONSEQUENCES FOR MATING SYSTEMS AND COEXISTENCE IN NEOTROPICAL DAMSELFLIES SO AMERICAN NATURALIST LA English DT Article ID DENSITY AB Male mating strategies of pseudostigmatid damselflies that breed in tree holes vary from resource defense to nonlocalized mate searching. Because females were most predictably found in forest light gaps and oviposited randomly with respect to tree-hole volume, morphology, and tree condition, the spatial distribution of neither females nor oviposition sites sufficiently accounted for differences in male mating strategies. Tree holes over 1 L in volume were the best larval habitats because they supported multiple cohorts per season. The two largest species emerged from larger tree holes than did the two smaller guild members. A laboratory experiment demonstrated that in large holes, small individuals of Megaloprepus eventually killed larger individuals of the two smaller Mecistogaster species, whereas Mecistogaster survived to emergence in small holes if they were the first to hatch there. A field experiment demonstrated that Mecistogaster colonized tree holes earlier in the wet season than did the two larger guild members, thereby gaining the head start in growth critical to its survival. The inferior competitive ability of its larvae countered any advantage that Mecistogaster adult males might otherwise derive from defending tree holes and resulted in seasonal clumping of emerging adults. In contrast, by defending large tree holes, male Megaloprepus coerulatus increased their chances of producing multiple offspring and sons of high quality. C1 SMITHSONIAN TROP RES INST,MIAMI,FL 34002. RP FINCKE, OM (reprint author), UNIV OKLAHOMA,DEPT ZOOL,NORMAN,OK 73019, USA. NR 17 TC 55 Z9 59 U1 0 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0003-0147 J9 AM NAT JI Am. Nat. PD JAN PY 1992 VL 139 IS 1 BP 80 EP 101 DI 10.1086/285314 PG 22 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA HC446 UT WOS:A1992HC44600006 ER PT J AU WESTEBERHARD, MJ AF WESTEBERHARD, MJ TI GENETICS, EPIGENETICS, AND FLEXIBILITY - A REPLY SO AMERICAN NATURALIST LA English DT Note C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 7 TC 3 Z9 3 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0003-0147 J9 AM NAT JI Am. Nat. PD JAN PY 1992 VL 139 IS 1 BP 224 EP 226 DI 10.1086/285323 PG 3 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA HC446 UT WOS:A1992HC44600015 ER PT J AU RAND, AS RYAN, MJ WILCZYNSKI, W AF RAND, AS RYAN, MJ WILCZYNSKI, W TI SIGNAL REDUNDANCY AND RECEIVER PERMISSIVENESS IN ACOUSTIC MATE RECOGNITION BY THE TUNGARA FROG, PHYSALAEMUS-PUSTULOSUS SO AMERICAN ZOOLOGIST LA English DT Article; Proceedings Paper CT 1990 ANNUAL MEETING OF THE AMERICAN SOC OF ZOOLOGISTS CY DEC 27-30, 1990 CL SAN ANTONIO, TX SP AMER SOC ZOOLOGISTS ID SEXUAL SELECTION; NEOTROPICAL FROG; SENSORY EXPLOITATION; TRACHOPS-CIRRHOSUS; COMPLEX CALLS; EATING BAT; COMMUNICATION; LEPTODACTYLIDAE; ADVERTISEMENT; MORPHOLOGY AB The tungara frog has an advertisement call with two structurally and functionally distinct components: the whine is both necessary and sufficient for species recognition, and addition of chucks further enhances call attractiveness. Only the fundamental frequency of the whine contributes to phonotaxis; the upper harmonics play no role. Furthermore, only a small portion of the whine, within the first 0-100 msec, is necessary to elicit phonotaxis; there is some redundancy since either the 0-50 msec or the 50-100 msec portion elicits a response. Most of the remainder of the whine's fundamental further enhances call attractiveness. Only the amphibian papilla in the peripheral auditory system is involved in decoding the whine. In stark contrast, several chuck variants, which stimulate either the amphibian papilla or the basilar papilla, and white noise are as effective in enhancing call attractiveness as is the normal chuck, showing that either peripheral end organ can be involved in the perception of a more attractive call. Thus there is greater receiver specificity for decoding stimuli in interspecific mate choice, and greater receiver permissiveness for decoding stimuli in intraspecific mate choice; it appears that intraspecific mate choice can take advantage of a greater array of neural pathways for call decoding than can interspecific mate choice. C1 UNIV TEXAS,DEPT ZOOL,AUSTIN,TX 78712. UNIV TEXAS,DEPT PSYCHOL,AUSTIN,TX 78712. RP RAND, AS (reprint author), SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 33 TC 59 Z9 64 U1 2 U2 6 PU AMER SOC ZOOLOGISTS PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 SN 0003-1569 J9 AM ZOOL JI Am. Zool. PY 1992 VL 32 IS 1 BP 81 EP 90 PG 10 WC Zoology SC Zoology GA JK512 UT WOS:A1992JK51200009 ER PT J AU HINES, AH AF HINES, AH TI CONSTRAINT ON REPRODUCTIVE OUTPUT IN BRACHYURAN CRABS - PINNOTHERIDS TEST THE RULE SO AMERICAN ZOOLOGIST LA English DT Article; Proceedings Paper CT SYMP ON THE COMPLEAT CRAB, AT THE 1990 ANNUAL MEETING OF THE AMERICAN SOC OF ZOOLOGISTS CY DEC 27-30, 1990 CL SAN ANTONIO, TX SP AMER SOC ZOOLOGISTS ID CRUSTACEA; FECUNDITY; DECAPODA AB Brood weight and number of eggs per brood are primarily determined by female body size in brachyuran crabs. Brood weight exhibits an isometric relationship spanning more than four orders of magnitude in body weight among 33 non-pinnotherid species, with brood size being constrained to about 10% of female body weight by the space available for yolk accumulation within the cephalothorax. In contrast, two pinnotherids (Pinnotheres ostreum, Fabia subquadrata) have relative brood sizes which are 66% and 97%, respectively, of body weight. The allometric constraint is circumvented in these extraordinarily large brood sizes by two pinnotherid features which allow more space for yolk accumulation. Unlike other brachyurans, their ovaries extend out of the cephalothorax into the abdomen, and calcification of their exoskeleton is greatly reduced, potentially allowing distension of the body. As in crabs, pinnotherid egg size is highly variable among species, which tends to increase the variance among species in fecundity per brood, making pinnotherid fecundities not extraordinary. The number of broods produced per year in these two species is limited by short reproductive seasons, which tends to bring their annual reproductive output in line with other brachyurans. The trade-offs among reproductive variables in pinnotherids is adaptive for the small body size and parasitic niche of these species. RP HINES, AH (reprint author), SMITHSONIAN ENVIRONM RES CTR,POB 28,EDGEWATER,MD 21037, USA. NR 15 TC 59 Z9 60 U1 0 U2 3 PU AMER SOC ZOOLOGISTS PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 SN 0003-1569 J9 AM ZOOL JI Am. Zool. PY 1992 VL 32 IS 3 BP 503 EP 511 PG 9 WC Zoology SC Zoology GA KR814 UT WOS:A1992KR81400019 ER PT J AU KNOWLTON, N AF KNOWLTON, N TI THRESHOLDS AND MULTIPLE STABLE STATES IN CORAL-REEF COMMUNITY DYNAMICS SO AMERICAN ZOOLOGIST LA English DT Article; Proceedings Paper CT SYMP ON LONG-TERM DYNAMICS OF CORAL REEFS, AT THE 1991 ANNUAL MEETING OF THE AMERICAN SOC OF ZOOLOGISTS CY DEC 27-30, 1991 CL ATLANTA, GA SP AMER SOC ZOOLOGISTS ID URCHIN DIADEMA-ANTILLARUM; DEPENDENT SIZE REGULATION; NATURAL COMMUNITIES; CHEMICAL DEFENSE; STABILITY; DENSITY; SYSTEMS; POINTS; PREY; HERBIVORES AB Multiple stable states occur when more than one type of community can stably persist in a single environmental regime. Simple theoretical analyses predict multiple stable states for (1) single species dynamics via the Allee effect, (2) two-species competitive interactions characterized by unstable coexistence, (3) some predator-prey interactions, and (4) some systems combining predation and competition. Potential examples of transitions between stable states on reefs include the failure of Diadema antillarum and Acropora cervicornis to recover following catastrophic mortality, and the replacement of microalgal turf by unpalatable macroalgae after rapid increase in the amount of substratum available for colonization by algae. Subtidal marine ecosystems in general, and reefs in particular, have several attributes which favor the existence of multiple stable states. Studies of transitions between states often need to rely upon poorly controlled, unreplicated natural ''experiments,'' as transitions typically require pulses of disturbance over very large spatial scales. The stability of a state must often be inferred from analyses of the dynamics of participants at that state, as generation times and the potential for further extrinsic disturbance preclude the use of persistence as an indicator of stability. The potential for multiple stable states strongly influences our interpretation of variability in space and time and our ability to predict reef responses to natural and man-made environmental change. RP KNOWLTON, N (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. NR 45 TC 321 Z9 330 U1 4 U2 65 PU AMER SOC ZOOLOGISTS PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 SN 0003-1569 J9 AM ZOOL JI Am. Zool. PY 1992 VL 32 IS 6 BP 674 EP 682 PG 9 WC Zoology SC Zoology GA KV055 UT WOS:A1992KV05500006 ER PT J AU JACKSON, JBC AF JACKSON, JBC TI PLEISTOCENE PERSPECTIVES ON CORAL-REEF COMMUNITY STRUCTURE SO AMERICAN ZOOLOGIST LA English DT Article; Proceedings Paper CT SYMP ON LONG-TERM DYNAMICS OF CORAL REEFS, AT THE 1991 ANNUAL MEETING OF THE AMERICAN SOC OF ZOOLOGISTS CY DEC 27-30, 1991 CL ATLANTA, GA SP AMER SOC ZOOLOGISTS ID ACANTHASTER-PLANCI; BUILDING CORALS; MASS MORTALITY; POPULATION-DYNAMICS; SPECIES-DIVERSITY; ACROPORA-PALMATA; HUON-PENINSULA; FRINGING REEFS; LIFE-CYCLES; WEST-INDIES AB Composition and zonation of coral reef communities are unstable on the scale of human lifetimes, but stable on average over thousands to hundreds of thousands of years. Traditional small-scale ecological studies can miss community patterns which are obscured by the noise of short-term change. Tests for stability require monitoring of populations over many generations-millenia for long-lived corals and forest trees. The only recourse is the fossil record. RP JACKSON, JBC (reprint author), SMITHSONIAN TROP RES INST,CTR TROP PALEOECOL,APARTADO 2072,BALBOA,PANAMA. NR 139 TC 115 Z9 122 U1 1 U2 7 PU AMER SOC ZOOLOGISTS PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 SN 0003-1569 J9 AM ZOOL JI Am. Zool. PY 1992 VL 32 IS 6 BP 719 EP 731 PG 13 WC Zoology SC Zoology GA KV055 UT WOS:A1992KV05500010 ER PT J AU HABBAL, SR AF HABBAL, SR TI CORONAL ENERGY-DISTRIBUTION AND X-RAY ACTIVITY IN THE SMALL-SCALE MAGNETIC-FIELD OF THE QUIET SUN SO ANNALES GEOPHYSICAE-ATMOSPHERES HYDROSPHERES AND SPACE SCIENCES LA English DT Article ID BRIGHT POINTS; TEMPORAL VARIATIONS; SPECTRO-HELIOMETER; TRANSITION ZONE; SOLAR; MACROSPICULES; NETWORK; HOLE; TELESCOPE; REGION AB We discuss, in this review, the energy distribution in the small scale magnetic field that pervades the solar surface, and its relationship to X-ray/coronal activity. The observed emission from the small scale structures, at temperatures characteristic of the chromosphere, transition region and corona, emanates from the boundaries of supergranular cells, within coronal bright points. This emission is characterized by a strong temporal and spatial variability with no definite pattern. The variability of the emission occurs on a time scale of a few (1-5) minutes. It is not always correlated in space or time between the different temperature emitting plasmas in a given structure. The analysis of simultaneous, multiwavelength EUV observations shows that the spatial density of the enhanced as well as variable emission from the small scale structures exhibits a pronounced temperature dependence with significant maxima at 10(5) K and 10(6) K. The radiative energy losses computed from the variable and enhanced components of the emission from the small scale structures are much smaller than those from the background quiet Sun. Within the limits of the spatial (1-5") and temporal (1-5 min) resolution of data available at present, the observed variability in the small scale structure cannot account for the coronal heating of the quiet Sun. The characteristics of their emission are more likely to be an indicator of the coronal heating mechanisms. RP HABBAL, SR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 52 TC 41 Z9 41 U1 0 U2 2 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0992-7689 J9 ANN GEOPHYS JI Ann. Geophys.-Atmos. Hydrospheres Space Sci. PD JAN-FEB PY 1992 VL 10 IS 1-2 BP 34 EP 46 PG 13 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA HL027 UT WOS:A1992HL02700004 ER PT J AU HUEBER, FM AF HUEBER, FM TI THOUGHTS ON THE EARLY LYCOPSIDS AND ZOSTEROPHYLLS SO ANNALS OF THE MISSOURI BOTANICAL GARDEN LA English DT Article ID NEW-YORK-STATE; SP-NOV; LYCOPODS; BARAGWANATHIA; LECLERCQIA; FLORA; RISE; GEN AB Morphological, anatomical, and reproductive characteristics of the modern lycopsids are of great value in tracing the ancient lineage of the group. The sporangium is the principal character: lack or misinterpretation of it in fossil specimens places an investigator in a predicament. An informed choice of a group of characters must be made from all those that remain. There are, of course, pitfalls and the defining characters of fossil species of the lycopsids have become confused. Differences in ontogeny of sporangia in early land plants are suggested as a way of separating the early rhyniophytoids with terminal, fusiform, indehiscent sporangia from the cooksonioid plants with terminal, globular or reniform, dehiscent sporangia. The rhyniophytoids are the source of later plant groups other than the lycopsids. Among the cooksonioids, change in the ontogeny of the sporangium in relation to the apical meristem is suggested as the point of differentiation and separation of the zosterophyll and lycopsid lineages. A reinterpretation of Kaulangiophyton suggests that its sporangia are borne adaxially on the leaves rather than terminally on stalks. The apical meristem of Asteroxylon is illustrated and described for the first time and compared with the apical meristem seen in species of Lycopodium. The genus Baragwanathia, questionably the earliest in the lycopsid lineage, is discussed in light of specimens ostensibly dated as of Gorstian age (lower Late Silurian) in Australia. Drepanophycus is perhaps the earliest recognizable member of the lycopsid lineage as opposed to Baragwanathia. The variation in the morphology of lycopsid leaves is of taxonomic value only in differentiating genera, particularly among those in the Devonian. Lineages are suggested diagrammatically. RP HUEBER, FM (reprint author), SMITHSONIAN INST,DEPT PALEOBIOL,NHB MRC 121,WASHINGTON,DC 20560, USA. NR 96 TC 57 Z9 59 U1 2 U2 9 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 SN 0026-6493 J9 ANN MO BOT GARD JI Ann. Mo. Bot. Gard. PY 1992 VL 79 IS 3 BP 474 EP 499 DI 10.2307/2399751 PG 26 WC Plant Sciences SC Plant Sciences GA JE556 UT WOS:A1992JE55600003 ER PT J AU BLANDFORD, RD NARAYAN, R AF BLANDFORD, RD NARAYAN, R TI COSMOLOGICAL APPLICATIONS OF GRAVITATIONAL LENSING SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS LA English DT Review DE MICROLENSING; ARCS; QUASARS; GALAXIES; CLUSTERS; COSMOGRAPHY; HUBBLE CONSTANT; DARK MATTER ID GIANT LUMINOUS ARCS; LIGHT TRAVEL TIME; MICROWAVE BACKGROUND-RADIATION; LOCALLY INHOMOGENEOUS UNIVERSE; ELLIPTICAL POTENTIAL WELLS; GALACTIC MASS-DISTRIBUTION; MULTIPLY IMAGED QUASARS; LARGE-SCALE STRUCTURE; LYMAN-ALPHA-FOREST; BL-LAC OBJECT C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP CALTECH, 130-33, PASADENA, CA 91125 USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 428 TC 301 Z9 302 U1 6 U2 14 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 1992 VL 30 BP 311 EP 358 PG 48 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JN532 UT WOS:A1992JN53200010 ER PT J AU CARROLL, SM PRESS, WH TURNER, EL AF CARROLL, SM PRESS, WH TURNER, EL TI THE COSMOLOGICAL CONSTANT SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS LA English DT Review DE GENERAL RELATIVITY; VACUUM ENERGY; AGE OF UNIVERSE; GALAXY COUNTS; GRAVITATIONAL LENSES ID COLD DARK MATTER; RR LYRAE STARS; QUANTUM-GRAVITY; GRAVITATIONAL LENSES; HUBBLE CONSTANT; BIG-BANG; INFLATIONARY UNIVERSE; SUPERSTRING MODELS; DENSITY PARAMETER; 3RD QUANTIZATION C1 PRINCETON UNIV OBSERV,PRINCETON,NJ 08544. RP CARROLL, SM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. RI Turner, Edwin/A-4295-2011 NR 227 TC 1056 Z9 1059 U1 6 U2 42 PU ANNUAL REVIEWS INC PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 SN 0066-4146 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 1992 VL 30 BP 499 EP 542 DI 10.1146/annurev.aa.30.090192.002435 PG 44 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JN532 UT WOS:A1992JN53200015 ER PT J AU MATHEWS, PM SHAPIRO, II AF MATHEWS, PM SHAPIRO, II TI NUTATIONS OF THE EARTH SO ANNUAL REVIEW OF EARTH AND PLANETARY SCIENCES LA English DT Review DE EARTH ROTATION; WOBBLES; NORMAL MODES; FREE CORE NUTATIONS ID CORE-MANTLE BOUNDARY; DIURNAL FREE-WOBBLE; NUMERICAL DETERMINATION; TIDE OBSERVATIONS; ELLIPTICAL EARTH; FORCED NUTATIONS; OCEANLESS EARTH; ROTATING EARTH; TRAVEL-TIMES; GRAVITY C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP UNIV MADRAS, DEPT THEORET PHYS, MADRAS 600025, TAMIL NADU, INDIA. NR 88 TC 23 Z9 23 U1 1 U2 3 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0084-6597 J9 ANNU REV EARTH PL SC JI Annu. Rev. Earth Planet. Sci. PY 1992 VL 20 BP 469 EP 500 PG 32 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA HT974 UT WOS:A1992HT97400017 ER PT B AU DALGARNO, A AF DALGARNO, A BE SINGH, PD TI ASTROCHEMISTRY OF COSMIC PHENOMENA - AN INTRODUCTION SO ASTROCHEMISTRY OF COSMIC PHENOMENA SE IAU SYMPOSIA LA English DT Proceedings Paper CT 150TH SYMP OF THE INTERNATIONAL ASTRONOMICAL UNION : ASTROCHEMISTRY OF COSMIC PHENOMENA CY AUG 05-09, 1991 CL SAO PAULO, BRAZIL SP INT ASTRON UNION RP DALGARNO, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA DORDRECHT BN 0-7923-1825-0 J9 IAU SYMP PY 1992 VL 150 BP 1 EP 6 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW54C UT WOS:A1992BW54C00001 ER PT B AU PRATAP, P MENTEN, KM REID, MJ MORAN, JM WALMSLEY, CM AF PRATAP, P MENTEN, KM REID, MJ MORAN, JM WALMSLEY, CM BE SINGH, PD TI VLBI OBSERVATIONS OF AMMONIA (9,6) MASERS SO ASTROCHEMISTRY OF COSMIC PHENOMENA SE IAU SYMPOSIA LA English DT Proceedings Paper CT 150TH SYMP OF THE INTERNATIONAL ASTRONOMICAL UNION : ASTROCHEMISTRY OF COSMIC PHENOMENA CY AUG 05-09, 1991 CL SAO PAULO, BRAZIL SP INT ASTRON UNION RP PRATAP, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA DORDRECHT BN 0-7923-1825-0 J9 IAU SYMP PY 1992 VL 150 BP 345 EP 346 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW54C UT WOS:A1992BW54C00077 ER PT B AU PRATAP, P SNYDER, LE BATRLA, W AF PRATAP, P SNYDER, LE BATRLA, W BE SINGH, PD TI A MODEL FOR THE MASER SOURCE NGC-7538 IRS-1 SO ASTROCHEMISTRY OF COSMIC PHENOMENA SE IAU SYMPOSIA LA English DT Proceedings Paper CT 150TH SYMP OF THE INTERNATIONAL ASTRONOMICAL UNION : ASTROCHEMISTRY OF COSMIC PHENOMENA CY AUG 05-09, 1991 CL SAO PAULO, BRAZIL SP INT ASTRON UNION RP PRATAP, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA DORDRECHT BN 0-7923-1825-0 J9 IAU SYMP PY 1992 VL 150 BP 347 EP 348 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW54C UT WOS:A1992BW54C00078 ER PT B AU CURIEL, S AF CURIEL, S BE SINGH, PD TI MOLECULAR STUDIES OF HERBIG-HARO OBJECTS SO ASTROCHEMISTRY OF COSMIC PHENOMENA SE IAU SYMPOSIA LA English DT Proceedings Paper CT 150TH SYMP OF THE INTERNATIONAL ASTRONOMICAL UNION : ASTROCHEMISTRY OF COSMIC PHENOMENA CY AUG 05-09, 1991 CL SAO PAULO, BRAZIL SP INT ASTRON UNION RP CURIEL, S (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MS 10,CAMBRIDGE,MA 02138, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA DORDRECHT BN 0-7923-1825-0 J9 IAU SYMP PY 1992 VL 150 BP 373 EP 378 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW54C UT WOS:A1992BW54C00087 ER PT J AU FAIRALL, AP WILLMER, CNA CALDERON, JH LATHAM, DW DACOSTA, LN PELLEGRINI, PS NUNES, MA FOCARDI, P VETTOLANI, G AF FAIRALL, AP WILLMER, CNA CALDERON, JH LATHAM, DW DACOSTA, LN PELLEGRINI, PS NUNES, MA FOCARDI, P VETTOLANI, G TI REDSHIFT OBSERVATIONS IN THE HYDRA CENTAURUS REGION SO ASTRONOMICAL JOURNAL LA English DT Article ID GALAXY REDSHIFTS; SUPERCLUSTER AB We report 406 redshifts for galaxies in the northern galactic hemisphere, south of delta = 0-degrees. A substantial fraction of the observed galaxies are located in the equatorial zone -17.5-degrees less-than-or-equal-to delta less-than-or-equal-to 0-degrees. By combining these new data with those available in the literature it is possible to extend the original CfA redshift survey of galaxies brighter than m(B(0)) = 14.5 to b = 30-degrees, south of delta = 0-degrees. New data taken at lower galactic latitudes also contribute to the existing surveys of the Hydra-Centaurus complex. C1 UNIV CALIF SANTA CRUZ,UCO,LICK OBSERV,SANTA CRUZ,CA 95064. OBSERV NACL,CNPQ,DEPT ASTRON,BR-20921 RIO DE JANEIRO,BRAZIL. OBSERV ASTRON,RA-5000 CORDOBA,ARGENTINA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV BOLOGNA,DIPARTMENTO ASTRON,I-40126 BOLOGNA,ITALY. CNR,IST RADIOASTRON,I-40126 BOLOGNA,ITALY. RP FAIRALL, AP (reprint author), UNIV CAPE TOWN,DEPT ASTRON,RONDEBOSCH 7700,SOUTH AFRICA. NR 22 TC 26 Z9 26 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 JAN PY 1992 VL 103 IS 1 BP 11 EP 27 DI 10.1086/116037 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GX221 UT WOS:A1992GX22100002 ER PT J AU HARVEY, BR JAUNCEY, DL WHITE, GL NOTHNAGEL, A NICOLSON, GD REYNOLDS, JE MORABITO, DD BARTEL, N AF HARVEY, BR JAUNCEY, DL WHITE, GL NOTHNAGEL, A NICOLSON, GD REYNOLDS, JE MORABITO, DD BARTEL, N TI ACCURATE RADIO AND OPTICAL POSITIONS FOR SOUTHERN RADIO-SOURCES SO ASTRONOMICAL JOURNAL LA English DT Article ID APPARENT PLACE COMPUTATIONS; IAU SYSTEM; TRANSFORMATION; CATALOG AB Accurate radio positions with a precision of about 0.01 arcsec are reported for eight compact extragalactic radio sources south of -45-degrees declination. The radio positions were determined using Very Long Baseline Interferometry (VLBI) at 8.4 GHz on the 9589 km Tidbinbilla (Australia) to Hartebeesthoek (South Africa) baseline. The sources were selected from the Parkes Catalogue to be strong, flat-spectrum radio sources with bright optical QSO counterparts. Optical positions of the QSOs were also measured from the ESO B Sky Survey plates with respect to stars from the Perth 70 Catalogue, to an accuracy of about 0.19 arcsec rms. These radio and optical positions are as precise as any presently available in the far southern sky. A comparison of the radio and optical positions confirms the estimated optical position errors and shows that there is overall agreement at the 0.1 arcsec level between the radio and Perth 70 optical reference frames in the far south. C1 CSIRO,AUSTRALIA TELESCOPE NATL FACIL,EPPING,NSW 2121,AUSTRALIA. HARTEBEESTHOEK RADIO ASTRON OBSERV,KRUGERSDORP 1740,SOUTH AFRICA. AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,CANBERRA,ACT 2601,AUSTRALIA. CALTECH,JET PROP LAB,PASADENA,CA 91109. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 15 TC 10 Z9 10 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 JAN PY 1992 VL 103 IS 1 BP 229 EP 233 DI 10.1086/116055 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GX221 UT WOS:A1992GX22100020 ER PT J AU YEOMANS, DK CHODAS, PW KEESEY, MS OSTRO, SJ CHANDLER, JF SHAPIRO, II AF YEOMANS, DK CHODAS, PW KEESEY, MS OSTRO, SJ CHANDLER, JF SHAPIRO, II TI ASTEROID AND COMET ORBITS USING RADAR DATA SO ASTRONOMICAL JOURNAL LA English DT Article ID ARAKI-ALCOCK 1983D; IMAGES AB For the 30 asteroids and 4 comets for which radar astrometric data were given by Ostro [AJ, 102, 1490 (1991b)], orbits have been computed using both the radar and the existing optical measurements. The techniques required to process radar data in orbit determination solutions are outlined and future radar observation opportunities for asteroids and comets are identified. For asteroids and comets that have only short intervals of optical astrometric data, the additional use of only a few radar observations allows a far more accurate extrapolation of their future motions. The use of radar data can often ensure an object's successful recovery at future Earth returns and greatly assist efforts in monitoring the motions of the rapidly growing population of known near-Earth objects, including their future close-Earth approaches. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP YEOMANS, DK (reprint author), CALTECH,JET PROP LAB,PASADENA,CA 91109, USA. NR 31 TC 38 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 JAN PY 1992 VL 103 IS 1 BP 303 EP 317 DI 10.1086/116062 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GX221 UT WOS:A1992GX22100027 ER PT J AU KAROVSKA, M NISENSON, P AF KAROVSKA, M NISENSON, P TI THE EFFECTS OF LIMB VARIATION ON THE DIAMETER MEASUREMENTS OF SN-1987-A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE SPECKLE INTERFEROMETRY; DIAMETERS; SN-1987-A ID SUPERNOVA AB We explore the effects of model brightness distributions on the estimated diameter from measurements of the supernova SN 1987 A envelope. The measurements were made using speckle interferometry techniques 265 days after the explosion. The results of this study show strong dependence of the diameter estimates for different model profiles. We conclude that the choice of the intensity distribution profile has an essential role in accurate determination of the supernova envelope diameter. RP KAROVSKA, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 8 TC 2 Z9 2 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 JAN PY 1992 VL 253 IS 1 BP 210 EP 212 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GY754 UT WOS:A1992GY75400028 ER PT J AU COMASTRI, A SETTI, G ZAMORANI, G ELVIS, M GIOMMI, P WILKES, BJ MCDOWELL, JC AF COMASTRI, A SETTI, G ZAMORANI, G ELVIS, M GIOMMI, P WILKES, BJ MCDOWELL, JC TI EXOSAT X-RAY-SPECTRA OF QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, NUCLEI; GALAXIES, SEYFERT; QUASARS, GENERAL; X-RAYS, GALAXIES ID SEYFERT-GALAXIES; ACTIVE GALAXIES; ABSORPTION; AGN AB We have measured the X-ray spectra in the 0.1-10 keV energy range for 17 AGNs (mostly PG quasars) using the EXOSAT Low and Medium Energy arrays. The sample has been selected on the basis of soft X-ray flux and includes all the AGNs in the 1981 Zamorani et al. and 1986 Tananbaum et al. publications with an Einstein flux greater than 6 x 10(-12) ergs cm-2 s-1. For each object we have determined the best-fit spectral parameters in the medium-energy range (approximately 2-10 keV), i.e., the power-law slope, the normalization, and the absorbing column density. In this energy range, all the spectra are well described by a single power law model, with a wide distribution of energy spectral indices in the range 0.4 < alpha < 1.3. The average spectral index is = 0.89 +/- 0.06, but most of the objects are distributed around alpha congruent-to 1.0. The overall distribution of spectral indices is significantly displaced toward steeper spectra, when compared to that found in the same energy band by Turner & Pounds, for a large sample of hard X-ray-selected Seyfert galaxies. This difference can be understood in terms of the different selection criteria of the two samples (soft versus hard X-ray selection), and it is concluded that the true distribution of hard X-ray spectral indices in AGNs is probably wider than previously suggested. Inclusion of lower energy data (approximately 0.1-2.0 keV) shows the presence of significant soft excess in six out of 17 cases. This soft excess emission can be modeled by either a steep power law with alpha a ranging from 2.7 to 4.2 or the high-energy tail of a blackbody with temperatures in the range 40-80 eV. The intersection of this soft excess emission with the hard X-ray power law is in the energy interval 0.35-0.75 keV, in the source rest frame. A correlation analysis performed on our data set does not reveal any correlation between the medium-energy spectral properties and other physical parameters of the sources. However, fits performed in the energy range 0.1-4.0 keV (comparable with the Einstein IPC energy range) show a significant correlation between radio-loudness and X-ray spectral properties, with the radio-loud objects having, on average, flatter slopes than the radio-quiet ones, in agreement with the findings of Wilkes & Elvis. The fact that the same correlation is not seen in our data at higher energy seems to be explained by a correlation between presence and strength of soft excess and "radio-quietness": the objects with significant soft excess emission tend to be the most radio-quiet quasars in our sample. C1 OSSERV ASTRON BOLOGNA,I-40126 BOLOGNA,ITALY. CNR,IST RADIOASTRON,I-40126 BOLOGNA,ITALY. EUROPEAN SO OBSERV,W-8046 GARCHING,GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP COMASTRI, A (reprint author), UNIV BOLOGNA,DIPARTMENTO ASTRON,VIA ZAMBONI 33,I-40126 BOLOGNA,ITALY. RI Comastri, Andrea/O-9543-2015; OI Comastri, Andrea/0000-0003-3451-9970; giommi, paolo/0000-0002-2265-5003; Zamorani, Giovanni/0000-0002-2318-301X; Wilkes, Belinda/0000-0003-1809-2364 NR 35 TC 84 Z9 84 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 JAN 1 PY 1992 VL 384 IS 1 BP 62 EP 71 DI 10.1086/170851 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GW612 UT WOS:A1992GW61200007 ER PT J AU PATTERSON, J STERNER, E HALPERN, JP RAYMOND, JC AF PATTERSON, J STERNER, E HALPERN, JP RAYMOND, JC TI ON THE CERTIFICATION OF AM-CANUM VENATICORUM AS A CATACLYSMIC VARIABLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE NOVAE, CATACLYSMIC VARIABLES; STARS, INDIVIDUAL (AM-CANUM VENATICORUM); STARS, OSCILLATIONS; WHITE DWARFS ID EARTH TELESCOPE OBSERVATIONS; HIGH-SPEED SPECTROSCOPY; RAPID BLUE VARIABLES; DB WHITE-DWARFS; SU-UMA STARS; ACCRETION DISKS; Z-CHAMAELEONTIS; V803 CEN; HZ 29; PERIOD AB We rediscuss the evidence that the peculiar faint blue star AM CVn (= HZ 29) is an ultra-short-period cataclysmic binary. The existence of at least two noncommensurate short periods in the light curve, plus the recent discovery of the class of pulsating DB white dwarfs, suggests a need for reappraisal of the binary star model. Reckoned as a cataclysmic variable, AM CVn is extremely unusual: it never erupts, never changes its spectrum, barely flickers, shows suspiciously blue colors, and fails to reveal a stable photometric period despite titanic efforts to discover it. But many of its properties suggest a similarity to the known DB pulsators. We present new photometry and spectroscopy of AM CVn, and also of five DB pulsators, to illustrate this similarity. It is quite possible that a significant fraction of the total light in AM CVn, perhaps most of it, comes from the photosphere of a pulsating white dwarf. On the other hand, while the original motivations for a binary star model have largely evaporated, several new pieces of evidence in its favor have emerged: the line He II lambda-4686 in emission, variable line profiles, an ultraviolet spectrum with strong heavy-element absorption features, rapid quasi-periodic oscillations, and the discovery of two apparently similar systems with more impressive binary star credentials (V803 Cen and CR Boo). These are not easy to understand in the context of a single-star model. The most severe obstacle to accepting AM CVn as a short-period binary is the instability of the photometric period. We suggest that this can be reconciled with a binary star model by postulating the existence of an eccentric accretion disk precessing around the white dwarf. This implies that the absorption-line profiles should be highly modulated not on the presumed 17 minute binary period but on the disk precession period of approximately 7-12 hr. C1 COLUMBIA ASTROPHYS LAB,NEW YORK,NY 10027. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP PATTERSON, J (reprint author), DEPT ASTRON,538 W 120TH ST,NEW YORK,NY 10027, USA. NR 57 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 JAN 1 PY 1992 VL 384 IS 1 BP 234 EP 248 DI 10.1086/170866 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GW612 UT WOS:A1992GW61200022 ER PT J AU CLAYTON, GC WHITNEY, BA STANFORD, SA DRILLING, JS JUDGE, PG AF CLAYTON, GC WHITNEY, BA STANFORD, SA DRILLING, JS JUDGE, PG TI THE UNUSUAL ULTRAVIOLET CHROMOSPHERIC SPECTRUM OF THE R-CORONAE-BOREALIS STAR, V854 CENTAURI (NSV-6708), AT MINIMUM LIGHT SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, CHROMOSPHERES; STARS, INDIVIDUAL (V854-CEN); ULTRAVIOLET, STARS ID RCB STARS; IUE; ARCTURUS AB The first IUE observations of a decline of the recently discovered R CrB star, V854 Cen, are reported. These observations are of particular interest because they include spectra taken at 7 mag below maximum light. This is the deepest minimum ever observed in an R CrB star with the IUE. The "chromospheric" emission spectra show striking differences from UV spectra of other R CrB stars in decline. In fact, the emission spectrum of V854 Cen at minimum light does not seem to have an analogue in any known emission-line object. Strong emission appears in several lines not normally seen in R CrB emission-line spectra, in particular at C II] lambda-2326, Mg I-lambda-2852, and C I-lambda-lambda-2965, 2967. Spectral evolution similar to that seen in visible spectra of R CrB stars is clearly seen in the ultraviolet for the first time. The differences between V854 Cen and other R CrB stars may be related to known abundance differences or to different temperature and density conditions in the emission-line regions of the various R CrB stars. The emission may also be significantly affected by the presence of dust in or near the emitting region. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. LOUISIANA STATE UNIV,DEPT PHYS & ASTRON,BATON ROUGE,LA 70803. HIGH ALTITUDE OBSERV,BOULDER,CO 80307. RP CLAYTON, GC (reprint author), UNIV COLORADO,CTR ASTROPHYS & SPACE ASTRON,CAMPUS BOX 389,BOULDER,CO 80309, USA. NR 40 TC 16 Z9 16 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 JAN 1 PY 1992 VL 384 IS 1 BP L19 EP L23 DI 10.1086/186253 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GW614 UT WOS:A1992GW61400005 ER PT J AU IKEBE, Y OHASHI, T MAKISHIMA, K TSURU, T FABBIANO, G KIM, DW TRINCHIERI, G HATSUKADE, I YAMASHITA, K KONDO, H AF IKEBE, Y OHASHI, T MAKISHIMA, K TSURU, T FABBIANO, G KIM, DW TRINCHIERI, G HATSUKADE, I YAMASHITA, K KONDO, H TI X-RAY STUDY OF NGC-1399 IN THE FORNAX CLUSTER OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (NGC-1399); GALAXIES, INTERGALACTIC MEDIUM; X-RAYS, GALAXIES ID SENSITIVITY; EVOLUTION; EMISSION; SPECTRA; GINGA AB Observations of the cD galaxy NGC 1399 in the Fornax cluster of galaxies with Ginga have detected extended X-ray emission out to a radius of more than approximately 360 kpc. The energy spectrum of this emission is well fitted with an optically thin thermal spectrum with kT = 1.46(-0 21)+0.05 keV with a strong iron emission line corresponding to an iron abundance of 1.1(-0.5)+1.3 times solar. The mass of the hot gas responsible for the X-ray emission is nearly the same as the total stellar mass of the cluster. Therefore, the presence of iron at near-solar abundance suggests that the mass of the hot gas ejected from galaxies is comparable to the total stellar mass. This result indicates that most of the hot gas in a very poor cluster is created through ejections from galaxies, rather than being primordial. C1 OSSERV ASTROFIS ARCETRI,I-50125 FLORENCE,ITALY. MIYAZAKI UNIV,DEPT ELECTR ENGN,MIYAZAKI 88921,JAPAN. INST SPACE & ASTRONAUT SCI,SAGAMIHARA,KANAGAWA 229,JAPAN. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP IKEBE, Y (reprint author), UNIV TOKYO,DEPT PHYS,7-3-1 HONGO,BUNKYO KU,TOKYO 113,JAPAN. NR 29 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 JAN 1 PY 1992 VL 384 IS 1 BP L5 EP L8 DI 10.1086/186227 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GW614 UT WOS:A1992GW61400002 ER PT J AU BABB, JF CHANG, ES AF BABB, JF CHANG, ES TI THE RYDBERG ELECTRONIC-TRANSITIONS OF THE HYDROGEN MOLECULE SO ATOMIC DATA AND NUCLEAR DATA TABLES LA English DT Article ID INFRARED-LASER SPECTROSCOPY; ANGULAR-MOMENTUM STATES; POLARIZATION-MODEL; H-2; D2; 6H-5G; H2 C1 UNIV MASSACHUSETTS,DEPT PHYS,AMHERST,MA 01003. RP BABB, JF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138, USA. OI Babb, James/0000-0002-3883-9501 NR 13 TC 3 Z9 3 U1 0 U2 3 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0092-640X J9 ATOM DATA NUCL DATA JI Atom. Data Nucl. Data Tables PD JAN PY 1992 VL 50 IS 1 BP 137 EP 176 DI 10.1016/0092-640X(92)90025-D PG 40 WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Physics GA HA438 UT WOS:A1992HA43800003 ER PT J AU LAYBOURNE, RC SABO, BA MORNINGSTAR, A AF LAYBOURNE, RC SABO, BA MORNINGSTAR, A TI BASIC TECHNIQUE FOR PREPARATION OF DOWN FOR EXAMINATION WITH THE SCANNING ELECTRON-MICROSCOPE SO AUK LA English DT Note ID FEATHERS C1 US FISH & WILDLIFE SERV,NATL FISH & WILDLIFE FORENS LAB,ASHLAND,OR 97520. RP LAYBOURNE, RC (reprint author), SMITHSONIAN INST,DIV BIRDS,WASHINGTON,DC 20560, USA. NR 9 TC 5 Z9 5 U1 0 U2 2 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 JAN PY 1992 VL 109 IS 1 BP 195 EP 197 PG 3 WC Ornithology SC Zoology GA HQ212 UT WOS:A1992HQ21200023 ER PT J AU DRAKE, BG AF DRAKE, BG TI A FIELD-STUDY OF THE EFFECTS OF ELEVATED CO2 ON ECOSYSTEM PROCESSES IN A CHESAPEAKE BAY WETLAND SO AUSTRALIAN JOURNAL OF BOTANY LA English DT Article ID CARBON-DIOXIDE ENRICHMENT; ELECTRON-TRANSPORT CAPACITY; LONG-TERM EXPOSURE; ATMOSPHERIC CO2; ESTUARINE MARSH; PHOTOSYNTHETIC ACCLIMATION; RIBULOSE 1,5-BISPHOSPHATE; TRANSPIRATION RESPONSES; CANOPY PHOTOSYNTHESIS; SOYBEAN CANOPIES AB Open top chambers are being used in a long-term project to determine the effects of elevated CO2 on ecosystem processes on a Chesapeake Bay wetland. Three communities are studied: mono-specific stands of the C3 sedge, Scirpus olneyi, and the C4 grass, Spartina patens, and a mixed community of these two species and the C4 grass, Distichlis spicata. Treatment began in the spring of 1987 and will continue through the 1994 growing season. During the first 4 years of exposure, elevated CO2 had the following effects on mono-specific stands of the C3 sedge, Scirpus olneyi: increased quantum yield and photosynthetic capacity, reduced dark respiration, increased numbers of shoots, roots and rhizomes, reduced nitrogen concentration of all tissues, increased nitrogen fixation and increased ecosystem carbon accumulation. In a mixed community of the sedge and C4 grass species, Spartina patens and Distichlis spicata, biomass of the C3 component increased over 100% and this was accompanied by decreased biomass in the C4 component of the community. Elevated CO2 reduced water loss, increased water potential and delayed senescence in all three species. Many factors contributed to CO2 stimulated carbon accumulation in the plant community dominated by the C3 sedge, Scirpus olneyi, including: sustained high photosynthetic capacity, decreased respiration, delayed senescence, and allocation of the additional carbon to roots and rhizomes. The complex interaction of these diverse responses suggests that the rising atmospheric CO2 may have a significant impact on ecosystem processes. RP DRAKE, BG (reprint author), SMITHSONIAN ENVIRONM RES CTR, POB 28, EDGEWATER, MD 21037 USA. NR 72 TC 80 Z9 82 U1 1 U2 16 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 0067-1924 J9 AUST J BOT JI Aust. J. Bot. PY 1992 VL 40 IS 4-5 BP 579 EP 595 DI 10.1071/BT9920579 PG 17 WC Plant Sciences SC Plant Sciences GA KA487 UT WOS:A1992KA48700014 ER PT J AU BOWMAN, TE BOTOSANEANU, L AF BOWMAN, TE BOTOSANEANU, L TI 1ST RECORD OF A TACHAEA SPECIES FROM SULAWESI (INDONESIA) WITH DESCRIPTION OF ITS MANCA STAGE (ISOPODA, FLABELLIFERA, CORALLANIDAE) SO BIJDRAGEN TOT DE DIERKUNDE LA English DT Note DE ISOPODA-CORALLANIDAE; TACHAEA; TAXONOMY; DISTRIBUTION; ECOLOGY; SULAWESI AB A corallanid isopod in the manca stage (lacking pereopod 7), collected from alluvial gravel along the Batui River in Sulawesi, Indonesia, and identified questionably as Tachaea lacustris Weber, 1892, is illustrated and described in detail. Tachaea lacustris was known previously only from freshwater lakes in Sumatra and Java. Its presence in river alluvial gravel should not be interpreted as possible adaptation to the hyporheic habitat. C1 UNIV AMSTERDAM,INST TAXON ZOOL,DEPT ENTOMOL,1018 DH AMSTERDAM,NETHERLANDS. RP BOWMAN, TE (reprint author), SMITHSONIAN INST,NHB 163,DEPT INVERTEBRATE ZOOL CRUSTACEA,WASHINGTON,DC 20560, USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU ARTIS LIBRARY COMMITTEE PI AMSTERDAM PA UNIVERSITEIT VAN AMSTERDAM PLANTAGE MIDDENLAAN 45A, 1018 AMSTERDAM, NETHERLANDS SN 0067-8546 J9 BIJDR DIERKD JI Bijdr. Tot Dierkunde PY 1992 VL 62 IS 2 BP 111 EP 115 PG 5 WC Zoology SC Zoology GA KE309 UT WOS:A1992KE30900005 ER PT B AU LATHAM, DW AF LATHAM, DW BE Duquennoy, A Mayor, M TI BINARIES AS TRACERS OF STELLAR FORMATION - INTRODUCTORY-REMARKS SO BINARIES AS TRACERS OF STELLAR FORMATION LA English DT Proceedings Paper CT Topical Workshop on Binaries as Tracers of Stellar Formation, to honour Roger Griffin CY SEP, 1991 CL BETTMERALP, SWITZERLAND C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 0 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE, CAMBS, ENGLAND CB2 1RP BN 0-521-43358-4 PY 1992 BP 1 EP 5 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BZ84Z UT WOS:A1992BZ84Z00001 ER PT B AU LATHAM, DW MATHIEU, RD MILONE, AAE DAVIS, RJ AF LATHAM, DW MATHIEU, RD MILONE, AAE DAVIS, RJ BE Duquennoy, A Mayor, M TI SPECTROSCOPIC BINARIES IN THE OPEN CLUSTER M67 SO BINARIES AS TRACERS OF STELLAR FORMATION LA English DT Proceedings Paper CT Topical Workshop on Binaries as Tracers of Stellar Formation, to honour Roger Griffin CY SEP, 1991 CL BETTMERALP, SWITZERLAND C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 0 TC 13 Z9 13 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE, CAMBS, ENGLAND CB2 1RP BN 0-521-43358-4 PY 1992 BP 132 EP 138 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BZ84Z UT WOS:A1992BZ84Z00011 ER PT B AU LATHAM, DW MAZEH, T TORRES, G CARNEY, BW STEFANIK, RP DAVIS, RJ AF LATHAM, DW MAZEH, T TORRES, G CARNEY, BW STEFANIK, RP DAVIS, RJ BE Duquennoy, A Mayor, M TI SPECTROSCOPIC BINARIES IN THE HALO SO BINARIES AS TRACERS OF STELLAR FORMATION LA English DT Proceedings Paper CT Topical Workshop on Binaries as Tracers of Stellar Formation, to honour Roger Griffin CY SEP, 1991 CL BETTMERALP, SWITZERLAND C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 0 TC 3 Z9 3 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE, CAMBS, ENGLAND CB2 1RP BN 0-521-43358-4 PY 1992 BP 139 EP 144 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BZ84Z UT WOS:A1992BZ84Z00012 ER PT J AU BRACCINI, E PEYPOUQUET, JP BENSON, RH AF BRACCINI, E PEYPOUQUET, JP BENSON, RH TI QUANTIZATION TEST OF THE EVOLUTION TREND OF PALEOCOSTA-PERVINQUIERI (OSTRACODE) DURING A 10-MILLION YEAR PERIOD (DJEBEL-DYR SECTION, PALEOGENE, ALGERIA) SO BIOSYSTEMS LA English DT Article DE PALEOBIOLOGY; OSTRACODE; PORE CANAL; THETA-RHO; LEAST SQUARE; EVOLUTION ID SEA AB Using a computerised technique that estimates differences or changes in the pattern defined by the distribution of 24 pore-canals of left valves of Paleocosta pervinquieri (Ostracode), we can speculate about the phylogenic evolution of the species ranging in age from Danian (66 My) to Ypresian (54 My) from the Djebel-Dyr section (North East of Algeria). This method is combined with traditional biometric and statistical studies and the analysis of architectural patterns of shells. Firstly, it reveals that Paleocosta pervinquieri is individualised in 6 morphs which evolve from the 'libyaenisis morph' to the 'mokkatamensis morph', between the Pl zone (66 My) to the P4 zone (56 My). During the P5 zone (55 My), we suggest that there has been a genation between the Paleocosta pervinquieri 'mokkatamensis morph' and the Reymensticosta sp. 'semi-reticulated morph'. Furthermore, the Theta-Rho method could be adapted and used for numerous paleontological and biological studies. C1 SMITHSONIAN INST,PALEOBIOL LAB,WASHINGTON,DC 20560. RP BRACCINI, E (reprint author), UNIV BORDEAUX 1,DEPT GEOL & OCEANOL,AVE FAC,F-33405 TALENCE,FRANCE. NR 13 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCI IRELAND LTD PI CLARE PA CUSTOMER RELATIONS MANAGER, BAY 15, SHANNON INDUSTRIAL ESTATE CO, CLARE, IRELAND SN 0303-2647 J9 BIOSYSTEMS JI Biosystems PY 1992 VL 28 IS 1-3 BP 153 EP 167 DI 10.1016/0303-2647(92)90017-S PG 15 WC Biology; Mathematical & Computational Biology SC Life Sciences & Biomedicine - Other Topics; Mathematical & Computational Biology GA KK977 UT WOS:A1992KK97700016 PM 1292660 ER PT J AU THOMAS, JD BARNARD, JL AF THOMAS, JD BARNARD, JL TI PODOCERUS-CHELONOPHILUS, A TESTUDINOUS AMPHIPOD NEWLY RECORDED FROM THE WESTERN ATLANTIC-OCEAN SO BULLETIN OF MARINE SCIENCE LA English DT Article AB Podocerus chelonophilus (= P. cheloniae), an amphipod inhabiting the carapace of the loggerhead turtle, Caretta caretta, is reported for the first time from the western Atlantic Ocean. C1 SMITHSONIAN INST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560. RP THOMAS, JD (reprint author), REEF FDN,POB 569,BIG PINE KEY,FL 33043, USA. NR 60 TC 7 Z9 7 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 JAN PY 1992 VL 50 IS 1 BP 108 EP 116 PG 9 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA HP379 UT WOS:A1992HP37900009 ER PT J AU WILKINSON, CR MACINTYRE, IG AF WILKINSON, CR MACINTYRE, IG TI SPECIAL ISSUE - THE ACANTHASTER DEBATE - PREFACE SO CORAL REEFS LA English DT Editorial Material ID GREAT BARRIER-REEF; PLANCI C1 SMITHSONIAN INST,WASHINGTON,DC 20560. RP WILKINSON, CR (reprint author), AUSTRALIAN INST MARINE SCI,TOWNSVILLE,QLD 4810,AUSTRALIA. NR 6 TC 7 Z9 9 U1 2 U2 2 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PY 1992 VL 11 IS 2 BP 51 EP 52 DI 10.1007/BF00357421 PG 2 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA JD265 UT WOS:A1992JD26500001 ER PT J AU ALLEN, LH DRAKE, BG ROGERS, HH SHINN, JH AF ALLEN, LH DRAKE, BG ROGERS, HH SHINN, JH TI FIELD TECHNIQUES FOR EXPOSURE OF PLANTS AND ECOSYSTEMS TO ELEVATED CO-2 AND OTHER TRACE GASES SO CRITICAL REVIEWS IN PLANT SCIENCES LA English DT Review DE FIELD TECHNIQUES; OTC; SPAR; FACE; COMPARISON ID OPEN-TOP CHAMBERS; ATMOSPHERIC CO2 ENRICHMENT; WATER-VAPOR EXCHANGE; CARBON-DIOXIDE CONCENTRATIONS; OPEN-AIR FUMIGATION; ESTUARINE MARSH; TRANSPIRATION RESPONSES; VENTILATED CHAMBER; SOYBEAN CANOPIES; PORTABLE CHAMBER C1 SMITHSONIAN ENVIRONM RES LABS,EDGEWATER,MD 21037. AUBURN UNIV,USDA ARS,AUBURN,AL 36831. LAWRENCE LIVERMORE NATL LAB,LIVERMORE,CA 94550. RP ALLEN, LH (reprint author), UNIV FLORIDA,USDA ARS,GAINESVILLE,FL 32611, USA. NR 207 TC 60 Z9 61 U1 1 U2 5 PU CRC PRESS INC PI BOCA RATON PA 2000 CORPORATE BLVD NW, JOURNALS CUSTOMER SERVICE, BOCA RATON, FL 33431 SN 0735-2689 J9 CRIT REV PLANT SCI JI Crit. Rev. Plant Sci. PY 1992 VL 11 IS 2-3 BP 85 EP 119 DI 10.1080/07352689209382333 PG 35 WC Plant Sciences SC Plant Sciences GA JW197 UT WOS:A1992JW19700004 ER PT J AU DUDLEY, R VERMEIJ, GJ AF DUDLEY, R VERMEIJ, GJ TI DO THE POWER REQUIREMENTS OF FLAPPING FLIGHT CONSTRAIN FOLIVORY IN FLYING ANIMALS SO FUNCTIONAL ECOLOGY LA English DT Letter RP DUDLEY, R (reprint author), SMITHSONIAN TROP RES INST,POB 2072,BALBOA,PANAMA. NR 0 TC 19 Z9 20 U1 0 U2 3 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PY 1992 VL 6 IS 1 BP 101 EP 104 PG 4 WC Ecology SC Environmental Sciences & Ecology GA HE054 UT WOS:A1992HE05400012 ER PT J AU HASHIMOTO, A AF HASHIMOTO, A TI THE EFFECT OF H2O GAS ON VOLATILITIES OF PLANET-FORMING MAJOR ELEMENTS .1. EXPERIMENTAL-DETERMINATION OF THERMODYNAMIC PROPERTIES OF CA-HYDROXIDE, AL-HYDROXIDE, AND SI-HYDROXIDE GAS MOLECULES AND ITS APPLICATION TO THE SOLAR NEBULA SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID ALLENDE METEORITE; RICH INCLUSIONS; CARBONACEOUS CHONDRITE; REFRACTORY INCLUSIONS; EVAPORATION KINETICS; MURCHISON METEORITE; GRAINED INCLUSIONS; CV3 CHONDRITE; ORIGIN; MINERALOGY AB Vapor pressures of Ca(OH)2(g) and Al(OH)3(g) were measured using the transpiration technique, employing the reactions CaO(s) + H2O(g) half-arrow-right-over-half-arrow-left Ca(OH)2(g); 2CaAl2O4(s) + H2O(g) half-arrow-right-over-half-arrow-left CaAl4O7(s) + Ca(OH)2(g); and CaAl4O7(s) + 3H2O(g) half-arrow-right-over-half-arrow-left CaAl2O4(s) + 2Al(OH)3(g). From these vapor pressures, enthalpy and entropy changes in the above reactions were determined for the average experimental temperature (1650 K). This, combined with literature thermodynamic data, gives the heats of formation and entropies of the hydroxide gas species at the standard state (1 atm and 298.15 K): DELTA-H(o) = -615.0 +/- 7.1 (2-sigma) kJ/mol and S0 = 284.5 +/- 7.9 (2-sigma) J/mol.K for Ca(OII)2(g), and DELTA-H0 = -1004.2 +/- 15.0 (2-sigma) kJ/mol and S0 = 313.8 +/- 7.9 (2-sigma) J/mol.K for Al(OH)3(g). The Si-tetrahydroxide molecule, Si(OH)4, was produced in the reaction SiO2(s) + 2H2O(g) half-arrow-right-over-half-arrow-left Si(OH)4(g) by application of the same technique. This is the first report of a stable Si-hydroxide gas species. Its heat of formation and entropy at 1600 K and 1 atm was determined to be -1342.7 +/- 2.7 (2-sigma) kJ/mol and 592.5 +/- 1.0 (2-sigma) J/mol.K, respectively. Using these values for the gas species investigated and literature thermodynamic data for other gas species, "volatilities" (the total of vapor pressures of gas species containing the element in question, over the pure condensed oxide of that element) of the five major planet-forming elements Fe, Mg, Si, Ca, and Al were calculated for a range of physical and chemical conditions (P, T, bulk system composition) appropriate to the solar nebula. The results indicate (1) volatilitics of all the elements investigated are significantly enhanced if the formation of hydroxide species by reaction with H2O(g) is taken into account, compared with previous calculations which neglected these species; (2) generally, hydroxide gas species predominatc at relatively low temperatures and/or in an oxidizing atmosphere, while monatomic and undersaturated-oxidized gas species are most abundant at high temperatures and/or in a reducing atmosphere; (3) hydroxide species of Ca and Al are relatively stable even at high temperatures compared to those of Si, Mg, and Fe; (4) these effects explain how Ca and Al could have evaporated from Ca,Al-rich inclusions in carbonaceous chondrites while Si, Mg, and Fc condensed onto them during the preaccretion alteration of CAIs. RP HASHIMOTO, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 52 TC 89 Z9 90 U1 0 U2 9 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 JAN PY 1992 VL 56 IS 1 BP 511 EP 532 DI 10.1016/0016-7037(92)90148-C PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA HB840 UT WOS:A1992HB84000037 ER PT J AU DALGARNO, A AF DALGARNO, A TI ASTROCHEMISTRY OF COSMIC PHENOMENA - AN INTRODUCTION SO IAU SYMPOSIA LA English DT Article AB A general introduction is given to the subject matter of the symposium. RP DALGARNO, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0074-1809 J9 IAU SYMP PY 1992 IS 150 BP 1 EP 6 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JQ128 UT WOS:A1992JQ12800001 ER PT J AU KENYON, SJ AF KENYON, SJ TI SYMBIOTIC BINARY STARS SO IAU SYMPOSIA LA English DT Article DE STARS-BINARIES-SYMBIOTICS; ACCRETION DISKS; STARS-MASS LOSS ID COMPONENTS; EVOLUTION; NOVAE; DUST AB This paper briefly reviews the physical properties of symbiotic stars: long-period interacting binaries composed of a red giant primary star and a hot companion. Two types of binaries produce symbiotic optical spectra: semi-detached systems with a main sequence secondary and detached systems with a white dwarf secondary. Semi-detached symbiotics resemble cataclysmic variables and Algol binaries, but on a much larger scale, and undergo dwarf nova-like eruptions. Wind accretion powers detached systems; occasional thermonuclear runaways produce symbiotic novae - distant cousins of classical novae. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 45 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0074-1809 J9 IAU SYMP PY 1992 IS 151 BP 137 EP 146 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JJ251 UT WOS:A1992JJ25100014 ER PT J AU KURUCZ, RL AF KURUCZ, RL TI MODEL ATMOSPHERES FOR POPULATION SYNTHESIS SO IAU SYMPOSIA LA English DT Article ID SOLAR; STAR AB I have used my newly calculated iron group line list together with my earlier atomic and molecular line data, 58,000,000 lines total, to compute new opacities for the temperature range 2000K to 200000K. Calculations have been completed at the San Diego Supercomputer Center for 56 temperatures, for 21 pressures, for microturbulent velocities 0, 1, 2, 4, and 8 km/s, for 3,500,000 wavelength points divided into 1221 intervals from 10 to 10000 nm, for scaled solar abundances [+1.0], [+0.5], [+0.3], [+0.2], [+0.1], [+0.0], [-0.1], [-0.2], [-0.3], [-0.5], [-1.0], [-1.5], [-2.0], [-2.5], [-3.0], [-3.5], [-4.01, [-4.5], and [-5.0]. I have rewritten my model atmosphere program to use the new line opacities, additional continuous opacities, and an approximate treatment of convective overshooting. The opacity calculation was checked by computing a new theoretical solar model that matches the observed irradiance. Thus far I have completed a grid of 7000 model atmospheres at 2 km/s for all the abundances, for the temperature range 3500K to 50000K, and for log g from 0.0 to 5.0. This grid will allow a consistent theoretical treatment of photometry from K stars to B stars. Fluxes are tabulated from .09 to 160 micrometers. Preliminary results are reported for many photometric systems. Work is underway on grids for other microturbulent velocities. Microturbulent velocity strongly affects the interpretation of Cepheid and RR Lyrae photometry. The models, fluxes, and colors are available on magnetic tape and will also be distributed on CD-ROMs. RP KURUCZ, RL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 19 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0074-1809 J9 IAU SYMP PY 1992 IS 149 BP 225 EP 232 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JF270 UT WOS:A1992JF27000031 ER PT J AU ROH, DG KIM, HR MINH, YC AUH, BR KOO, BC AF ROH, DG KIM, HR MINH, YC AUH, BR KOO, BC TI MOLECULAR LINE OBSERVATIONS TOWARDS W58 AND GL490 SO IAU SYMPOSIA LA English DT Article AB We observed 3 mm transitions of several interstellar molecules toward star-forming regions in W58 and GL490 using the 14 m Daeduk Radio Telescope (Korea). We derive molecular abundances for the "broad" components observed with a high spectral resolution, which could represent the abundances of outflowing materials. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP ROH, DG (reprint author), INST SPACE SCI & ASTRON, RADIO ASTRON SECT, SEOUL, SOUTH KOREA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0074-1809 J9 IAU SYMP PY 1992 IS 150 BP 225 EP 226 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JQ128 UT WOS:A1992JQ12800051 ER PT J AU AIELLO, S PESTELLINI, CC TINE, S AF AIELLO, S PESTELLINI, CC TINE, S TI RADIATION TRANSFER AND PHOTOCHEMICAL EFFECTS IN INHOMOGENEOUS DENSE CLOUDS SO IAU SYMPOSIA LA English DT Article ID STELLAR DARK CLOUDS; INTERSTELLAR DUST; FIELD AB UV radiation leads to photodissociation and photoionization of molecular species in diffuse clouds and in the extended envelopes of dark regions. In the inner part of heavily-obscured objects, the residual external field may be negligible; alternative mechanisms, such as cosmic-ray-induced H-2 emission, appear to be efficient in photodestruction processes. We evaluate the relative importance of these radiation sources, and give some estimates of their effects on the mean lifetime of interstellar molecules, taking into account the cloud structure that significantly affects the penetration depth of UV radiation. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP AIELLO, S (reprint author), UNIV FLORENCE, DIP ASTRON & SCI SPAZIO, I-50121 FLORENCE, ITALY. NR 17 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0074-1809 J9 IAU SYMP PY 1992 IS 150 BP 231 EP 236 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JQ128 UT WOS:A1992JQ12800053 ER PT J AU PRATAP, P MENTEN, KM REID, MJ MORAN, JM WALMSLEY, CM AF PRATAP, P MENTEN, KM REID, MJ MORAN, JM WALMSLEY, CM TI VLBI OBSERVATIONS OF AMMONIA (9,6) MASERS SO IAU SYMPOSIA LA English DT Article ID W51 AB We present the first VLBI measurement of interstellar ammonia (NH3) masers. Two masers were found toward the ultracompact HII regions, W51-e1 and e2. The masers are unresolved in angle and smaller than 0.1 milliarcseconds. Unless these masers are highly beamed, they appear to be saturated. C1 MAX PLANCK INST RADIOASTRON, W-5300 BONN 1, GERMANY. RP PRATAP, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0074-1809 J9 IAU SYMP PY 1992 IS 150 BP 345 EP 346 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JQ128 UT WOS:A1992JQ12800077 ER PT J AU PRATAP, P SNYDER, LE BATRLA, W AF PRATAP, P SNYDER, LE BATRLA, W TI A MODEL FOR THE MASER SOURCE NGC-7538 IRS-1 SO IAU SYMPOSIA LA English DT Article ID FORMALDEHYDE MASER; EMISSION AB High resolution observations of the molecular cloud around NGC 7538 IRS 1 in the J=1-0 transition of (CO)-C-13 show that the lower bound for density in that region is about 2 x 10(3) cm-3. The study of various molecular transitions and the continuum measurements of the H II region indicate that the conditions required by the Boland and de Jong model for the excitation of the H2CO maser are not very stringent or unique. C1 UNIV ILLINOIS, DEPT ASTRON, URBANA, IL 61801 USA. FACHHSCH COBURG, ABT MUENCHBERG, W-8660 MUENCHBERG, GERMANY. RP PRATAP, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0074-1809 J9 IAU SYMP PY 1992 IS 150 BP 347 EP 348 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JQ128 UT WOS:A1992JQ12800078 ER PT J AU RAWLINGS, JMC HARTQUIST, TW MENTEN, KM WILLIAMS, DA AF RAWLINGS, JMC HARTQUIST, TW MENTEN, KM WILLIAMS, DA TI INFALL IN COLLAPSING PROTOSTARS SO IAU SYMPOSIA LA English DT Article ID STAR FORMATION; CLOUDS C1 MAX PLANCK INST EXTRATERRESTR PHYS, W-8046 GARCHING, GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV MANCHESTER, INST SCI & TECHNOL, DEPT MATH, MANCHESTER M60 1QD, LANCS, ENGLAND. RP RAWLINGS, JMC (reprint author), UNIV OXFORD, DEPT PHYS, NUCL PHYS LAB, KEBLE RD, OXFORD OX1 3RH, ENGLAND. NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0074-1809 J9 IAU SYMP PY 1992 IS 150 BP 357 EP 358 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JQ128 UT WOS:A1992JQ12800081 ER PT J AU CURIEL, S AF CURIEL, S TI MOLECULAR STUDIES OF HERBIG-HARO OBJECTS SO IAU SYMPOSIA LA English DT Article ID STAR-FORMATION REGION; HYDROGEN EMISSION; HIGH-RESOLUTION; CEPHEUS-A; LINE; EXCITATION; CONTINUUM; COMPLEXES; OUTFLOWS; IMAGES AB Recent ultraviolet, infrared, millimeter and centimeter-wavelength observations have revealed that HH objects axe also sources of molecular line emission. Infrared observations have shown that H-2 line emission in HH objects presents a wide and complex variety of morphologies, being in most of the cases similar to that observed at optical wavelengths. New high-angular resolution radio observations of molecular lines have revealed that small high-density condensations axe frequently found in association with HH objects. Below, a brief review of molecular emission in HH objects is presented. RP CURIEL, S (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, MS 10, CAMBRIDGE, MA 02138 USA. NR 42 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0074-1809 J9 IAU SYMP PY 1992 IS 150 BP 373 EP 378 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JQ128 UT WOS:A1992JQ12800087 ER PT J AU LATHAM, DW MATHIEU, RD MILONE, AAE DAVIS, RJ AF LATHAM, DW MATHIEU, RD MILONE, AAE DAVIS, RJ TI TIDAL CIRCULARIZATION AMONG THE CLOSE BINARIES IN M67 SO IAU SYMPOSIA LA English DT Article ID SOLAR-TYPE STARS; OPEN CLUSTER M67; MULTIPLICITY C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV WISCONSIN, DEPT ASTRON, MADISON, WI 53706 USA. NATL UNIV CORDOBA, CORDOBA OBSERV, RA-5000 CORDOBA, ARGENTINA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0074-1809 J9 IAU SYMP PY 1992 IS 151 BP 471 EP 472 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JJ251 UT WOS:A1992JJ25100073 ER PT J AU MILONE, AAE LATHAM, DW MATHIEU, RD MORSE, JA DAVIS, RJ AF MILONE, AAE LATHAM, DW MATHIEU, RD MORSE, JA DAVIS, RJ TI CAN EVOLUTION IN CLOSE BINARIES ACCOUNT FOR THE BLUE STRAGGLERS IN M67 SO IAU SYMPOSIA LA English DT Article ID STELLAR C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NATL UNIV CORDOBA, CORDOBA OBSERV, RA-5000 CORDOBA, ARGENTINA. UNIV WISCONSIN, DEPT ASTRON, MADISON, WI 53706 USA. UNIV N CAROLINA, DEPT PHYS & ASTRON, CHAPEL HILL, NC 27599 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0074-1809 J9 IAU SYMP PY 1992 IS 151 BP 473 EP 474 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JJ251 UT WOS:A1992JJ25100074 ER PT J AU MILONE, AAE LATHAM, DW AF MILONE, AAE LATHAM, DW TI THE BLUE STRAGGLER F190 - A CASE FOR MASS-TRANSFER SO IAU SYMPOSIA LA English DT Article ID CLOSE BINARY-SYSTEMS; OPEN CLUSTER M67; EVOLUTION; STARS AB The blue straggler F190 is a member of the old open cluster M67. We argue that F190 may still be in the final stages of the mass transfer that has made it into a blue straggler. We use the turnoff mass of the cluster and the mass function derived from the spectroscopic orbit for F190 to constrain the masses of each member of the binary, both before mass transfer and now. We find that the mass transfer must have been nearly 100 percent efficient. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NATL UNIV CORDOBA, CORDOBA OBSERV, RA-5000 CORDOBA, ARGENTINA. NR 22 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0074-1809 J9 IAU SYMP PY 1992 IS 151 BP 475 EP 478 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JJ251 UT WOS:A1992JJ25100075 ER PT J AU TORRES, G LATHAM, DW MAZEH, T CARNEY, BW STEFANIK, RP DAVIS, RJ LAIRD, JB AF TORRES, G LATHAM, DW MAZEH, T CARNEY, BW STEFANIK, RP DAVIS, RJ LAIRD, JB TI TIDAL CIRCULARIZATION AMONG THE CLOSE BINARIES IN THE HALO SO IAU SYMPOSIA LA English DT Article ID PROPER-MOTION STARS; ORBITAL CIRCULARIZATION; SPECTROSCOPIC BINARIES AB For a sample of halo binaries, we find that the transition between circular and eccentric orbits occurs at a period of at least 18.7 days. This is consistent with the Goldman & Mazeh theory of tidal circularization on the main sequence. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NATL UNIV CORDOBA, CORDOBA OBSERV, RA-5000 CORDOBA, ARGENTINA. TEL AVIV UNIV, RAYMOND & BEVERLY SACKLER FAC EXACT SCI, SCH PHYS & ASTRON, IL-69978 TEL AVIV, ISRAEL. UNIV N CAROLINA, DEPT PHYS & ASTRON, CHAPEL HILL, NC 27599 USA. BOWLING GREEN STATE UNIV, DEPT PHYS & ASTRON, BOWLING GREEN, OH 43403 USA. NR 23 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0074-1809 J9 IAU SYMP PY 1992 IS 151 BP 491 EP 495 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JJ251 UT WOS:A1992JJ25100079 ER PT J AU HARMON, JK SULZER, MP PERILLAT, PJ CHANDLER, JF AF HARMON, JK SULZER, MP PERILLAT, PJ CHANDLER, JF TI MARS RADAR MAPPING - STRONG BACKSCATTER FROM THE ELYSIUM BASIN AND OUTFLOW CHANNEL SO ICARUS LA English DT Note ID POLARIZATION C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP HARMON, JK (reprint author), NATL ASTRON & IONOSPHERE CTR,ARECIBO,PR 00613, USA. NR 16 TC 25 Z9 25 U1 0 U2 0 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD JAN PY 1992 VL 95 IS 1 BP 153 EP 156 DI 10.1016/0019-1035(92)90197-F PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA HF734 UT WOS:A1992HF73400011 ER PT J AU EKLUND, J AF EKLUND, J TI THE FINAL WORD ON THE BUG SO IEEE ANNALS OF THE HISTORY OF COMPUTING LA English DT Letter RP EKLUND, J (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 SN 1058-6180 J9 IEEE ANN HIST COMPUT JI IEEE Ann. Hist. Comput. PY 1992 VL 14 IS 3 BP 6 EP 6 PG 1 WC Computer Science, Theory & Methods; History & Philosophy Of Science SC Computer Science; History & Philosophy of Science GA JE068 UT WOS:A1992JE06800001 ER PT J AU ROISIN, Y AF ROISIN, Y TI DEVELOPMENT OF NONREPRODUCTIVE CASTES IN THE NEOTROPICAL TERMITE GENERA CORNITERMES, EMBIRATERMES AND RHYNCHOTERMES (ISOPTERA, NASUTITERMITINAE) SO INSECTES SOCIAUX LA English DT Article DE ISOPTERA; TERMITIDAE; NASUTITERMITINAE; CASTE DIFFERENTIATION; PHYLOGENY; EVOLUTION ID SECRETIONS AB The developmental pattern of the neuter castes was studied in the mandibulate nasute genera Cornitermes, Embiratermes and Rhynchotermes. In Cornitermes walkeri, all the workers and soldiers are male. There are two larval and a single worker instar. Workers can molt into presoldiers. In Embiratermes chagresi and Rhynchotermes perarmatus, both sexes are present among the neuters. A slight sexual dimorphism (males > females) is discernible among both larval instars and among workers of E. chagresi; female workers can molt into presoldiers. In R. perarmatus, the sexual dimorphism is conspicuous from the first larval instar on. Male larvae go through two instars, then give rise to workers, which do not molt. In R. perarmatus, there is no worker stage in females, but a third larval instar, preceding the presoldier. Hypotheses are proposed as to the evolution of these caste patterns, attempting to conciliate present knowledge of Nasutitermitinae phylogeny and known evolutionary trends affecting termite caste patterns, according to the species' ecology. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP ROISIN, Y (reprint author), UNIV LIBRE BRUXELLES,BIOL ANIMALE & CELLULAIRE LAB,CP 160-12,AVE FD ROOSEVELT 50,B-1050 BRUSSELS,BELGIUM. RI Roisin, Yves/C-1378-2010 NR 31 TC 20 Z9 21 U1 0 U2 2 PU BIRKHAUSER VERLAG AG PI BASEL PA PO BOX 133 KLOSTERBERG 23, CH-4010 BASEL, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PY 1992 VL 39 IS 3 BP 313 EP 324 DI 10.1007/BF01323951 PG 12 WC Entomology SC Entomology GA JQ491 UT WOS:A1992JQ49100007 ER PT J AU WALTERS, HRJ SCHOLZ, TT SCOTT, MP BURKE, PG AF WALTERS, HRJ SCHOLZ, TT SCOTT, MP BURKE, PG TI ELECTRON HYDROGEN SCATTERING AT INTERMEDIATE ENERGIES SO INSTITUTE OF PHYSICS CONFERENCE SERIES LA English DT Article ID DIFFERENTIAL CROSS-SECTIONS; PHOTON ANGULAR-CORRELATIONS; ATOMIC-HYDROGEN; ELASTIC-SCATTERING; IMPACT EXCITATION; 2P STATE; TRANSITIONS; 1S->2P; 1S-2S; 2S AB Calculations of 1s --> 1s elastic scattering and 1s --> 2s and 1s --> 2p excitation are reported for the intermediate energy range from 13.6 to 54.4 eV. Different methods have been employed for different intervals of the total orbital angular momentum L: (i) in 0 less-than-or-equal-to L less-than-or-equal-to 4 the new intermediate energy R-matrix method of Burke et al (1987) has been used; (ii) in 5 less-than-or-equal-to L less-than-or-equal-to L(max), where L(max) varies between 10 and 16, coupled pseudostate calculations have been performed using the 1s, 2s, 3sBAR, 4sBAR, 2p, 3pBAR, 4pBAR, 3dBAR, 4dBAR basis of Fon et al (1981); (iii) in L(max) + 1 less-than-or-equal-to L < infinity the plane wave second Born approximation has been used. The second Born approximation has also been employed to provide corrections for angular symmetries omitted in (i) and (ii). Integrated and differential cross sections, and alignment and orientation parameters are presented and compared with experiment. For elastic scattering there is good agreement. For the 1s --> 2s and 1s --> 2p transitions the quality of agreement is not quite so satisfactory with some notable discrepancies appearing, especially at 54.4 eV. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, ITAMP, CAMBRIDGE, MA 02138 USA. RP WALTERS, HRJ (reprint author), QUEENS UNIV BELFAST, DEPT APPL MATH & THEORET PHYS, BELFAST BT7 1NN, ANTRIM, NORTH IRELAND. NR 27 TC 0 Z9 0 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0951-3248 J9 INST PHYS CONF SER JI Inst. Phys. Conf. Ser. PY 1992 IS 122 BP 59 EP 69 PG 11 WC Physics, Multidisciplinary SC Physics GA HV058 UT WOS:A1992HV05800008 ER PT J AU BLUNDELL, R MILLER, RE GUNDLACH, KH AF BLUNDELL, R MILLER, RE GUNDLACH, KH TI UNDERSTANDING NOISE IN SIS RECEIVERS SO INTERNATIONAL JOURNAL OF INFRARED AND MILLIMETER WAVES LA English DT Article DE SUPERCONDUCTING MIXER; HETERODYNE RECEIVER; JOSEPHSON NOISE ID MIXER; GHZ; ASTRONOMY; GAIN AB A simple laboratory test receiver has been built and used to examine some interesting aspects of heterodyne mixing with superconductor-insulator-superconductor tunnel junctions. Experiments made over the frequency range 220 GHz - 490 GHz using junctions of both the Pb/Bi/In-type and the Pb/In/Au-type indicate that, in the majority of cases, a receiver may be characterized through a few simple measurements made external to it's dewar. We also show that, at high local oscillator drive levels, excess mixer noise may be generated which may be removed by the application of a magnetic field. This is of particular relevance to high frequency mixing where Josephson interference may be strong. Finally, it is observed that even in the presence of severe interference a stable bias point, free from excess mixer noise, is often possible. RP BLUNDELL, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 13 TC 50 Z9 51 U1 0 U2 3 PU PLENUM PUBL CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 SN 0195-9271 J9 INT J INFRARED MILLI JI Int. J. Infrared Millimeter Waves PD JAN PY 1992 VL 13 IS 1 BP 3 EP 14 DI 10.1007/BF01011203 PG 12 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA HB200 UT WOS:A1992HB20000001 ER PT J AU EBERHARD, WG AF EBERHARD, WG TI WEB CONSTRUCTION BY MODISIMUS-SP (ARANEAE, PHOLICIDAE) SO JOURNAL OF ARACHNOLOGY LA English DT Article AB The behavior used by Modisimus sp. to construct its domed sheet web is more stereotyped and organized than is apparent from the finished structure. A simple program involving attaching the non-sticky dragline to the substrate beyond the previous limits of the web, and then filling in the newly formed angle is probably used to construct the skeleton sheet and the tangle above it. A set of sticky lines is then laid, filling in this sheet. Construction behavior resembles that of orb weavers in commencing with a skeleton scaffold of non-sticky lines which is then filled in with other non-sticky lines, in adding sticky lines after the support structure of non-sticky lines is complete, and in being organized around a central area. RP EBERHARD, WG (reprint author), UNIV COSTA RICA,SMITHSONIAN TROP RES INST,SAN JOSE,COSTA RICA. NR 0 TC 14 Z9 15 U1 0 U2 1 PU AMER ARACHNOLOGICAL SOC PI NEW YORK PA C/O NORMAN I PLATNICK, AMER MUSEUM NATURAL HISTORY, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024 SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 1992 VL 20 IS 1 BP 25 EP 34 PG 10 WC Entomology SC Entomology GA JK450 UT WOS:A1992JK45000003 ER PT J AU ZEH, DW ZEH, JA AF ZEH, DW ZEH, JA TI ON THE FUNCTION OF HARLEQUIN BEETLE-RIDING IN THE PSEUDOSCORPION, CORDYLOCHERNES-SCORPIOIDES (PSEUDOSCORPIONIDA, CHERNETIDAE) SO JOURNAL OF ARACHNOLOGY LA English DT Article AB The pseudoscorpion, Cordylochernes scorpioides, frequently occurs under the elytra of the giant harlequin beetle, Acrocinus longimanus. Here. we assess four hypotheses/scenarios which have been proposed to account for this phenomenon: (1) accidental boarding; (2) obligate symbiosis; (3) phagophily, and (4) phoretic dispersal. Field and laboratory observations of embarkation behavior clearly refute the accidental boarding hypothesis. Contrary to the obligate symbiosis scenario, pseudoscorpion offspring production does not occur on the beetle and the primary habitat of C. scorpioides is decaying trees. The phagophily hypothesis, i.e., that pseudoscorpions mount harlequins for the primary purpose of preying upon the beetles' phoretic mites, is also not supported. Pseudoscorpions collected from trees were found to be in better nutritional condition than beetle-riding individuals. Finally, evidence from a companion study supports the dispersal hypothesis, and also indicates that large male C. scorpioides defend beetles' abdomens as strategic sites for intercepting and inseminating dispersing females. RP ZEH, DW (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO 34002-0948,BALBOA,PANAMA. NR 0 TC 10 Z9 12 U1 0 U2 6 PU AMER ARACHNOLOGICAL SOC PI NEW YORK PA C/O NORMAN I PLATNICK, AMER MUSEUM NATURAL HISTORY, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024 SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 1992 VL 20 IS 1 BP 47 EP 51 PG 5 WC Entomology SC Entomology GA JK450 UT WOS:A1992JK45000006 ER PT J AU RHYMER, JM AF RHYMER, JM TI AN EXPERIMENTAL-STUDY OF GEOGRAPHIC-VARIATION IN AVIAN GROWTH AND DEVELOPMENT SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE MALLARDS; GEOGRAPHIC VARIATION; GENOTYPE-ENVIRONMENT; TRANSPLANTS; GROWTH AB Reciprocal transplant and "common garden" experiments were done to distinguish the genetic and environmental components of geographic variation in growth, development and morphological characters of Mallard Ducks (Anas platyrhynchos) from California, USA and Manitoba, Canada. Most of the variation in growth and development could be attributed to differences in nesting phenology and local environmental conditions. Differences in morphological characters typical of birds in the two wild populations could be induced by transplanting young between localities. All differences between populations disappeared in the F1 offspring from captive breeding crosses, reared in a common environment. These results suggest that population-level variation in growth, development and morphology of Mallards in the wild is environmentally induced. RP RHYMER, JM (reprint author), SMITHSONIAN INST,CTR MUSEUM SUPPORT,MOLEC SYSTEMAT LAB,WASHINGTON,DC 20560, USA. NR 0 TC 32 Z9 32 U1 3 U2 6 PU BIRKHAUSER VERLAG AG PI BASEL PA PO BOX 133 KLOSTERBERG 23, CH-4010 BASEL, SWITZERLAND SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PY 1992 VL 5 IS 2 BP 289 EP 306 DI 10.1046/j.1420-9101.1992.5020289.x PG 18 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA HX996 UT WOS:A1992HX99600006 ER PT J AU DINEEN, JF HINES, AH AF DINEEN, JF HINES, AH TI INTERACTIVE EFFECTS OF SALINITY AND ADULT EXTRACT UPON SETTLEMENT OF THE ESTUARINE BARNACLE BALANUS-IMPROVISUS (DARWIN, 1854) SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE BALANUS-IMPROVISUS; BARNACLE; ESTUARY; LARVAL SETTLEMENT; SALINITY; SETTLEMENT FACTOR ID MARINE INVERTEBRATE LARVAE; CYPRIS LARVAE; INTERTIDAL BARNACLE; NATURAL-PRODUCTS; METAMORPHOSIS; BALANOIDES; ATTACHMENT; AMPHITRITE; INHIBITION; RECRUITMENT AB Balanus improvisus (Darwin, 1854) is distributed in mesohaline regions of esturaries worldwide. In Chesapeake Bay, USA, it occurs intermediately along a horizontal salinity gradient between two congeners, oligohaline B. subalbidus (Henry, 1973) and the more polyhaline B. eburneus (Gould, 1841). Laboratory reared cyprids of B. improvisus were exposed to slate substrata treated or untreated with conspecific settlement factor as salinity was varied. Peak settlement occurred at salinities of 10 and 15 parts per thousand on treated substrata, reflecting an interactive effect of these two parameters. Settlement on untreated substrata was low and showed no salinity pattern. Cyprids of B. improvisus settled in significantly greater numbers on intra-than on interspecific settlement factor adsorbed to slate, and they settled in lowest numbers on settlement factor from B. eburneus compared to B. subalbidus. In addition, surface effects upon settlement were less obvious as age of cyprids increased. RP DINEEN, JF (reprint author), SMITHSONIAN ENVIRONM RES CTR,POB 28,EDGEWATER,MD 21037, USA. NR 60 TC 35 Z9 36 U1 0 U2 9 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. PY 1992 VL 156 IS 2 BP 239 EP 252 DI 10.1016/0022-0981(92)90249-A PG 14 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA HU907 UT WOS:A1992HU90700008 ER PT J AU ZEH, DW ZEH, JA AF ZEH, DW ZEH, JA TI FAILED PREDATION OR TRANSPORTATION - CAUSES AND CONSEQUENCES OF PHORETIC BEHAVIOR IN THE PSEUDOSCORPION DINOCHEIRUS-ARIZONENSIS (PSEUDOSCORPIONIDA, CHERNETIDAE) SO JOURNAL OF INSECT BEHAVIOR LA English DT Article DE DINOCHEIRUS-ARIZONENSIS; DISPERSAL; ODONTOLOXOZUS-LONGICORNIS; PHORESY; PREDATION; PSEUDOSCORPIONIDA AB The pseudoscorpion Dinocheirus arizonensis inhabits rotting saguaro cactus in the Sonoran Desert and has also been found attached to the legs of the cactophilic neriid fly, Odontoloxozus longicornis. Laboratory experiments demonstrated a higher incidence of phoresy on eclosing versus postteneral adult flies, a female bias in phoresy, and an increased rate in female phoresy through time. The pseudoscorpion may also prey on the fly, but predation rate was unaffected by fly category, pseudoscorpion gender, or food deprivation. A study of pseudoscorpion colonization in the field indicated that females were the first to colonize and the first to abandon the transient habitat of a saguaro rot and, thus, corroborated patterns of phoretic behavior in the laboratory. Taken together, these results establish that phoresy is a behavior functioning specifically for dispersal. The hypothesis that pseudoscorpion transport by other arthropods is accidental, motivated by hunger, and occurs because pseudoscorpions are incapable of consuming their hosts is rejected. RP ZEH, DW (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,BALBOA,PANAMA. NR 0 TC 12 Z9 13 U1 0 U2 5 PU PLENUM PUBL CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 SN 0892-7553 J9 J INSECT BEHAV JI J. Insect Behav. PD JAN PY 1992 VL 5 IS 1 BP 37 EP 49 DI 10.1007/BF01049156 PG 13 WC Entomology SC Entomology GA HA617 UT WOS:A1992HA61700003 ER PT J AU CHOI, JK COATS, DW BROWNLEE, DC SMALL, EB AF CHOI, JK COATS, DW BROWNLEE, DC SMALL, EB TI MORPHOLOGY AND INFRACILIATURE OF 3 SPECIES OF EUTINTINNUS (CILIOPHORA, TINTINNINA) WITH GUIDELINES FOR INTERPRETING PROTARGOL-STAINED TINTINNINE CILIATES SO JOURNAL OF PROTOZOOLOGY LA English DT Article DE TAXONOMY; ZOOID ID LORICA; CYCLE AB The infraciliatures of three Chesapeake Bay species of Eutintinnus conforming in lorica morphology to E. angustatus, E. pectinis, and E. tenuis were compared following Protargol silver impregnation. The kinetome of these species had a number of shared attributes including: 1) a right and left field that were of similar length and kinetal spacing; 2) two, rarely three, long dorsal kineties composed of monokinetids; 3) a ventral kinety; and 4) the absence of a true posterior kinety. Nonetheless, the specific organization of infraciliary components varied considerably among species. For example, the organization of the ventral kinety and several kineties along the border of the left field was different in all three species. In addition, the dorsal kineties of E. angustatus differed positionally from those of E. pectinis and E. tenuis. Some divergence in oral infraciliature was also noted, with the arrangement of infundibular oral polykinetids in E. pectinis and E. tenuis being distinct from that of E. angustatus. The amount of variation in the infraciliature of Eutintinnus spp. was much greater than previously noted for congeneric species of tintinnines and supports the separation E. angustatus, E. pectinis, and E. tenuis at the generic or subgeneric level. C1 SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. INHA UNIV,DEPT OCEANOG,INCHON 402751,SOUTH KOREA. DEPT PLANNING & ZONING,PRINCE FREDERICK,MD 20678. UNIV MARYLAND,DEPT ZOOL,COLLEGE PK,MD 20742. NR 28 TC 20 Z9 22 U1 0 U2 1 PU SOC PROTOZOOLOGISTS PI LAWRENCE PA 810 E 10TH ST, LAWRENCE, KS 66044 SN 0022-3921 J9 J PROTOZOOL PD JAN-FEB PY 1992 VL 39 IS 1 BP 80 EP 92 DI 10.1111/j.1550-7408.1992.tb01286.x PG 13 WC Zoology SC Zoology GA HG564 UT WOS:A1992HG56400012 ER PT J AU QUADRELLI, BM LORENZINI, EC AF QUADRELLI, BM LORENZINI, EC TI DYNAMICS AND STABILITY OF A TETHERED CENTRIFUGE IN LOW EARTH ORBIT SO JOURNAL OF THE ASTRONAUTICAL SCIENCES LA English DT Article AB The three dimensional attitude dynamics of a spaceborne tethered centrifuge for artificial gravity experiments in low Earth orbit is analyzed using two different methods. First, the tethered centrifuge is modelled as a dumbbell with a straight viscoelastic tether, point tip-masses, and sophisticated environmental models such as non-spherical gravity, thermal perturbations, and a dynamic atmospheric model. The motion of the centrifuge during spin-up, de-spin, and steady-rotation is then simulated. Second, a continuum model of the tether is developed for analyzing the stability of lateral tether oscillations. Results indicate that the maximum fluctuation about the 1-g radial acceleration level is less than 10(-3) g; the time required for spin-up and de-spin is less than one orbit; and lateral oscillations are stable for any practical values of the system parameters. RP QUADRELLI, BM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,DIV RADIO & GEOASTRON,CAMBRIDGE,MA 02138, USA. NR 17 TC 3 Z9 3 U1 1 U2 2 PU AMER ASTRONAUTICAL SOC PI SPRINGFIELD PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 SN 0021-9142 J9 J ASTRONAUT SCI JI J. Astronaut. Sci. PD JAN-MAR PY 1992 VL 40 IS 1 BP 3 EP 25 PG 23 WC Engineering, Aerospace SC Engineering GA HP051 UT WOS:A1992HP05100002 ER PT J AU HOLZENBEIN, S MARCHINTON, RL AF HOLZENBEIN, S MARCHINTON, RL TI EMIGRATION AND MORTALITY IN ORPHANED MALE WHITE-TAILED DEER SO JOURNAL OF WILDLIFE MANAGEMENT LA English DT Article ID DISPERSAL AB We radiotracked 15 male white-tailed deer (Odocoileus virginianus) orphaned as weaned fawns (less-than-or-equal-to 10 months old) and 19 that matured with their dams (controls), because little is known about the fate of fawns under regimes of high female harvest. Monthly emigration rates were progressively higher (P = 0.003) in control than in orphaned deer. By 30 months, 9.1% of orphans and 86.5% of controls had emigrated from natal ranges. Overall survival rates from all risks between 7 and 30 months of age were 46.2% for orphans and 6.7% for controls, whereas survival rates for nonhunting risks were 67.3% and 15.6%, respectively. Monthly survival rates from all risks and from nonhunting risks were higher (P = 0.02 in each case) for orphans than controls. These results have been useful in convincing hunters to adequately control females and spare young males on their lease or property. C1 SMITHSONIAN INST,NATL ZOOL PK,CTR CONSERVAT & RES,FRONT ROYAL,VA 22630. UNIV GEORGIA,SCH FOREST RESOURCES,ATHENS,GA 30602. NR 33 TC 30 Z9 31 U1 0 U2 9 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 JAN PY 1992 VL 56 IS 1 BP 147 EP 153 DI 10.2307/3808802 PG 7 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA HA129 UT WOS:A1992HA12900018 ER PT J AU HERRERA, A JACKSON, JBC AF HERRERA, A JACKSON, JBC TI ENVIRONMENTAL VERSUS TAXONOMIC VARIATION IN LOPHOPHORE MORPHOLOGY OF PANAMANIAN CHEILOSTOME BRYOZOANS SO MARINE BIOLOGY LA English DT Article ID FEEDING CURRENT VELOCITY; AMBIENT FLOW VELOCITY; PARTICLE CONCENTRATION; UPSTREAM COLONIES; NEOGENE BRYOZOAN; LATERAL CILIA; MARINE; EVOLUTION; SUCCESS; TEMPO AB The morphology of the lophophore and mouth was measured for freshly collected colonies of seven common bryozoan reef species at three sites along the central Caribbean coast of Panama during the dry season, from the end of December 1988 through May 1989. Characters measured or scored include the number of tentacles, circumference of the lophophore, abanal and anal tentacle length, abanal and anal tentacle spacing, and perimeter of the mouth. Taxa studied include three species each of Stylophoma Levinsen, and Steginoporella (Smitt), and one species of Trematooecia Osburn. Individuals were collected from both continental and offshore fringing reefs from depths of 1 to > 30 m. Terrestrial runoff from heavy tropical rains, sedimentation, and sea exposure vary greatly between sites. Congeneric species showed small but consistent differences in lophophore size, but little or no difference in spacing of tentacles or perimeter of the mouth. This suggests that closely related species feed on similarly sized particles despite their overall differences in zooidal size. Lopophore morphology also varied intraspecifically between reefs, particularly in the length of the tentacles and spacing between tentacles. Patterns of variation were similar for all species, which implies that species shift their diets in similar directions between the different reefs. The combination of these patterns suggests that niche diversification in feeding does not occur among congeneric species in the cheilostomes examined. RP HERRERA, A (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. NR 32 TC 7 Z9 7 U1 0 U2 1 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD JAN PY 1992 VL 112 IS 1 BP 99 EP 106 DI 10.1007/BF00349733 PG 8 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA GZ546 UT WOS:A1992GZ54600013 ER PT J AU FITZGERALD, S LEAVENS, PB NELEN, JA AF FITZGERALD, S LEAVENS, PB NELEN, JA TI CHEMICAL VARIATION IN VESUVIANITE SO MINERALOGY AND PETROLOGY LA English DT Article ID CRYSTAL-STRUCTURE; BEARING VESUVIANITE; CHEMISTRY AB Microprobe analyses of 44 vesuvianite specimens of different color, morphology, and occurrence indicate the chemical variation of the species. Vesuvianites can be divided into four types, based on chemistry and color; most vesuvianites can be assigned to one of these types with confidence. Type 1 vesuvianites contain approximately 2 atoms of Mg, <0.25 atoms of Ti, and variable Fe, apparently trivalent, in a formula based on 50 non-H cations. They are dark to pale green, white, or pink. Type 2 vesuvianites contain >2.5 atoms of Mg, variable (divalent?) Fe, and <0.5 atoms of Ti. In color they are yellow, yellow-brown, or yellow-green. Type 3 vesuvianites contain divalent Fe, 0.5 to 1.5 atoms of Ti and close to 18 atoms of Si (full occupancy of tetrahedral sites). They are yellow, brown, red-brown, or black. Type 4 vesuvianites are manganoan or cuprian; the studied samples are from Pajsberg, Sweden, Franklin, New Jersey, and Telemark, Norway. In color they are red-brown, purple, blue ("cyprine"), or green. Iron and much of the Mn is apparently trivalent. Unlike garnets, which they resemble structurally, vesuvianites contain almost exclusively Ca in the eight-fold sites in the structure. Silicon occupies 95% or more of the tetrahedral sites. Aluminum fills the smaller octahedral site, A. Chemical variation occurs predominantly in the more open, octahedral, general or G site and in the five-coordinated B site. Simple substitutions in G include Fe3+ or Mn3+ for Al3+, and Fe2+, Mn2+, or Zn2+ for Mg2+. Coupled substitutions include TiO = AlOH, MgTi = AlAl and AlAl = MgSi. The B site may contain CU2+, Fe2+, Fe3+, or Al3+. Changes in the amounts of O and OH in two different positions give a range of anion charge from 146(O67OH12) to about 148 (O69OH10). C1 UNIV DELAWARE,DEPT GEOL,NEWARK,DE 19711. SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560. NR 17 TC 19 Z9 19 U1 1 U2 3 PU SPRINGER-VERLAG WIEN PI VIENNA PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 VIENNA, AUSTRIA SN 0930-0708 J9 MINER PETROL JI Mineral. Petrol. PY 1992 VL 46 IS 2 BP 163 EP 178 DI 10.1007/BF01160185 PG 16 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA JC910 UT WOS:A1992JC91000005 ER PT J AU VANDIVER, P DRUZIK, J AF VANDIVER, P DRUZIK, J TI ART AND TECHNOLOGY SO MRS BULLETIN LA English DT Article RP VANDIVER, P (reprint author), SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MATERIALS RESEARCH SOCIETY PI PITTSBURGH PA 9800 MC KNIGHT ROAD SUITE 327, PITTSBURGH, PA 15237 SN 0883-7694 J9 MRS BULL JI MRS Bull. PD JAN PY 1992 VL 17 IS 1 BP 14 EP 17 PG 4 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA HB562 UT WOS:A1992HB56200003 ER PT J AU WARD, DC AF WARD, DC TI JERVIS,JOHN,B. - AN AMERICAN ENGINEERING PIONEER - LARKIN,FD SO NEW YORK HISTORY LA English DT Book Review RP WARD, DC (reprint author), SMITHSONIAN INST,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 JAN PY 1992 VL 73 IS 1 BP 105 EP 106 PG 2 WC History SC History GA HU364 UT WOS:A1992HU36400012 ER PT J AU BREMER, K JANSEN, RK KARIS, PO KALLERSJO, M KEELEY, SC KIM, KJ MICHAELS, HJ PALMER, JD WALLACE, RS AF BREMER, K JANSEN, RK KARIS, PO KALLERSJO, M KEELEY, SC KIM, KJ MICHAELS, HJ PALMER, JD WALLACE, RS TI A REVIEW OF THE PHYLOGENY AND CLASSIFICATION OF THE ASTERACEAE SO NORDIC JOURNAL OF BOTANY LA English DT Review ID CONFIDENCE-LIMITS; BOOTSTRAP AB The Asteraceae are commonly divided into two large subfamilies, the Cichorioideae (syn. Lactucoideae; Mutisieae, Cardueae, Lactuceae, Vernonieae, Liabeae, Arctoteae) and the Asteroideae (Inuleae, Astereae, Anthemideae, Senecioneae, Calenduleae, Heliantheae, Eupatorieae). Recent phylogenetic analyses based on morphological and chloroplast DNA data conclusively show that the Mutisieae-Barnadesiinae are the sister group to the rest of the family and that the Asteroideae tribes form a monophyletic group. The Vernonieae and Liabeae are sister tribes and the Eupatorieae are nested within a paraphyletic Heliantheae; otherwise tribal interrelationships are still largely uncertain. The Mutisieae-Barnadesiinae are excluded from the Mutisieae and elevated to the new subfamily Barnadesioideae. The two subfamilies Barnadesioideae and Asteroideae are monophyletic, whereas the status of the Cichorioideae remains uncertain. Analyses of chloroplast DNA data support the monophyly of the Cichorioideae; however, morphological data indicate that the subfamily is paraphyletic. Further studies are needed to test the monophyly of the Cichorioideae, as well as to further resolve tribal interrelationships in the two larger subfamilies. C1 UNIV UPPSALA,DEPT SYSTEMAT BOT,S-75121 UPPSALA,SWEDEN. UNIV TEXAS,DEPT BOT,AUSTIN,TX 78713. SWEDISH MUSEUM NAT HIST,DEPT PHANEROGAM BOT,S-10405 STOCKHOLM,SWEDEN. SMITHSONIAN INST,MOLEC SYSTEMAT LAB,WASHINGTON,DC 20560. UNIV HAWAII,DEPT BOT,HONOLULU,HI 96822. BOWLING GREEN STATE UNIV,DEPT BIOL,BOWLING GREEN,OH 43402. INDIANA UNIV,DEPT BIOL,BLOOMINGTON,IN 47405. IOWA STATE UNIV SCI & TECHNOL,DEPT BOT,AMES,IA 50011. RI Jansen, Robert/F-6272-2011; Palmer, Jeffrey/P-6747-2014 OI Palmer, Jeffrey/0000-0002-4626-2220 NR 42 TC 34 Z9 38 U1 3 U2 24 PU NORDIC JOURNAL OF BOTANY PI COPENHAGEN K PA THE SECRETARY BOTANICAL MUSEUM GOTHERSGADE 130, DK-1123 COPENHAGEN K, DENMARK SN 0107-055X J9 NORD J BOT JI Nord. J. Bot. PY 1992 VL 12 IS 2 BP 141 EP 148 DI 10.1111/j.1756-1051.1992.tb01281.x PG 8 WC Plant Sciences SC Plant Sciences GA JE046 UT WOS:A1992JE04600001 ER PT J AU WOLDA, H AF WOLDA, H TI TRENDS IN ABUNDANCE OF TROPICAL FOREST INSECTS SO OECOLOGIA LA English DT Article DE POPULATION FLUCTUATIONS; TRENDS; FOREST INSECTS; NEOTROPICS; PANAMA ID FLUCTUATIONS; PATTERNS; COMMUNITIES; DIVERSITY; DYNAMICS; SUMATRA; INDEXES; BEETLE; SIZE AB The stability of a large variety of insect populations was studied using 14 years of light-trap data collected in a relatively undisturbed tropical forest in Panama. Special emphasis was placed on trends in abundance over time. A large between-species variation was found in stability, ranging from nearly constant to violently fluctuating. Over a 14-year period 22% of the species with more than 26 individuals caught showed an average trend of more than 10% of their mean abundance per year, and 4% a trend of more than 20% per year. Even among the 78 species represented by more than 1000 individuals, 7 species, 9%, showed a trend of more than 10% of mean abundance per year. These results appear to be incompatible with the generally held tenet that natural populations in undisturbed environments fluctuate within rather narrow abundance limits, and may indicate that at least a certain proportion of natural populations are not kept within such limits by regulatory processes. Actual fluctuating patterns vary a great deal between species, suggesting the absence of some dominant environmental process affecting several species at the same time. The total number of species and individuals, and the associated value of the alpha-diversity index remained at the same level over the 14 years. RP SMITHSONIAN TROP RES INST, BALBOA, PANAMA. NR 32 TC 77 Z9 79 U1 0 U2 15 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 JAN PY 1992 VL 89 IS 1 BP 47 EP 52 DI 10.1007/BF00319014 PG 6 WC Ecology SC Environmental Sciences & Ecology GA HA234 UT WOS:A1992HA23400007 PM 28313394 ER PT J AU FORMAN, P AF FORMAN, P TI INVENTING THE MASER IN POSTWAR AMERICA SO OSIRIS LA English DT Article RP FORMAN, P (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,DIV ELECT & MODERN PHYS,WASHINGTON,DC 20560, USA. NR 132 TC 13 Z9 15 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0369-7827 J9 OSIRIS JI Osiris PY 1992 VL 7 BP 105 EP 134 DI 10.1086/368707 PG 30 WC History & Philosophy Of Science SC History & Philosophy of Science GA KD402 UT WOS:A1992KD40200006 ER PT J AU ZDERO, C BOHLMANN, F KING, RM AF ZDERO, C BOHLMANN, F KING, RM TI SECO-LABDANES FROM TAMAULIPA-AZUREA AND CONSTITUENTS FROM OTHER EUPATORIEAE SO PHYTOCHEMISTRY LA English DT Article DE TAMAULIPA-AZUREA; BISHOPIELLA-ELEGANS; CAMPULUCLINIUM-MEGACEPHALUM; ASANTHUS-SOLIDAGINIFOLIUS; CRONQUISTIANTHUS-TRIANAE; COMPOSITAE; EUPATORIEAE; DITERPENES; SECO-LABDANES; SESQUITERPENE LACTONES ID OCCURRING TERPENE DERIVATIVES; SESQUITERPENE LACTONES AB Tamaulipa azurea gave two new seco-labdanes. Bishopiella elegans gave a known nerolidol derivative and a guaianolide. Campuluclinium megacephalum gave a tremetone derivative while Asanthus solidaginifolius afforded, in addition to polyalthic acid, two known germacranolides and large amounts of a cyclopropanogermacranolide, so far only isolated in trace amounts from a Cronquistia species. Cronquistianthus trianae also afforded germacranolides. C1 SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560. RP ZDERO, C (reprint author), TECH UNIV BERLIN,INST ORGAN CHEM,W-1000 BERLIN 12,GERMANY. NR 15 TC 3 Z9 3 U1 1 U2 3 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 JAN PY 1992 VL 31 IS 1 BP 155 EP 157 DI 10.1016/0031-9422(91)83025-G PG 3 WC Biochemistry & Molecular Biology; Plant Sciences SC Biochemistry & Molecular Biology; Plant Sciences GA GZ495 UT WOS:A1992GZ49500024 ER PT J AU GANZER, U JAKUPOVIC, J BOHLMANN, F KING, RM AF GANZER, U JAKUPOVIC, J BOHLMANN, F KING, RM TI A HIGHLY OXYGENATED GERMACRANE FROM ASPILIA-EENII AND CONSTITUENTS FROM OTHER ASPILIA SPECIES SO PHYTOCHEMISTRY LA English DT Article DE ASPILIA SP; COMPOSITAE; KAURANE DERIVATIVES; GERMACRANE DERIVATIVE ID OCCURRING TERPENE DERIVATIVES; EREMOPHILANE-DERIVATIVES; SESQUITERPENE LACTONES; SENECIO; STEIRACTINOLIDES; WEDELIA AB Investigation of 11 Aspilia species afforded several known kaurane derivatives and other diterpenes. From A. eenii a highly oxygenated germacrane bisepoxide was isolated. Comparison of the H-1 NMR data with those of several germacrane derivatives from Senecio and Ligularia species, spin decoupling and NOED led to corrections of the structures of several compounds. C1 SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560. RP GANZER, U (reprint author), TECH UNIV BERLIN,INST ORGAN CHEM,W-1000 BERLIN 12,GERMANY. NR 15 TC 12 Z9 13 U1 1 U2 3 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 JAN PY 1992 VL 31 IS 1 BP 209 EP 212 DI 10.1016/0031-9422(91)83037-L PG 4 WC Biochemistry & Molecular Biology; Plant Sciences SC Biochemistry & Molecular Biology; Plant Sciences GA GZ495 UT WOS:A1992GZ49500036 ER PT J AU ZDERO, C BOHLMANN, F KING, RM AF ZDERO, C BOHLMANN, F KING, RM TI CLERODANE DERIVATIVES FROM DIPLOSTEPHIUM SO PHYTOCHEMISTRY LA English DT Article DE DIPLOSTEPHIUM-FLORIBUNDUM, D-ERICOIDES; COMPOSITAE; DITERPENES; CLERODANE DERIVATIVES ID DITERPENES; CONSTITUENTS; ACID AB The aerial parts of D. floribundum afforded, in addition to known compounds, 10 new clerodane derivatives while D. ericoides gave 2-beta-hydroxyhardwickiic acid and widespread compounds. The structures were elucidated by high field NMR spectroscopy. The chemotaxonomic aspects are discussed briefly. C1 SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560. RP ZDERO, C (reprint author), TECH UNIV BERLIN,INST ORGAN CHEM,W-1000 BERLIN 12,GERMANY. NR 15 TC 8 Z9 9 U1 0 U2 0 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 JAN PY 1992 VL 31 IS 1 BP 213 EP 216 DI 10.1016/0031-9422(91)83038-M PG 4 WC Biochemistry & Molecular Biology; Plant Sciences SC Biochemistry & Molecular Biology; Plant Sciences GA GZ495 UT WOS:A1992GZ49500037 ER PT J AU ZIMBELMAN, JR EDGETT, KS AF ZIMBELMAN, JR EDGETT, KS TI THE THARSIS-MONTES, MARS - COMPARISON OF VOLCANIC AND MODIFIED LANDFORMS SO PROCEEDINGS OF LUNAR AND PLANETARY SCIENCE LA English DT Article ID OLYMPUS-MONS AUREOLE; DEPOSITS; REGION AB The three Tharsis Montes shield volcanos, Arsia Mons, Pavonis Mons, and Ascraeus Mons, have broad similarities that have been recognized since the Mariner 9 reconnaissance in 1972. Upon closer examination the volcanos are seen to have significant differences that are due to individual volcanic histories. All three volcanos exhibit the following characteristics: gentle (<5-degrees) flank slopes, entrants in the northwestern and southeastern flanks that were the source for lavas extending away from each shield, summit caldera(s), and enigmatic lobe-shaped features extending over the plains to the west of each volcano. The three volcanos display different degrees of circumferential graben and trough development in the summit regions, complexity of preserved caldera collapse events, secondary summit-region volcanic construction, and erosion on the lower western flanks due to mass wasting and the processes that formed the large lobe-shaped features. All three lobe-shaped features start at elevations of 10 to 11 km and terminate at 6 km. The complex morphology of the lobe deposits appear to involve some form of catastrophic mass movement followed by effusive and perhaps pyroclastic volcanism. C1 ARIZONA STATE UNIV,DEPT GEOL,TEMPE,AZ 85287. RP ZIMBELMAN, JR (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,CTR EARTH & PLANETARY STUDIES,WASHINGTON,DC 20560, USA. NR 42 TC 32 Z9 32 U1 0 U2 2 PU LUNAR AND PLANETARY INST PI HOUSTON PA 3600 BAY AREA BLVD, HOUSTON, TX 77058 SN 0270-9511 J9 P LUNAR PLANET SCI PY 1992 VL 22 BP 31 EP 44 PG 14 WC Geosciences, Multidisciplinary SC Geology GA MG416 UT WOS:A1992MG41600003 ER PT S AU ZIMBELMAN, JR EDGETT, KS AF ZIMBELMAN, JR EDGETT, KS BE Ryder, G Sharpton, VL TI THE THARSIS-MONTES, MARS - COMPARISON OF VOLCANIC AND MODIFIED LANDFORMS SO PROCEEDINGS OF LUNAR AND PLANETARY SCIENCE, VOL 22 SE PROCEEDINGS OF LUNAR AND PLANETARY SCIENCE LA English DT Proceedings Paper CT 22ND ANNUAL LUNAR AND PLANETARY CONF CY MAR 18-22, 1991 CL HOUSTON, TX SP LUNAR & PLANETARY INST, NASA, JOHNSON SPACE CTR, AMER ASSOC PETR GEOLOGISTS, AMER GEOPHY UNION, AMER ASTRON SOC, DIV PLANETARY SCI, GEOL SOC AMER, INT UNION GEOL SCI, METEORIT SOC RP ZIMBELMAN, JR (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,CTR EARTH & PLANETARY STUDIES,WASHINGTON,DC 20560, USA. NR 0 TC 32 Z9 32 U1 0 U2 2 PU LUNAR & PLANETARY INST PI HOUSTON PA HOUSTON SN 0270-9511 BN 0-942862-06-6 J9 P LUNAR PLANET SCI PY 1992 VL 22 BP 31 EP 44 PG 14 WC Geosciences, Multidisciplinary SC Geology GA BZ04N UT WOS:A1992BZ04N00003 ER PT J AU MATHIS, WN AF MATHIS, WN TI THE 1ST SHORE FLY OF THE GENUS GLENANTHE-HALIDAY FROM THE AUSTRALASIAN REGION (DIPTERA, EPHYDRIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE GLENANTHE; AUSTRALASIAN REGION AB The first species of Glenanthe from the Australasian Region is described (G. ismayi type locality: Papua New Guinea. Central Province: Lea Lea). The genus is diagnosed, including characterization of the male terminalia. RP MATHIS, WN (reprint author), SMITHSONIAN INST,DEPT ENTOMOL,NHB 169,WASHINGTON,DC 20560, USA. NR 0 TC 3 Z9 3 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 JAN PY 1992 VL 94 IS 1 BP 78 EP 82 PG 5 WC Entomology SC Entomology GA HB422 UT WOS:A1992HB42200006 ER PT J AU KROMBEIN, KV AF KROMBEIN, KV TI HOST RELATIONSHIPS, ETHOLOGY AND SYSTEMATICS OF PSEUDOMETHOCA ASHMEAD (HYMENOPTERA, MULTILLIDAE, ANDRENIDAE, HALICTIDAE AND ANTHOPHORIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE PSEUDOMETHOCA; PARASITOID; COMMUNAL AND SOLITARY BEES; ANDRENIDAE; HALICTIDAE; ANTHOPHORIDAE AB Two new species of Pseudomethoca are described and figured, perditrix from Arizona and New Mexico, and bethae from Arizona, New Mexico, and the states of Jalisco and Puebla in Mexico; behavioral notes are included for each. Brief taxonomic notes and figures, and/or behavioral notes are given for eight other taxa of Pseudomethoca. Ps. perditrix parasitizes larvae of the communal andrenid bee, Perdita portalis Timberlake, in New Mexico. Ps. toumeyi (Fox) is a putative parasitoid of Pe. portalis in New Mexico. The Floridian Pe. graenicheri Timberlake may be a host of Ps. torrida Krombein. The eumenid wasp, Ancistrocerus lutonidus Bohart, is considered to be an improbable host of Ps. frigida. Ps. bethae was found in Arizona in a nest of the communal anthophorid bee, Exomalopsis solani Cockerell. Ps. mulaiki Mickel from Texas may have species of the anthophorid, Exomalopsis, and/or the halictid, Agapostemon, as hosts. Ps. propinqua (Cresson) may have as hosts the halictid, Nomia melanderi Cockerell, and the anthophorid, Melissodes pallidisignata Cockerell in Wyoming. Ps. sanbornii aeetis (Fox) has the halictid, Nomia nevadensis bakeri Cockerell, as a putative host in coastal South Carolina. Ps. donaeanae (Cockerell and Fox) has an unknown bee host in Arizona, based on collection of a female bearing numerous pollen grains around the mouthparts. A table is included of known or putative hosts of Pseudomethoca in America north of Mexico and the authorities for each association. RP KROMBEIN, KV (reprint author), SMITHSONIAN INST,DEPT ENTOMOL,NHB STOP 105,WASHINGTON,DC 20560, USA. NR 0 TC 4 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 JAN PY 1992 VL 94 IS 1 BP 91 EP 106 PG 16 WC Entomology SC Entomology GA HB422 UT WOS:A1992HB42200008 ER PT J AU EIROA, C TORRELLES, JM GOMEZ, JF SAKAMOTO, S HASEGAWA, T KAWABE, R HAYASHI, M CASALI, MM AF EIROA, C TORRELLES, JM GOMEZ, JF SAKAMOTO, S HASEGAWA, T KAWABE, R HAYASHI, M CASALI, MM TI MOLECULAR OUTFLOWS IN THE SERPENS CLOUD CORE - FIRS-1 AND SVS-4 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Note DE ISM INDIVIDUAL (SERPENS); ISM JETS AND OUTFLOWS; ISM MOLECULES; STARS PRE-MAIN SEQUENCE ID YOUNG STELLAR OBJECTS; HERBIG-HARO OBJECTS; CARBON-MONOXIDE; MAGNETIC-FIELD; STAR FORMATION; DRIVEN WINDS; FLOWS; REGION AB We report on CO(J=1-->0) high-velocity wing emission toward two young objects of the Serpens molecular cloud. FIRS 1 and SVS 4. These observations were carried out with the 45-m telescope of the Nobeyama Radio Observatory. Different kinds of CO wing profiles found toward these two regions suggest that the previously reported extended (greater-than-or-equal-to 6') molecular outflow in the region is the result of perturbations on the ambient molecular gas by local outflows associated with various young objects. C1 CSIC,INST ASTROFIS ANDALUCIA,E-18080 GRANADA,SPAIN. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV TOKYO,FAC SCI,DEPT ASTRON,BUNKYO KU,TOKYO 113,JAPAN. NOBEYAMA RADIO OBSERV,NAGANO 38413,JAPAN. JOINT ASTRON CTR,HILO,HI 96720. UNIV TOKYO,INST ASTRON,MITAKA,TOKYO 181,JAPAN. RP EIROA, C (reprint author), OBSERV ASTRON MADRID,IGN,ALFONSO XII 3,E-28014 MADRID,SPAIN. OI Torrelles, Jose Maria/0000-0002-6896-6085 NR 24 TC 8 Z9 8 U1 0 U2 0 PU ASTRONOMICAL SOC JAPAN PI TOKYO PA C/O NATIONAL ASTRONOM OBSERV MITAKA-SHI, TOKYO 181, JAPAN SN 0004-6264 J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PY 1992 VL 44 IS 2 BP 155 EP 158 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JA637 UT WOS:A1992JA63700012 ER PT J AU KAWABE, R SUZUKI, M HIRANO, N AKABANE, K BARSONY, M NAJITA, JR KAMEYA, O ISHIGURO, M AF KAWABE, R SUZUKI, M HIRANO, N AKABANE, K BARSONY, M NAJITA, JR KAMEYA, O ISHIGURO, M TI APERTURE SYNTHESIS CS OBSERVATIONS OF NGC-7538 IRS-1-3 - RING OF DENSE GAS AROUND IRS-1 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE INTERSTELLAR-MOLECULES; NEBULAE-H-II REGIONS; NEBULAE-INDIVIDUAL (NGC-7538); STARS-FORMATION ID H-II REGIONS; VLA OBSERVATIONS; FORMALDEHYDE MASER; MOLECULAR CLOUD; H2O MASERS; EMISSION; NGC-2071; OUTFLOW; FLOWS AB We have carried out aperture synthesis CS (J = 2-1) observations of the dense molecular gas around a young stellar object NGC 7538 IRS 1-3 with 6" resolution using the Nobeyama Millimeter Array (NMA). We have found that the dense molecular gas has a ring-like structure centered on an infrared source NGC 7538 IRS 1. The ring has a diameter of 20" (0.26 pc) and an H-2 mass of 230 M.. The velocity structure of CS (2-1) emission indicates the existence of an expanding motion of the ring (V(exp) approximately 1 km s-1/sini, where i is the inclination angle of the ring). These results suggest that the observed structure is a nearly face-on view of a protostellar disk of molecular gas with a central hole formed by wind from IRS 1. IRS 2 and IRS 3 are apparently on the ring. In addition to the structure, several clumps of dense gas have been found around the ring. These clumps have a typical size of 10" (0.13 pc) and a velocity dispersion of 1-2 km s-1; the H-2 Masses range from 20 to 60 M.. It is suggested that these clumps are gravitationally bound, and would be protostellar condensations. C1 TOHOKU UNIV,DEPT ASTRON,AOBA KU,SENDAI,MIYAGI 980,JAPAN. HITOTSUBASHI UNIV,ASTRON & GEOPHYS LAB,KUNITACHI,TOKYO 186,JAPAN. TOYAMA UNIV,DEPT PHYS,TOYAMA 930,JAPAN. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. MIZUSAWA ASTROGEODYNAM OBSERV,MIZUSALIA,IWATE 023,JAPAN. RP KAWABE, R (reprint author), NOBEYAMA RADIO OBSERV,MINAMIMAKI,NAGANO 38413,JAPAN. NR 37 TC 15 Z9 15 U1 0 U2 0 PU ASTRONOMICAL SOC JAPAN PI TOKYO PA C/O NATIONAL ASTRONOM OBSERV MITAKA-SHI, TOKYO 181, JAPAN SN 0004-6264 J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PY 1992 VL 44 IS 4 BP 435 EP 446 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA JN670 UT WOS:A1992JN67000010 ER PT B AU KURUCZ, RL AF KURUCZ, RL BE BARBUY, B RENZINI, A TI MODEL ATMOSPHERES FOR POPULATION SYNTHESIS SO STELLAR POPULATIONS OF GALAXIES SE IAU SYMPOSIA LA English DT Proceedings Paper CT 149TH SYMP OF THE INTERNATIONAL ASTRONOMICAL UNION : THE STELLAR POPULATIONS OF GALAXIES CY AUG 05-09, 1991 CL ANGRA DOS REIS, BRAZIL SP INT ASTRON UNION, UNIV SAO PAULO, PROJETO BANCO INT DESENVOLVIMENTO, FUNDACAO AMPARO PESQUISA ESTADO SAO PAULO, FUNDACAO AMPARO PESQUISA ESTADO RIO GRANDE SUL, CONSELHO NACL DESENVOLVIMENTO CIENT & TECNOL, FINANCIADORA ESTUDOS & PROJETOS, UNIV SAO PAULO, INST ASTRON & GEOFIS, OBSERV NACL RP KURUCZ, RL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 0 TC 122 Z9 124 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA DORDRECHT BN 0-7923-1699-1 J9 IAU SYMP PY 1992 VL 149 BP 225 EP 232 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BW09B UT WOS:A1992BW09B00031 ER PT J AU KENSLEY, B AF KENSLEY, B TI NEW RECORDS OF INTERSTITIAL ANTHURIDEA INCLUDING CURASSANTHURA, FROM THE WESTERN ATLANTIC (CRUSTACEA, ISOPODA) SO STYGOLOGIA LA English DT Article DE INTERSTITIAL ISOPODA; ANTHURIDEA; CURASSANTHURA; WESTERN ATLANTIC AB The male and ovigerous female of Curassanthura halma are recorded for the first time, from Curacao. Curassanthura bermudensis is recorded for the second time, from Walsingham Cave, Bermuda. The fourth species of the genus, Curassanthura jamaicensis n. sp., is described from an anchialine sinkhole on Jamaica. RP KENSLEY, B (reprint author), SMITHSONIAN INST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. NR 0 TC 1 Z9 2 U1 0 U2 1 PU S P B ACADEMIC PUBLISHING BV PI LELYSTAD PA PLATINASTRAAT 33, 8211 AR LELYSTAD, NETHERLANDS SN 0169-3662 J9 STYGOLOGIA PY 1992 VL 7 IS 3 BP 187 EP 192 PG 6 WC Limnology; Marine & Freshwater Biology; Water Resources SC Marine & Freshwater Biology; Water Resources GA KA637 UT WOS:A1992KA63700006 ER PT J AU ROTHENBERG, M AF ROTHENBERG, M TI EYE ON THE SKY - LICK-OBSERVATORYS 1ST-CENTURY - OSTERBROCK,DE SO TECHNOLOGY AND CULTURE LA English DT Book Review RP ROTHENBERG, M (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 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JAN PY 1992 VL 33 IS 1 BP 169 EP 169 DI 10.2307/3105829 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA HN102 UT WOS:A1992HN10200024 ER PT J AU KIDWELL, PA AF KIDWELL, PA TI VONNEUMANN,JOHN AND THE ORIGINS OF MODERN COMPUTING - ASPRAY,W SO TECHNOLOGY AND CULTURE LA English DT Book Review RP KIDWELL, PA (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,MATH SECT,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 JAN PY 1992 VL 33 IS 1 BP 174 EP 175 DI 10.2307/3105832 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA HN102 UT WOS:A1992HN10200028 ER PT J AU WILDT, DE MONFORT, SL DONOGHUE, AM JOHNSTON, LA HOWARD, J AF WILDT, DE MONFORT, SL DONOGHUE, AM JOHNSTON, LA HOWARD, J TI EMBRYOGENESIS IN CONSERVATION BIOLOGY - OR, HOW TO MAKE AN ENDANGERED SPECIES EMBRYO SO THERIOGENOLOGY LA English DT Article; Proceedings Paper CT 1992 ANNUAL CONF OF THE INTERNATIONAL EMBRYO TRANSFER SOC CY JAN 12-14, 1992 CL DENVER, CO SP INT EMBRYO TRANSFER SOC DE CONSERVATION; EMBRYO; ARTIFICIAL INSEMINATION; EMBRYO TRANSFER; INVITRO FERTILIZATION ID DEER DAMA-DAMA; CAT FOLLICULAR OOCYTES; PUMA FELIS-CONCOLOR; DOMESTIC CAT; FALLOW DEER; ARTIFICIAL-INSEMINATION; FERTILIZATION INVITRO; CHEETAH; PREGNANCY; LEOPARD AB Embryo technologies have not as yet contributed to practical conservation of rare wildlife species. Production of young following artificial insemination (AI), embryo transfer (ET) or in vitro fertilization (IVF) has been sporadic, and it is now clear that biological differences among species limit our abilities to adapt these techniques easily to rare species. Nonetheless, there is encouraging progress at two levels. First, there is more acceptance that rare wildlife species safely tolerate the manipulations necessary to collect basic reproductive information or to test artificial breeding. This has increased access to rare animal populations and helped develop organized captive breeding programs, many of which emphasize the need for more research. Secondly, a gradually developing database about how these species reproduce is driving more systematic experimentation and artificial breeding attempts. Studies in our laboratory focus on producing embryos in vivo or in vitro. When essential information is available on fundamental reproductive processes, and, especially when comparative data are available from a domesticated animal model, then AI techniques are adapted to the endangered species. When few data are available, then studies emphasize using IVF (often in combination with in vitro oocyte maturation) to examine the factors regulating embryo formation and viability. These strategies are illustrated by recent progress involving (i) AI of select species of cervids, felids and inustelids, (ii) oocyte maturation in felids and (iii) IVF and ET in felids. Offspring have been produced, but perhaps more important are the answers to fundamental and mechanistic questions about why some wildlife species thrive and others do not. If reality-based conservation is defined as a continual data-gathering process that assimilates any and all information ultimately useful for preserving species, than embryo technologies are making considerable contributions to conservation biology. RP WILDT, DE (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 52 TC 84 Z9 87 U1 2 U2 18 PU BUTTERWORTH-HEINEMANN PI WOBURN PA 225 WILDWOOD AVE #UNITB PO BOX 4500, WOBURN, MA 01801-2084 SN 0093-691X J9 THERIOGENOLOGY JI Theriogenology PD JAN PY 1992 VL 37 IS 1 BP 161 EP 184 DI 10.1016/0093-691X(92)90253-N PG 24 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA GX284 UT WOS:A1992GX28400012 ER PT B AU WEEKES, TC AF WEEKES, TC BE Fleury, P Vacanti, G TI QUO-VADIS SO TOWARDS A MAJOR ATMOSPHERIC CERENKOV DETECTOR FOR TEV ASTRO/PARTICLE PHYSICS LA English DT Proceedings Paper CT 1st Palaiseau Workshop - Towards a Major Atmospheric Cerenkov Detector for TeV Astro/particle Physics CY JUN 11-12, 1992 CL PALAISEAU, FRANCE C1 HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,CAMBRIDGE,MA 02138. NR 0 TC 0 Z9 0 U1 0 U2 0 PU EDITIONS FRONTIERES PI DREUX PA 7 AVENUE KENNEDY, 28100 DREUX, FRANCE BN 2-86332-126-9 PY 1992 BP 323 EP 329 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BB74V UT WOS:A1992BB74V00028 ER PT J AU CORRELL, DL JORDAN, TE WELLER, DE AF CORRELL, DL JORDAN, TE WELLER, DE TI CROSS MEDIA INPUTS TO EASTERN UNITED-STATES WATERSHEDS AND THEIR SIGNIFICANCE TO ESTUARINE WATER-QUALITY SO WATER SCIENCE AND TECHNOLOGY LA English DT Review DE WATER QUALITY; LAND USE; ATMOSPHERIC DEPOSITION; RIPARIAN FOREST; NUTRIENTS; DIFFUSE SOURCES; SEDIMENTS; TOXICS; GROUND WATER; STORM WATER ID RHODE RIVER ESTUARY; CHESAPEAKE BAY; DEPOSITION; NITROGEN; NUTRIENT; GROUNDWATER; ATRAZINE; DYNAMICS; PATTERNS; RUNOFF AB Extensive research on Chesapeake Bay estuary, its drainage basin, and its airshed have now demonstrated that atmospheric deposition and diffuse land discharges are the largest sources for many parameters affecting estuarine water quality. For example, phosphorus and sediments are transported to the Bay largely in overland storm flows, nitrate largely in atmospheric deposition and in ground water, many pesticides and other toxic materials in surface waters and atmospheric deposition, and silicate primarily in ground water. Concerns over point sources such as sewage treatment outfalls and industrial outfalls have led to greatly improved treatment methods, alleviating the relative magnitude of these sources. The realization of the magnitude and importance of diffuse sources has led to research on improved land use practices, including better patterns of land use in the Chesapeake Bay landscape. One example is the use of and improved management of forested riparian buffer zones in the coastal plain part of the drainage basin. RP CORRELL, DL (reprint author), SMITHSONIAN ENVIRONM RES CTR,BOX 28,EDGEWATER,MD 21037, USA. NR 37 TC 4 Z9 4 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0273-1223 J9 WATER SCI TECHNOL JI Water Sci. Technol. PY 1992 VL 26 IS 12 BP 2675 EP 2683 PG 9 WC Engineering, Environmental; Environmental Sciences; Water Resources SC Engineering; Environmental Sciences & Ecology; Water Resources GA KJ403 UT WOS:A1992KJ40300004 ER PT J AU CARLSTEAD, K BROWN, JL MONFORT, SL KILLENS, R WILDT, DE AF CARLSTEAD, K BROWN, JL MONFORT, SL KILLENS, R WILDT, DE TI URINARY MONITORING OF ADRENAL RESPONSES TO PSYCHOLOGICAL STRESSORS IN DOMESTIC AND NONDOMESTIC FELIDS SO ZOO BIOLOGY LA English DT Article DE PSYCHOGENIC STRESS; ACTH; CORTISOL; GLUCOCORTICOIDS; STRESS AB The potential of assessing adrenal responses to psychological stressors through the radioimmunoassay of free cortisol in urine was examined in the domestic cat (Felis catus) and in three nondomestic felid species (Felis geoffroyi, Felis bengalensis, and Felis concolor). To determine the approximate clearance rate of an acute increase in glucocorticoid secretion, serial plasma and bladder urine samples were collected from eight domestic cats after a 0.125 mg adrenocorticotropic hormone (ACTH) challenge. Within 30 min of administration, mean serum cortisol concentrations increased tenfold. Urinary cortisol concentrations increased twofold by 2 hr post-ACTH and were correlated with the serum responses. Also, 16 domestic cats were anesthetized, injected with 0.125 mg ACTH, and serially bled for 3 hr. All urine was collected for 24 hr post-ACTH. Urinary cortisol concentrations were significantly elevated compared to pretreatment concentrations and were correlated to the serum cortisol response (net area under the response curve). In another experiment, urine was collected daily for a 7-day baseline period from 16 domestic cats housed in standard laboratory cages. Subsequently, 8 cats were subjected to 8 consecutive days of "stress," consisting of relocation, physical restraint, and jugular venipuncture. The other 8 cats were neither moved, nor handled, nor bled for the same period of time. Two patterns of response were observed among the "stressed" cats: urinary cortisol concentrations either increased or decreased between baseline and treatment periods. These response profiles differed from those of controls, which remained basal and unchanged over time. A fourth experiment involved relocating a female Geoffroy's cat, 4 leopard cats, and 2 pumas to a novel environment for 8-10 days. Urinary cortisol concentrations rose on the first day of relocation and remained RP CARLSTEAD, K (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 0 TC 68 Z9 68 U1 1 U2 10 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 1992 VL 11 IS 3 BP 165 EP 176 DI 10.1002/zoo.1430110305 PG 12 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA JN395 UT WOS:A1992JN39500004 ER PT J AU KLEIMAN, DG AF KLEIMAN, DG TI BEHAVIOR RESEARCH IN ZOOS - PAST, PRESENT, AND FUTURE SO ZOO BIOLOGY LA English DT Editorial Material DE ETHOLOGY; CONSERVATION; ANIMAL WELFARE; DATA COLLECTION AB This paper reviews the historical emphases in zoo behavioral research and the contribution of these studies to animal management and to advancement in the behavioral sciences. Some examples are provided from research conducted at the National Zoological Park and elsewhere. The potential for doing behavior studies of excellence in zoos and aquariums has become more complicated in recent years by 1) changes in the aims and objectives of modern zoological parks, especially the increasing emphasis on conservation, 2) changes in focus in the science of animal behavior itself, and 3) the tendency of trained behaviorists to assume positions as curators and directors without time for research. These issues represent challenges to be overcome so that zoos can continue to be important sites for the study of animal behavior and contribute to the science of animal management and conservation, as well as the advancement of theory in biology. RP KLEIMAN, DG (reprint author), SMITHSONIAN INST,NATL ZOOL,DEPT ZOOL RES,WASHINGTON,DC 20008, USA. NR 0 TC 23 Z9 24 U1 5 U2 24 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 1992 VL 11 IS 5 BP 301 EP 312 DI 10.1002/zoo.1430110502 PG 12 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA JV793 UT WOS:A1992JV79300001 ER PT J AU WEEKES, TC AF WEEKES, TC TI VERY-HIGH-ENERGY GAMMA-RAY ASTRONOMY - OVERVIEW AND PROSPECTS SO ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article ID MOLECULAR CLOUDS RP WEEKES, TC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, WHIPPLE OBSERV, POB 97, AMADO, AZ 85645 USA. NR 22 TC 0 Z9 0 U1 0 U2 0 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 E 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PD DEC 28 PY 1991 VL 647 BP 326 EP 333 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA JQ044 UT WOS:A1991JQ04400027 ER PT J AU MCCLINTOCK, J AF MCCLINTOCK, J TI BLACK-HOLES IN THE GALAXY SO ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRUM; CYGNUS X-1; LMC X-3; BINARY A0620-00; NEUTRON STARS; HDE 226868; DISCOVERY; SPECTROSCOPY; EMISSION RP MCCLINTOCK, J (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NR 47 TC 0 Z9 0 U1 0 U2 0 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 E 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PD DEC 28 PY 1991 VL 647 BP 495 EP 502 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA JQ044 UT WOS:A1991JQ04400047 ER PT J AU GOLDWIRTH, DS ZAGLAUER, HW AF GOLDWIRTH, DS ZAGLAUER, HW TI IS THERE A BIG-BUBBLE PROBLEM IN EXTENDED INFLATION SO PHYSICAL REVIEW LETTERS LA English DT Article ID VACUUM DECAY; UNIVERSE AB We present a generalization of the thin-wall formalism to calculate the evolution of true-vacuum bubbles in "extended" inflation. For inflaton quartic couplings of the order M/M(PI), gravity will lead to the recollapse of bubbles during most of the extended-inflation period thereby altering the bubble size distribution. The completion of the phase transition will proceed through tiny bubbles satisfying homogeneity constraints of the microwave background for arbitrary values of omega. Thus, it is possible to construct models that agree with experiments even for the original version of extended inflation. RP GOLDWIRTH, DS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 17 TC 17 Z9 17 U1 0 U2 0 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 23 PY 1991 VL 67 IS 26 BP 3639 EP 3642 DI 10.1103/PhysRevLett.67.3639 PG 4 WC Physics, Multidisciplinary SC Physics GA GW006 UT WOS:A1991GW00600002 ER PT J AU MOULD, JR STAVELEYSMITH, L SCHOMMER, RA BOTHUN, GD HALL, PJ HAN, MS HUCHRA, JP ROTH, J WALSH, W WRIGHT, AE AF MOULD, JR STAVELEYSMITH, L SCHOMMER, RA BOTHUN, GD HALL, PJ HAN, MS HUCHRA, JP ROTH, J WALSH, W WRIGHT, AE TI THE VELOCITY-FIELD OF CLUSTERS OF GALAXIES WITHIN 100 MEGAPARSECS .1. SOUTHERN CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY; GALAXIES, CLUSTERING; GALAXIES, REDSHIFTS; RADIO SOURCES, 21 CM RADIATION ID TULLY-FISHER RELATION; NEUTRAL HYDROGEN OBSERVATIONS; HYDRA-CENTAURUS SUPERCLUSTER; DISTANCE SCALE; WIDTH RELATION; LOCAL GROUP; PECULIAR VELOCITY; GREAT ATTRACTOR; MALMQUIST BIAS; IRAS GALAXIES AB Distances from the Tully-Fisher relation have been measured with the Parkes radio telescope for eight additional southern clusters of galaxies in the redshift range 2500-5000 km s-1. Most of them have large (average 1000 km s-1) positive peculiar velocities in a comoving frame in which the microwave background radiation shows no dipole anisotropy. In five out of eight cases these measurements have a significance at or above the 2 sigma-level. Outflow is seen on both sides of the Galactic plane. The source of this large-scale flow, if gravitational in origin, lies at or beyond the limit of our sample. C1 AUSTRALIA TELESCOPE NATL FACIL,EPPING,NSW 2121,AUSTRALIA. CERRO TOLOLO INTERAMER OBSERV,LA SERENA,CHILE. UNIV OREGON,EUGENE,OR 97403. PAUL WILD OBSERV,NARRABRI,NSW 2390,AUSTRALIA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CARNEGIE INST WASHINGTON,LAS CAMPANAS OBSERV,WASHINGTON,DC 20005. UNIV SYDNEY,DEPT ASTROPHYS,SYDNEY,NSW 2006,AUSTRALIA. PARKES OBSERV,PARKES,NSW 2870,AUSTRALIA. RP MOULD, JR (reprint author), CALTECH,PALOMAR OBSERV,105-24,PASADENA,CA 91125, USA. RI Staveley-Smith, Lister/A-1683-2011 OI Staveley-Smith, Lister/0000-0002-8057-0294 NR 66 TC 92 Z9 92 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 20 PY 1991 VL 383 IS 2 BP 467 EP 486 DI 10.1086/170806 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GW194 UT WOS:A1991GW19400001 ER PT J AU ROGERS, RD AF ROGERS, RD TI RELATIVISTIC ENHANCEMENT OF THE COMPTON-REFLECTED COMPONENT IN ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMIC BACKGROUND RADIATION; GALAXIES, NUCLEI; X-RAYS, SOURCES ID COLD MATTER AB Compton reflection may be an important process in active galactic nuclei (AGNs), since it provides an improvement over power-law fits to AGN spectra observed by Ginga and can also explain the spectrum of the cosmic X-ray background. In this paper we calculate the fraction of the total X-ray luminosity which is incident upon a thin steady alpha-disk if the X-rays are produced by inverse-Compton scattering of soft, disk photons off relativistic electrons located above the disk. We call this fraction the Compton reflection covering factor, f, and find that it can range between 0.5 and 0.88. This large range in f, due to a relativistic kinematic effect first calculated in this connection by Ghisellini et al. is sufficient to explain the typical covering (almost-equal-to 0.5) observed in bright AGNs by Ginga as well as the large covering factor (almost-equal-to 0.9) required to explain the cosmic X-ray background in the Compton reflection model. RP ROGERS, RD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MS 10,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 12 TC 11 Z9 11 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 20 PY 1991 VL 383 IS 2 BP 550 EP 553 DI 10.1086/170812 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GW194 UT WOS:A1991GW19400007 ER PT J AU KETO, ER LATTANZIO, JC MONAGHAN, JJ AF KETO, ER LATTANZIO, JC MONAGHAN, JJ TI GRAVITATIONAL FRAGMENTATION - A COMPARISON WITH W49A SO ASTROPHYSICAL JOURNAL LA English DT Article DE HYDRODYNAMICS; INTERSTELLAR, MOLECULES; NEBULAE, H-II REGIONS; NEBULAE, INDIVIDUAL (W49); STARS, FORMATION ID COLLAPSE; CLOUDS AB We investigate the process of gravitational fragmentation of molecular clouds through a comparison of numerical and observational results. We calculate the expected millimeter wave molecular line emission from a model fragmenting cloud generated by a numerical hydrodynamic simulation and compare with observations of HCO+ from the star-forming region W49A. Our investigation suggests that the rotating ring of H II regions, the necklace in W49A, may have formed in the gravitational fragmentation of a flattened rotating molecular cloud. C1 UNIV ILLINOIS,ASTRON IMAGING LAB,URBANA,IL 61801. UNIV CALIF LAWRENCE LIVERMORE NATL LAB,INST GEOPHYS & PLANETARY PHYS,LIVERMORE,CA 94550. MONASH UNIV,DEPT MATH,CLAYTON,VIC 3168,AUSTRALIA. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. RP KETO, ER (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 19 TC 22 Z9 22 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 20 PY 1991 VL 383 IS 2 BP 639 EP 644 DI 10.1086/170821 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GW194 UT WOS:A1991GW19400016 ER PT J AU BALLY, J LANGER, WD LIU, WH AF BALLY, J LANGER, WD LIU, WH TI INFRARED DUST AND MILLIMETER-WAVE CARBON-MONOXIDE EMISSION IN THE ORION REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE INFRARED, SOURCES; INTERSTELLAR, GRAINS; INTERSTELLAR, MOLECULES; NEBULAE, INDIVIDUAL (ORION-A, ORION-B) ID MOLECULAR CLOUDS; INTERSTELLAR GRAINS; GAMMA-RAYS; GALAXY; GAS; BARNARD-5; OUTFLOWS; OBJECTS; MASS; LINE AB We analyze the far-infrared dust emission seen by the IRAS satellite in the Orion region as a function of the local radiation field intensity and compare the dust temperature and opacity with (CO)-C-12 and (CO)-C-13 emission. We interpret the infrared radiation in the framework of a single component large grain model and a multicomponent grain model consisting of subpopulations of grains with size-dependent temperatures. We find a strong dependence of the 100-mu-m optical depth derived using the large grain model on the average line-of-sight dust temperature and radiation field. In the hot environment surrounding high-luminosity sources and H II regions, all dust along the line-of-sight radiates at 100-mu-m, and the dust-to-gas ratio, based on the 100-mu-m opacity and I((CO)-C-13), appears to be in agreement with the standard value, about 1% by mass. However, in cold regions of the molecular cloud, which comprise over 90% of the projected area on the sky, only a few percent of the total dust is detectable by IRAS. The dust-to-gas ratio, based on the 100-mu-m intensity and the grain temperature derived from the 60-100-mu-m intensity ratio using a large grain model, is an order of magnitude or more below that found in the hot regions. The large grain model leads to an overestimate of the temperature of most of the dust in a cold cloud, which results in a severe underestimate of the total dust column density. We find a relationship between the inferred dust-to-gas ratio and the radiation field intensity responsible for heating the dust which can be used to estimate the gas column density from the dust opacity derived from the 60 and 100-mu-m IRAS fluxes. A multicomponent grain model is required to interpret 60 and 100-mu-m data when small warm grains make a major contribution to the 60-mu-m intensity. We attempted to use the 12-mu-m intensity as a measure of the contribution of small stochastically heated warm grains to the longer wavelength infrared flux. With this model the spatial structure of the resulting column density distribution is nonphysical; the column density increases toward the cloud exterior. This behavior may be due to errors in the zero point offset in the infrared intensity distributions, changes in small grain abundance, and variations in the radiation field intensity. The computed dust optical depth is extremely sensitive to small changes in grain temperature. Submillimeter wavelength observations directly sensitive to the large grain emission are required to study the dust column density in most molecular clouds. In cold regions, there is an inverse correlation between the peak (CO)-C-12 temperature and the dust temperature. We find that the dust opacity correlates better with peak (CO)-C-12 temperature than with I((CO)-C-13). These results may be explained by small stochastically heated grains dominating even the 100-mu-m flux in the irradiated surface layers of the cloud. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP BALLY, J (reprint author), AT&T BELL LABS,HOH L245,HOLMDEL KEYPORT RD,HOLMDEL,NJ 07733, USA. OI BALLY, JOHN/0000-0001-8135-6612 NR 40 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 DEC 20 PY 1991 VL 383 IS 2 BP 645 EP & DI 10.1086/170822 PN 1 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GW194 UT WOS:A1991GW19400017 ER PT J AU KENYON, SJ HARTMANN, LW AF KENYON, SJ HARTMANN, LW TI THE DUSTY ENVELOPES OF FU ORIONIS VARIABLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE INTERSTELLAR, GRAINS; STARS, CIRCUMSTELLAR SHELLS; STARS, PRE-MAIN-SEQUENCE ID HERBIG-HARO OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; MAIN-SEQUENCE EVOLUTION; T-TAURI STARS; YOUNG STARS; INFRARED OBSERVATIONS; ACCRETION DISKS; V1057 CYGNI; MOLECULAR CLOUD; EXCITING STARS AB We discuss the spectral energy distributions of FU Orionis variables, using new ground-based infrared photometry and IRAS ADDSCAN measurements. Nearly half of the recognized FU Orionis variables are heavily extincted, so further analysis is difficult. Three (V1057 Cyg, V1515 Cyg, Z CMa) of the remaining five objects have much larger far-infrared fluxes than can be explained by the simple accretion disk models that match their spectral energy distributions for lambda < 10-mu-m. The 10-20-mu-m excess emission in V1057 Cyg has decreased proportionately with the decline in optical light, which demonstrates that the far-infrared flux arises in a dust shell reprocessing light from the central object. The amount of dust required to explain the far-infrared excess emission of V1057 Cyg is much larger than that implied by the optical extinction, so the dust distribution is not spherically symmetric. In principle, a geometrically flared disk can account for the far-infrared emission, but in practice the large solid angle the disk must subtend at the star appears difficult to achieve in a resonable physical model. We suggest instead that the far-infrared excesses arise in somewhat flattened dusty envelopes with a covering factor in solid angle of roughly 1/2, which is consistent with the fraction of FU Orionis variables that are heavily embedded. The dusty envelope in V1057 Cyg must have an inner radius of approximately 10 AU to explain the excess emission at 10-mu-m, and this envelope probably cannot be static so close to the central star. We propose that the dusty envelope falls onto the outer disk at a rate of approximately 5 x 10(-6) M. yr-1. This rate is sufficient to replenish disk material accreted during a FU Orionis outburst and allow repetitive eruptions on time scales of several thousand years. C1 INFRARED TELESCOPE FACIL,HONOLULU,HI. KITT PEAK NATL OBSERV,TUCSON,AZ 85726. RP KENYON, SJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 91 TC 84 Z9 84 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 20 PY 1991 VL 383 IS 2 BP 664 EP 673 DI 10.1086/170823 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GW194 UT WOS:A1991GW19400018 ER PT J AU CALVET, N HARTMANN, L KENYON, SJ AF CALVET, N HARTMANN, L KENYON, SJ TI ON THE NEAR-INFRARED SPECTRUM OF FU ORIONIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE INFRARED, SPECTRA; SPECTROPHOTOMETRY; STARS, ACCRETION; STARS, INDIVIDUAL (FU ORIONIS) ID T-TAURI STARS; V1057 CYGNI; ACCRETION; ROTATION; SYSTEMS; DISKS AB We have calculated the near-infrared spectrum of a steady accretion-disk model intended to represent the pre-main-sequence object FU Ori. The theoretical models quantitatively match the strong water vapor absorption of FU Ori observed between approximately 1.4 and 2.4-mu-m. The first-overtone 2.3-mu-m CO absorption lines found in FU Ori are also reproduced fairly well by the model calculations. The rotational broadening of the model CO lines, scaled to the observed rotational broadening at optical wavelengths, is in slightly better agreement with observations than in previous simple models. The models predict additional molecular features, which should be observed to provide further tests of the theory. Our calculations further demonstrate that steady accretion-disk models can provide quantitative explanations of the spectrum of FU Ori. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP CALVET, N (reprint author), CTR INVEST ASTRON,AP POSTAL 264,MERIDA 5101A,VENEZUELA. OI Kenyon, Scott/0000-0003-0214-609X NR 21 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 DEC 20 PY 1991 VL 383 IS 2 BP 752 EP 756 DI 10.1086/170832 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GW194 UT WOS:A1991GW19400027 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 SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID TRANSITION MOMENTS; IONS; DISSOCIATION; IONIZATION; STATES AB Configuration interaction wave functions and potential energy curves have been calculated for the four lowest states of 2-PI and 2-SIGMA + symmetry and the lowest state of 4-SIGMA-, 2-SIGMA-, 2-DELTA, and 4-PI symmetry for the molecular ion HCl+. Dipole moment functions of the X-2-PI and A 2-SIGMA+ states are presented as well as dipole moments for transitions from the X state to dipole-allowed excited states. The electronic wave functions were constructed to give a balanced description of Rydberg-valence interactions. The computed radiative lifetime of the X 2-PI(upsilon = 1) is found to be in good agreement with previous theoretical and experimental values. Oscillator strengths, transition probabilities, and radiative lifetimes are calculated for the A 2-SIGMA+ -X 2-CHI transition for vibrational levels upsilon' less-than-or-equal-to 6 and compared to previous theoretical and experimental results. Vibrational levels upsilon' greater-than-or-equal-to 7 of the A 2-SIGMA+ state are predissociated by the 4-PI, 4-SIGMA-, and 2-SIGMA- states. Theoretical photodissociation cross sections are calculated showing that photodissociation occurs primarily through absorption into the (3) 2-PI and (3) 2-SIGMA+ states in the wavelength region lambda < 100 nm and also the 2-SIGMA-, 2-DELTA, and (2) 2-PI states for wavelengths lambda > 100 nm. C1 MIT,DEPT PHYS,CAMBRIDGE,MA 02139. RP PRADHAN, AD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 18 TC 69 Z9 71 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 DEC 15 PY 1991 VL 95 IS 12 BP 9009 EP 9023 DI 10.1063/1.461232 PG 15 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA GV825 UT WOS:A1991GV82500030 ER PT J AU KAIS, S MORGAN, JD HERSCHBACH, DR AF KAIS, S MORGAN, JD HERSCHBACH, DR TI ELECTRONIC TUNNELING AND EXCHANGE ENERGY IN THE D-DIMENSIONAL HYDROGEN-MOLECULE ION SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID COUPLED ANHARMONIC OSCILLATORS; CLASSICAL PATH APPROXIMATION; BOLTZMANN DENSITY MATRIX; SYMMETRY-BREAKING; 2-ELECTRON ATOMS; FALSE VACUUM; H+H2; COLLISIONS; EXPANSIONS; SYSTEM AB Dimensional scaling generates an effective potential for the electronic structure of atoms and molecules, but this potential may acquire multiple minima for certain ranges of nuclear charges or geometries that produce symmetry breaking. Tunneling among such minima is akin to resonance among valence bond structures. Here we treat the D-dimensional H-2+ molecule ion as a prototype test case. In spheroidal coordinates it offers a separable double-minimum potential and tunneling occurs in only one coordinate; in cylindrical coordinates the potential is nonseparable and tunneling occurs in two coordinates. We determine for both cases the ground state energy splitting DELTA-E(D) as a function of the internuclear distance R. By virtue of exact interdimensional degeneracies, this yields the exchange energy for all pairs of g, u states of the D = 3 molecule that stem from separated atom states with m = l = n - 1, for n = 1 --> infinity. We evaluate DELTA-E(D) by two semiclassical techniques, the asymptotic and instanton methods, and obtain good agreement with exact numerical calculations over a wide range of R. We find that for cylindrical coordinates the instanton path for the tunneling trajectory differs substantially from either a straightline or adiabatic path, but is nearly parabolic. Path integral techniques provide relatively simple means to determine the exact instanton path and contributions from fluctuations around it. Generalizing this approach to treat multielectron tunneling in several degrees of freedom will be feasible if the fluctuation calculations can be made tractable. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. RP KAIS, S (reprint author), HARVARD UNIV,DEPT CHEM,CAMBRIDGE,MA 02138, USA. OI Kais, Sabre/0000-0003-0574-5346 NR 59 TC 28 Z9 28 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 DEC 15 PY 1991 VL 95 IS 12 BP 9028 EP 9041 DI 10.1063/1.461182 PG 14 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA GV825 UT WOS:A1991GV82500032 ER PT J AU LIVIO, M SOKER, N MATSUDA, T ANZER, U AF LIVIO, M SOKER, N MATSUDA, T ANZER, U TI ON THE FLIP-FLOP INSTABILITY OF BONDI-HOYLE ACCRETION FLOWS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article ID INHOMOGENEOUS-MEDIUM; ANGULAR-MOMENTUM; STABILITY AB Using a highly simplified analytic treatment of the shock cone obtained in Bondi-Hoyle accretion flows past a compact object and the results of stability analyses of the accretion line, we demonstrate that the 'flip-flop' instability discovered recently in numerical calculations, in which the wake oscillates from side to side, has a relatively simple physical interpretation. The results of our analysis are in agreement with those obtained in multidimensional numerical hydrodynamic calculations. C1 TECHNION ISRAEL INST TECHNOL,DEPT PHYS,IL-32000 HAIFA,ISRAEL. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. KYOTO UNIV,DEPT AERONAUT ENGN,KYOTO 606,JAPAN. MAX PLANCK INST ASTROPHYS,W-8046 GARCHING,GERMANY. RP LIVIO, M (reprint author), UNIV ILLINOIS,DEPT ASTRON,URBANA,IL 61801, USA. NR 20 TC 33 Z9 33 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 DEC 15 PY 1991 VL 253 IS 4 BP 633 EP 636 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GV327 UT WOS:A1991GV32700010 ER PT J AU STEWART, MM RAND, AS AF STEWART, MM RAND, AS TI VOCALIZATIONS AND THE DEFENSE OF RETREAT SITES BY MALE AND FEMALE FROGS, ELEUTHERODACTYLUS-COQUI SO COPEIA LA English DT Article ID GRADED AGGRESSIVE CALLS; PUERTO-RICAN FROG; TROPICAL FROG; ACOUSTIC COMMUNICATION; 2-NOTE CALL; TREEFROG; BEHAVIOR; LEPTODACTYLIDAE; TERRITORIALITY; COMPETITION AB Both female and male Eleutherodactylus coqui give aggressive calls while defending retreat sites. In 60 staged contests, 67% of residents responded aggressively when diurnal retreats were entered by a conspecific. Residents won 93% of the contests. Aggressive calls of males and females differ in length, spectral composition, and number and length of notes. Aggressive calls comprise a graded signaling system. In this high density, territorial species, aggressive calls may assist in spacing frogs during the day. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP STEWART, MM (reprint author), SUNY ALBANY,DEPT BIOL SCI,ALBANY,NY 12222, USA. NR 51 TC 47 Z9 49 U1 0 U2 3 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 DEC 13 PY 1991 IS 4 BP 1013 EP 1024 DI 10.2307/1446096 PG 12 WC Zoology SC Zoology GA GW221 UT WOS:A1991GW22100013 ER PT J AU FRANX, M ILLINGWORTH, G DEZEEUW, T AF FRANX, M ILLINGWORTH, G DEZEEUW, T TI THE ORDERED NATURE OF ELLIPTIC GALAXIES - IMPLICATIONS FOR THEIR INTRINSIC ANGULAR MOMENTA AND SHAPES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, FORMATION; GALAXIES, INTERNAL MOTIONS; GALAXIES, STRUCTURE; STARS, STELLAR DYNAMICS ID CCD SURFACE PHOTOMETRY; MINOR-AXIS ROTATION; COLD DARK MATTER; MODELS; DISKS; HALOS; KINEMATICS; DYNAMICS; TRIAXIALITY; GAS AB The observations of rotation along the major and minor axes of 38 elliptical galaxies are analyzed to determine their intrinsic structure. Rotation along the minor axis occurs (i) as a result of projection effects in triaxial systems and/or (ii) because of real misalignment of the angular momentum axis from the intrinsic short axis, as is allowed in triaxial systems. The intrinsic angular momentum can point anywhere in the plane containing the short and the long axis. The distribution of apparent misalignments is a function only of the triaxiality T of a galaxy and its intrinsic misalignment, and is independent of the flattening of the galaxy in the plane containing the long and the short axis. The observed misalignment of the rotation axes and the short axes ranges from 0-degrees to 90-degrees, with most ellipticals having misalignments that are small. This is not expected if ellipticals are generically triaxial systems with uniformly distributed angular momentum direction, and requires that particular constraints be imposed during the formation process. Some specific galaxies have dynamical subsystems with observed angular momenta that are offset 90-degrees from the angular momenta of the main part of the galaxy. These galaxies are probably rotating about their long axis in the outer parts. The analysis of the observed misalignments requires us to derive the intrinsic ellipticity distribution for ellipticals. The resulting distribution, based on CCD data, shows a pronounced lack of round galaxies, unlike that previously derived from catalogs. The distribution of triaxiality and intrinsic misalignment of the angular momentum cannot be derived uniquely, since one observable (apparent misalignment) is used to determine two internal parameters (triaxiality and intrinsic misalignment). Various assumptions regarding the intrinsic shapes and the direction of the angular momentum were used. An exploration of the solution space showed a wide range of valid distributions, ranging from models with only nearly oblate shapes, oblate and prolate shapes, to distributions with only triaxial shapes, with varying distributions of intrinsic misalignments. However, all the models have a sizable fraction of galaxies (greater-than-or-equal-to 35%) with intrinsic misalignments less than 15-degrees. The results were compared with predictions from several groups for hierarchical formation scenarios. The predicted distributions for halos are skewed significantly toward prolate-triaxial shapes. Our data show that the luminous parts of ellipticals do not have such high triaxialities. The shapes of the dark halos may well be different from the shapes of the luminous matter in ellipticals, despite their similar dynamics. This may result, for example, from the effect of gaseous dissipation. C1 UNIV CALIF SANTA CRUZ OBSERV,SANTA CRUZ,CA 95064. UNIV CALIF SANTA CRUZ,LICK OBSERV,MT HAMILTON,CA 95140. HUYGENS LAB,2300 RA LEIDEN,NETHERLANDS. CALTECH,PASADENA,CA 91125. RP FRANX, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 65 TC 238 Z9 238 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 DEC 10 PY 1991 VL 383 IS 1 BP 112 EP 134 DI 10.1086/170769 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GT975 UT WOS:A1991GT97500012 ER PT J AU GREENHOUSE, MA WOODWARD, CE THRONSON, HA PUETTER, RC AF GREENHOUSE, MA WOODWARD, CE THRONSON, HA PUETTER, RC TI NEAR-INFRARED [FE-II] EMISSION OF M82 SUPERNOVA-REMNANTS - IMPLICATIONS FOR TRACING THE SUPERNOVA CONTENT OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (M82, NGC 3034); GALAXIES, STELLAR CONTENT; INFRARED SPECTRA; SPECTROPHOTOMETRY ID MOLECULAR-HYDROGEN; LINE EMISSION; STARBURST GALAXIES; PHOTO-IONIZATION; STAR FORMATION; CORONAL LINES; NOVA REMNANT; CRAB-NEBULA; SPECTROSCOPY; SEYFERT AB We report near-infrared [Fe II] and Pa-beta spectra of two young supernova remnants and one H II region within the central 15 kpc of M82. Comparison of these spectra reveal a [Fe II]/Pa-beta ratio similar to that observed in Galactic supernova remnants and H II regions, and show that the [Fe II] background emission in M82 has local maxima at the position of the supernova remnants observed in the radio continuum. The new observations show that the enhanced infrared [Fe II] emission observed in Galactic supernova remnants occurs in remnants spanning a wide range of radio luminosities. These results, and a growing body of Galactic and extragalactic observations by others, suggest that the total [Fe II] luminosity of galaxies is uncontaminated by emission due to H II regions, their associated photodissociation regions, and other ionized regions which do not contain shock-processed grains or enriched supernova ejecta. The available data on infrared [Fe II] emission in galaxies suggests that (1) the iron depletion of the interstellar medium of galaxies is controlled by supernova activity independent of their nuclear classification; (2) the infrared [Fe II] luminosity of galaxies traces their relative supernova content; and (3) the [Fe II] 1.644-mu-m and uspilon = 1 --> 0 S(1) H-2 emission of galaxies are correlated, suggesting that the latter is also related to supernova activity. We conclude that infrared [Fe II] lines can provide a new relative measure of supernova activity in galaxies. Comparison of infrared [Fe II] and H II luminosities may be useful for determining the relative age of starbursts, and comparison of [Fe II] and H-2 luminosities may provide new insight into understanding the production of global H-2 emission in galaxies. C1 SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560. UNIV WYOMING,WYOMING INFRARED OBSERV,LARAMIE,WY 82071. AEROSPACE CORP,SPACE SCI LAB,LOS ANGELES,CA 90009. UNIV CALIF SAN DIEGO,CTR ASTROPHYS & SPACE SCI,LA JOLLA,CA 92093. RI Thronson, Harley/E-3382-2012 NR 72 TC 60 Z9 60 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 1991 VL 383 IS 1 BP 164 EP 173 DI 10.1086/170772 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GT975 UT WOS:A1991GT97500015 ER PT J AU RAYMOND, JC WALLERSTEIN, G BALICK, B AF RAYMOND, JC WALLERSTEIN, G BALICK, B TI EVIDENCE FOR A THERMALLY UNSTABLE SHOCK-WAVE IN THE VELA SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE NEBULAE, INDIVIDUAL (VELA SUPERNOVA REMNANT); NEBULAE, SUPERNOVA REMNANTS; SHOCK WAVES; STARS, INDIVIDUAL (HD-72088) ID INTER-STELLAR MEDIUM; CYGNUS LOOP; OPTICAL-EMISSION; RADIATIVE SHOCKS; ABSORPTION-LINES; EMITTING GAS; MODELS; UV; ABUNDANCES AB The emission- and absorption-line signatures of supernova remnant shock waves provide complementary diagnostic capabilities. This paper presents IUE spectra of the nebulosity and new spectra of HD 72088. We use models of the emission and absorption lines from shocked gas to derive a shock velocity and elemental depletions. There is evidence from the absorption-line strengths and widths for thermally unstable cooling behind a 150 km s-1 shock. We confirm the shock velocity and swept-up column density estimates of Wallerstein & Balick, and we find evidence for a nonthermal contribution to the pressure. C1 UNIV WASHINGTON,DEPT ASTRON FM-20,SEATTLE,WA 98195. RP RAYMOND, JC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 34 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 DEC 10 PY 1991 VL 383 IS 1 BP 226 EP 232 DI 10.1086/170778 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GT975 UT WOS:A1991GT97500021 ER PT J AU BECK, SC FISCHER, J SMITH, HA AF BECK, SC FISCHER, J SMITH, HA TI INFRARED RECOMBINATION LINES OF HYDROGEN FROM YOUNG OBJECTS IN THE SOUTHERN GALACTIC PLANE SO ASTROPHYSICAL JOURNAL LA English DT Article DE INFRARED, SOURCES; INFRARED SPECTRA; STARS, PRE-MAIN-SEQUENCE; STARS, WINDS ID HERBIG-HARO OBJECTS; RADIO-CONTINUUM EMISSION; STELLAR OBJECTS; MILKY-WAY; REGIONS; STARS AB We have observed near infrared recombination lines of hydrogen in twelve young objects in the southern Galactic plane. The sample includes Herbig-Haro objects and IRAS dark cloud point sources from the 1987 catalog of Persson and Campbell. In four of the IRAS sources we have measured two or three infrared lines, and their intensity ratios are consistent with models of optically thick ionized winds. The intrinsic line shapes, which we retrieve from maximum entropy deconvolutions, indicate gas velocities of 100 km s-1 or more as expected from ionized winds. These sources are apparently embedded pre-main-sequence objects with outflows. They include some of the brightest known YSOs. C1 TEL AVIV UNIV,RAYMOND & BEVERLY SACKLER FAC EXACT SCI,SCH PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL. TEL AVIV UNIV,WISE OBSERV,IL-69978 TEL AVIV,ISRAEL. USN,RES LAB,CTR ADV SPACE SENSING,WASHINGTON,DC 20375. RP BECK, SC (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,3726,WASHINGTON,DC 20560, USA. NR 32 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 10 PY 1991 VL 383 IS 1 BP 336 EP 343 DI 10.1086/170791 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GT975 UT WOS:A1991GT97500034 ER PT J AU LELLOUCH, E GOLDSTEIN, JJ BOUGHER, SW PAUBERT, G ROSENQVIST, J AF LELLOUCH, E GOLDSTEIN, JJ BOUGHER, SW PAUBERT, G ROSENQVIST, J TI 1ST ABSOLUTE WIND MEASUREMENTS IN THE MIDDLE ATMOSPHERE OF MARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE PLANETS, ATMOSPHERES; PLANETS, MARS; RADIO SOURCES, SPECTRA ID WAVE INDUCED DRAG; GRAVITY-WAVE; GENERAL-CIRCULATION; MESOSPHERE; DIFFUSION; BREAKING AB The first absolute wind measurements in the middle atmosphere of Mars (40-70 km) were obtained from Doppler shifts in the J = 2-1 CO transition at 230.538 GHz. During the 1988 opposition, this line was observed at 100 kHz resolution with the IRAM 30 m telescope. The 12" FWHM beam of the facility allowed spatial resolution of the Martian disk (23."8). The high S/N of the data allowed measurement of winds with a 1-sigma absolute line-of-sight accuracy of 20 m s-1. The measurements, performed during Southern summer solstice (L(s) = 279-degrees), stress the Southern hemisphere and clearly indicate a global easterlies flow. If modeled by a broad easterly jet with a maximum centered at 20 S, and extending 80-degrees in latitude, the jet core velocity is found to have a chi-2 minimum at 160 m s-1 (+/- 80 m s-1 at the 95% confidence level), generally consistent with predictions for broad summer easterly jets near 50 km as proposed by theoretical models. If the flow is modeled instead by a planet-wide solid rotator zonal flow which is restricted to the Southern hemisphere or equatorial regions, the velocity of the easterlies is nearly the same. These wind measurements, together with the temperature measurements of Deming et al., provide the first experimental rough picture of the middle atmosphere circulation of Mars, in general agreement with the Jaquin axisymmetric middle atmosphere model and the current Mars GCM model of Pollack et al. C1 SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560. INST RADIOASTRON MILLIMETR,GRANADA,SPAIN. UNIV ARIZONA,LUNAR & PLANETARY LAB,TUCSON,AZ 85721. RP LELLOUCH, E (reprint author), OBSERV PARIS,DEPT RECH SPATIALES,F-92195 MEUDON,FRANCE. RI Bougher, Stephen/C-1913-2013 OI Bougher, Stephen/0000-0002-4178-2729 NR 20 TC 27 Z9 27 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 1991 VL 383 IS 1 BP 401 EP 406 DI 10.1086/170797 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GT975 UT WOS:A1991GT97500040 ER PT J AU KOPER, E DAME, TM ISRAEL, FP THADDEUS, P AF KOPER, E DAME, TM ISRAEL, FP THADDEUS, P TI A COMPLETE CO SURVEY OF M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INTERSTELLAR MATTER; GALAXIES, LOCAL GROUP; INTERSTELLAR, MATTER; INTERSTELLAR, MOLECULES ID RADIO-CONTINUUM SURVEY; SPIRAL ARM; INFRARED-EMISSION; MOLECULAR CLOUDS; GALAXY; M-31; MHZ AB M31 was fully surveyed at an angular resolution of 8.'7 in the J = 1 --> 0 rotational transition of CO. The 153' x 45' area observed covers the entire galaxy to a radius of at least 16 kpc, well beyond the optical disk and Population I peak at 10 kpc. The bulk of the CO emission lies between 8 and 11 kpc from the galactic center. Compared with H I, the CO emission is more confined to optical Population I and tends to peak approximately 1 kpc closer to the center. Although previously few CO observations have been directed toward the NE tangent of the Population I ring, it appears as rich in molecular gas as the SW tangent. Little CO emission is found within 8 kpc of the center of M31. Using the Galactic value for the conversion of integrated CO intensity to H-2 mass, the total molecular mass of M31 is approximately 2.5 x 10(8) M., less than one-fourth the molecular mass of the Milky Way computed in the same way. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP KOPER, E (reprint author), LEIDEN OBSERV,POB 9513,2300 RA LEIDEN,NETHERLANDS. NR 34 TC 28 Z9 28 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 1991 VL 383 IS 1 BP L11 EP L14 DI 10.1086/186229 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GT976 UT WOS:A1991GT97600003 ER PT J AU TAMURA, Y KOYAMA, M FISKE, RS AF TAMURA, Y KOYAMA, M FISKE, RS TI PALEOMAGNETIC EVIDENCE FOR HOT PYROCLASTIC DEBRIS FLOW IN THE SHALLOW SUBMARINE SHIRAHAMA GROUP (UPPER MIOCENE-PLIOCENE), JAPAN SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID TEMPERATURES; DEPOSITS AB The cooling history of coarse andesite blocks erupted and deposited proximally in the shallow marine environment has been investigated by paleomagnetic studies and heat conductivity calculations. Six to 13 samples were cored and measured from six essential andesite blocks 1-5 m in diameter. Thermal demagnetization techniques were used to detect the directional change of remanence through demagnetization steps, each representing different blocking temperatures (T(b)). Each sample has three components of remanent magnetization (C1, C2, and C3). C1 is characterized by a T(b) of 250-degrees-C and an orientation coincident with the present geomagnetic field. C2 has a T(b) of 250-degrees-500-degrees-C and shows a consistent direction with reversed polarity. C3 has a T(b) of 500-degrees-600-degrees-C, and its orientation is nearly consistent from samples collected from nearby parts of the same clast and are random from samples from different clasts. On the basis of the remanence direction of each component, the differing T(b), and the petrography of the samples, C1 is interpreted as secondary viscous remanence, whereas C2 and C3 are the partial thermoremanent magnetizations obtained during and immediately after emplacement. C3 was probably acquired while the blocks were rolling or sliding downslope, and C2 formed during continued cooling of the blocks after they came to rest. Heat conductivity calculations suggest that the blocks were emplaced less than an hour after being erupted. If the eruptive vent was only 2-3 km distant, as suggested by field relations, a downslope transport rate of less than 36 km/h is implied. C1 SHIZUOKA UNIV,FAC EDUC,OYA,SHIZUOKA 422,JAPAN. SMITHSONIAN INST,WASHINGTON,DC 20560. RP TAMURA, Y (reprint author), UNIV TOKYO,DEPT EARTH & PLANETARY PHYS,BUNKYO KU,TOKYO 113,JAPAN. NR 14 TC 21 Z9 21 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD DEC 10 PY 1991 VL 96 IS B13 BP 21779 EP 21787 DI 10.1029/91JB02258 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA GW578 UT WOS:A1991GW57800021 ER PT J AU WATANABE, S KOMINE, H AF WATANABE, S KOMINE, H TI ADIABATIC-EXPANSION METHOD APPLIED TO DIAMAGNETIC RYDBERG ATOMS SO PHYSICAL REVIEW LETTERS LA English DT Article ID STRONG MAGNETIC-FIELD; HYDROGEN-ATOM AB We report on a successful implementation of the diabatic-by-sector method as applied to the computation of positive-energy diamagnetic Rydberg spectra of the alkali-metal atoms in a laboratory field (approximately 6 T). The method provides the quantum-defect parameters directly, and opens up the possibility of accounting for various spectral features quantum mechanically. C1 KANSAS STATE UNIV AGR & APPL SCI,MANHATTAN,KS 66506. HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. RP WATANABE, S (reprint author), UNIV ELECTROCOMMUN,DEPT APPL PHYS & CHEM,1-5-1 CHOFU GA OKA,CHOFU,TOKYO 182,JAPAN. NR 19 TC 35 Z9 36 U1 2 U2 4 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 2 PY 1991 VL 67 IS 23 BP 3227 EP 3230 DI 10.1103/PhysRevLett.67.3227 PG 4 WC Physics, Multidisciplinary SC Physics GA GT014 UT WOS:A1991GT01400007 ER PT J AU FLECKNER, JA AF FLECKNER, JA TI DEAR JANE,MARY - SOME REFLECTIONS ON BEING AN ARCHIVIST SO AMERICAN ARCHIVIST LA English DT Editorial Material RP FLECKNER, JA (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,ARCHIVAL PROGRAM,WASHINGTON,DC 20560, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 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 1991 VL 54 IS 1 BP 8 EP 13 PG 6 WC History; Information Science & Library Science SC History; Information Science & Library Science GA GP396 UT WOS:A1991GP39600005 ER PT J AU JOHNSTON, PF AF JOHNSTON, PF TI THE PERIPLUS-MARIS-ERYTHRAEI - CASSON,L SO AMERICAN NEPTUNE LA English DT Book Review RP JOHNSTON, PF (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU PEABODY MUSEUM PI SALEM PA E INDIA MARINE HALL, SALEM, MA 01970 SN 0003-0155 J9 AM NEPTUNE JI Am. Neptune PD WIN PY 1991 VL 51 IS 1 BP 54 EP 55 PG 2 WC History SC History GA FR978 UT WOS:A1991FR97800009 ER PT J AU GUNTER, AC AF GUNTER, AC TI THE ART OF PLAYING + ORIENTAL GAMES AND LEISURE - INTRODUCTION SO ASIAN ART LA English DT Editorial Material RP GUNTER, AC (reprint author), SMITHSONIAN INST,SACKLER GALLERY,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS UNITED KINGDOM PI OXFORD PA WALTON ST JOURNALS DEPT, OXFORD, ENGLAND OX2 6DP SN 0894-234X J9 ASIAN ART PD WIN PY 1991 VL 4 IS 1 BP 2 EP 5 PG 4 WC Art SC Art GA FX003 UT WOS:A1991FX00300001 ER PT J AU KENT, SM DEZEEUW, T AF KENT, SM DEZEEUW, T TI APPROXIMATE 3RD INTEGRALS IN AXISYMMETRICAL GALAXIES AND THE TILT OF THE VELOCITY ELLIPSOID IN THE SOLAR NEIGHBORHOOD SO ASTRONOMICAL JOURNAL LA English DT Article ID SURFACE MASS DENSITY; GALACTIC DISK; SUN AB We present three different methods for calculating approximate third integrals of the motion for orbits in axisymmetric potentials. All three methods are based on approximating the orbits by motion in a separable potential. The results are applied to the Carlberg-Innanen potential for the Galaxy and allow a determination of the tilt of the velocity ellipsoid in the solar neighborhood. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. STERREWACHT LEIDEN,2300 RA LEIDEN,NETHERLANDS. NR 29 TC 17 Z9 17 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 DEC PY 1991 VL 102 IS 6 BP 1994 EP 2000 DI 10.1086/116022 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GR851 UT WOS:A1991GR85100011 ER PT J AU SEWARD, FD FABRICANT, DG KIRSHNER, RP MCCLINTOCK, JE SMITH, RC REMILLARD, RA AF SEWARD, FD FABRICANT, DG KIRSHNER, RP MCCLINTOCK, JE SMITH, RC REMILLARD, RA TI A LARGE RADIO GALAXY BEHIND THE SUPERNOVA REMNANT HB9 SO ASTRONOMICAL JOURNAL LA English DT Article AB HB9 is a 2-degrees diameter radio shell with x-ray emission from a broad diffuse band in the interior. Within this band, a weak unresolved x-ray source coincides with the radio source 4C 46.09. To identify this source we have obtained CCD I and V band pictures and a spectrum. The source is a galaxy at redshift 0.195, and is therefore only accidentally aligned with HB9. The galaxy is large and bright and has the characteristics of a cD galaxy, often found at the center of clusters. If the galaxy is centered in a cluster, some of the surrounding diffuse x-rays may also be extragalactic. C1 MIT,CTR SPACE RES,CAMBRIDGE,MA 02139. RP SEWARD, FD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 14 TC 4 Z9 4 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 DEC PY 1991 VL 102 IS 6 BP 2047 EP 2048 DI 10.1086/116027 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GR851 UT WOS:A1991GR85100016 ER PT J AU SMITH, PL STARK, G YOSHINO, K ITO, K STEVENS, MH AF SMITH, PL STARK, G YOSHINO, K ITO, K STEVENS, MH TI LABORATORY ABSORPTION-SPECTRA OF MOLECULES AT INTERSTELLAR CLOUD TEMPERATURES - 1ST MEASUREMENTS ON CO AT APPROXIMATELY 97 NM SO ASTRONOMY & ASTROPHYSICS LA English DT Letter DE ATOMIC AND MOLECULAR DATA; ATOMIC AND MOLECULAR PROCESSES; INTERSTELLAR MEDIUM, ABUNDANCES; INTERSTELLAR MEDIUM, MOLECULES; SPECTROSCOPY ID VUV SPECTROSCOPIC FACILITY; 115 NM; PHOTODISSOCIATION AB In the 91 - 100 nm spectral region, where absorption of photons by interstellar CO usually leads to dissociation, laboratory spectra obtained at approximately 295 K show that most CO bands are both overlapped and perturbed. Reliable band oscillator strengths cannot be extracted from such spectra. As a consequence, synthetic extreme-ultraviolet absorption spectra for CO at the low temperatures that prevail in interstellar clouds are uncertain. We have used a supersonic expansion technique to cool CO to approximately 30 K and have studied, with high spectral resolution, three bands in the 97 nm region. The measured spectrum at 30 K is in reasonable agreement with some published modelled spectra, but our ratios of integrated cross sections are somewhate different from those determined from low resolution spectra obtained at 295 K, in which the bands are blended. The significance of the low temperature cross section measurements for interstellar and circumstellar chemistry remains to be investigated. C1 WELLESLEY COLL, DEPT PHYS, WELLESLEY, MA 02181 USA. NATL LAB HIGH ENERGY PHYS, PHOTON FACTORY, TSUKUBA, IBARAKI 305, JAPAN. JOHNS HOPKINS UNIV, DEPT EARTH & PLANETARY SCI, BALTIMORE, MD 21218 USA. RP SMITH, PL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 15 TC 4 Z9 4 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 DEC PY 1991 VL 252 IS 1 BP L13 EP L15 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GT517 UT WOS:A1991GT51700004 ER PT J AU PELETIER, RF WILLNER, SP AF PELETIER, RF WILLNER, SP TI INFRARED IMAGES, VIRGO SPIRALS, AND THE TULLY-FISHER LAW SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERING; GALAXIES, DISTANCES; INFRARED, SOURCES; PHOTOMETRY ID VELOCITY-WIDTH RELATION; EXTRAGALACTIC DISTANCE SCALE; POPULATION INCOMPLETENESS BIAS; H-I OBSERVATIONS; ROTATION CURVES; MALMQUIST BIAS; FIELD GALAXIES; CLUSTER AREA; ELLIPTICAL GALAXIES; NEARBY GALAXIES AB For a complete (but magnitude-limited) sample of Virgo Cluster spiral galaxies, we present 1.65-mu-m photometry derived from images. Both galaxy inclinations and H-magnitudes are derived from the new data. The new photometry agrees with previous measurements. The infrared inclinations from the present data are usable for galaxies having inclinations greater than 45-degrees, but deeper images would be needed for galaxies more face-on than this. The inclinations are the major observational uncertainty in the Tully-Fisher relation, but the relation in Virgo must have an intrinsic dispersion amounting to approximately 0.4 mag. Sample selection is critical for determination of the intrinsic dispersion. RP PELETIER, RF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Peletier, Reynier/B-9633-2012 NR 72 TC 31 Z9 31 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 1991 VL 382 IS 2 BP 382 EP 395 DI 10.1086/170729 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GR012 UT WOS:A1991GR01200004 ER PT J AU ADAMS, FC AF ADAMS, FC TI ASYMPTOTIC THEORY FOR THE SPATIAL-DISTRIBUTION OF PROTOSTELLAR EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE SPECTROPHOTOMETRY; STARS, EVOLUTION; STARS, FORMATION; STARS, PRE-MAIN-SEQUENCE ID MOLECULAR CLOUD CORES; RADIATIVE-TRANSFER; STAR FORMATION; PROTOSTARS; DUST; EVOLUTION; COLLAPSE AB In order to facilitate the interpretation of observations of protostellar sources, we develop an analytic theory of protostellar emission. We focus our discussion on submillimeter wavelengths where protostellar sources can be spatially resolved. For a given protostellar envelope (i.e., given density and temperature distributions), we determine an asymptotic expansion for the specific intensity. We then calculate the convolution of specific intensity profiles with the Gaussian response function of a telescope. Using these analytic results, we calculate the monochromatic luminosity ratio L-nu(R)/L-nu(0)-a directly observable quantity-in terms of the underlying physical quantities. Observations of L-nu(R)/L-nu(0) can be used in conjunction with the results of this paper to estimate the physical parameters of protostellar envelopes (in particular, the effective powerlaw indices p and q of the density and temperature distributions). RP ADAMS, FC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 30 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 DEC 1 PY 1991 VL 382 IS 2 BP 544 EP 554 DI 10.1086/170741 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GR012 UT WOS:A1991GR01200016 ER PT J AU LADD, EF ADAMS, FC CASEY, S DAVIDSON, JA FULLER, GA HARPER, DA MYERS, PC PADMAN, R AF LADD, EF ADAMS, FC CASEY, S DAVIDSON, JA FULLER, GA HARPER, DA MYERS, PC PADMAN, R TI FAR-INFRARED AND SUBMILLIMETER WAVELENGTH OBSERVATIONS OF STAR-FORMING DENSE CORES .2. IMAGES SO ASTROPHYSICAL JOURNAL LA English DT Article DE SPECTROPHOTOMETRY; STARS, CIRCUMSTELLAR SHELLS; STARS, PRE-MAIN-SEQUENCE ID MOLECULAR CLOUD CORES; DARK CLOUDS; CONTINUUM OBSERVATIONS; PROTOSTARS; MASSES; OPTICS; DISK; DUST AB This paper reports on far-infrared and submillimeter wavelength observations of low-mass protostellar candidates. The data set comprises emission maps of nine sources observed over a wavelength range 100-800-mu-m. The emission is extended at all wavelengths longer than 100-mu-m. The apparent size of the emission regions is weakly correlated with the beam size and is consistent with an underlying specific intensity profile which is scale-free (i.e., I-nu decreases as a power law with distance). The observed emission maps are not circular, but have a mean aspect ratio of 1.3, and the position angles are similar to those determined from maps of molecular emission. The observational results are used in conjunction with theoretical considerations to constrain the physical properties of the putative protostellar envelopes. The best constrained parameter is the sum p + q of the power-law indices of the density and temperature distributions; this sum is shown to lie in the range 1.8 less-than-or-equal-to p + q less-than-or-equal-to 2.3 for the sources L1489 and L1527. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. YERKES OBSERV,WILLIAMS BAY,WI 53191. UNIV CAMBRIDGE,CAVENDISH LAB,CAMBRIDGE CB3 0HE,ENGLAND. RP LADD, EF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MS-42,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 35 TC 62 Z9 62 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 1991 VL 382 IS 2 BP 555 EP 569 DI 10.1086/170742 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GR012 UT WOS:A1991GR01200017 ER PT J AU HARTIGAN, P KENYON, SJ HARTMANN, L STROM, SE EDWARDS, S WELTY, AD STAUFFER, J AF HARTIGAN, P KENYON, SJ HARTMANN, L STROM, SE EDWARDS, S WELTY, AD STAUFFER, J TI OPTICAL EXCESS EMISSION IN T-TAURI STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE SPECTROPHOTOMETRY; STARS, ACCRETION; STARS, PRE-MAIN-SEQUENCE ID YOUNG STELLAR OBJECTS; ROTATING PROTOSTARS; CIRCUMSTELLAR DISKS; RADIAL-VELOCITIES; ADDITIONAL UBVRI; ACCRETION DISKS; FORBIDDEN-LINE; SPECTRA; EVOLUTION; PHOTOMETRY AB We present a set of simultaneous high-resolution spectroscopic and spectrophotometric observations of 22 K7-M1 T Tauri stars in the Taurus-Auriga dark cloud. Analysis of the high-resolution data makes it possible to separate the optical excess ("veiling") emission from the photospheric fluxes in these stars. The amount of optical excess emission at 5500 angstrom ranges from undetectable (less-than-or-similar-to 10% of the photosphere) to as much as 10 times the photospheric flux in the most extreme objects. We use the spectrophotometry to derive improved reddening corrections and determine the spectral energy distributions of the excess emission between 3500 and 8400 angstrom. Spectra of the excesses are flat in F-lambda or rise slowly toward the blue at optical wavelengths, and most objects have a Balmer emission jump. The optical excess emission can contribute significantly to the total flux in both the V and R passbands, and the excesses have caused previous estimates of the visual extinction to be as much as 50% too low for several T Tauri stars. New values for the stellar luminosities of the program objects do not differ significantly from those obtained from near-infrared studies. Simple models indicate that the optical excesses arise from regions with densities approximately 10(14) cm-3, temperatures of approximately 9000 K, optical depths between approximately 0.2 and 5, and covering factors of approximately 5% of the stellar surface area. The mass accretion rates inferred from the excesses are typically approximately 10(-7) M. yr-1. Disk models for the near-infrared excesses indicate that accretion energy and reprocessed light from the central star contribute roughly equally to the near-infrared excesses of objects with moderate optical excesses. Our observations are consistent with the idea that optical excess emission in T Tauri stars comes from the boundary layer of an accretion disk. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. PENN STATE UNIV,DEPT ASTRON & ASTROPHYS,UNIV PK,PA 16802. RP HARTIGAN, P (reprint author), UNIV MASSACHUSETTS,FIVE COLL RADIO ASTRON OBSERV,AMHERST,MA 01003, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 38 TC 180 Z9 181 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 1991 VL 382 IS 2 BP 617 EP 635 DI 10.1086/170749 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GR012 UT WOS:A1991GR01200024 ER PT J AU REYNOLDS, PT CAWLEY, MF FEGAN, DJ HILLAS, AM KWOK, PW LAMB, RC LANG, MJ LEWIS, DA MACOMB, DJ OFLAHERTY, KS VACANTI, G WEEKES, TC AF REYNOLDS, PT CAWLEY, MF FEGAN, DJ HILLAS, AM KWOK, PW LAMB, RC LANG, MJ LEWIS, DA MACOMB, DJ OFLAHERTY, KS VACANTI, G WEEKES, TC TI SEARCH FOR TEV GAMMA-RAY EMISSION FROM HERCULES-X-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GAMMA-RAYS, GENERAL; STARS, INDIVIDUAL (HERCULES-X-1, HZ-HERCULIS) ID ASTRONOMY AB Six years of observations of Hercules X-1 with the Whipple Observatory gamma-ray telescope have been subjected to a Fourier analysis to search for emission at the 0.8079 Hz neutron star frequency. Evidence for a signal is found at the 99.5% confidence level for data taken with the medium-resolution imaging camera (spanning the first 4 years, 1984-1987) with some indications of emission at frequencies blueshifted from the fundamental frequency. However, analysis of the high-resolution camera data base (the subsequent 2 years of data, 1988-1989) have failed to substantiate this effect. selection of events on the basis of gamma-ray-like image parameters did not enhance the signal from the medium-resolution data nor produce any indication of a signal from the high-resolution data. The overall conclusion is that no statistically significant evidence for TeV gamma-ray emission was found in the Whipple Observatory data base when the 6 years of data are taken as a whole. C1 IOWA STATE UNIV SCI & TECHNOL,DEPT PHYS & ASTRON,AMES,IA 50011. ST PATRICKS COLL,DEPT PHYS,MAYNOOTH,KILDARE,IRELAND. NATL UNIV IRELAND UNIV COLL DUBLIN,DEPT PHYS,DUBLIN 4,IRELAND. UNIV LEEDS,DEPT PHYS,LEEDS LS2 9JT,W YORKSHIRE,ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,CAMBRIDGE,MA 02138. OI Lang, Mark/0000-0003-4641-4201 NR 28 TC 7 Z9 7 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 DEC 1 PY 1991 VL 382 IS 2 BP 640 EP 646 DI 10.1086/170751 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GR012 UT WOS:A1991GR01200026 ER PT J AU HABBAL, SR GRACE, E AF HABBAL, SR GRACE, E TI THE CONNECTION BETWEEN CORONAL BRIGHT POINTS AND THE VARIABILITY OF THE QUIET-SUN EXTREME-ULTRAVIOLET EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE SUN, CORONA; ULTRAVIOLET, SPECTRA ID SOLAR TRANSITION ZONE; SPECTRO-HELIOMETER; REGION; MICROFLARES; NETWORK; WIND; HOLE AB We determine the characteristics of the significant variable EUV emission from the quiet Sun by analyzing the EUV/Skylab data recorded at six wavelengths simultaneously scanning the chromosphere to the corona, from a coronal hole and a quiet region. We adopt the criterion that changes in the intensity of emission in consecutive spectroheliograms, 5.5 minute apart, are significant if larger than sigma (where sigma is the root mean square deviation from the mean in a source free region). We find that, in both regions studied, the significant variable emission is preferentially localized in EUV bright points which form the enhanced EUV emission from the quiet Sun. The spatial density of the enhanced and variable emission has a marked temperature dependence. We interpret the minimum at 3 x 10(5) K as evidence for two favored temperature distributions of closed magnetic field structures in the quiet Sun, one below 3 x 10(5) K and one at coronal temperatures, implying that not all structures in the quiet Sun necessarily reach coronal temperatures. The enhanced emission occupies between 10% and 25% of the solar surface, depending on the temperature, while the variable emission covers a smaller fraction, between 5% and 15% of the solar surface. These estimates are likely to vary with the solar cycle, since the number of bright points is known to be solar cycle dependent. The spatial density of the variable emission derived in this study represents the spatial density of random fluctuations and is an upper limit if the actual spatial scale of the variability is less than the 5" spatial resolution of the data. The radiative energy losses associated with the variable emission are a significant fraction (about 40%) of the corresponding losses from the enhanced emission. These losses, which provide a lower limit to the energy input into the variable and enhanced emission, are much smaller than the heating budget requirements of the quiet Sun. RP HABBAL, SR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 24 TC 17 Z9 18 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 1991 VL 382 IS 2 BP 667 EP & DI 10.1086/170754 PN 1 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GR012 UT WOS:A1991GR01200029 ER PT J AU CARLSTEAD, K SEIDENSTICKER, J AF CARLSTEAD, K SEIDENSTICKER, J TI SEASONAL-VARIATION IN STEREOTYPIC PACING IN AN AMERICAN BLACK BEAR URSUS-AMERICANUS SO BEHAVIOURAL PROCESSES LA English DT Article AB The behaviour of a male American black bear Ursus americanus was observed for over 2400 h across all seasons of the year. Stereotypic pacing was most frequent, oriented away from the exhibit, and performed mainly after feeding during the period May-July; from August-November pacing was oriented towards the exhibit and performed mainly around feeding time. Placing bear odors in the enclosure slightly reduced pacing and increased exploring/foraging in the late spring. Hiding small food items in the exhibit almost completely eliminated pacing in the fall and replaced it with foraging. Comparison with seasonal changes in the behaviour of wild bears suggest that the stereotypy of this bear, and probably zoo bears in general, developed from two main primary behaviours that cannot be performed in a barren zoo environment: mate-seeking behaviour predominating in the late spring and foraging behaviour in the late summer and fall. RP CARLSTEAD, K (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 22 TC 29 Z9 32 U1 7 U2 30 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0376-6357 J9 BEHAV PROCESS JI Behav. Processes PD DEC PY 1991 VL 25 IS 2-3 BP 155 EP 161 DI 10.1016/0376-6357(91)90017-T PG 7 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA GX013 UT WOS:A1991GX01300009 PM 24923974 ER PT J AU JOHNSTON, LA DONOGHUE, AM OBRIEN, SJ WILDT, DE AF JOHNSTON, LA DONOGHUE, AM OBRIEN, SJ WILDT, DE TI RESCUE AND MATURATION INVITRO OF FOLLICULAR OOCYTES COLLECTED FROM NONDOMESTIC FELID SPECIES SO BIOLOGY OF REPRODUCTION LA English DT Article ID DOMESTIC CAT; DEVELOPMENTAL COMPETENCE; FERTILIZATION INVITRO; GENETIC-VARIATION; CHEETAH; EJACULATE; LEOPARD; BENGALENSIS; CAPACITY; TRAITS AB The potential for rescuing immature oocytes from the ovaries of females of rare felid species which die or undergo medical ovariohysterectomy was evaluated. Ovaries were recovered from 13 species representing 35 individuals in good-to-poor health. Although the majority of females were 10 yr of age or older and in fair-to-poor health, a total of 846 oocytes were recovered of which 608 (71.9%) were classified as fair-to-excellent quality. One hundred of these oocytes were used for initial maturation classification and as parthogenetic controls. Overall, of the 508 fair-to-excellent quality oocytes placed in culture, 164 (32.3%) matured to metaphase II in vitro. For species in which 3 or more individuals yielded oocytes, mean oocyte maturation rates were as follows: 36.2%, tiger; 27.9% leopard; and 8.3%, cheetah. In vitro insemination of oocytes resulted in fertilization (2 polar bodies, 2 pronuclei, or cleavage) rates of 9.1 % to 28.6% (leopard) using homologous fresh spermatozoa and 4.0% (lion) to 40.0% (puma) using homologous frozen-thawed spermatozoa. Inseminations using heterologous (domestic cat) spermatozoa also resulted in fertilized oocytes in the tiger, leopard, snow leopard, puma, serval, and Geoffroy's cat (range in fertilization rate, 5.0% for leopard to 46.2% for puma). Cleaved embryos resulted from the insemination of leopard oocytes with homologous sperm (n = 1 embryo) and puma oocytes with domestic cat sperm (n = 3 embryos). These results demonstrate that immature ovarian oocytes from rare felid species can be stimulated to mature in vitro despite an excision-to-culture interval as long as 36 h. These oocytes are capable of fertilization in vitro, although fertilization rates do not approach those achieved in parallel studies in domestic cats. Our observations of successful cross-species sperm-oocyte interaction in vitro (including the production of cleaved embryos) confirms that the oocytes of certain felid species have not developed mechanisms for excluding penetration or fertilization by heterologous felid spermatozoa. C1 SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008. NCI,VIRAL CARCINOGENESIS LAB,FREDERICK,MD 21701. FU NICHD NIH HHS [HD 23853] NR 34 TC 64 Z9 65 U1 2 U2 6 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD DEC PY 1991 VL 45 IS 6 BP 898 EP 906 DI 10.1095/biolreprod45.6.898 PG 9 WC Reproductive Biology SC Reproductive Biology GA GR668 UT WOS:A1991GR66800014 PM 1805993 ER PT J AU WHIGHAM, DF OLMSTED, I CANO, EC HARMON, ME AF WHIGHAM, DF OLMSTED, I CANO, EC HARMON, ME TI THE IMPACT OF HURRICANE GILBERT ON TREES, LITTERFALL, AND WOODY DEBRIS IN A DRY TROPICAL FOREST IN THE NORTHEASTERN YUCATAN PENINSULA SO BIOTROPICA LA English DT Article ID PATTERNS AB Hurricane Gilbert struck the northeastern portion of the Yucaran Peninsula in an area where we have been conducting studies of the vegetation and avifauna in a dry tropical forest since 1984. All trees in our study area were completely defoliated and most suffered heavy structural damage. Although few trees were killed outright, many died over the next 17 months, especially those that had been heavily damaged. Tree recovery was rapid as relative diameter growth for most species for the first year after the hurricane were greater than average diameter growth rates for three of the five prehurricane years. Biomass of litterfall (leaves and wood less than 10 cm in diameter) and nutrients generated by the hurricane exceeded the totals produced during any of the five previous years. The hurricane increased the mass and nutrients in coarse woody debris (wood greater than 10 cm in diameter) by approximately 50 percent. Mortality caused by fire was much greater than morrality caused by the hurricane. C1 CTR INVEST QUINTANA ROO,CHETUMAL 77100,QUINTANA ROO,MEXICO. OREGON STATE UNIV,DEPT FOREST SCI,CORVALLIS,OR 97331. RP WHIGHAM, DF (reprint author), SMITHSONIAN ENVIRONM RES CTR,BOX 28,EDGEWATER,MD 21037, USA. OI Whigham, Dennis/0000-0003-1488-820X NR 31 TC 136 Z9 145 U1 2 U2 13 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 DEC PY 1991 VL 23 IS 4 BP 434 EP 441 DI 10.2307/2388263 PN A PG 8 WC Ecology SC Environmental Sciences & Ecology GA HB622 UT WOS:A1991HB62200018 ER PT J AU LYNCH, JF AF LYNCH, JF TI EFFECTS OF HURRICANE GILBERT ON BIRDS IN A DRY TROPICAL FOREST IN THE YUCATAN PENINSULA SO BIOTROPICA LA English DT Article AB On 14 September 1988 Hurricane Gilbert, the strongest tropical storm ever recorded in the Western Hemisphere, passed through an area of tropical forest in Quintana Roo, Mexico, where I had been studying winter bird populations since 1984. The hurricane defoliated the forest, and created a nearly impenetrable rangle of fallen branches and vines at ground level. Point counts and mist-netting conducted 5-6 mo after the storm revealed an influx of field- and shrub-associated bird species. Most previously common insectivores and feeding generalists were present in February-March 1989, but many had declined significantly in abundance. Resident frugivores and nectarivores were especially scarce after the hurricane. Wildfires that swept through northeastern Quintana Roo in the summer of 1989 had a greater effect on birds than did the storm itself. By late winter 1990 the bird community within unburned forest was clearly converging toward its prehurricane composition. In contrast, the bird community in burned forest resembled that associated with recently abandoned agricultural fields and pastures. As a group, overwintering nearctic migrants appeared to be more resilient than year-round residents to the effects of both the hurricane and the associated fires. RP LYNCH, JF (reprint author), SMITHSONIAN ENVIRONM RES CTR,POB 28,EDGEWATER,MD 21037, USA. NR 15 TC 42 Z9 45 U1 1 U2 5 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 DEC PY 1991 VL 23 IS 4 BP 488 EP 496 DI 10.2307/2388271 PN A PG 9 WC Ecology SC Environmental Sciences & Ecology GA HB622 UT WOS:A1991HB62200026 ER PT J AU POSEY, MH HINES, AH AF POSEY, MH HINES, AH TI COMPLEX PREDATOR-PREY INTERACTIONS WITHIN AN ESTUARINE BENTHIC COMMUNITY SO ECOLOGY LA English DT Article DE BENTHIC; BENTHIC FOOD WEBS; CHESAPEAKE BAY; ESTUARINE NEAR-SHORE COMMUNITIES; FIELD EXPERIMENTS; OMNIVORY; PALAEMONETES; PREDATION; SHRIMP PREDATION ON BENTHIC FAUNA ID KILLIFISH FUNDULUS-HETEROCLITUS; SOFT-BOTTOM COMMUNITIES; TIDAL SALT-MARSH; FOOD WEBS; GRASS SHRIMP; PALAEMONETES-PUGIO; COMMON MUMMICHOG; CHESAPEAKE BAY; SEA OTTERS; BLUE CRABS AB Indirect predator-prey interactions have been suggested to be important in a variety of communities. However, we still understand little about the factors determining the relative importance of indirect and direct effects of predation or what forms indirect predator-prey interactions may take. We examined the direct effects of predation by an omnivorous grass shrimp, Palaemonetes pugio, and the indirect effects for prey species of interactions between this shrimp and other predators in an estuarine benthic community. Direct and indirect effects of predation were examined in the field using a combination of large- and small-scale enclosure/exclosure experiments. Specific interactions and mechanisms of effects were examined in laboratory predation studies, utilizing both two-species and multi-species systems. Grass shrimp predation reduced the densities of a variety of benthic fauna, but the effects varied seasonally and with prey size. Interactions between grass shrimp and other predators took two forms: reduction of an infaunal predator by shrimp predation and predation on grass shrimp by fish. Both types of interactions had a mixed effect on lower trophic levels, with enhancement of certain benthic prey and no effect on other species. Interactions between grass shrimp and their fish predators resulted in changes in shrimp distribution independent of changes in shrimp abundance, creating spatial refugia for shrimp prey. The dynamics of indirect interactions in this community are strongly affected by the omnivorous nature of the major predators. Our results emphasize the general importance of omnivory in regulating predator-prey interactions and in predicting the relative importance of indirect predator effects. C1 SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. NR 78 TC 112 Z9 114 U1 2 U2 24 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE, NW, STE 400, WASHINGTON, DC 20036 SN 0012-9658 J9 ECOLOGY JI Ecology PD DEC PY 1991 VL 72 IS 6 BP 2155 EP 2169 DI 10.2307/1941567 PG 15 WC Ecology SC Environmental Sciences & Ecology GA GV769 UT WOS:A1991GV76900023 ER PT J AU TOWE, KM AF TOWE, KM TI AEROBIC CARBON CYCLING AND CERIUM OXIDATION - SIGNIFICANCE FOR ARCHEAN OXYGEN LEVELS AND BANDED IRON-FORMATION DEPOSITION SO GLOBAL AND PLANETARY CHANGE LA English DT Article; Proceedings Paper CT WORKSHOP ON ATMOSPHERIC OXYGEN VARIATION THROUGH GEOLOGIC TIME CY JUL 16-18, 1990 CL PENN STATE UNIV, EARTH SYST SCI CTR, STATE COLLEGE, PA SP PENN STATE UNIV HO PENN STATE UNIV, EARTH SYST SCI CTR ID RARE-EARTH ELEMENTS; WESTERN-AUSTRALIA; PRECAMBRIAN ATMOSPHERE; HAMERSLEY GROUP; SEA-WATER; ORIGIN; OCEAN; PALEOATMOSPHERE; GEOCHEMISTRY; SEDIMENTS AB The amounts of organic carbon and iron generally estimated to have been preserved in early Precambrian sediments suggest by implication that only the rapid, oxidative recycling of organic carbon by aerobic heterotrophy could plausibly have kept pace with the oxygen produced annually by net photosynthesis, even with a low global primary productivity of less than 1% of modern global values (Towe, 1990). A global aerobic recycling process would require at least a moderately oxygenated atmosphere to operate. The presence of such an atmosphere as far back in Earth history as 3.8 Ga ago is consistent with, but not proven by, the abundance of organic carbon and the "anomalous" distribution of rare earths in the banded iron-formations of the Isua sediments (Dymek and Klein, 1988). The absence of positive cerium anomalies and the presence of positive europium anomalies in these and other banded iron-formations (Klein and Beukes, 1989; Derry and Jacobsen, 1990) imply that iron oxidation during BIF deposition took place in waters at some depth below the zone of mixing rather than at the surface. A modified Klein-Beukes model using shallow, seasonal downwelling in an otherwise deep-water stratified basin under a moderately oxygenated atmosphere may help explain the origin of some of these enigmatic deposits. RP TOWE, KM (reprint author), SMITHSONIAN INST,DEPT PALEOBIOL,WASHINGTON,DC 20560, USA. NR 56 TC 4 Z9 4 U1 1 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-8181 J9 GLOBAL PLANET CHANGE JI Glob. Planet. Change PD DEC PY 1991 VL 97 IS 1-2 BP 113 EP 123 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA GZ960 UT WOS:A1991GZ96000011 ER PT J AU WELDON, PJ MCNEASE, L AF WELDON, PJ MCNEASE, L TI DOES THE AMERICAN ALLIGATOR DISCRIMINATE BETWEEN VENOMOUS AND NONVENOMOUS SNAKE PREY SO HERPETOLOGICA LA English DT Article DE ALLIGATOR MISSISSIPPIENSIS; SNAKES; CROTALINAE; COLUBRIDAE AB McIlhenny reported that the American alligator (Alligator mississippiensis) vigorously shakes venomous (Crotalinae) but not nonvenomous (Colubridae) snakes during predatory attacks. He suggested that these snakes are discriminated by chemical cues. Juvenile and adult alligators in our study ingested whole carcasses or carcass pieces of crotaline and colubrid snakes without shaking them. Moreover, no significant differences were detected in the times spent by juveniles ingesting pieces of the carcasses of these snakes. Snake scent gland secretions, a source of chemicals to which alligators may respond, did not elicit vigorous head-shaking when presented on pieces of chicken; alligators generally disgorged chicken pieces treated with these exudates. Observations of staged encounters between juvenile alligators and live snakes indicated that alligators vigorously shake a variety of snakes, not just crotalines, during predatory attacks. C1 TEXAS A&M UNIV SYST,DEPT BIOL,COLLEGE STN,TX 77843. ROCKEFELLER WILDLIFE REFUGE,GRAND CHENIER,LA 70643. RP WELDON, PJ (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT HERPETOL,WASHINGTON,DC 20008, USA. NR 9 TC 4 Z9 4 U1 0 U2 6 PU HERPETOLOGISTS LEAGUE PI JOHNSON CITY PA EAST TENNESSEE STATE UNIV, DEPT BIOLOGICAL SCIENCES, BOX 70726, JOHNSON CITY, TN 37614-0726 SN 0018-0831 J9 HERPETOLOGICA JI Herpetologica PD DEC PY 1991 VL 47 IS 4 BP 403 EP 406 PG 4 WC Zoology SC Zoology GA GU137 UT WOS:A1991GU13700003 ER PT J AU MANNING, RD AF MANNING, RD TI THE ROMANCE OF CULTURE IN AN URBAN CIVILIZATION - PARK,ROBERT,E. ON RACE AND ETHNIC-RELATIONS IN CITIES - LAL,BB SO INTERNATIONAL MIGRATION REVIEW LA English DT Book Review C1 SMITHSONIAN INST,WASHINGTON,DC 20560. RP MANNING, RD (reprint author), AMERICAN UNIV,WASHINGTON,DC 20016, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CENTER MIGRATION STUDIES PI STATEN ISL PA 209 FLAGG PLACE, STATEN ISL, NY 10304 SN 0197-9183 J9 INT MIGR REV JI Int. Migr. Rev. PD WIN PY 1991 VL 25 IS 4 BP 959 EP 961 DI 10.2307/2546856 PG 3 WC Demography SC Demography GA HB881 UT WOS:A1991HB88100018 ER PT J AU GINGERICH, O AF GINGERICH, O TI THOREN,VICTOR,E. 13 MAY 1935-9 MARCH 1991 SO ISIS LA English DT Item About an Individual RP GINGERICH, O (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, 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 DEC PY 1991 VL 82 IS 314 BP 693 EP 694 DI 10.1086/355931 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA GY321 UT WOS:A1991GY32100006 ER PT J AU HART, S AF HART, S TI CURATORS AND CULTURE - THE MUSEUM MOVEMENT IN AMERICA, 1740-1870 - OROSZ,JJ SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review RP HART, S (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGANIZATION AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47408 SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD DEC PY 1991 VL 78 IS 3 BP 1052 EP 1053 DI 10.2307/2078829 PG 2 WC History SC History GA GX178 UT WOS:A1991GX17800029 ER PT J AU SHEETS, P HOOPES, J MELSON, W MCKEE, B SEVER, T MUELLER, M CHENAULT, M BRADLEY, J AF SHEETS, P HOOPES, J MELSON, W MCKEE, B SEVER, T MUELLER, M CHENAULT, M BRADLEY, J TI PREHISTORY AND VOLCANISM IN THE ARENAL AREA, COSTA-RICA SO JOURNAL OF FIELD ARCHAEOLOGY LA English DT Article C1 UNIV KANSAS,LAWRENCE,KS 66045. SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560. NASA,STENNIS SPACE CTR,EARTH RESOURCES LAB,NSTL STN,MS. SAN JUAN COLL,CULTURAL RESOURCES MANAGEMENT PROGRAM,FARMINGTON,NM. RP SHEETS, P (reprint author), UNIV COLORADO,DEPT ANTHROPOL,CAMPUS BOX 233,BOULDER,CO 80309, USA. NR 57 TC 8 Z9 9 U1 0 U2 1 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 1991 VL 18 IS 4 BP 445 EP 465 DI 10.2307/530407 PG 21 WC Archaeology SC Archaeology GA GQ071 UT WOS:A1991GQ07100003 ER PT J AU BORDEN, M ZILCZER, JK STUART, J GUGGENHEIM, CE AF BORDEN, M ZILCZER, JK STUART, J GUGGENHEIM, CE TI KNOWLEDGE COLLABORATIONS IN THE ARTS, THE SCIENCES, AND THE HUMANITIES - EDITED EXCERPTS FROM A SMITHSONIAN SEMINAR SERIES .1. THE ARTS SO KNOWLEDGE-CREATION DIFFUSION UTILIZATION LA English DT Discussion C1 SMITHSONIAN INST,FREER GALLERY ART,WASHINGTON,DC 20560. SMITHSONIAN INST,ARTHUR M SACKLER GALLERY,WASHINGTON,DC 20560. RP BORDEN, M (reprint author), SMITHSONIAN INST,HIRSHHORN MUSEUM & SCULPTURE GARDEN,DEPT PAINTING & SCULPTURE,WASHINGTON,DC 20560, USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU SAGE SCIENCE PRESS PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 SN 0164-0259 J9 KNOWLEDGE PD DEC PY 1991 VL 13 IS 2 BP 193 EP 215 PG 23 WC Social Sciences, Interdisciplinary SC Social Sciences - Other Topics GA GR765 UT WOS:A1991GR76500005 ER PT J AU KAEPPLER, AL AF KAEPPLER, AL TI THE RUSSIAN DISCOVERY OF HAWAII - THE ETHNOGRAPHIC AND HISTORIC RECORD - BARRATT,G SO MAN LA English DT Book Review RP KAEPPLER, AL (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ROYAL ANTHROPOLOGICAL INST PI LONDON PA 50 FITZROY STREET, LONDON, ENGLAND W1P 5HS SN 0025-1496 J9 MAN PD DEC PY 1991 VL 26 IS 4 BP 750 EP 751 DI 10.2307/2803788 PG 2 WC Anthropology SC Anthropology GA GV487 UT WOS:A1991GV48700019 ER PT J AU LOVEJOY, TE DWIGHT, RH AF LOVEJOY, TE DWIGHT, RH TI BIOLOGICAL DIVERSITY AND NEPTUNE REALM SO MARINE TECHNOLOGY SOCIETY JOURNAL LA English DT Article ID CORAL REEFS; RESPONSES AB The diverse biological life in both terrestrial and marine environments offers mankind many practical and potential resources. These natural pools of wealth are under continuous pressure from various humanly induced alterations. Areas of current research are attempting to challenge the assorted problems, but many of the issues have yet to be addressed fully. Global climate change and soaring extinction rates appear to be the consequence of anthropogenic effects. Important preventive action is needed to restrict the forcing mechanisms for climate change being created by altered atmospheric composition. RP LOVEJOY, TE (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 38 TC 0 Z9 0 U1 1 U2 4 PU MARINE TECHNOLOGY SOC INC PI WASHINGTON PA C/O I CLAYION MATTHEWS, 1828 L ST, NW, 9TH FL, WASHINGTON, DC 20036 SN 0025-3324 J9 MAR TECHNOL SOC J JI Mar. Technol. Soc. J. PD WIN PY 1991 VL 25 IS 4 BP 7 EP 12 PG 6 WC Engineering, Ocean; Oceanography SC Engineering; Oceanography GA HG985 UT WOS:A1991HG98500002 ER PT J AU CAILLET, C MACPHERSON, GJ ZINNER, EK AF CAILLET, C MACPHERSON, GJ ZINNER, EK TI AL-MG ISOTOPIC RECORD OF RECRYSTALLIZATION OF A REFRACTORY INCLUSION DURING ACCRETION INTO THE LEOVILLE PARENT BODY SO METEORITICS LA English DT Meeting Abstract C1 SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560. WASHINGTON UNIV,DEPT PHYS,ST LOUIS,MO 63130. WASHINGTON UNIV,MCDONNELL CTR SPACE SCI,ST LOUIS,MO 63130. NR 1 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 DEC PY 1991 VL 26 IS 4 BP 326 EP 326 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA HF779 UT WOS:A1991HF77900045 ER PT J AU FREDRIKSSON, K WLOTZKA, F SPETTEL, B AF FREDRIKSSON, K WLOTZKA, F SPETTEL, B TI TO MAKE, PERHAPS, OR NOT TO MAKE CHONDRULES SO METEORITICS LA English DT Meeting Abstract C1 SMITHSONIAN INST,WASHINGTON,DC 20560. MAX PLANCK INST CHEM,KOSMOCHEM ABT,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 DEC PY 1991 VL 26 IS 4 BP 335 EP 335 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA HF779 UT WOS:A1991HF77900069 ER PT J AU WOOD, JA AF WOOD, JA TI ALKALI FRACTIONATION AMONG CHONDRULES OF THE MEZO-MADARAS CHONDRITE SO METEORITICS LA English DT Meeting Abstract C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 2 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 DEC PY 1991 VL 26 IS 4 BP 410 EP 410 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA HF779 UT WOS:A1991HF77900257 ER PT J AU WARD, DC AF WARD, DC TI THE SELECTED LETTERS OF SUMNER,CHARLES - PALMER,BW SO NEW ENGLAND QUARTERLY-A HISTORICAL REVIEW OF NEW ENGLAND LIFE AND LETTERS LA English DT Book Review RP WARD, DC (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU NEW ENGLAND QUARTERLY INC PI BOSTON PA MESERVE HALL 243 NORTHEASTERN UNIV 360 HUNTINGTON AVE, BOSTON, MA 02115 SN 0028-4866 J9 NEW ENGL QUART JI New Engl. Q.-Hist. Rev. New Engl. Life Lett. PD DEC PY 1991 VL 64 IS 4 BP 670 EP 673 DI 10.2307/366195 PG 4 WC History; Literature, American SC History; Literature GA GX035 UT WOS:A1991GX03500012 ER PT J AU ROBBINS, RK AF ROBBINS, RK TI COST AND EVOLUTION OF A FACULTATIVE MUTUALISM BETWEEN ANTS AND LYCAENID LARVAE (LEPIDOPTERA) SO OIKOS LA English DT Article ID MYRMECOPHILOUS RELATIONSHIPS; FUNCTIONAL-ANALYSIS; ATTENDANT ANTS; CATERPILLARS; HYMENOPTERA; BUTTERFLIES; FORMICIDAE; HERBIVORY; SYMBIOSIS AB Larvae of Arawacus lincoides (Lycaenidae) reared in the lab with ants took 0.68 d longer to complete development than larvae without ants. Pupal weight was independent of whether a larva had been ant-tended. A 0.68 d delay in reaching age of first reproduction represents an estimated 1.0%-2.2% lowered intrinsic rate of increase for this continuously brooded species. I show that mutualism will be favored when the ratio of larval survival with ants to that without ants is greater than exp (dr), where d is the additional larval development time caused by feeding ants and r is the intrinsic rate of increase. Other things being equal, species with higher intrinsic rates of increase will be less likely to be mutualistic than their relatives with lower rates of increase. RP ROBBINS, RK (reprint author), SMITHSONIAN INST,NHB STOP 127,WASHINGTON,DC 20560, USA. NR 35 TC 28 Z9 30 U1 1 U2 2 PU MUNKSGAARD INT PUBL LTD PI COPENHAGEN PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK SN 0030-1299 J9 OIKOS JI Oikos PD DEC PY 1991 VL 62 IS 3 BP 363 EP 369 DI 10.2307/3545502 PG 7 WC Ecology SC Environmental Sciences & Ecology GA HB140 UT WOS:A1991HB14000013 ER PT J AU Towe, KM AF Towe, Kenneth M. TI Aerobic carbon cycling and cerium oxidation: significance for Archean oxygen levels and banded iron-formation deposition SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article AB The amounts of organic carbon and iron generally estimated to have been preserved in early Precambrian sediments suggest by implication that only the rapid, oxidative recycling of organic carbon by aerobic heterotrophy could plausibly have kept pace with the oxygen produced annually by net photosynthesis, even with a low global primary productivity of less than 1% of modern global values (Towe, 1990). A global aerobic recycling process would require at least a moderately oxygenated atmosphere to operate. The presence of such an atmosphere as far back in Earth history as 3.8 Ga ago is consistent with, but not proven by, the abundance of organic carbon and the "anomalous" distribution of rare earths in the banded iron-formations of the Isua sediments (Dymek and Klein, 1988). The absence of positive cerium anomalies and the presence of positive europium anomalies in these and other banded iron-formations (Klein and Beukes, 1989; Derry and Jacobsen, 1990) imply that iron oxidation during BIF deposition took place in waters at some depth below the zone of mixing rather than at the surface. A modified Klein-Beukes model using shallow, seasonal downwelling in an otherwise deep-water stratified basin under a moderately oxygenated atmosphere may help explain the origin of some of these enigmatic deposits. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Towe, KM (reprint author), Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. NR 56 TC 16 Z9 16 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD DEC PY 1991 VL 97 IS 1-2 BP 113 EP 123 DI 10.1016/0031-0182(91)90187-V PG 11 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA V43VU UT WOS:000202963400011 ER PT J AU ARP, WJ DRAKE, BG AF ARP, WJ DRAKE, BG TI INCREASED PHOTOSYNTHETIC CAPACITY OF SCIRPUS-OLNEYI AFTER 4 YEARS OF EXPOSURE TO ELEVATED CO2 SO PLANT CELL AND ENVIRONMENT LA English DT Article DE CARBON DIOXIDE; PHOTOSYNTHESIS; PHOTOSYNTHETIC ACCLIMATION ID ATMOSPHERIC CO2; CARBON-DIOXIDE; ESTUARINE MARSH; PLANTS; LEAVES; INSITU; FIELD; C-3 AB While a short-term exposure to elevated atmospheric CO2 induces a large increase in photosynthesis in many plants, long-term growth in elevated CO2 often results in a smaller increase due to reduced photosynthetic capacity. In this study, it was shown that, for a wild C3 species growing in its natural environment and exposed to elevated CO2 for four growing seasons, the photosynthetic capacity has actually increased by 31%. An increase in photosynthetic capacity has been observed in other species growing in the field, which suggests that photosynthesis of certain field grown plants will continue to respond to elevated levels of atmospheric CO2. C1 SMITHSONIAN ENVIRONM RES CTR,POB 28,EDGEWATER,MD 21037. NR 19 TC 90 Z9 93 U1 2 U2 11 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 DEC PY 1991 VL 14 IS 9 BP 1003 EP 1006 DI 10.1111/j.1365-3040.1991.tb00971.x PG 4 WC Plant Sciences SC Plant Sciences GA GY055 UT WOS:A1991GY05500015 ER PT J AU KINMAN, TD STRYKER, LL HESSER, JE GRAHAM, JA WALKER, AR HAZEN, ML NEMEC, JM AF KINMAN, TD STRYKER, LL HESSER, JE GRAHAM, JA WALKER, AR HAZEN, ML NEMEC, JM TI NEW FIELD RR LYRAE VARIABLES IN THE OUTER PARTS OF THE LMC AND THE PROPERTIES OF THE LMC HALO SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE RR LYRAE STARS; VARIABLE STARS; LARGE MAGELLANIC CLOUD ID LARGE MAGELLANIC CLOUD; GLOBULAR-CLUSTERS; HIGH-VELOCITY; LIGHT RATIOS; STARS; PHOTOMETRY; GALAXIES; NGC-2257; MASS AB Four new type-ab RR Lyrae variables that belong to the field of the LMC were found in the direction of NGC 1466; a possible field variable was found near the Reticulum system. A King model that fits the surface densities of the known LMC field RR Lyrae stars of type ab has a limiting radius of 15 kpc. An exponential disk model that fits these densities has a scale length of 2.6 kpc. These models contain approximately 10(4) type-ab RR Lyrae stars and have a central surface density of approximately 200 of these stars per square degree. The LMC field halo of Population II stars has M-upsilon approximately -15.2 and a mass of approximately 1.6 x 10(8) M. This halo therefore makes up about 2% of the mass of the LMC, a similar percentage to that found for our Galactic halo. Thus, the efficiencies of the earliest star-formation processes may have been comparable in the two systems. The LMC field RR Lyraes have a period-frequency distributions similar to those found in the outer halo of our Galaxy. The ratio (rho) of the surface density of these RR Lyraes to that of the older long-period variables (OLPV) (found by Hughes et al. 1991) is approximately 13 at some 3 to 4 kpc from the LMC center. This measure of the relative strengths of the halo to an "old-disk" population is within a factor of two of that which would be seen in our Galaxy at the solar distance from its center. The central visual surface brightness of the LMC halo is approximately 25.5 mag per square arc sec. Its average visual surface brightness (over the area within the effective radius (approximately 4 kpc) is approximately 26.4 mag per square arc sec. It would be difficult to detect a halo of this faintness in an external galaxy unless the halo could be resolved into individual stars. C1 ARIZONA STATE UNIV,DEPT PHYS & ASTRON,TEMPE,AZ 85287. DOMINION ASTROPHYS OBSERV,HERZBERG INST ASTROPHYS,VICTORIA V8X 4M6,BC,CANADA. CARNEGIE INST WASHINGTON,DEPT TERR MAGNETISM,WASHINGTON,DC 20015. CERRO TOLOLO INTERAMER OBSERV,NATL OPT ASTRON OBSERV,LA SERENA,CHILE. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV BRITISH COLUMBIA,DEPT ASTRON,VANCOUVER V6T 1W5,BC,CANADA. RP KINMAN, TD (reprint author), KITT PEAK NATL OBSERV,NATL OPT ASTRON OBSERV,POB 26732,TUCSON,AZ 85726, USA. NR 45 TC 47 Z9 47 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 DEC PY 1991 VL 103 IS 670 BP 1279 EP 1291 DI 10.1086/132947 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GX014 UT WOS:A1991GX01400005 ER PT J AU RAND, H AF RAND, H TI TORAHS INCIPIENT AESTHETICS SO RELIGIOUS EDUCATION LA English DT Article RP RAND, H (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER ART,WASHINGTON,DC 20560, USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU RELIGIOUS EDUCATION ASSOC PI NEW HAVEN PA 409 PROSPECT ST, NEW HAVEN, CT 06511-2177 SN 0034-4087 J9 RELIG EDUC JI Relig. Educ. PD WIN PY 1991 VL 86 IS 1 BP 20 EP 29 PG 10 WC Religion SC Religion GA EZ762 UT WOS:A1991EZ76200002 ER PT J AU EMMONS, LH BIUN, A AF EMMONS, LH BIUN, A TI MALAYSIAN TREESHREWS SO RESEARCH & EXPLORATION LA English DT Article ID TREE SHREWS; PIKAS AB We radiotracked four treeshrews (Tupaiidae) in Sabah, Malaysia (Borneo), and observed maternal behavior of one treeshrew (Tupaia tana). These observations confirmed the peculiar "absentee" system previously known only from captive treeshrews. For the first month of life, the young resided in a "nursery" nest apart from the mother, who visited them once every other day to nurse them for about two minutes. However, when the young emerged from the nest, the mother spent much time with them daily for at least three weeks. This shows that treeshrews receive more maternal care than was previously suspected. The male that shared the mother's territory interacted often with the mother during the nestling stage, but had no contact with the young. He left the area when the young emerged. We present the first preliminary data on the social organization of T. tana and its relationship to the raising of young. C1 KINABALU PK,SABAH PARKS,SABAH,MALAYSIA. RP EMMONS, LH (reprint author), SMITHSONIAN INST,DIV MAMMALS,WASHINGTON,DC 20560, USA. NR 22 TC 1 Z9 1 U1 0 U2 1 PU NATL GEOGRAPHIC SOC PI WASHINGTON PA 17TH AND M STS NW, WASHINGTON, DC 20036 SN 8755-724X J9 RES EXPLOR JI Res. Explor. PD WIN PY 1991 VL 7 IS 1 BP 70 EP 81 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA GQ718 UT WOS:A1991GQ71800007 ER PT J AU KLASSEN, GJ MOOI, RD LOCKE, A AF KLASSEN, GJ MOOI, RD LOCKE, A TI CONSISTENCY INDEXES AND RANDOM DATA SO SYSTEMATIC ZOOLOGY LA English DT Article ID HOMOPLASY EXCESS; PHYLOGENETIC TREES; RETENTION INDEX; INFORMATION AB This study was undertaken to determine the range of consistency index (CI) values obtainable from random data sets. We generated multiple random data matrices for each of 49 different matrix sizes ranging from 5 taxa and 4 (binary) characters to 49 taxa and 124 characters. The CI of the minimum-length tree(s) was calculated for each. CIs decreased in a monotonic, nonlinear fashion with addition of either taxa or characters. The influence of addition of taxa was far greater than that of addition of characters, and an interaction effect was recognized. The general curvilinear relation we found between CIs and number of taxa is consistent with results obtained by other authors, but our random data CIs were lower than those of other studies. Mean random CIs varied from 0.70 for the smallest data sets to 0.072 for the largest. Maximum random CIs reached 0.80. A regression through means of random CIs against number of taxa was calculated with a 95% confidence interval. This CI(random) is the minimum value that real data sets should exceed to be considered to contain phylogenetic information. The CIs of real data sets can be adjusted with the CI(random), and these values are found to meet current criteria for adequate measures of homoplasy. However, the homoplasy indices that are uncorrelated with taxa are also insensitive to internal data set structure, and no current index is adequate for comparison of homoplasy among data sets. C1 UNIV TORONTO,DEPT ZOOL,TORONTO M5S 1A1,ONTARIO,CANADA. SMITHSONIAN INST,DIV FISH,WASHINGTON,DC 20560. RP KLASSEN, GJ (reprint author), ROYAL ONTARIO MUSEUM,DEPT ICHTHYOL & HERPETOL,100 QUEENS PK,TORONTO M5S 2C6,ONTARIO,CANADA. NR 16 TC 103 Z9 105 U1 1 U2 4 PU SOC SYSTEMATIC ZOOLOGY PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY 10TH AND CONSTITUTION NW, WASHINGTON, DC 20560 SN 0039-7989 J9 SYST ZOOL PD DEC PY 1991 VL 40 IS 4 BP 446 EP 457 DI 10.2307/2992239 PG 12 WC Zoology SC Zoology GA JE500 UT WOS:A1991JE50000005 ER PT J AU FRIEDBERG, AL AF FRIEDBERG, AL TI IS THE UNITED-STATES CAPABLE OF ACTING STRATEGICALLY SO WASHINGTON QUARTERLY LA English DT Article ID TRADE-POLICY C1 SMITHSONIAN INST,WOODROW WILSON INT CTR,WASHINGTON,DC 20560. NR 35 TC 8 Z9 8 U1 0 U2 3 PU MIT PRESS PI CAMBRIDGE PA 55 HAYWARD ST JOURNALS DEPT, CAMBRIDGE, MA 02142 SN 0163-660X J9 WASH QUART JI Wash. Q. PD WIN PY 1991 VL 14 IS 1 BP 5 EP 23 PG 19 WC International Relations; Law SC International Relations; Government & Law GA EJ992 UT WOS:A1991EJ99200001 ER PT J AU BERCAW, ND AF BERCAW, ND TI SOLID OBJECTS, MUTABLE MEANINGS - FANCYWORK AND THE CONSTRUCTION OF BOURGEOIS CULTURE, 1840-1880 SO WINTERTHUR PORTFOLIO-A JOURNAL OF AMERICAN MATERIAL CULTURE LA English DT Article ID AMERICA C1 SMITHSONIAN INST,WASHINGTON,DC 20560. RP BERCAW, ND (reprint author), UNIV PENN,DEPT AMER CIVILIZAT,PHILADELPHIA,PA 19104, USA. NR 90 TC 14 Z9 14 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0084-0416 J9 WINTERTHUR PORTFOLIO JI Winterthur Portfol.-J. Amer. Mater. Cult. PD WIN PY 1991 VL 26 IS 4 BP 231 EP 247 DI 10.1086/496545 PG 17 WC Art SC Art GA JG730 UT WOS:A1991JG73000002 ER PT J AU OFTEDAL, OT AF OFTEDAL, OT TI THE NUTRITIONAL CONSEQUENCES OF FORAGING IN PRIMATES - THE RELATIONSHIP OF NUTRIENT INTAKES TO NUTRIENT-REQUIREMENTS SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY OF LONDON SERIES B-BIOLOGICAL SCIENCES LA English DT Article ID MONKEYS CEBUS-ALBIFRONS; FOOD SELECTION; PROTEIN-REQUIREMENTS; HOWLER MONKEYS; RHESUS-MONKEY; CHEMISTRY; DIGESTION; CHOICE; BLACK AB Many studies have examined the proportion of time that primates devote to feeding on various types of food, but relatively little is known about the intake rates associated with each food. However, the nutritional consequences of foraging can only be interpreted by comparing nutrient intakes with estimated nutrient requirements. The energy available to primates from ingested foods will depend both on the composition of the food and the extent to which various constituents, including fibre fractions, are digested. Both human and non-human primates have relatively low requirements for protein as a consequence of slow growth rates, small milk Yields and relatively dilute milk. Because the nutrient demands of growth and reproduction are spread out over time, it appears that primates do not need to seek out foods of particularly high nutrient density, except perhaps during weaning. Although food selection in some species of primates appears to be correlated with the protein concentration of foods, it is unlikely that high dietary protein levels are required, at least when foods of balanced amino acid composition (such as leaves) are included in the diet. RP OFTEDAL, OT (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008, USA. NR 54 TC 88 Z9 96 U1 2 U2 20 PU ROYAL SOC LONDON PI LONDON PA 6 CARLTON HOUSE TERRACE, LONDON, ENGLAND SW1Y 5AG SN 0962-8436 J9 PHILOS T ROY SOC B JI Philos. Trans. R. Soc. Lond. Ser. B-Biol. Sci. PD NOV 29 PY 1991 VL 334 IS 1270 BP 161 EP 170 DI 10.1098/rstb.1991.0105 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA GU375 UT WOS:A1991GU37500001 PM 1685574 ER PT J AU DUPREE, AK WHITNEY, BA AF DUPREE, AK WHITNEY, BA TI CA-II EMISSION FROM OLD RED GIANTS IN THE GLOBULAR CLUSTER-M15 SO NATURE LA English DT Article ID FK COMAE; STARS AB MURPHY et al. 1 recently observed characteristic emission of Ca II from the globular cluster M15, and argued that this emission came from a population of primordial binary stars. Their conclusion appears theoretically attractive in relation to the study of the dynamics and evolution of globular clusters 2,3. We argue here, however, that the Ca II K-line emission in various types of hard binary systems differs in strength and width from the M15 spectra, and we demonstrate that the M15 emission closely resembles that from metal-deficient red giants of the halo population in our Galaxy. Chromospheric activity, indicated by emission in Ca II, H-alpha and Mg II, occurs in red giants in both globular clusters and halo-population field giants 4-6. A simple detection of Ca II emission is thus not a unique signature of binaries, and in the case of M15 we argue that red giants are the more likely cause. RP DUPREE, AK (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 17 TC 3 Z9 3 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 28 PY 1991 VL 354 IS 6351 BP 284 EP 286 DI 10.1038/354284a0 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA GT204 UT WOS:A1991GT20400039 ER PT J AU SCOTTI, JV RABINOWITZ, DL MARSDEN, BG AF SCOTTI, JV RABINOWITZ, DL MARSDEN, BG TI NEAR MISS OF THE EARTH BY A SMALL ASTEROID SO NATURE LA English DT Article AB THE 0.91-m Spacewatch Telescope, on Kitt Peak in Arizona, is being used to search for new Earth-approaching asteroids. On the night of 18 January 1991 a streaked image extending over more than 161 arcseconds was recorded. Further observations over the next 4.6 hours showed that the images were of an object travelling in an independent orbit around the Sun; it was given the asteroidal designation 1991 BA. Orbital computations, presented here, indicate that 1991 BA was only 0.0053 AU from the Earth at the time of discovery, closing to 0.0033 AU at the last detection. Extrapolation of the calculated orbit shows that the object passed only 0.0011 AU (170,000 km) from the Earth 12 hours after it was found. The observed brightness translates into an absolute visual magnitude 28.9, corresponding to a diameter of only 5-10 m. 1991 BA is the closest and smallest asteroid yet observed outside the Earth's atmosphere. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP SCOTTI, JV (reprint author), UNIV ARIZONA,LUNAR & PLANETARY LAB,TUCSON,AZ 85721, USA. NR 12 TC 18 Z9 18 U1 1 U2 3 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD NOV 28 PY 1991 VL 354 IS 6351 BP 287 EP 289 DI 10.1038/354287a0 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA GT204 UT WOS:A1991GT20400040 ER PT J AU THOMSON, JD HERRE, EA HAMRICK, JL STONE, JL AF THOMSON, JD HERRE, EA HAMRICK, JL STONE, JL TI GENETIC MOSAICS IN STRANGLER FIG TREES - IMPLICATIONS FOR TROPICAL CONSERVATION SO SCIENCE LA English DT Article ID BARRO-COLORADO-ISLAND; FICUS; CONSEQUENCES; COEVOLUTION; PHENOLOGY; EVOLUTION; PANAMA AB Single trees of six species of strangler figs (Ficus spp., Moraceae) in Panama were found to be made up of multiple genotypes, presumably formed by the fusion of different individuals. The phenomenon is frequent enough that strangler fig populations will contain considerably more genetic variation than would be expected from the number of trees. How this cryptic variation affects populations depends on the flowering phenology of composite trees. If the genetically different portions of trees flower asynchronously, populations of pollinating wasps may be more resistant to low host population sizes than previously thought. If different portions flower synchronously, attempts to infer mating-system parameters from the parentage of fruit crops will be misleading. The fruiting of figs, which are considered a keystone species in tropical forests, is important for maintaining biodiversity but is also particularly susceptible to failure at small population sizes. It is therefore important to know both the number of trees and the number of genotypes in a population. C1 DEPT BOT,ATHENS,GA 30602. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. DEPT GENET,ATHENS,GA 30602. RP THOMSON, JD (reprint author), SUNY STONY BROOK,DEPT ECOL & EVOLUT,STONY BROOK,NY 11794, USA. NR 20 TC 27 Z9 28 U1 3 U2 22 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD NOV 22 PY 1991 VL 254 IS 5035 BP 1214 EP 1216 DI 10.1126/science.254.5035.1214 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA GQ834 UT WOS:A1991GQ83400051 PM 17776412 ER PT J AU TONG, CYE WU, K AF TONG, CYE WU, K TI PROPAGATION CHARACTERISTICS OF THIN-FILM SUPERCONDUCTING MICROSTRIP LINE FOR TERAHERTZ APPLICATIONS SO ELECTRONICS LETTERS LA English DT Article DE MICROSTRIP; SUPERCONDUCTORS; SUPERCONDUCTING DEVICES; TRANSMISSION LINES ID PLANAR AB Thin film superconducting microstrip line has been studied using the method of lines. By modelling the superconductor with its complex conductivity, the approach explicitly includes the effects of the finite thickness of the superconducting strip which is comparable to that of the dielectric layer. The solution confirms that this type of guiding structure is ideally suited to terahertz applications. C1 UNIV VICTORIA,DEPT ELECT & COMP ENGN,VICTORIA V8W 3P6,BC,CANADA. RP TONG, CYE (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Tong, Edward/0000-0002-7736-4203 NR 11 TC 4 Z9 4 U1 0 U2 2 PU IEE-INST ELEC ENG PI HERTFORD PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD, ENGLAND SG1 2AY SN 0013-5194 J9 ELECTRON LETT JI Electron. Lett. PD NOV 21 PY 1991 VL 27 IS 24 BP 2299 EP 2300 DI 10.1049/el:19911421 PG 2 WC Engineering, Electrical & Electronic SC Engineering GA GU370 UT WOS:A1991GU37000061 ER PT J AU VOGELEY, MS GELLER, MJ HUCHRA, JP AF VOGELEY, MS GELLER, MJ HUCHRA, JP TI VOID STATISTICS OF THE CFA REDSHIFT SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY; GALAXIES, CLUSTERING ID LARGE-SCALE STRUCTURE; COLD DARK MATTER; POINT CORRELATION-FUNCTIONS; EXTRAGALACTIC OBJECTS; LUMINOSITY FUNCTION; GALAXY DISTRIBUTION; SHANE-WIRTANEN; SURVEY SLICES; UNIVERSE; DENSITY AB We study clustering properties of two samples from the CfA redshift survey each containing approximately 2500 galaxies. Comparison of the velocity distributions using a K-S test reveals structure on scales comparable with the extent of the survey. We use the void probability function (VPF) for these samples to examine the structure and to test for scaling relations in the galaxy distribution. Using moments of galaxy counts we calculate the galaxy correlation function and find that xiBAR(R) = <(delta-rho/rho)2> = 1 on a scale R = 7h-1 Mpc. The shape and amplitude of the correlation function roughly agree with previous determinations. The VPFs for distance-limited samples of the CfA survey do not match the scaling relation predicted by hierarchical clustering models. On scales less-than-or-similar-to 10h-1 Mpc, the VPFs for these samples roughly follow the hierarchical pattern. However, on scales greater-than-or-similar-to 10h-1 Mpc we find large variations between the VPFs for distance-limited subsamples of each survey region. Variations in the VPF for different samples depend on the different large-scale features and sampling density in these samples. We introduce a variant of the VPF which uses nearly all the data in magnitude-limited samples. This statistic, P0(NBAR), accounts for the variation of the sampling density with velocity in a magnitude-limited survey. For samples with a range of limiting apparent magnitude, P0(NBAR) behaves like P0 is-proportional-to exp (- NBAR/N(cluster) where N(cluster) almost-equal-to 7-8. Agreement of P0 for NBAR less-than-or-similar-to 15 indicates that the Northern and Southern galactic regions of the survey are similarly clustered on scales less-than-or-similar-to 10h-1 Mpc. The similar behavior of P0 for the two survey regions, which include qualitatively different large-scale features, suggests that this statistic is robust with respect to variations in individual structures within the survey and may provide a useful discriminant among n-body models. RP VOGELEY, MS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 61 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 NOV 20 PY 1991 VL 382 IS 1 BP 44 EP 54 DI 10.1086/170691 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GP641 UT WOS:A1991GP64100005 ER PT J AU TRINCHIERI, G FABBIANO, G AF TRINCHIERI, G FABBIANO, G TI THE DISCRETE X-RAY SOURCE POPULATION IN M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (M31); GALAXIES, INTERSTELLAR MATTER; GALAXIES, X-RAYS ID EARLY-TYPE GALAXIES; IONIZED-GAS; BULGE; VARIABILITY; SAMPLE AB We report the results of the analysis of the entire set of Einstein imaging observations of M31. We detect 108 individual X-ray sources, with (0.2-4.0 keV) luminosities ranging from 5 x 10(36) ergs s-1 to above 10(38) ergs s-1 at the distance of M31 (690 kpc). Fourteen of these sources are luminous enough to perform a spectral fit of the X-ray data. Fourteen sources are found to vary between Einstein observations, in addition to the two sources already reported by Collura, Reale, and Peres. We do not find any substantial difference between the luminosity distributions of X-ray sources in the bulge and in the disk, contrary to earlier reports. The luminosity distribution of these X-ray sources is well represented by a power law with slopes between -1 and -0.66 (1-sigma). About 20%-30% of the counts detected in the bulge region are not accounted for by the individual sources. This additional emission can be easily explained by the integrated contribution of sources below the detection threshold. Nevertheless, if we use this component to set a conservative upper limit on the emission of a putative gaseous component, we find that no more than approximately 2 x 10(6) M. of hot gas can be present in the bulge. This limit is consistent with optical, H I, and IR estimates and implies the presence of galactic winds in M31. We present contour maps of the X-ray emission in the central region, and we compare the radial distribution of the surface brightness with the optical profiles. This comparison suggests that the disk is relatively underluminous in X-rays, relative to the stellar content. We compare the spatial distribution of bulge sources with that of optical novae and with emission-line images of the bulge. These comparisons constrain models of formation of low-mass X-ray binaries. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP TRINCHIERI, G (reprint author), OSSERV ASTROFIS ARCETRI,LARGO E FERMI 5,I-50125 FLORENCE,ITALY. NR 42 TC 104 Z9 104 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 1991 VL 382 IS 1 BP 82 EP & DI 10.1086/170696 PN 1 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GP641 UT WOS:A1991GP64100010 ER PT J AU DAVIES, MB BENZ, W HILLS, JG AF DAVIES, MB BENZ, W HILLS, JG TI STELLAR ENCOUNTERS INVOLVING RED GIANTS IN GLOBULAR-CLUSTER CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE CLUSTERS, GLOBULAR; STARS, LATE-TYPE; STARS, STELLAR DYNAMICS ID 3-DIMENSIONAL HYDRODYNAMICAL SIMULATIONS; MAIN-SEQUENCE; WHITE-DWARFS; BINARY STARS; EVOLUTION; COLLISIONS; SUPERNOVAE AB Collisions between a 0.8 M. red giant and impactors of mass 0.4 and 0.6 M. are simulated using a three-dimensional smoothed particle hydrodynamics (SPH) code. The red giant is modeled as a massive core surrounded by a gaseous envelope, while the impactor, assumed to be a white dwarf or a main-sequence star, is treated as single particle. Encounters at various impact parameters and with relative velocities pertinent to globular clusters (10 km s-1) are studied. The effect of the encounter on the red giant depends strongly on the impact parameter. We find that if the impactor passes within twice the radius of the red giant (2R(RG)), mass loss occurs from the red giant envelope and both objects are left bound in elliptical orbits. Calculations suggest that if the impactor has an initial distance at closest approach of approximately 1.6R(RG) or less, the impactor will spiral in to the red giant envelope on subsequent periastron passages. For bound systems with a greater separation, the orbit may circularize with a radius approximately double that of the initial encounter. In both cases the system will undergo a common envelope phase: in the latter case the red giant will eventually fill its Roche lobe as it expands up the giant branch. In the case of a sufficiently small closest approach (R(min) < R(RG)), the impactor is immediately captured by the core of the red giant. Both objects form a binary system orbiting inside a common envelope formed from the original envelope of the giant. Acting like an "eggbeater," the system spins up the surrounding gas, leading to further mass loss while spiraling together. With a white drawf impactor, the likely outcome of the common envelope phase will be a tight white dwarf/white dwarf binary that will merge in less than a Hubble time. In the case of a main-sequence star impactor, a tight binary comprised of the main-sequence star and a white dwarf (the red giant core) is likely to be produced, with the main-sequence star filling its Roche lobe. C1 UNIV CALIF LOS ALAMOS SCI LAB,DIV THEORET,LOS ALAMOS,NM 87545. RP DAVIES, MB (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 27 TC 68 Z9 68 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 10 PY 1991 VL 381 IS 2 BP 449 EP 461 DI 10.1086/170668 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GN112 UT WOS:A1991GN11200011 ER PT J AU CORNELL, J AF CORNELL, J TI NEWS WITHOUT CIRCULATION - THE IGNORED THIRD-WORLD SO ARBOR-CIENCIA PENSAMIENTO Y CULTURA LA Spanish DT Article RP CORNELL, J (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU LIBRERIA CIENTIFICA MEDINACELI PI MADRID PA DUQUE DE MEDINACELI 4, 14 MADRID, SPAIN SN 0210-1963 J9 ARBOR JI Arbor-Cienc. Pensam. Cult. PD NOV-DEC PY 1991 VL 140 IS 551-52 BP 15 EP 26 PG 12 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA HG610 UT WOS:A1991HG61000002 ER PT J AU LIGHTMAN, AP AF LIGHTMAN, AP TI SCIENCE AND LITERATURE SO ARBOR-CIENCIA PENSAMIENTO Y CULTURA LA Spanish DT Article RP LIGHTMAN, AP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU LIBRERIA CIENTIFICA MEDINACELI PI MADRID PA DUQUE DE MEDINACELI 4, 14 MADRID, SPAIN SN 0210-1963 J9 ARBOR JI Arbor-Cienc. Pensam. Cult. PD NOV-DEC PY 1991 VL 140 IS 551-52 BP 51 EP 58 PG 8 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA HG610 UT WOS:A1991HG61000005 ER PT J AU BEERS, TC FORMAN, W HUCHRA, JP JONES, C GEBHARDT, K AF BEERS, TC FORMAN, W HUCHRA, JP JONES, C GEBHARDT, K TI A DYNAMIC ANALYSIS OF 12 CLUSTERS OF GALAXIES SO ASTRONOMICAL JOURNAL LA English DT Article ID RICH CLUSTERS; BOUND POPULATIONS; VELOCITY DATA; CD GALAXIES; EVOLUTION; CATALOG; SUBSTRUCTURE; SAMPLE; SCALE AB We report 428 new redshifts for galaxies in the vicinity of twelve rich clusters. The clusters we have observed-A85, A569, A957, A1069, A1185, A1750, A1991, A2063, A2440, A2589, A2593, and A2657-exhibit a wide range of optical and x-ray properties, from extremely luminous x-ray emitters with apparently dense central regions, to clusters which exhibit a bimodal or clumpy appearance in their galaxy and x-ray surface brightness distributions. Several of the clusters (and subclusters) contain dominant galaxies with multiple nuclei embedded in an extended luminous halo. We discuss the velocity distributions for each of these clusters, and obtain dynamical mass estimates. Application of a simple two-body dynamical model has implications for several of the clusters studied. The subclusters in A569 are likely to be gravitationally bound to one another and presently coming together prior to the final relaxation of the system. The formal result of the two-body analysis for A957 indicates that the system is not gravitationally bound, but the uncertainty in the radial velocity difference between the subclusters allows for bound solutions with equal probability. The cluster A1069, which appears to be a double cluster in a previously published map of the galaxy distribution, is shown to be a clear case of foreground/background superposition. The two main subclusters in A1750 are apparently gravitationally bound to one another and infalling, although unbound solutions are also allowed with roughly a 10% probability. The cluster A2440 is shown to be comprised of two primary subclusters which are gravitationally bound to each other, and in the process of infall. The clusters A2589 and A2593 apparently form a bound pair which are presently expanding away from one another prior to turn around, although unbound solutions are also allowed with somewhat lower likelihood. We consider our measurements of the relative velocities of brightest cluster member galaxies (usually morphologically classified as D or cD) with respect to the remaining galaxies in each cluster, and argue that when significantly large differences are observed this is strong evidence for the existence of substructure within the cluster. Based on the significant velocity offsets of the D/cD galaxies in the clusters A85, A1185, A2063, and A2589, we expect that the substructure will be revealed in these clusters when more complete spatial and velocity data become available. The subcluster A957W may also harbor unresolved substructure. Finally, we consider the distribution of measured velocity scales for clusters in our sample, and show that velocity dispersions derived when substructure is present (but ignored) can be high by a factor as large as 2. We conclude that the limiting dispersions of rich clusters is still not well constrained. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP BEERS, TC (reprint author), MICHIGAN STATE UNIV,DEPT PHYS & ASTRON,E LANSING,MI 48824, USA. NR 62 TC 156 Z9 157 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 NOV PY 1991 VL 102 IS 5 BP 1581 EP 1609 DI 10.1086/115982 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GL774 UT WOS:A1991GL77400001 ER PT J AU CARILLI, CL BARTEL, N LINFIELD, RP AF CARILLI, CL BARTEL, N LINFIELD, RP TI VLBI OBSERVATIONS OF THE NUCLEAR JET IN CYGNUS-A SO ASTRONOMICAL JOURNAL LA English DT Article ID RADIO-SOURCES; MOTION; GALAXY AB We present an image of the "core" and inner jet of Cygnus A at an angular resolution of 2 mas obtained from Mark III VLBI observations at 6 cm wavelength with an array of nine antennas. The core is resolved, at least partly due to its being broadened by scattering in the Galactic interstellar medium. The jet has several condensations out to a distance of approximately 25 mas from the core and has a fairly constant FWHM of approximately 2.2 mas. The parsec-scale jet points toward the arcsec-scale jet observed with the VLA to within 4-degrees. The ratio between the flux density of the jet and that of the counterjet is > 15:1. From a comparison with an earlier VLBI image of Cygnus A, we find an upper limit to the apparent velocity of the brightest knot in the jet of about 2c, where c is the speed of light (for H0 = 60 km s-1 Mpc-1,q0 = 0). C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. RP CARILLI, CL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 32 TC 18 Z9 18 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 NOV PY 1991 VL 102 IS 5 BP 1691 EP 1695 DI 10.1086/115988 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GL774 UT WOS:A1991GL77400007 ER PT J AU FABRICANT, DG MCCLINTOCK, JE BAUTZ, MW AF FABRICANT, DG MCCLINTOCK, JE BAUTZ, MW TI GALAXY EVOLUTION IN DISTANT, X-RAY-SELECTED CLUSTERS OF GALAXIES .1. CL 1358+6245 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERING; GALAXIES, PHOTOMETRY; GALAXIES, STRUCTURE; GALAXIES, X-RAYS ID MEDIUM-SENSITIVITY SURVEY; RICH CLUSTERS; VELOCITY DISPERSIONS; REDSHIFT CLUSTERS; NEARBY CLUSTERS; STANDARD STARS; ABELL CLUSTERS; COOLING FLOWS; COMA CLUSTER; PHOTOMETRY AB A photometric and spectroscopic survey of a cluster of galaxies at z = 0.327 is presented. This is the first cluster we have studied from our sample of five distant, high X-ray luminosity clusters, which have been selected from the Einstein Observatory Medium Sensitivity Survey Catalog. Studies by others of optically selected clusters at z > 0.2 have led to the important conclusion that the galaxy population in such clusters is markedly different than in comparable, nearby clusters. Our study of the galaxy population in an X-ray-selected sample will allow us to assess the importance of optical selection biases. In addition, the use of different selection criteria may help to clarify the causes of galaxy evolution in clusters. We have obtained V, R, and I photometry of 288 stars and galaxies in a region 5.'7 x 6.'5 which is approximately centered on the dominant galaxy at the cluster center. The photometry is complete to rest band M(V) = -19.5 (19 kpc diameter aperture). We have obtained the spectra of 70 galaxies which lie within approximately 2' (approximately R30) of the cluster center, to a magnitude limit of M(V) approximately -20.5; approximately 90% of these galaxies are cluster members. The large velocity dispersion of the cluster, 1125(-94)+126 km s-1, is consistent with its high X-ray luminosity, approximately 7 x 10(44) ergs s-1 (0.2-4.5 keV). We find evidence for evolution of the galaxy population as compared with clusters at the present epoch. Approximately 17% of the cluster members have "E + A" spectra, with strong Balmer absorption lines, the normal absorption features of E/SO galaxies, and no emission lines. In comparable nearby clusters, on the other hand only approximately 1% of the galaxies have E + A spectra. Approximately 10% of the cluster members have emission-line spectra compared with approximately 5% in present epoch clusters. The total "active" population, defined as the sum of the E + A and emission-line populations, represents approximately 27% of the population in the cluster core. These results are consistent with the size of the active population found in optically selected samples of distant clusters at similar redshifts. C1 MIT,CTR SPACE RES,CAMBRIDGE,MA 02139. RP FABRICANT, DG (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 70 TC 86 Z9 86 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 1991 VL 381 IS 1 BP 33 EP & DI 10.1086/170626 PN 1 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GM575 UT WOS:A1991GM57500004 ER PT J AU GOLDSTEIN, JJ MUMMA, MJ KOSTIUK, T DEMING, D ESPENAK, F ZIPOY, D AF GOLDSTEIN, JJ MUMMA, MJ KOSTIUK, T DEMING, D ESPENAK, F ZIPOY, D TI ABSOLUTE WIND VELOCITIES IN THE LOWER THERMOSPHERE OF VENUS USING INFRARED HETERODYNE SPECTROSCOPY SO ICARUS LA English DT Article ID NATURAL LASER-EMISSION; GENERAL-CIRCULATION; NIGHT AIRGLOW; ZONAL WINDS; TEMPERATURE; ATMOSPHERE; MESOSPHERE; MODEL; TRANSITIONS; DYNAMICS C1 NASA,GODDARD SPACE FLIGHT CTR,EXTRATERR PHYS LAB,PLANETARY SYST BRANCH,GREENBELT,MD 20771. UNIV MARYLAND,ASTRON PROGRAM,COLLEGE PK,MD 20742. RP GOLDSTEIN, JJ (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560, USA. RI mumma, michael/I-2764-2013; Kostiuk, Theodor/A-3077-2014 NR 44 TC 49 Z9 49 U1 3 U2 3 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD NOV PY 1991 VL 94 IS 1 BP 45 EP 63 DI 10.1016/0019-1035(91)90140-O PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GR704 UT WOS:A1991GR70400004 ER PT J AU CHERNIN, LM BLUNDELL, R TONG, CYE AF CHERNIN, LM BLUNDELL, R TONG, CYE TI HARMONIC EFFECTS IN SUPERCONDUCTING TUNNEL JUNCTION MIXERS SO INTERNATIONAL JOURNAL OF INFRARED AND MILLIMETER WAVES LA English DT Article AB We have performed five-port model simulations of a superconducting tunnel junction mixer based on the quantum mixer theory. In particular, we have investigated the performance of a fundamental mixer as a function of the mixer omega-CR product and the embedding admittance at the 2nd harmonic. As expected, when the admittance at the second harmonic tunes out the junction capacitance, harmonic conversion is most significant. We show that there are two main effects of reducing the omega-CR product: (1) the mixer becomes easier to tune as the range of admittances over which conversion gain is obtained increases, and (2) 2nd harmonic conversion becomes much more significant relative to fundamental conversion. Our simulations indicate that, in the absence of Josephson effects, an optimal fundamental mixer would have as small a omega-CR product as possible and capacitive terminations at the higher harmonics. RP CHERNIN, LM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Tong, Edward/0000-0002-7736-4203 NR 7 TC 2 Z9 2 U1 0 U2 1 PU PLENUM PUBL CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 SN 0195-9271 J9 INT J INFRARED MILLI JI Int. J. Infrared Millimeter Waves PD NOV PY 1991 VL 12 IS 11 BP 1265 EP 1273 DI 10.1007/BF01014684 PG 9 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA GM378 UT WOS:A1991GM37800004 ER PT J AU JACOBBERGER, PA HOOPER, DM AF JACOBBERGER, PA HOOPER, DM TI GEOMORPHOLOGY AND REFLECTANCE PATTERNS OF VEGETATION-COVERED DUNES AT THE TSODILO HILLS, NORTH-WEST BOTSWANA SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID HERBACEOUS VEGETATION; SOUTHERN-AFRICA; KALAHARI; RANGELANDS AB Seasonal reflectance variations in semi-arid environments provide a means of assessing vegetation health and density as well as monitoring landform processes. We have used multi-temporal Landsat Thematic Mapper scenes with field measurements to map geomorphology and vegetation density in a stabilized dune environment and to measure seasonal reflectance changes for a series of ten geomorphological and vegetation units on the Kalahari-age linear dunes near the Tsodilo Hills, northwestern Botswana. Dune morphology is degraded and dunes are stabilized by mopane woodland vegetation. Units were chosen based on differences in landform and proportion of trees, forbs and bare soil. Reflectance curves and Normalized Difference Vegetation Indices (NDVI) calculated for December 1986 and March, June and August 1987 show that dune crests have the strongest seasonal variability in colour and brightness. Interdune corridors show a few percentage variation and sandy plains units in general showed little seasonal variation. The geomorphological link with reflectance and NDVI values may be due to biomass production and zoning of vegetation with slope, drainage and subtle soil differences. RP JACOBBERGER, PA (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,CTR EARTH & PLANETARY STUDIES,WASHINGTON,DC 20560, USA. NR 22 TC 7 Z9 7 U1 1 U2 2 PU TAYLOR & FRANCIS LTD PI LONDON PA ONE GUNDPOWDER SQUARE, LONDON, ENGLAND EC4A 3DE SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD NOV PY 1991 VL 12 IS 11 BP 2321 EP 2342 PG 22 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA GM647 UT WOS:A1991GM64700011 ER PT J AU ALEXANDER, SA COLDWELL, RL MONKHORST, HJ MORGAN, JD AF ALEXANDER, SA COLDWELL, RL MONKHORST, HJ MORGAN, JD TI MONTE-CARLO EIGENVALUE AND VARIANCE ESTIMATES FROM SEVERAL FUNCTIONAL OPTIMIZATIONS SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CONFIGURATION INTERACTION CALCULATIONS; POTENTIAL-ENERGY SURFACE; TRANSFORM WAVE-FUNCTIONS; HELIUM-LIKE IONS; GAUSSIAN FUNCTIONS; QUANTUM-CHEMISTRY; HYDROGEN MOLECULE; RANDOM-WALK; STATE; CONVERGENCE AB Using several simple systems as examples, we show that the choice of optimization functional can have a significant influence on the accuracy of variational Monte Carlo calculations. In addition, we demonstrate that the Monte Carlo analog of the Rayleigh-Ritz procedure, which explicitly orthogonalizes ground and excited states, can be used to produce accurate eigenvalue and variance estimates of excited states. C1 HARVARD UNIV,DEPT CHEM & PHYS,CAMBRIDGE,MA 02138. HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. UNIV DELAWARE,DEPT PHYS & ASTRON,NEWARK,DE 19716. INST ASTROPHYS & PLANETARY EXPLORAT,ALACHUA,FL 32615. UNIV FLORIDA,QUANTUM THEORY PROJECT,GAINESVILLE,FL 32611. RP ALEXANDER, SA (reprint author), UNIV FLORIDA,DEPT PHYS,GAINESVILLE,FL 32611, USA. NR 51 TC 48 Z9 48 U1 0 U2 3 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 1 PY 1991 VL 95 IS 9 BP 6622 EP 6633 DI 10.1063/1.461532 PG 12 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA GL753 UT WOS:A1991GL75300045 ER PT J AU CHEUNG, ASC LI, JPL WONG, TW LI, MG RADFORD, HE AF CHEUNG, ASC LI, JPL WONG, TW LI, MG RADFORD, HE TI FAR-INFRARED LASER MAGNETIC-RESONANCE SPECTRUM OF SO IN THE X3-SIGMA- STATE SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Note ID SULFUR MONOXIDE C1 MIT,DEPT CHEM,CAMBRIDGE,MA 02139. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP CHEUNG, ASC (reprint author), UNIV HONG KONG,DEPT CHEM,POKFULAM RD,HONG KONG,HONG KONG. NR 24 TC 0 Z9 0 U1 2 U2 6 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD NOV PY 1991 VL 150 IS 1 BP 285 EP 288 DI 10.1016/0022-2852(91)90213-T PG 4 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA GL971 UT WOS:A1991GL97100025 ER PT J AU BARNARD, JL AF BARNARD, JL TI AMPHIPODOLOGICAL AGREEMENT WITH PLATNICK SO JOURNAL OF NATURAL HISTORY LA English DT Letter RP BARNARD, JL (reprint author), SMITHSONIAN INST,JLB NMNH STOP 163,WASHINGTON,DC 20560, USA. NR 3 TC 6 Z9 6 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI LONDON PA ONE GUNDPOWDER SQUARE, LONDON, ENGLAND EC4A 3DE SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PD NOV-DEC PY 1991 VL 25 IS 6 BP 1675 EP 1676 DI 10.1080/00222939100771031 PG 2 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA GZ667 UT WOS:A1991GZ66700016 ER PT J AU AMBLER, JW FERRARI, FD FORNSHELL, JA AF AMBLER, JW FERRARI, FD FORNSHELL, JA TI POPULATION-STRUCTURE AND SWARM FORMATION OF THE CYCLOPOID COPEPOD DIOITHONA-OCULATA NEAR MANGROVE CAYS SO JOURNAL OF PLANKTON RESEARCH LA English DT Article ID RED-SEA BREAM; SHIJIKI BAY; AGGREGATIONS; BEHAVIOR; WATERS AB The cyclopoid copepod Dioithona oculata forms swarms in water < 30 cm deep among prop roots of red mangroves (Rhizophora mangle) which fringe protected areas of two lagoonal cays, Twin Cays, Belize. During 7 of 8 months surveyed by in situ observation, swarms were present but differed in size from small cylindrical swarms (5-10 cm diameter) to bands extending up to 1200 m. Swarms were never observed at night. Swarms formed at dawn when light intensities reached an average value of 13.82 (log10 quanta cm-2 s-1) and dispersed at dusk at similar intensities. Swarms observed in June formed earlier and dispersed later in the day than swarms observed in January; their swarming behavior followed seasonal changes in light intensity. Mean dioithonan density in swarms (10 ml-1) was much higher than the mean density (0.15 ml-1) of non-swarming dioithonans around mangrove prop roots. In open water 3-5 m away from the mangroves, mean dioithonan density was 7.9 x 10(-5) ml-1 during the day, and 2.68 x 10(-3) ml-1 at night. Swarms were composed predominantly of adults and copepodid stages IV and V, although younger copepodid stages could be present. Nauplii were never present. The 'average copepodid stage' for all 95 swarms sampled was 5.3, where 6.0 represents a swarm with only adults. In open water 3-5 m away from the mangroves, the youngest copepodids (stage one) dominated the dioithonan population during the day. At night when swarms dispersed to open waters, average copepodid stage was higher (3.5) compared with the day value (1.2) in open waters. Although densities in swarms were higher in June than January, average copepodid stage in June was higher (5.6) than that in January (4.9). A higher percentage of adults were females during June than January. Therefore higher densities did not result from increases of smaller stages in swarms, but perhaps changes in behavior or population structure. C1 TEXAS A&M UNIV SYST,DEPT OCEANOG,COLLEGE STN,TX 77843. SMITHSONIAN INST,MUSEUM NAT HIST,SMITHSONIAN OCEANOG SORTING CTR,WASHINGTON,DC 20560. THOMAS JEFFERSON HIGH SCH SCI & TECHNOL,ALEXANDRIA,VA 22312. NR 30 TC 45 Z9 48 U1 0 U2 0 PU OXFORD UNIV PRESS UNITED KINGDOM PI OXFORD PA WALTON ST JOURNALS DEPT, OXFORD, ENGLAND OX2 6DP SN 0142-7873 J9 J PLANKTON RES JI J. Plankton Res. PD NOV PY 1991 VL 13 IS 6 BP 1257 EP 1272 DI 10.1093/plankt/13.6.1257 PG 16 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA GM245 UT WOS:A1991GM24500009 ER PT J AU KUTEPOV, AA KUNZE, D HUMMER, DG RYBICKI, GB AF KUTEPOV, AA KUNZE, D HUMMER, DG RYBICKI, GB TI THE SOLUTION OF RADIATIVE-TRANSFER PROBLEMS IN MOLECULAR BANDS WITHOUT THE LTE ASSUMPTION BY ACCELERATED LAMBDA ITERATION METHODS SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article ID OPERATORS; LEVEL AB An iterative method based on the use of approximate transfer (or LAMBDA) operators, which was designed initially to solve multilevel NLTE line formation problems in stellar atmospheres, is adapted and applied to the solution of the NLTE molecular band radiative transfer in planetary atmospheres. The matrices to be constructed and inverted are much smaller than those used in the traditional Curtis matrix technique, which makes possible the treatment of more realistic problems (including rotational NLTE, overlapping of lines in the bands and overlapping of bands with continuua) using relatively small computers. This technique converges much more rapidly than straightforward iteration between the transfer equation and the equations of statistical equilibrium (LAMBDA-iteration). A test application of this new technique to the solution of NLTE radiative transfer problems for optically-thick and thin bands (the 4.3-mu-m CO2 band in the Venusian atmosphere and the 4.7 and 2.3-mu-m CO bands in the Earth's atmosphere) is described. The necessity for careful treatment of rotational NLTE in weak lines of the 4.3-mu-m CO2 fundamental band is shown. The possible influence of neglecting or treating approximately the CO2 10-mu-m laser transitions and also effects of the overlap of the 4.3-mu-m CO2 with the continuum are investigated. The rotational NLTE effects in the 4.7-mu-m CO band in the upper Earth's atmosphere are estimated. C1 UNIV KARLSRUHE,KERNFORSCHUNGZENTRUM,INST METEOROL & KLIMAFORSCH,W-7500 KARLSRUHE 1,GERMANY. NATL INST STAND & TECHNOL,BOULDER,CO 80309. UNIV COLORADO,JOINT INST LAB ASTROPHYS,BOULDER,CO 80309. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. MAX PLANCK INST ASTROPHYS,W-8046 GARCHING,GERMANY. RP KUTEPOV, AA (reprint author), UNIV MUNICH,INST ASTRON & ASTROPHYS,SCHEINERSTR 1,W-8000 MUNICH 80,GERMANY. NR 17 TC 14 Z9 14 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV PY 1991 VL 46 IS 5 BP 347 EP 365 DI 10.1016/0022-4073(91)90038-R PG 19 WC Optics; Spectroscopy SC Optics; Spectroscopy GA GR458 UT WOS:A1991GR45800001 ER PT J AU BROWN, JL WILDT, DE RAATH, JR DEVOS, V JANSSEN, DL CITINO, SB HOWARD, JG BUSH, M AF BROWN, JL WILDT, DE RAATH, JR DEVOS, V JANSSEN, DL CITINO, SB HOWARD, JG BUSH, M TI SEASONAL-VARIATION IN PITUITARY GONADAL-FUNCTION IN FREE-RANGING IMPALA (AEPYCEROS-MELAMPUS) SO JOURNAL OF REPRODUCTION AND FERTILITY LA English DT Article DE IMPALA; LH; FSH; TESTOSTERONE; TESTIS; RECEPTORS ID LUTEINIZING-HORMONE; CERVUS-ELAPHUS; RED DEER; HERPESTES-AUROPUNCTATUS; TESTOSTERONE SECRETION; GONADOTROPIN-SECRETION; OVARIECTOMIZED EWES; LH; RESPONSIVENESS; FSH AB Blood, testicular biopsies and electroejaculates were collected from adult male impala, free-ranging in the Kruger National Park (Republic of South Africa), during the breeding (rut; April-May) and nonbreeding (September-October) seasons. Blood samples were collected at 5-min intervals for 120 min from anaesthetized males (n = 7 impala/group) treated intravenously with saline, gonadotrophin-releasing hormone (GnRH: 1-mu-g/kg body weight) or human chorionic gonadotrophin (hCG: 10 or 30 iu/kg). Semen was collected from six more animals during the breeding season and 12 animals during the nonbreeding season using a standardized electroejaculation protocol. Ejaculates obtained during the nonbreeding season were of inferior quality to those collected during the breeding season, and were characterized by lower sperm concentrations, poorer sperm motility and more morphologically abnormal sperm forms. Within season, there were no differences in testosterone secretion between the two hCG doses, and these responses were similar to those observed after GnRH, but during the rut, testosterone secretion stimulated by both GnRH and hCG was approximately nine times greater than during the nonbreeding season. This seasonal increase in testosterone production was associated with a doubling in testicular volume and concentrations of luteinizing hormone (LH) receptors. Although concentrations of testicular follicle-stimulating hormone (FSH) receptors were similar between seasons, receptor content increased during rut as a result of increased testicular volume. In contrast to testosterone secretion, basal LH and FSH secretions were unaffected by season and GnRH-induced gonadotrophin secretion was reduced during rut. These data indicate that: (i) seminal quality in free-ranging impala undergoes seasonal changes coincident with alterations in testicular steroidogenic activity, and (ii) the increased testosterone secretion observed during rut is associated with increased testicular sensitivity to LH (via increased gonadotrophin receptors) rather than to increased circulating gonadotrophin concentrations or pituitary responsiveness to GnRH. C1 SAN DIEGO ZOOL SOC,DEPT VET SERV,SAN DIEGO,CA 92112. MIAMI METRO ZOO,MIAMI,FL 33177. SMITHSONIAN INST,NATL ZOOL PK,DEPT ANIM HLTH,WASHINGTON,DC 20008. KRUGER NATL PK,SKUKUZA 1350,SOUTH AFRICA. RP BROWN, JL (reprint author), UNIFORMED SERV UNIV HLTH SCI,DEPT OBSTET & GYNECOL,BETHESDA,MD 20814, USA. NR 44 TC 8 Z9 8 U1 0 U2 3 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 NOV PY 1991 VL 93 IS 2 BP 497 EP 505 PG 9 WC Reproductive Biology SC Reproductive Biology GA HA966 UT WOS:A1991HA96600030 PM 1787471 ER PT J AU DOLAN, JR GALLEGOS, CL AF DOLAN, JR GALLEGOS, CL TI TROPHIC COUPLING OF ROTIFERS, MICROFLAGELLATES, AND BACTERIA DURING FALL MONTHS IN THE RHODE RIVER ESTUARY SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article ID PLANKTONIC BACTERIA; LABORATORY CULTURES; CHESAPEAKE BAY; SIZE; FOOD; BACTERIOPLANKTON; PHYTOPLANKTON; GROWTH; WATER; ZOOPLANKTON AB Field patterns and experimental results suggested that rotifers, by grazing heterotrophic microflagellates, may have exerted an indirect effect on bacterioplankton concentration. A rotifer population (Synchaeta sp.) oscillated out of phase with total microflagellate (autotrophic and heterotrophic) concentration, and heterotrophic microflagellate concentrations oscillated out of phase with bacterial abundance in the Rhode River (USA). Similar patterns were found in a time-course study of isolated water samples. Grazing experiments indicate that the rotifer cleared the water of both heterotrophic and autotrophic microflagellates at 10 to 16-mu-l h-1 rotifer-1. The apparent predator-prey relationships of rotifer-microflagellate and heterotrophic microflagellate-bacteria were formally defined in a model of a rotifer-microflagellate-bacteria food web using grazing and growth rates from field patterns and experiments. The model successfully mimicked field abundance patterns supporting the hypothesis that rotifers, microflagellates and bacteria form a highly interactive system in which rotifers exert an indirect effect on bacterioplankton. RP DOLAN, JR (reprint author), SMITHSONIAN ENVIRONM RES CTR, POB 28, EDGEWATER, MD 21037 USA. RI Dolan, John/A-4513-2009; OI Dolan, John/0000-0002-9454-1355; Gallegos, Charles/0000-0001-5112-0166 NR 40 TC 66 Z9 69 U1 0 U2 2 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD NOV PY 1991 VL 77 IS 2-3 BP 147 EP 156 DI 10.3354/meps077147 PG 10 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA GV756 UT WOS:A1991GV75600005 ER PT J AU BAIN, AL AF BAIN, AL TI THE MUSES MEMORY + MUSEUM ARCHIVES SO MUSEUM NEWS LA English DT Article RP BAIN, AL (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD NOV-DEC PY 1991 VL 70 IS 6 BP 36 EP 39 PG 4 WC Art SC Art GA GM881 UT WOS:A1991GM88100005 ER PT J AU GEARY, CM AF GEARY, CM TI MUSEUM IMAGE BANK - PHOTOGRAPHIC ARCHIVES OF 3 SMITHSONIAN INSTITUTION MUSEUMS SO MUSEUM NEWS LA English DT Article RP GEARY, CM (reprint author), SMITHSONIAN INST,NAT MUSEUM AFRICAN ART,WASHINGTON,DC 20560, USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD NOV-DEC PY 1991 VL 70 IS 6 BP 53 EP 57 PG 5 WC Art SC Art GA GM881 UT WOS:A1991GM88100010 ER PT J AU MYERS, CR UMRIGAR, CJ SETHNA, JP MORGAN, JD AF MYERS, CR UMRIGAR, CJ SETHNA, JP MORGAN, JD TI FOCKS EXPANSION, KATOS CUSP CONDITIONS, AND THE EXPONENTIAL ANSATZ SO PHYSICAL REVIEW A LA English DT Article ID 3-BODY ATOMIC WAVEFUNCTIONS; HELIUM ISOELECTRONIC SEQUENCE; ANALYTIC EXPANSIONS; COORDINATE SYSTEMS; WAVE-FUNCTIONS; VARIATIONAL CALCULATIONS; CONVERGENCE; STATE AB We have examined the recent solution of the Fock expansion through O(r2) for the ground state of the helium atom and have verified that it correctly treats the discontinuity in the local energy characteristic of the triple-collision point. We have also developed an exponential representation of the Fock expansion that satisfies Kato's cusp conditions for two-particle collisions even when the expansion is truncated at a finite order. C1 CORNELL UNIV,ATOM & SOLID STATE PHYS LAB,ITHACA,NY 14853. CORNELL UNIV,CORNELL THEORY CTR,ITHACA,NY 14853. HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. HARVARD UNIV,DEPT PHYS,CAMBRIDGE,MA 02138. HARVARD UNIV,DEPT CHEM,CAMBRIDGE,MA 02138. UNIV DELAWARE,DEPT PHYS & ASTRON,NEWARK,DE 19716. NR 40 TC 70 Z9 72 U1 1 U2 10 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 1 PY 1991 VL 44 IS 9 BP 5537 EP 5546 DI 10.1103/PhysRevA.44.5537 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA GP388 UT WOS:A1991GP38800025 ER PT J AU PRESNYAKOV, LP AF PRESNYAKOV, LP TI PHASE-SHIFT EQUATIONS IN THE SCATTERING-THEORY OF PARTICLES AND WAVES SO PHYSICAL REVIEW A LA English DT Article AB The phase-shift equations are derived in a form that is convenient for the analysis of both the radial Schrodinger equation and the problem of wave propagation in nonhomogeneous media. In the case of bound quantum states, the conservation condition is discussed for the sum of the classical action (or eikonal) and the phase. The expression for the reflection coefficient describes exactly two opposite limiting cases: the Fresnel reflection and the short-wavelength limit. In the case of wave propagation in symmetric media, both transmission and reflection coefficients are given as elementary functions of the phase shifts only. C1 PN LEBEDEV PHYS INST,MOSCOW 117333,USSR. RP PRESNYAKOV, LP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138, USA. NR 12 TC 13 Z9 13 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 NOV 1 PY 1991 VL 44 IS 9 BP 5636 EP 5641 DI 10.1103/PhysRevA.44.5636 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA GP388 UT WOS:A1991GP38800036 ER PT J AU GUZMAN, HM LOPEZ, JD AF GUZMAN, HM LOPEZ, JD TI DIET OF THE CORALLIVOROUS PUFFERFISH AROTHRON-MELEAGRIS (PISCES, TETRAODONTIDAE) AT GORGONA-ISLAND, COLOMBIA SO REVISTA DE BIOLOGIA TROPICAL LA English DT Article DE CORALLIVORY; COLOMBIA; CORAL REEFS; EASTERN PACIFIC AB The density and diet of Arothron meleagris and the abundance of corals are compared between Playa Blanca and La Azufrada reefs at Gorgona Island, Colombia. Corals, an important food resource for A. meleagris, are abundant after the widespread coral mortality caused by the El Nino event in 1982-83. Both puffer density and percent live coral cover were similar between reefs. The diet of A. meleagris showed strong preferences for the abundant Pocillopora spp. Arothron may affect the recovery of some eastern Pacific reefs, where the fish has been reported feeding on rare or less abundant corals. In contrast, the effect of A meleagris on Gorgona reefs may be non significant; in fact, the fish may help the process of recovery, by fragmenting and dispersing colonies while feeding on pocilloporid corals, but not feeding on rare coral species. RP GUZMAN, HM (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. NR 0 TC 16 Z9 16 U1 0 U2 1 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, COSTA RICA SN 0034-7744 J9 REV BIOL TROP JI Rev. Biol. Trop. PD NOV PY 1991 VL 39 IS 2 BP 203 EP 206 PG 4 WC Biology SC Life Sciences & Biomedicine - Other Topics GA HQ734 UT WOS:A1991HQ73400003 ER PT J AU GUZMAN, HM ROBERTSON, DR DIAZ, ML AF GUZMAN, HM ROBERTSON, DR DIAZ, ML TI DISTRIBUTION AND ABUNDANCE OF CORALS AT ISLA IGUANA, PACIFIC OF PANAMA SO REVISTA DE BIOLOGIA TROPICAL LA Spanish DT Article DE EASTERN PACIFIC; CORAL REEFS; IGUANA-ISLAND; PANAMA AB Data on the age, abundance and distribution of reef corals at the Refugio de Vida Silvestre Isla Iguana (Panama) are presented. Coral community structure of this reef, which is 16 ha in area, is similar to that in other eastern Pacific reefs in Panama. In 1989 we found a total living coral cover of 30.6% (mean total cover 36.7%) and 11 species of corals. Pocilloporids were the main reef-building corals, and represented 95% of the live coral coverage. Porites and Pavona spp. constituted 2.4% and 1.7%, respectively, of coral cover. Massive coral colonies (Porites and Pavona) such as those observed at Iguana are now rare on other reefs in Panama and apparently the eastern Pacific in general. Consequently, Iguana reef needs to be more than another "paper park". Although this reef was declared a park in 1981, effects of the lack of protection and management are obvious; large reef areas have been destroyed at a faster rate during the past three years due to human activities. RP GUZMAN, HM (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. NR 0 TC 5 Z9 5 U1 0 U2 2 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, COSTA RICA SN 0034-7744 J9 REV BIOL TROP JI Rev. Biol. Trop. PD NOV PY 1991 VL 39 IS 2 BP 225 EP 231 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA HQ734 UT WOS:A1991HQ73400007 ER PT J AU COOPER, MR KENSLEY, BF AF COOPER, MR KENSLEY, BF TI AN EARLY PLEISTOCENE DECAPOD CRUSTACEAN FAUNA FROM ZULULAND SO SOUTH AFRICAN JOURNAL OF SCIENCE LA English DT Article AB The early Pleistocene Port Durnford Formation has yielded the first substantial fossil decapod crustacean fauna to be recorded from southern Africa. The fauna is clearly of warm-water Indo-West Pacific origin, and is dominated by the portunid crab Scylla serrata (Forskal), with fewer Podophthalmus vigil (Fabricius) and Myra fugax (Fabricius). In addition, there are two xanthid crabs of Atergatis-Atergatopsis type, a single example of a portunid identified as Charybdis (Goniohellenus) cf. hoplites var. longicollis Leene, and thalassinidean burrows assigned to the ichnogenus Ophiomorpha. C1 SMITHSONIAN INST,DEPT CRUSTACEA,WASHINGTON,DC 20560. RP COOPER, MR (reprint author), UNIV DURBAN,DEPT GEOL,PRIVATE BAG X54001,DURBAN 4000,SOUTH AFRICA. NR 15 TC 6 Z9 7 U1 1 U2 3 PU BUREAU SCIENTIFIC PUBL PI PRETORIA PA P O BOX 1758, PRETORIA 0001, SOUTH AFRICA SN 0038-2353 J9 S AFR J SCI JI S. Afr. J. Sci. PD NOV-DEC PY 1991 VL 87 IS 11-12 BP 601 EP 604 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA GZ608 UT WOS:A1991GZ60800021 ER PT J AU RYAN, MJ AF RYAN, MJ TI SEXUAL SELECTION AND COMMUNICATION IN FROGS SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID BLANCHARD CRICKET FROG; PHYSALAEMUS-PUSTULOSUS; SENSORY EXPLOITATION; MATING SYSTEM; TUNGARA FROG; SIZE; COMPETITION; PERFORMANCE; PARASITES; CHOICE AB Anuran communication has been a useful model for understanding behavioral and neural aspects of species recognition. By extending this paradigm to intraspecific mate choice, and by supplementing it with studies of phylogenetics, some new advances have been made in understanding sexual selection. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP RYAN, MJ (reprint author), UNIV TEXAS,DEPT ZOOL,AUSTIN,TX 78712, USA. NR 35 TC 62 Z9 65 U1 4 U2 21 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 NOV PY 1991 VL 6 IS 11 BP 351 EP 355 DI 10.1016/0169-5347(91)90224-L PG 5 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA GM466 UT WOS:A1991GM46600005 PM 21232507 ER PT J AU HALZEN, F ZAS, E MACGIBBON, JH WEEKES, TC AF HALZEN, F ZAS, E MACGIBBON, JH WEEKES, TC TI GAMMA-RAYS AND ENERGETIC PARTICLES FROM PRIMORDIAL BLACK-HOLES SO NATURE LA English DT Review ID ASTRONOMICAL OBJECTS; NONROTATING HOLE; COSMIC STRINGS; EMISSION RATES; EARLY UNIVERSE; BURSTS; EXPLOSIONS; SEARCH; RADIATION; SPECTRUM AB Black holes of almost arbitrarily small mass may have formed in the very early Universe. Their presence today would be revealed by the energetic radiation they would produce by means of the quantum-gravitational Hawking mechanism, allowing observational limits to be set on their density today and on their past significance. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,AMADO,AZ 85645. RP HALZEN, F (reprint author), UNIV WISCONSIN,DEPT PHYS,MADISON,WI 53706, USA. RI zas, enrique/I-5556-2015 OI zas, enrique/0000-0002-4430-8117 NR 54 TC 97 Z9 100 U1 0 U2 2 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD OCT 31 PY 1991 VL 353 IS 6347 BP 807 EP 815 DI 10.1038/353807a0 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA GM732 UT WOS:A1991GM73200049 ER PT J AU MICELA, G HARNDEN, FR ROSNER, R SCIORTINO, S VAIANA, GS AF MICELA, G HARNDEN, FR ROSNER, R SCIORTINO, S VAIANA, GS TI THE DIFFUSE SOFT-X-RAY BACKGROUND AS SEEN WITH THE EINSTEIN-OBSERVATORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE X-RAYS, SOURCES ID SUPERNOVA-REMNANTS; GALACTIC RIDGE; STARS; EMISSION; QUASARS; GAS AB We present a systematic survey of the diffuse soft X-ray background as seen directly with the Einstein Observatory. Using 1633 selected 1-degrees x 1-degrees fields of view obtained by the Imaging Proportional Counter (IPC) to provide almost-equal-to 5% sky coverage, with some bias toward the Galactic plane, we are able to spatially resolve the background in the 0.16-3.5 keV spectral region on this angular scale. The moderate energy resolution of the IPC also enables us to characterize and produce maps of the background at different energies within the Einstein passband. We confirm that the Galactic ridge is not present at energies below 0.33 keV and demonstrate that the appearance of the ridge above this energy is not due to hard Galactic sources with a flux above 10(-13) ergs cm-2 s-1. We have identified a southern Galactic region, with l between 80-degrees and 180-degrees and b less than -5-degrees, where the mean background intensity has the lowest value and is homogeneous within better than 9%; the background in this region likely represents an isotropic component with mean intensity, in the (9.16-2.7 keV energy range) of almost-equal-to 19 keV cm-2 keV-1 sr-1, approximately 2.5 times more than the value extrapolated from higher energy measurements. We discuss the implications of our results for Galactic structure and for the nature of the extragalactic X-ray background. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CHICAGO,CTR ASTRON & ASTROPHYS,CHICAGO,IL 60637. UNIV CHICAGO,ENRICO FERMI INST,CHICAGO,IL 60637. RP MICELA, G (reprint author), OSSERV ASTRON PALERMO,PIAZZA PARLAMENTO 1,PALAZZO NORMANNI,I-90134 PALERMO,ITALY. NR 70 TC 12 Z9 12 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 OCT 20 PY 1991 VL 380 IS 2 BP 495 EP & DI 10.1086/170607 PN 1 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GJ954 UT WOS:A1991GJ95400020 ER PT J AU PAVLOV, GG BEZCHASTNOV, VG MESZAROS, P ALEXANDER, SG AF PAVLOV, GG BEZCHASTNOV, VG MESZAROS, P ALEXANDER, SG TI RADIATIVE WIDTHS AND SPLITTING OF CYCLOTRON LINES IN SUPERSTRONG MAGNETIC-FIELDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC PROCESSES; MAGNETIC FIELDS; RADIATION MECHANISMS; STARS, NEUTRON; X-RAY, SPECTRA ID GAMMA-RAY BURSTS; ABSORPTION FEATURE; ONE-PHOTON; EMISSION; SPECTRUM; SCATTERING; PLASMAS; GINGA AB We calculate the radiative line widths of the Landau levels in a superstrong magnetic field and give simple analytic expressions and fits for these which are valid over a wide range of the principal quantum number and the magnetic field strength. If one does not allow for QED corrections, all levels but the first are doubly degenerate, corresponding to the two possible spin projections. However, the interaction with the QED vacuum removes this degeneracy, leading to an energy splitting of each level which exceeds the radiative line width for low Landau levels if the magnetic field is not too large (B less-than-or-similar-to 10(13) G). We present estimations of the splitting in various limits as a function of field strength and Landau number. The possibility of observing this splitting in accreting X-ray pulsars and in gamma-ray bursters is discussed. C1 PENN STATE UNIV,DAVEY LAB 525,UNIVERSITY PK,PA 16802. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP PAVLOV, GG (reprint author), AF IOFFE PHYSICOTECH INST,LENINGRAD 194064,USSR. NR 30 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 OCT 20 PY 1991 VL 380 IS 2 BP 541 EP 549 DI 10.1086/170611 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GJ954 UT WOS:A1991GJ95400024 ER PT J AU MENTEN, KM AF MENTEN, KM TI THE DISCOVERY OF A NEW, VERY STRONG, AND WIDESPREAD INTERSTELLAR METHANOL MASER LINE SO ASTROPHYSICAL JOURNAL LA English DT Article DE INTERSTELLAR, MOLECULES; MASERS; NEBULAE, H-II REGIONS; RADIO SOURCES, LINES; STARS, FORMATION ID H-II REGIONS; OH MASERS; GHZ AB We report the first detection of very strong maser emission in the 6.6 GHz 5(1) --> 6(0) A+ transition of methanol toward a large number of star-forming regions. Essentially all 6.6 GHz maser sources found are associated with interstellar OH masers. Toward a number of sources, the 6.6 GHz emission has flux densities of several thousand Jy, exceeding that of any known OH maser. Since all known masers in the 12 GHz 2(0) --> 3-1 E transition observationally accesible to us have been found to have 6.6 GHz counterparts, the latter line is undoubtedly a Class II methanol maser transition. In all cases the 6.6 GHz luminosity exceeds the 12 GHz luminosity, often by large factors. Toward Class I methanol maser regions, the 6.6 GHz line is observed in absorption, as has been predicted by pumping models for this variety of sources. RP MENTEN, KM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 16 TC 190 Z9 193 U1 2 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 OCT 20 PY 1991 VL 380 IS 2 BP L75 EP L78 DI 10.1086/186177 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GJ956 UT WOS:A1991GJ95600008 ER PT J AU DAVID, LP FORMAN, W JONES, C AF DAVID, LP FORMAN, W JONES, C TI ENRICHMENT AND HEATING OF THE INTRACLUSTER MEDIUM THROUGH GALACTIC WINDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ABUNDANCES; GALAXIES, INTERGALACTIC MEDIUM; LUMINOSITY FUNCTION ID ELLIPTICAL GALAXIES; HOT PLASMA; CLUSTERS; GAS; EINSTEIN; EVOLUTION; SUPERNOVAE; MATTER; MODEL AB In previous papers we presented the results of simulations concerning the dynamic and X-ray evolution of the interstellar medium in elliptical galaxies. We found that all model galaxies developed Type II supernova-driven winds at early epochs and that low-luminosity ellipticals (L(B) less-than-or-similar-to 10(9.5)) maintained galactic winds for most of their lifetime. Since the galaxy population of rich regular clusters is dominated by elliptical and SO galaxies, we examine in this paper what effect these galactic winds have on the heavy element abundance and energetics of the intracluster medium. Substantial injection of highly enriched gas occurs within 3 x 10(8) yr after galaxy formation through galactic winds. The resulting iron abundance of the intracluster medium through galactic winds varies considerably with the assumed stellar initial mass function, Type I supernova rate, and the primordial mass fraction of the cluster gas. The combined mechanical luminosity of the winds from the galaxies in a cluster can greatly exceed the present optical luminosity of a cluster. Any residual gas remaining in a cluster after the cessation of galaxy formation can be heated to temperatures exceeding that produced by gravitational heating alone. Assuming the distribution of galaxy luminosities in a cluster can be described by a Schechter luminosity function, our calculations show that the observed iron abundance, oxygen-to-iron mass ratio, and gas temperature in clusters can all be simultaneously reproduced only if the first generation of stars formed with a relatively flat initial mass function. Results from calculations using a Salpeter initial mass function do not agree with observations. RP DAVID, LP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 38 TC 100 Z9 100 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 1991 VL 380 IS 1 BP 39 EP 48 DI 10.1086/170560 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GH912 UT WOS:A1991GH91200006 ER PT J AU MORRIS, SL STOCKE, JT GIOIA, IM SCHILD, RE WOLTER, A MACCACARO, T DELLACECA, R AF MORRIS, SL STOCKE, JT GIOIA, IM SCHILD, RE WOLTER, A MACCACARO, T DELLACECA, R TI THE LUMINOSITY FUNCTION AND COSMOLOGICAL EVOLUTION OF X-RAY-SELECTED BL LACERTAE OBJECTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL LACERTAE OBJECTS; GALAXIES, NUCLEI; GALAXIES, REDSHIFTS; X-RAYS, SOURCES ID MEDIUM-SENSITIVITY SURVEY; RADIO GALAXIES; BLAZARS; SAMPLE; QUASARS; DENSITY; SPECTRA AB We present redshifts for an X-ray-selected, flux-limited sample of BL Lac objects. We derive a median X-ray luminosity of 10(19.83) W Hz-1. We also find a correlation between the optical and radio luminosity of these objects. The complete redshift information allows measurement of the objects' evolution with redshift and calculation of a luminosity function at zero redshift. We find evidence for strong "negative" evolution (BL Lac objects were either less common or less luminous in the recent past). We discuss the differences between radio- and X-ray-selected samples of BL Lac objects, and suggest that X-ray selection picks out chiefly beamed FR I radio galaxies, while radio selection finds a mix of beamed and microlensed quasars, along with extreme examples of beamed FR I radio galaxies. C1 OSSERV ASTRON MILANO,I-20121 MILAN,ITALY. UNIV COLORADO,CTR ASTROPHYS & SPACE ASTRON,COLORADO SPRINGS,CO 80907. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OSSERV ASTRON BOLOGNA,I-40126 BOLOGNA,ITALY. UNIV BOLOGNA,DIPARTMENTO ASTRON,I-40126 BOLOGNA,ITALY. CNR,IST RADIOASTRON,I-40126 BOLOGNA,ITALY. RP MORRIS, SL (reprint author), OBSERV CARNEGIE INST WASHINGTON,813 SANTA BARBARA ST,PASADENA,CA 91101, USA. RI Morris, Simon/G-7981-2011; Gioia, Isabella/B-6982-2012 OI Morris, Simon/0000-0003-4866-110X; Gioia, Isabella/0000-0003-3127-498X NR 49 TC 159 Z9 159 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 1991 VL 380 IS 1 BP 49 EP 65 DI 10.1086/170561 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GH912 UT WOS:A1991GH91200007 ER PT J AU SCHOLZ, TT WALTERS, HRJ AF SCHOLZ, TT WALTERS, HRJ TI COLLISIONAL RATES AND COOLING WITHIN ATOMIC-HYDROGEN PLASMAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC PROCESSES; PLASMAS; TRANSITION PROBABILITIES ID ELECTRON-IMPACT IONIZATION; SCATTERING AB Accurate collisional rates for electron impact ionization of the ground state of atomic hydrogen are evaluated by convolving the experimental cross section with a Maxwellian distribution of electronic energies. An extension of previous work on 1s-2s and 1s-2p scattering rates is also reported. These results are supplemented by semiempirical collisional rates for other excitation processes to yield the cooling rate for optically thin hydrogen plasmas. Our numerical results are evaluated for temperatures ranging from 2 x 10(3) K to 1 x 10(8) K and fitted to simple analytic formulae designed to be easily incorporated into computer programs. C1 QUEENS UNIV BELFAST,DEPT APPL MATH & THEORET PHYS,BELFAST BT7 1NN,ANTRIM,NORTH IRELAND. RP SCHOLZ, TT (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 13 TC 41 Z9 41 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 OCT 10 PY 1991 VL 380 IS 1 BP 302 EP 306 DI 10.1086/170587 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GH912 UT WOS:A1991GH91200033 ER PT J AU PANAGIA, N GILMOZZI, R MACCHETTO, F ADORF, HM KIRSHNER, RP AF PANAGIA, N GILMOZZI, R MACCHETTO, F ADORF, HM KIRSHNER, RP TI PROPERTIES OF THE SN-1987A CIRCUMSTELLAR RING AND THE DISTANCE TO THE LARGE MAGELLANIC CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, DISTANCES; GALAXIES, MAGELLANIC CLOUDS; STARS, CIRCUMSTELLAR SHELLS; STARS, INDIVIDUAL (SN-1987A); STARS, SUPERNOVAE ID LINES AB We have determined the distance to SN 1987A by comparing the angular size of its circumstellar ring, measured from an HST image obtained in a narrow [O III] 5007 angstrom filter, with its absolute size derived from an analysis of the light curves of narrow UV lines (N v lambda-1240, N IV] lambda-1486, N III] lambda-1750, and C III] lambda-1909) measured with IUE. Our analysis confirms that the observed elliptical structure is indeed a circular ring seen at an inclination of = 42.8-degrees +/- 2.6-degrees and provides a determination of its absolute diameter of (1.27 +/- 0.07) x 10(18) cm. Its ratio to the angular diameter of 1.66" +/- 0.03" (Jakobsen et al.) gives an accurate determination of the distance to SN 1987A, i.e., d(1987A) = 51.2 +/- 3.1 kpc. Estimating the relative position of SN 1987A within the Large Magellanic Cloud on the basis of radial velocity data, the distance to the center of the LMC turns out to be 50.1 +/- 3.1 kpc and its distance modulus 18.50 +/- 0.13. This value agrees very well with the determinations obtained from light-curve analyses of variable stars. C1 EUROPEAN SPACE AGCY,DEPT SPACE SCI,DIV ASTROPHYS,BALTIMORE,MD 21218. EUROPEAN SO OBSERV,SPACE TELESCOPE EUROPEAN COORDINATING FACIL,W-8046 GARCHING,GERMANY. UNIV CATANIA,I-95124 CATANIA,ITALY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP PANAGIA, N (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. NR 21 TC 263 Z9 264 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 1991 VL 380 IS 1 BP L23 EP & DI 10.1086/186164 PN 2 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GH914 UT WOS:A1991GH91400006 ER PT J AU DALGARNO, A AF DALGARNO, A TI ASTRONOMY - ELUSIVE H-3+ ION TRACKED DOWN SO NATURE LA English DT Editorial Material ID SPECTRUM; VOYAGER; JUPITER RP DALGARNO, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 11 TC 7 Z9 7 U1 0 U2 1 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD OCT 10 PY 1991 VL 353 IS 6344 BP 502 EP 503 DI 10.1038/353502a0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA GJ643 UT WOS:A1991GJ64300035 ER PT J AU BARNARD, JL SANDVED, K THOMAS, JD AF BARNARD, JL SANDVED, K THOMAS, JD TI TUBE-BUILDING BEHAVIOR IN GRANDIDIERELLA, AND 2 SPECIES OF CERAPUS SO HYDROBIOLOGIA LA English DT Article; Proceedings Paper CT 7TH INTERNATIONAL COLLOQUIUM ON AMPHIPODA CY SEP 14-16, 1990 CL UNIV MARINE, DARLING MARINE CTR, WALPOLE, ME HO UNIV MARINE, DARLING MARINE CTR AB Individuals of Grandidierella bonnieroides and Cerapus sp. R commence tube formation by enrolling themselves in a blanket of detritus and gluing together clumps of the material with strands of silk in a few minutes. The initial tubes are very ragged. G. bonnieroides then expands the initial tube by simply dragging in more detritus. In contrast, Cerapus sp. R. commences building an architectured tube outward from the ragged initial tube using very fine detritus collected either by grasping nearby benthic material or by filter feeding particles from the water column. The diameter of the nearly circular architectured tube is tailored very exactly to the height of the body for which we propose a formula. The more advanced Cerapus sp. K skips the initial phase of blanket-tube formation and only makes short architectured tubes as long as the body, carries these about in a fashion analogous to hermit crabs, and attaches them temporarily to epfloral-faunal substrates well above the sediment surface; therefore, no detritus masses are available to Cerapus sp. K. Tube-building in amphipods is roughly classified into 12 kinds having many subdivisions. Advancement of, or specialization in tube building, lacks apparent correlation with morphological advancement or systematic and evolutionary deployment. C1 REEF FDN,BIG PINE KEY,FL 33043. RP BARNARD, JL (reprint author), SMITHSONIAN INST,NHB 163,WASHINGTON,DC 20560, USA. NR 18 TC 6 Z9 6 U1 0 U2 2 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PD OCT 4 PY 1991 VL 223 BP 239 EP 254 DI 10.1007/BF00047643 PG 16 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA GR167 UT WOS:A1991GR16700023 ER PT J AU GEARY, CM AF GEARY, CM TI OLD PICTURES NEW APPROACHES + DOCUMENTING COLONIAL AFRICA - RESEARCHING HISTORICAL PHOTOGRAPHS SO AFRICAN ARTS LA English DT Article RP GEARY, CM (reprint author), SMITHSONIAN INST,NATL MUSEUM AFRICAN ART,WASHINGTON,DC 20560, USA. NR 15 TC 5 Z9 5 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD OCT PY 1991 VL 24 IS 4 BP 36 EP & DI 10.2307/3337042 PG 0 WC Art SC Art GA GQ638 UT WOS:A1991GQ63800008 ER PT J AU GEARY, CM AF GEARY, CM TI MISSIONARY PHOTOGRAPHY - PRIVATE AND PUBLIC READINGS SO AFRICAN ARTS LA English DT Article ID CAMEROON; AFRICA RP GEARY, CM (reprint author), SMITHSONIAN INST,NATL MUSEUM AFRICAN ART,WASHINGTON,DC 20560, USA. NR 45 TC 9 Z9 9 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD OCT PY 1991 VL 24 IS 4 BP 48 EP & DI 10.2307/3337044 PG 0 WC Art SC Art GA GQ638 UT WOS:A1991GQ63800010 ER PT J AU BIEDER, RE AF BIEDER, RE TI THE RETURN OF CULTURAL TREASURES - GREENFIELD,J SO AMERICAN HISTORICAL REVIEW LA English DT Book Review C1 SMITHSONIAN INST,WASHINGTON,DC 20560. RP BIEDER, RE (reprint author), LAJOS KOSSUTH UNIV,H-4010 DEBRECEN,HUNGARY. 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 1991 VL 96 IS 4 BP 1154 EP 1154 DI 10.2307/2165021 PG 1 WC History SC History GA GN055 UT WOS:A1991GN05500013 ER PT J AU MILLER, LB AF MILLER, LB TI CATLIN AND HIS CONTEMPORARIES - THE POLITICS OF PATRONAGE - DIPPIE,BW SO AMERICAN HISTORICAL REVIEW LA English DT Book Review RP MILLER, LB (reprint author), SMITHSONIAN INST,NATL PORTRAIT GALLERY,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 1991 VL 96 IS 4 BP 1274 EP 1275 DI 10.2307/2165181 PG 2 WC History SC History GA GN055 UT WOS:A1991GN05500176 ER PT J AU SNOW, AA SPIRA, TP AF SNOW, AA SPIRA, TP TI DIFFERENTIAL POLLEN-TUBE GROWTH-RATES AND NONRANDOM FERTILIZATION IN HIBISCUS-MOSCHEUTOS (MALVACEAE) SO AMERICAN JOURNAL OF BOTANY LA English DT Article ID GAMETOPHYTIC SELECTION; RAPHANUS-RAPHANISTRUM; AMSINCKIA-GRANDIFLORA; CAMPSIS-RADICANS; SEXUAL SELECTION; INCOMPATIBILITY; POLLINATIONS; CONSEQUENCES; PATERNITY; CALLOSE AB The prevalence of nonrandom fertilization due to postpollination events has rarely been studied in natural populations, despite important implications for outcrossing rates, mate choice, and plant fitness. Nonrandom paternity within fruits can be caused by both unequal fertilization and unequal embryo abortion. Using self-compatible Hibiscus moscheutos, we studied the potential for nonrandom fertilization by comparing growth rates of pollen-tubes from different donors. The branched style of Hibiscus allowed within-flower comparisons between pollen donors. Relative pollen-tube growth rates were determined by applying pollen from pairs of donors to different stigmas on adjacent stylar branches. We then measured the number of callose plugs per tube in cross-sectional transects across the style after 3 hr. We demonstrate that rates of callose plug formation can be used as a sensitive indicator of relative pollen-tube growth rate. Differences between pollen donors were common and repeatable. Self-pollen-tubes grew slower than outcross pollen-tubes in some crosses and faster in others. Allozyme variation in glucose phosphate isomerase was used to show that individuals with fast-growing pollen-tubes sired a disproportionate number of seeds following mixed pollinations (up to 72%). Since seed abortion was negligible, we conclude that variation in pollen-tube growth rates leads to nonrandom paternity within fruits. C1 UNIV MICHIGAN,BIOL STN,PELLSTON,MI 49769. GEORGIA SO UNIV,DEPT BIOL,STATESBORO,GA 30460. SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. NR 34 TC 95 Z9 99 U1 4 U2 15 PU BOTANICAL SOC AMER INC PI COLUMBUS PA OHIO STATE UNIV-DEPT BOTANY 1735 NEIL AVE, COLUMBUS, OH 43210 SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD OCT PY 1991 VL 78 IS 10 BP 1419 EP 1426 DI 10.2307/2445280 PG 8 WC Plant Sciences SC Plant Sciences GA GL395 UT WOS:A1991GL39500010 ER PT J AU WASHBURN, WE AF WASHBURN, WE TI THE MALL IN WASHINGTON, 1791-1991 - LONGSTRETH,R 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 1991 VL 29 IS 2 BP 79 EP 80 PG 2 WC History SC History GA GJ882 UT WOS:A1991GJ88200008 ER PT J AU SOKER, N BORKOWSKI, KJ SARAZIN, CL AF SOKER, N BORKOWSKI, KJ SARAZIN, CL TI INTERACTION OF PLANETARY-NEBULAE WITH THE INTERSTELLAR-MEDIUM - THEORY SO ASTRONOMICAL JOURNAL LA English DT Article ID GLOBULAR-CLUSTER M22; EVOLUTION; MOTIONS AB We performed hydrodynamical simulations of the interaction between planetary nebulae (PNs) and the interstellar medium (ISM), in order to provide a theoretical framework for observations of interacting PNs. Our results validate a thin-shell approximation {originally developed by Smith [MNRAS, 175, 419 (1976)]} to calculate the expected displacement of central stars from PN centers, for a typical nebula in which the shocked ISM gas cools down to a characteristic nebular temperature of approximately 10(4) K. This simple picture breaks down for high-velocity PNs in a low density environment, where the shocked ISM cools slowly. In this case, a Rayleigh-Taylor instability develops, leading to shell fragmentation on roughly the same timescale on which the shell is decelerated. We use our results to interpret observations of two interacting nebulae of particular interest, NGC 246 and the PN in the globular cluster M22. C1 UNIV VIRGINIA,VIRGINIA INST THEORET ASTRON,CHARLOTTESVILLE,VA 22903. UNIV VIRGINIA,DEPT ASTRON,CHARLOTTESVILLE,VA 22903. RP SOKER, N (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MAIL STOP 15,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 38 TC 55 Z9 55 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 OCT PY 1991 VL 102 IS 4 BP 1381 EP 1392 DI 10.1086/115963 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GG675 UT WOS:A1991GG67500014 ER PT J AU OSTRO, SJ CAMPBELL, DB CHANDLER, JF SHAPIRO, II HINE, AA VELEZ, R JURGENS, RF ROSEMA, KD WINKLER, R YEOMANS, DK AF OSTRO, SJ CAMPBELL, DB CHANDLER, JF SHAPIRO, II HINE, AA VELEZ, R JURGENS, RF ROSEMA, KD WINKLER, R YEOMANS, DK TI ASTEROID RADAR ASTROMETRY SO ASTRONOMICAL JOURNAL LA English DT Article ID 433-EROS; IMAGES AB We report all useful measurements of time delay and Doppler frequency for asteroid radar echoes obtained at Arecibo and Goldstone during 1980-1990. New radar astrometry is presented for 23 near-Earth asteroids and three mainbelt asteroids. These measurements, which are orthogonal to optical, angular-position measurements, and typically have a fractional precision between 10(-5) and 10(-8), permit significant improvement in estimates of orbits and hence in the accuracy of prediction ephemerides. We also report estimates of radar cross section and circular polarization ratio for all asteroids observed astrometrically during 1980-1990. C1 CORNELL UNIV, NATL ASTRON & IONOSPHERE CTR, ITHACA, NY 14853 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NATL ASTRON & IONOSPHERE CTR, ARECIBO, PR 00613 USA. RP OSTRO, SJ (reprint author), CALTECH, JET PROP LAB, PASADENA, CA 91109 USA. NR 34 TC 45 Z9 46 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 1991 VL 102 IS 4 BP 1490 EP 1502 DI 10.1086/115975 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GG675 UT WOS:A1991GG67500026 ER PT J AU MARSDEN, BG AF MARSDEN, BG TI THE COMPUTATION OF ORBITS IN INDETERMINATE AND UNCERTAIN CASES SO ASTRONOMICAL JOURNAL LA English DT Article AB The GEM form of the Gaussian method of three-observation orbit determination is modified in order to obtain physically meaningful results in mathematically indeterminate cases. The modified procedure can enable the user to isolate situations where at least one observation is erroneous. A logical extension of the procedure then provides a mechanism for using only two observations of a minor planet to identify additional data. Though in some respects analogous to the "modified" Vaisala method, the new procedure is more convenient to apply in practice and has distinct advantages in the case of Apollo objects, which in the Vaisala method must unrealistically be presumed at aphelion. It is also shown that the three-observation procedure can readily be extended to incorporate additional observations. Further comments are made on the rather unfortunate manner in which the Gauss method is presented in the standard texts, including the one by Taff. There is a discussion of the relative performance of the GEM method and traditional orbit-determination methods in cases of discrete, nontrivial multiple solutions. RP MARSDEN, BG (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 44 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 OCT PY 1991 VL 102 IS 4 BP 1539 EP 1552 DI 10.1086/115979 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GG675 UT WOS:A1991GG67500030 ER PT J AU SOLANKI, SK STEINER, O UITENBROECK, H AF SOLANKI, SK STEINER, O UITENBROECK, H TI 2-DIMENSIONAL MODELS OF THE SOLAR CHROMOSPHERE .1. THE CA-II-K-LINE AS A DIAGNOSTIC - 1.5-D RADIATIVE-TRANSFER SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE THE SUN, CHROMOSPHERE; THE SUN, MAGNETIC FIELDS; CA-II; RADIATIVE TRANSFER; LINE PROFILES ID TEMPERATURE-MINIMUM REGION; MAGNETIC-FLUX TUBES; SPECTROMETER OBSERVATIONS; PARTIAL REDISTRIBUTION; PHYSICAL-PROPERTIES; TRANSITION REGION; CARBON-MONOXIDE; ACTIVE REGIONS; ENERGY-BALANCE; COOL STARS AB Profiles of the Ca II K line are calculated for a 5 level atom and partial frequency redistribution along multiple rays (1.5-D) passing through two-dimensional (2-D) MHD models of magnetic flux tubes in the solar atmosphere. Temperature stratifications corresponding to various empirical chromospheric models are incorporated into the models. The influence of a number of model parameters on individual and spatially averaged line profiles is considered in detail. The profiles are also compared with observations. It is found that the present models can, at least qualitatively, reproduce a wide variety of observations if the temperature within the magnetic component lies between that of model F of Vernazza et al. (1981) and of model VALP of Ayres et al. (1986) and if the temperature in the non-magnetic part of the atmosphere corresponds to that of the COOLC model of Ayres et al. The observations that are consistent with such a model include: 1. The spatially averaged Ca II K quiet Sun profile. 2. The spatial scale and the amplitude of horizontal K2 intensity variations in the quiet Sun (including the network). 3. The qualitative form of the relationship between the K line core intensity and the magnetic flux density in an active region, including the presence of a "basal" flux, i.e. a chromospheric emission in the local absence of a photospheric magnetic field. 4. The presence of a cool fraction of the solar chromosphere with temperatures below 4000 K, as suggested by observations of infrared CO lines. 5. The presence of magnetic canopies in the lower or middle chromosphere of the quiet Sun and the presence of lower lying canopies in active regions. 6. The highly intermittent nature of the photospheric magnetic field. Points 4 and 6 are a direct consequence of the model input. C1 STERREKUNDIG INST UTRECHT, 3508 TA UTRECHT, NETHERLANDS. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP SOLANKI, SK (reprint author), SWISS FED INST TECHNOL, INST ASTRON, CH-8092 ZURICH, SWITZERLAND. RI Solanki, Sami/E-2487-2013 OI Solanki, Sami/0000-0002-3418-8449 NR 71 TC 48 Z9 48 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 OCT PY 1991 VL 250 IS 1 BP 220 EP 234 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GK744 UT WOS:A1991GK74400025 ER PT J AU BIRKINSHAW, M HUGHES, JP ARNAUD, KA AF BIRKINSHAW, M HUGHES, JP ARNAUD, KA TI A MEASUREMENT OF THE VALUE OF THE HUBBLE CONSTANT FROM THE X-RAY-PROPERTIES AND THE SUNYAEV-ZELDOVICH EFFECT OF ABELL-665 SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY; GALAXIES CLUSTERING; GALAXIES INTERGALACTIC MEDIUM; GALAXIES X-RAYS ID MICROWAVE BACKGROUND-RADIATION; LUMINOSITY FUNCTION; DISTANCE SCALE; RICH CLUSTERS; GAS CONTENTS; 3 CLUSTERS; HOT PLASMA; GALAXIES; ABELL-2218; EVOLUTION AB A comparison of the X-ray properties and the Sunyaev-Zel'dovich effect for a cluster of galaxies may be used to measure the distance of the cluster, and hence the Hubble constant. We have applied this method to the rich cluster Abell 665 using IPC, HRI, and MPC data from the Einstein Observatory, LAC data from the Ginga satellite, and Sunyaev-Zel'dovich data from the OVRO 40 m telescope. The X-ray and Sunyaev-Zel'dovich effect data are consistent in their description of the cluster gas and may be fitted by a simple isothermal beta-model with beta almost-equal-to 0.66, cluster core radius almost-equal-to 1.6, and gas temperature almost-equal-to 8.2 keV. The relative normalizations of the X-ray and Sunyaev-Zel'dovich effect data then lead to an estimated Hubble constant H0 = 40 +/- 9 km s-1 Mpc-1 if only the random errors are included. When the possible systematic errors (which are most important if they are present in the Sunyaev-Zel'dovich data) are added in quadrature, the range of possible values of the Hubble constants expands to (40 to 50) +/- 12 km s-1 Mpc-1. The most immediate improvements in the error in this estimate for the Hubble constant would be produced by setting better limits on the zero level of the Sunyaev-Zel'dovich effect data (involving extensive observation), and by improved X-ray observations of the cluster, possibly with ROSAT, Astro-D, and AXAF. However, systematic errors associated with the unknown detailed thermal and density structures of the gas (clumping and low-surface brightness structures) provide limits to the accuracy of the method in principle. C1 UNIV MARYLAND,ASTRON PROGRAM,COLLEGE PK,MD 20742. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP BIRKINSHAW, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 55 TC 143 Z9 144 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 OCT 1 PY 1991 VL 379 IS 2 BP 466 EP 481 DI 10.1086/170522 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GH078 UT WOS:A1991GH07800004 ER PT J AU KWOK, PW CHENG, KS LAU, MM AF KWOK, PW CHENG, KS LAU, MM TI A MODEL OF UNPULSED VERY-HIGH-ENERGY GAMMA-RAYS FROM THE CRAB-NEBULA AND PULSAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE GAMMA RAYS GENERAL; NEBULAE CRAB NEBULA; PULSARS ID RAPIDLY SPINNING PULSARS; RADIATION AB The angular resolution of gamma-ray detectors does not allow one to separate the nebula from the pulsar in the Crab. It is generally assumed that the steady emission of gamma rays comes from the nebula. Using the "outer magnetospheric gap" model, we propose an alternative mechanism in which the steady emission of gamma rays could come from a compact region, a couple of light cylinder radii beyond the pulsar. In that region, the magnetic field has been transformed from a dipole field to a swirling field. In the model, two mono-energetic beams of gap primary e+(e-) if OMEGA . B(s) > 0 (< 0) with a Lorentz factor approximately 4 x 10(7) are streaming out from the outer gaps through the light cylinder. The gap primary e+(e-) beam from the first outer gap can produce approximately 10 TeV primary very high energy (VHE) gamma rays through inverse Compton scattering with the IR photons from the second gap, and vice versa. The primary VHE gamma rays are sufficiently energetic to produce secondary e+/- pairs by collision with the same pulsed IR photons. Since the mean free path of these conversion processes is comparable to the local radius of curvature, the pitch angles of the secondary pairs are large enough to result in isotropic secondary VHE gamma rays with E-gamma approximately TeV. Comparisons between the model spectra and the observed data are discussed in the text. C1 CITY POLYTECH HONG KONG,DEPT APPL SCI,HONG KONG,HONG KONG. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV HONG KONG,DEPT PHYS,HONG KONG,HONG KONG. RP KWOK, PW (reprint author), NASA,GODDARD SPACE FLIGHT CTR,CODE 662,GREENBELT,MD 20771, USA. RI Cheng, Kwong Sang/D-3073-2009 NR 25 TC 16 Z9 16 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 1991 VL 379 IS 2 BP 653 EP 658 DI 10.1086/170538 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GH078 UT WOS:A1991GH07800020 ER PT J AU CHANG, ES AVRETT, EH MAUAS, PJ NOYES, RW LOESER, R AF CHANG, ES AVRETT, EH MAUAS, PJ NOYES, RW LOESER, R TI FORMATION OF THE INFRARED-EMISSION LINES OF MG I IN THE SOLAR ATMOSPHERE SO ASTROPHYSICAL JOURNAL LA English DT Article DE LINE FORMATION SUN; ATMOSPHERE SUN; ECLIPSES SUN; MAGNETIC FIELDS ID 12 MICRONS; CROSS-SECTIONS; QUIET SUN; MAGNESIUM AB The Mg I emission lines at 7 and 12-mu-m provide a sensitive measure of the magnetic and electric field strengths in the layers of the solar atmosphere where the observed emission originates. Hence it is important to know how and where these lines are formed. Their strong limb brightening suggests a chromospheric origin; however, theoretical studies by Lemke and Holweger and by Hoang-Binh, and observations by Deming et al., suggest an origin at or below the temperature minimum, with the emission being produced by the underpopulation of lower atomic levels relative to the upper ones. Such underpopulations are caused by radiative depopulation of lower levels, together with collisional coupling of higher levels with the Mg II continuum. We investigate these effects with a 41 level atomic model, including collisions with hydrogen atoms as well as with electrons, and including the charge exchange process Mg+ + H(n) <--> Mg(nl) + H+ between magnesium and hydrogen. Using an average quiet Sun atmospheric model, we calculate emission-line profiles that resemble the observed ones, that is, broad absorption troughs with narrow central emission, and significant limb brightening. The charge exchange rates are significant, but the effects of high-n coupling between Mg and Mg+ (due to collisions with electrons and with hydrogen atoms) together with radiative losses between low-n transitions are of greater importance. We confirm that the emission cores are formed no higher than the temperature minimum region, and that the emission is caused by non-LTE effects rather than by the chromospheric temperature rise. This photospheric origin explains why the brightness temperature of the trough, or minimum intensity in the line wings, is unrelated to the temperature minimum between the photosphere and chromosphere. The model calculations indicate that the line core is sensitive to magnetic fields located almost 400 km above those measured in ordinary magnetograms; the gas pressure decreases 20-fold between these two heights. The electron density decreases by a factor of 8 between the heights at which the trough and emission core originate, consistent with observed Stark shifts. The behavior of the emission lines as seen during a total solar eclipse should provide a strong test of these model calculations and inferred formation mechanisms. C1 UNIV MASSACHUSETTS, DEPT PHYS & ASTRON, AMHERST, MA 01003 USA. OSSERV ASTROFIS ARCETRI, I-50125 FLORENCE, ITALY. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 30 TC 39 Z9 39 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 OCT 1 PY 1991 VL 379 IS 2 BP L79 EP L82 DI 10.1086/186158 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GH081 UT WOS:A1991GH08100009 ER PT J AU ROBERGE, WG JONES, D LEPP, S DALGARNO, A AF ROBERGE, WG JONES, D LEPP, S DALGARNO, A TI INTERSTELLAR PHOTODISSOCIATION AND PHOTOIONIZATION RATES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE INTERSTELLAR, GRAINS; INTERSTELLAR, MOLECULES; MOLECULAR PROCESSES ID INTER-STELLAR CLOUDS; RADIATION-FIELD; DENSE CLOUDS; ULTRAVIOLET; MOLECULES; GRAINS; GAS AB The rates of photoionization and photodissociation of molecules are calculated as functions of visual extinction into plane-parallel clouds illuminated by the average interstellar radiation field. An accurate technique is used to calculate the attenuation of the ultraviolet radiation due to scattering and absorption by dust grains inside the clouds. As a plausible and self-consistent model for the grains in diffuse clouds and the outer layers of dense clouds, the graphite-silicate grain mixture of Mathis, Rumpl, & Nordsieck is adopted, together with the wave-length-dependent grain optical properties calculated by Draine & Lee. Depth-dependent photodissociation and photoionization rates are presented for a wide range of molecules, and the results are compared with the rates of photodestruction resulting from internal photons generated by cosmic rays. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP ROBERGE, WG (reprint author), RENSSELAER POLYTECH INST,DEPT PHYS,TROY,NY 12180, USA. RI Jones, Dylan/O-2475-2014 OI Jones, Dylan/0000-0002-1935-3725 NR 30 TC 127 Z9 127 U1 2 U2 6 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 OCT PY 1991 VL 77 IS 2 BP 287 EP 297 DI 10.1086/191604 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GH386 UT WOS:A1991GH38600003 ER PT J AU BEISSINGER, SR WALTMAN, JR AF BEISSINGER, SR WALTMAN, JR TI EXTRAORDINARY CLUTCH SIZE AND HATCHING ASYNCHRONY OF A NEOTROPICAL PARROT SO AUK LA English DT Article ID BROOD REDUCTION; BREEDING BIOLOGY; SNAIL KITES; BIRDS; HYPOTHESIS; INCUBATION; WEIGHT AB We studied the nesting biology of the Green-rumped Parrotlet (Forpus passerinus) in the llanos of Venezuela. Clutch size averaged 7 eggs (range: 5-10), and eggs were typically laid daily or every other day over 7-16 days (xBAR = 10). Incubation began with the first egg. Clutches hatched over 2-14 days (xBAR = 8.6) and fledged over 4-17 days (xBAR = 9.7). An average of 5.7 chicks hatched (range: 2-10) and 4.7 chicks fledged (range: 1-8) per successful nest. The number of young fledging increased slightly with clutch size, but parents that hatched more eggs were able to fledge significantly more young. Chicks fledged at 28-35 days of age, and chicks that hatched later and in nests with larger broods took significantly longer to fledge. Hatching success was significantly lower for last eggs in large clutches than for eggs laid earlier or in smaller clutches. However, fertility and volume of last eggs were similar to other eggs. Fledging success was uniformly high for nestlings in small broods, declined slightly for the last two chicks in medium sized broods, and declined sharply for the last two nestlings in large broods. Last-hatched and penultimately hatched chicks were found dead with empty crops significantly more often than earlier-hatched chicks, which implies death by starvation. We evaluated these results in relation to current hypotheses for the evolution of clutch size in tropical birds and the causes of hatching asynchrony. We propose the limited breeding-opportunities hypothesis to explain both the large clutch size and hatching asynchrony in F. passerinus. When opportunities to nest are limited through intra- or interspecific competition, females might be expected to invest heavily in reproductive effort and guard their clutches from nest-site takeovers. This could lead to large clutches, incubation beginning with the first egg, and a large hatching interval. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. RP BEISSINGER, SR (reprint author), YALE UNIV,SCH FORESTRY & ENVIRONM STUDIES,NEW HAVEN,CT 06511, USA. RI Beissinger, Steven/F-3809-2012 NR 45 TC 89 Z9 90 U1 0 U2 9 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 1991 VL 108 IS 4 BP 863 EP 871 PG 9 WC Ornithology SC Zoology GA GQ237 UT WOS:A1991GQ23700012 ER PT J AU PETERSEN, CW AF PETERSEN, CW TI VARIATION IN FERTILIZATION RATE IN THE TROPICAL REEF FISH, HALICHOERES-BIVATTATUS - CORRELATES AND IMPLICATIONS SO BIOLOGICAL BULLETIN LA English DT Article ID MATING SYSTEM; SEX CHANGE; SOCIAL-ORGANIZATION; SERRANUS-FASCIATUS; POPULATION-DENSITY; FEMALE CHOICE; MIYAKE-JIMA; BEHAVIOR; CONSEQUENCES; LABRIDAE AB Fertilization rates were estimated for natural spawns in the tropical wrasse, Halichoeres bivattatus. Fertilization rate averaged 88%, but varied with both sea conditions and with the addition of males (streakers) to pair spawns. As sea conditions became rougher, the mean fertilization rate for a day decreased. This effect was due to the two days with the roughest sea conditions and the lowest mean fertilization rates; there was no obvious trend when these two days were excluded from the analysis. On a given day, pair spawns, with a single male and female, had fertilization rates approximately 7% lower than spawns where 1-2 streakers joined the pair spawn. These results suggest that variation in fertilization rate must be considered as a potential selective force in shaping reproductive behavior in fishes with external fertilization of pelagic eggs. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 34 TC 50 Z9 50 U1 1 U2 3 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 PY 1991 VL 181 IS 2 BP 232 EP 237 DI 10.2307/1542094 PG 6 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA GP152 UT WOS:A1991GP15200005 ER PT J AU KRESS, WJ AF KRESS, WJ TI NEW TAXA OF HELICONIA (HELICONIACEAE) FROM ECUADOR SO BRITTONIA LA English DT Article DE HELICONIA; ECUADOR AB Three new species (Heliconia fredberryana, H. litana, and H. lutheri) and one new subspecies (H. obscura ssp. dichroma) from Ecuador are described, illustrated, and discussed. RP KRESS, WJ (reprint author), SMITHSONIAN INST,DEPT BOT,NHB-166,WASHINGTON,DC 20560, USA. NR 0 TC 2 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 1991 VL 43 IS 4 BP 253 EP 260 DI 10.2307/2807286 PG 8 WC Plant Sciences SC Plant Sciences GA HB630 UT WOS:A1991HB63000003 ER PT J AU COLE, DG AF COLE, DG TI AN ATLAS OF MASSACHUSETTS RIVER SYSTEMS - ENVIRONMENTAL DESIGNS FOR THE FUTURE - BICKFORD,WE, DYMON,UJ SO CARTOGRAPHY AND GEOGRAPHIC INFORMATION SYSTEMS LA English DT Book Review RP COLE, DG (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER CONGR SURVEYING & MAPPING PI BETHESDA PA 5410 GROSVENOR LANE, BETHESDA, MD 20814 SN 1050-9844 J9 CARTOGR GEOGR INFORM PD OCT PY 1991 VL 18 IS 4 BP 282 EP 282 PG 1 WC Geography SC Geography GA GP408 UT WOS:A1991GP40800015 ER PT J AU WRIGHT, SJ AF WRIGHT, SJ TI SEASONAL DROUGHT AND THE PHENOLOGY OF UNDERSTORY SHRUBS IN A TROPICAL MOIST FOREST SO ECOLOGY LA English DT Article DE BARRO-COLORADO ISLAND; DRY SEASON; FOREST; IRRIGATION; PANAMA; PIPER; PLANT PHENOLOGY; PSYCHOTRIA; TROPICAL FOREST; WATER STRESS ID SUBGENUS PSYCHOTRIA RUBIACEAE; HYBANTHUS-PRUNIFOLIUS; WATER-STRESS; COSTA-RICA; GROWTH; TREES; PANAMA; COMMUNITY; LOWLANDS; REVISION AB The vegetative and reproductive growth of tropical forest plants often occurs in short bursts separated by longer quiescent periods. Seasonal changes in moisture availability may be a cause and, if so, may cue growth in a proximate sense or limit growth in an ultimate sense. Two 2.25-ha plots of mature forest were irrigated for three consecutive dry seasons on Barro Colorado Island, Panama, to discriminate among the various possibilities. The responses of three Piper species and four Psychotria species are reported. Irrigation disrupted the timing of leaf flush for all seven species. Irrigation increased annual leaf production for just one species, however, and had no effect on annual inflorescence production for the Psychotria nor on stem radial growth. These responses are consistent with the hypothesis that water stress constrains the timing of growth while only rarely limiting total annual growth. However, leaf turgor potentials observed among control plants may not have been sufficiently low to constrain leaf and inflorescence production, and other effects of irrigation cannot be discounted. Possible phenological cues that were affected by irrigation include soil moisture content, air temperature, relative humidity, and the timing of nutrient inputs from decaying litter. There was no evidence that a "water stress requirement" must be met during the dry season before wet season budbreak. The gradual decay in synchrony for leaf production for all four Psychotria species suggests that endogenous rhythms contribute to growth periodicities in this genus. RP WRIGHT, SJ (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 57 TC 92 Z9 108 U1 5 U2 29 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE, NW, STE 400, WASHINGTON, DC 20036 SN 0012-9658 J9 ECOLOGY JI Ecology PD OCT PY 1991 VL 72 IS 5 BP 1643 EP 1657 DI 10.2307/1940964 PG 15 WC Ecology SC Environmental Sciences & Ecology GA GK823 UT WOS:A1991GK82300012 ER PT J AU LEMAITRE, R RODRIGUES, SD AF LEMAITRE, R RODRIGUES, SD TI LEPIDOPHTHALMUS-SINUENSIS - A NEW SPECIES OF GHOST SHRIMP (DECAPODA, THALASSINIDEA, CALLIANASSIDAE) OF IMPORTANCE TO THE COMMERCIAL CULTURE OF PENAEID SHRIMPS ON THE CARIBBEAN COAST OF COLOMBIA, WITH OBSERVATIONS ON ITS ECOLOGY SO FISHERY BULLETIN LA English DT Article ID CRUSTACEA AB A new species of ghost shrimp Lepidophthalmus sinuensis is described from the Caribbean coast of Colombia, and general ecological observations are made on the conditions under which it was found. The new species can be distinguished from others in the genus by the presence of large subrectangular lateral projections on the frontal region of the carapace. The new species was discovered in ponds of a commercial penaeid shrimp farm where its burrow densities range up to 2093 burrow openings/m2 in pond bottoms consisting of fine sand. It appears that, on at least a temporary basis, activities of L. sinuensis may negatively impact penaeid shrimp culture. C1 UNIV SAO PAULO,INST BIOCIENCIAS,DEPT ECOL GERAL,BR-05499 SAO PAULO,BRAZIL. RP LEMAITRE, R (reprint author), NATL MUSEUM NAT HIST,SMITHSONIAN OCEANOG SORTING CTR,WASHINGTON,DC 20560, USA. NR 24 TC 28 Z9 29 U1 0 U2 0 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD OCT PY 1991 VL 89 IS 4 BP 623 EP 630 PG 8 WC Fisheries SC Fisheries GA GU460 UT WOS:A1991GU46000007 ER PT J AU RADFORD, HE EVENSON, KM MATUSHIMA, F ZINK, LR GALVAO, GP SEARS, TJ AF RADFORD, HE EVENSON, KM MATUSHIMA, F ZINK, LR GALVAO, GP SEARS, TJ TI FAR INFRARED-LASER FREQUENCIES OF CH3OD AND N2H4 SO INTERNATIONAL JOURNAL OF INFRARED AND MILLIMETER WAVES LA English DT Article DE CH3OD; N2H4; MOLECULAR LASER LINES; LASER FREQUENCY MEASUREMENTS; OPTICALLY PUMPED FAR INFRARED LASERS AB The frequencies of 26 laser lines with wavelengths between 57 and 534-mu-m have been measured in the optically pumped laser gases CH3OD and N2H4. A pair of stabilized cw (CO2)-C-12 lasers was used as a frequency standard for the heterodyne frequency measurements. Seven of the 26 lines are new. C1 NATL INST STAND & TECHNOL,DIV TIME & FREQUENCY,BOULDER,CO 80303. BROOKHAVEN NATL LAB,DEPT CHEM,UPTON,NY 11973. TOYAMA UNIV,DEPT PHYS,TOYAMA 930,JAPAN. INST NACL PESQUISAS ESPACIAIS,BR-12201 SAO JOSE CAMPOS,SP,BRAZIL. RP RADFORD, HE (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,DIV ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138, USA. RI Sears, Trevor/B-5990-2013 OI Sears, Trevor/0000-0002-5559-0154 NR 5 TC 14 Z9 14 U1 0 U2 0 PU PLENUM PUBL CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 SN 0195-9271 J9 INT J INFRARED MILLI JI Int. J. Infrared Millimeter Waves PD OCT PY 1991 VL 12 IS 10 BP 1161 EP 1166 DI 10.1007/BF01008558 PG 6 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA GJ575 UT WOS:A1991GJ57500005 ER PT J AU WU, K TONG, CYE VAHLDIECK, R AF WU, K TONG, CYE VAHLDIECK, R TI MICROWAVE CHARACTERISTICS OF HIGH-SPEED TRAVELING-WAVE ELECTROOPTIC MODULATORS ON III-V-SEMICONDUCTORS SO JOURNAL OF LIGHTWAVE TECHNOLOGY LA English DT Article ID TRANSMISSION-LINE; GUIDE; BANDWIDTH; SWITCH; DESIGN; GHZ AB Microwave characteristics of III-V semiconductor traveling wave electrooptic modulators have been studied rigorously by using the method of lines. This approach makes it possible to construct a complete computer model of double-rib, multilayer strip waveguide modulators which are out of reach of the classical methods. Both p-i-n junction and Schottky-barrier junction controlled devices have been investigated. The fringing microwave field has been found to play an important role in improving the modulator's bandwidth. For the first time, a nonperfect electrode of finite thickness has been modeled. The method of lines algorithm has proved to be a valuable CAD tool for design and optimization of high-speed modulators. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP WU, K (reprint author), UNIV VICTORIA,DEPT ELECT & COMP ENGN,VICTORIA V8W 2Y2,BC,CANADA. OI Tong, Edward/0000-0002-7736-4203 NR 22 TC 9 Z9 9 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017-2394 SN 0733-8724 J9 J LIGHTWAVE TECHNOL JI J. Lightwave Technol. PD OCT PY 1991 VL 9 IS 10 BP 1295 EP 1304 DI 10.1109/50.90927 PG 10 WC Engineering, Electrical & Electronic; Optics; Telecommunications SC Engineering; Optics; Telecommunications GA GG490 UT WOS:A1991GG49000010 ER PT J AU FAUST, MA AF FAUST, MA TI MORPHOLOGY OF CIGUATERA-CAUSING PROROCENTRUM-LIMA (PYRROPHYTA) FROM WIDELY DIFFERING SITES SO JOURNAL OF PHYCOLOGY LA English DT Article ID DINOFLAGELLATE EVOLUTION; OKADAIC ACID; IDENTIFICATION AB Clones of ciguatoxigenic Prorocentrum lima (Ehr.) Dodge 1975 were examined from different geographical areas (Pacific and Atlantic oceans) and compared with the earliest descriptions between 1881 and 1933 and light and electron micrographs of other researchers. Surface morphology of the widely distributed clones was remarkably similar, and morphological variability of ecotypes of this species is minimal. The number of valve pores (58-85 per valve) and marginal pores (55-72 per valve) is characteristic of the species. Marginal pores are located adjacent to the intercalary band in a regular pattern, are readily distinguishable by light microscopy, and are a good criterion for identifying P. lima. The periflagellar area of P. lima is a unique taxonomic feature; however, it can only be seen with the scanning electron microscope at high magnification. The anterior periflagellar area is a broad triangule, where the left valve margin is flat and the right valve has a V-shaped depression. It accommodates a flagellar and an auxiliary pore and a flared, protuberant apical collar enclosed by eight small plates. The protuberant apical collar of P. lima has only been observed in one other Prorocentrum species, P. hoffmannianum, which has an areolated valve surface. In contrast, the valve surface of P. lima is smooth. Cells possess chloroplasts, a centrally located pyrenoid, a posterior nucleus, and two flagella. The shape and size of P. lima are variable and less useful for identifying specimens. RP FAUST, MA (reprint author), SMITHSONIAN INST,MUSEUM SUPPORT CTR,DEPT BOT,4201 SILVER HILL RD,SUITLAND,MD 20746, USA. NR 40 TC 61 Z9 65 U1 0 U2 2 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 OCT PY 1991 VL 27 IS 5 BP 642 EP 648 DI 10.1111/j.0022-3646.1991.00642.x PG 7 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA GM316 UT WOS:A1991GM31600015 ER PT J AU SODHI, NS WARKENTIN, IG JAMES, PC OLIPHANT, LW AF SODHI, NS WARKENTIN, IG JAMES, PC OLIPHANT, LW TI EFFECTS OF RADIOTAGGING ON BREEDING MERLINS SO JOURNAL OF WILDLIFE MANAGEMENT LA English DT Article ID RADIO PACKAGES; URBAN MERLINS; RED GROUSE; BEHAVIOR; TRANSMITTERS; SURVIVAL; DISPERSAL; MOVEMENTS; PHEASANTS; MARKING AB We examined the impact of radiotagging on breeding merlins (Falco columbarius) in Saskatoon (Canada) between May and July, 1987-90. We compared reproductive and hatching success between 12 tagged and 71 untagged males. We also collated return rates between 21 tagged (both M and F) and 112 untagged merlins, We did not observe any long-lasting abnormal behavior in tagged birds during the postrelease period. Breeding output, hatching success, and survival did not differ significantly (P > 0.05) between radio-tagged and untagged birds. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. SASKATCHEWAN MUSEUM NAT HIST,REGINA S4P 3V7,SASKATCHEWAN,CANADA. UNIV SASKATCHEWAN,WESTERN COLL VET MED,DEPT VET ANAT,SASKATOON S7N 0W0,SASKATCHEWAN,CANADA. RP SODHI, NS (reprint author), UNIV SASKATCHEWAN,DEPT BIOL,SASKATOON S7N 0W0,SASKATCHEWAN,CANADA. NR 26 TC 14 Z9 14 U1 1 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 1991 VL 55 IS 4 BP 613 EP 616 DI 10.2307/3809507 PG 4 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA GW663 UT WOS:A1991GW66300011 ER PT J AU EBERHARD, WG AF EBERHARD, WG TI ARTIFICIAL-INSEMINATION - CAN APPROPRIATE STIMULATION IMPROVE SUCCESS RATES SO MEDICAL HYPOTHESES LA English DT Article ID COPULATORY-BEHAVIOR; MESOCRICETUS-AURATUS; FEMALE RAT; PSEUDOPREGNANCY; GENITALIA; INDUCTION AB Studies of other animal species suggest that stimulation during copulation has important effect on the probability of conception. Thus appropriate stimulation during artificial insemination may improve rates of conception. 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 30 TC 0 Z9 0 U1 0 U2 2 PU CHURCHILL LIVINGSTONE PI EDINBURGH PA JOURNAL PRODUCTION DEPT, ROBERT STEVENSON HOUSE, 1-3 BAXTERS PLACE, LEITH WALK, EDINBURGH, MIDLOTHIAN, SCOTLAND EH1 3AF SN 0306-9877 J9 MED HYPOTHESES JI Med. Hypotheses PD OCT PY 1991 VL 36 IS 2 BP 152 EP 154 DI 10.1016/0306-9877(91)90259-2 PG 3 WC Medicine, Research & Experimental SC Research & Experimental Medicine GA GR021 UT WOS:A1991GR02100013 PM 1779918 ER PT J AU HOGAN, KP SMITH, AP ZISKA, LH AF HOGAN, KP SMITH, AP ZISKA, LH TI POTENTIAL EFFECTS OF ELEVATED CO2 AND CHANGES IN TEMPERATURE ON TROPICAL PLANTS SO PLANT CELL AND ENVIRONMENT LA English DT Review DE CLIMATE CHANGE; ELEVATED CO2; PHOTOSYNTHESIS; STRESS; TEMPERATURE; TROPICAL; WATER USE EFFICIENCY ID ULTRAVIOLET-B RADIATION; GLOBAL CARBON-CYCLE; WATER RELATIONS; RAIN-FOREST; ATMOSPHERIC CO2; CLIMATE CHANGE; COSTA-RICA; PHOTOSYNTHETIC RESPONSES; AMAZON DEFORESTATION; INSECT HERBIVORE AB Very little attention has been directed at the responses of tropical plants to increases in global atmospheric CO2 concentrations and the potential climatic changes. The available data, from greenhouse and laboratory studies, indicate that the photosynthesis, growth and water use efficiency of tropical plants can increase at higher CO2 Concentrations. However, under field conditions abiotic (light, water or nutrients) or biotic (competition or herbivory) factors might limit these responses. In general, elevated atmospheric CO2 concentrations seem to increase plant tolerance to stress, including low water availability, high or low temperature, and photoinhibition. Thus, some species may be able to extend their ranges into physically less favourable sites, and biological interactions may become relatively more important in determining the distribution and abundance of species. Tropical plants may be more narrowly adapted to prevailing temperature regimes than are temperate plants, so expected changes in temperature might be relatively more important in the tropics. Reduced transpiration due to decreased stomatal conductance could modify the effects of water stress as a cue for vegetative or reproductive phenology of plants of seasonal tropical areas. The available information suggests that changes in atmospheric CO2 concentrations could affect processes as varied as plant/herbivore interactions, decomposition and nutrient cycling, local and geographic distributions of species and community types, and ecosystem productivity. However, data on tropical plants are few, and there seem to be no published tropical studies carried out in the field. Immediate steps should be undertaken to reduce our ignorance of this critical area. C1 USDA ARS,BELTSVILLE AGR RES CTR,CLIMATE STRESS LAB,BELTSVILLE,MD 20705. RP HOGAN, KP (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. NR 166 TC 79 Z9 81 U1 1 U2 23 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 OCT PY 1991 VL 14 IS 8 BP 763 EP 778 DI 10.1111/j.1365-3040.1991.tb01441.x PG 16 WC Plant Sciences SC Plant Sciences GA GP369 UT WOS:A1991GP36900003 ER PT J AU DRAKE, BG LEADLEY, PW AF DRAKE, BG LEADLEY, PW TI CANOPY PHOTOSYNTHESIS OF CROPS AND NATIVE PLANT-COMMUNITIES EXPOSED TO LONG-TERM ELEVATED CO2 SO PLANT CELL AND ENVIRONMENT LA English DT Review DE ELEVATED CO2; CANOPY PHOTOSYNTHESIS; ECOSYSTEM CARBON BUDGET; UNMANAGED ECOSYSTEMS; GAS EXCHANGE; C3 AND C4 ID ATMOSPHERIC CARBON-DIOXIDE; ESTUARINE MARSH; TRANSPIRATION RESPONSES; SOYBEAN PHYSIOLOGY; TUSSOCK TUNDRA; SALT-MARSH; CO2-ENRICHMENT; TEMPERATURE; ENRICHMENT; GROWTH AB There have been seven studies of canopy photosynthesis of plants grown in elevated atmospheric CO2: three of seed crops, two of forage crops and two of native plant ecosystems. Growth in elevated CO2 increased canopy photosynthesis in all cases. The relative effect of CO2 was correlated with increasing temperature: the least stimulation occurred in tundra vegetation grown at an average temperature near 10-degrees-C and the greatest in rice grown at 43-degrees-C. In soybean, effects of CO2 were greater during leaf expansion and pod fill than at other stages of crop maturation. In the longest running experiment with elevated CO2 treatment to date, monospecific stands of a C3 sedge, Scirpus olneyi (Grey), and a C4 grass, Spartina patens (Ait.) Muhl., have been exposed to twice normal ambient CO2 concentrations for four growing seasons, in open top chambers on a Chesapeake Bay salt marsh. Net ecosystem CO2 exchange per unit green biomass (NCE(b)) increased by an average of 48% throughout the growing season of 1988, the second year of treatment. Elevated CO2 increased net ecosystem carbon assimilation by 88% in the Scirpus olneyi community and 40% in the Spartina patens community. RP DRAKE, BG (reprint author), SMITHSONIAN INST,ENVIRONM RES CTR,POB 28,EDGEWATER,MD 21037, USA. RI Leadley, Paul/E-4773-2012 NR 42 TC 135 Z9 137 U1 3 U2 18 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 OCT PY 1991 VL 14 IS 8 BP 853 EP 860 DI 10.1111/j.1365-3040.1991.tb01448.x PG 8 WC Plant Sciences SC Plant Sciences GA GP369 UT WOS:A1991GP36900010 ER PT J AU SMITH, MP BARROWS, EM AF SMITH, MP BARROWS, EM TI EFFECTS OF LARVAL CASE SIZE AND HOST PLANT-SPECIES ON CASE INTERNAL TEMPERATURE IN THE BAGWORM, THYRIDOPTERYX-EPHEMERAEFORMIS (HAWORTH) (LEPIDOPTERA, PSYCHIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE PSYCHIDAE; THYRIDOPTERYX-EPHEMERAEFORMIS; THERMOBIOLOGY; JUNIPERUS; ROBINIA AB We examined the internal temperatures of cases of bagworms, Thyridopteryx ephemeraeformis, that fed on and made cases from Juniperus chinensis pfitzeriana, J. virginiana, and Robinia pseudoacacia. Case size and host-plant species affected case internal temperatures during heating under laboratory conditions. Case size affected case internal temperature of bagworms from R. pseudoacacia that were heated by the sun outdoors. RP SMITH, MP (reprint author), SMITHSONIAN INST,MARINE SYST LAB,WASHINGTON,DC 20560, USA. NR 0 TC 3 Z9 3 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 1991 VL 93 IS 4 BP 834 EP 838 PG 5 WC Entomology SC Entomology GA GU465 UT WOS:A1991GU46500004 ER PT J AU KENYON, SJ HARTMANN, LW KOLOTILOV, EA AF KENYON, SJ HARTMANN, LW KOLOTILOV, EA TI ON THE FU ORIONIS VARIABLE V1515 CYGNI SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE VARIABLE STAR; FU ORIONIS TYPE; CIRCUMSTELLAR MATTER ID MASS-LOSS; STARS; OBJECTS; WINDS; EVOLUTION; ACCRETION; SPECTRA; LINES; DUST AB We present optical/infrared photometric and spectroscopic observations of the pre-main-sequence FU Ori object V1515 Cyg. Our observations show this variable star has many features in common with other FU Orionis objects, including a variation of spectral type with wavelength of observation, strong 2.3-mu-m CO absorption bands, and a large infrared excess. These features are consistent with our accretion disk model for FU Ori eruptions. We interpret the 1980 optical photometric minimum as a dust condensation event in the outflowing wind of V1515 Cyg-the slow recovery from the minimum was caused by expansion of the dust cloud in the wind. The depth of the minimum and the recovery time suggest dust formation occurred in material with a temperature of 500 K-700 K at a radial distance of 1-2 x 10(15) cm from the mass-losing source. A mass-loss rate of 1-3 x 10(-5) M. yr-1 can produce the conditions required for dust formation in the wind of V1515 Cyg; this result agrees with previous estimates of the mass-loss rate in this system. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. PK STERNBERG STATE ASTRON INST,CRIMEAN LAB,CRIMEA 334413,UKRAINE,USSR. OI Kenyon, Scott/0000-0003-0214-609X NR 41 TC 30 Z9 30 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 OCT PY 1991 VL 103 IS 668 BP 1069 EP 1076 DI 10.1086/132926 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GN363 UT WOS:A1991GN36300002 ER PT J AU FAN, CZ WANG, CS WANG, SJ ZHANG, MS CHASE, WT HAN, ZQ AF FAN, CZ WANG, CS WANG, SJ ZHANG, MS CHASE, WT HAN, ZQ TI A STUDY ON THE CHEMICAL MECHANISM FOR POWDER CORROSION OF BRONZE ALLOY SO SCIENCE IN CHINA SERIES B-CHEMISTRY LIFE SCIENCES & EARTH SCIENCES LA English DT Article DE ELEMENT LINE ANALYSIS; CRYSTAL-GAP CORROSION GROOVE; VICIOUS CIRCLE AB A Cu-Sn-Pb alloy modelled after an antique was cast and the powder-corrosion (P-C) was prepared on it under simulated natural conditions. The main components of the corrosion are much like those of the ancient bronze powder corrosion. It is found that chloride, water and oxygen are the essential factors for P-C formation of which chlorine plays the most important role. According to the results of experiments and thermodynamic calculations, the chemical mechanism of the copper desease was studied. It is pointed out that the fast spread of P-C is caused by two vicious circles. C1 SMITHSONIAN INST,ARTHUR M SACKLER GALLERY FREER GALLERY ART,WASHINGTON,DC 20560. MUSEUM FUYANG,FUYANG 236004,PEOPLES R CHINA. RP FAN, CZ (reprint author), UNIV SCI & TECHNOL CHINA,HEFEI 230026,PEOPLES R CHINA. NR 6 TC 0 Z9 1 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 1001-652X J9 SCI CHINA SER B JI Sci. China Ser. B-Chem. Life Sci. Earth Sci. PD OCT PY 1991 VL 34 IS 10 BP 1164 EP 1173 PG 10 WC Chemistry, Multidisciplinary SC Chemistry GA GR877 UT WOS:A1991GR87700002 ER PT J AU GREEN, DWE AF GREEN, DWE TI UFOS ARE REAL SO SCIENTIFIC AMERICAN LA English DT Letter RP GREEN, DWE (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 0 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 OCT PY 1991 VL 265 IS 4 BP 12 EP 12 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA GL869 UT WOS:A1991GL86900006 ER PT J AU LUBAR, S AF LUBAR, S TI THE TRANSFORMATION OF ANTEBELLUM PATENT-LAW SO TECHNOLOGY AND CULTURE LA English DT Article RP LUBAR, S (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,DIV ENGN & IND,WASHINGTON,DC 20560, USA. NR 86 TC 21 Z9 21 U1 0 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 1991 VL 32 IS 4 BP 932 EP 959 DI 10.2307/3106157 PG 28 WC History & Philosophy Of Science SC History & Philosophy of Science GA HD288 UT WOS:A1991HD28800006 ER PT J AU JANSSEN, BS AF JANSSEN, BS TI PAPERS RELATING TO THE ADMINISTRATION OF THE UNITED-STATES PATENT OFFICE DURING THE SUPERINTENDENCY OF THORNTON,WILLIAM, 1802-1828 - HARRIS,CM, PRESTON,D SO TECHNOLOGY AND CULTURE LA English DT Book Review RP JANSSEN, BS (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,DIV TEXT,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 1991 VL 32 IS 4 BP 1111 EP 1113 DI 10.2307/3106169 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA HD288 UT WOS:A1991HD28800018 ER PT J AU SHARRER, GT AF SHARRER, GT TI THE BUSINESS OF BREEDING - HYBRID CORN IN ILLINOIS, 1890-1940 - FITZGERALD,D SO TECHNOLOGY AND CULTURE LA English DT Book Review RP SHARRER, GT (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 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 1991 VL 32 IS 4 BP 1117 EP 1119 DI 10.2307/3106173 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA HD288 UT WOS:A1991HD28800022 ER PT J AU MORRISON, JC BOTTCHER, C BOTTRELL, G AF MORRISON, JC BOTTCHER, C BOTTRELL, G TI SPLINE CALCULATIONS OF THE PHOTOIONIZATION OSCILLATOR-STRENGTHS OF H-3+ SO THEORETICA CHIMICA ACTA LA English DT Article DE NUMERICAL CALCULATION; OSCILLATOR STRENGTH; MOLECULAR ION ID BODY PERTURBATION-THEORY; NUMERICAL HARTREE-FOCK; DIATOMIC-MOLECULES; SCF CALCULATIONS; BASIS-SETS AB We apply spline methods to the problem of calculating continuum excitation probabilities of molecular systems under the influence of electromagnetic fields. Numerical results are given for the H-3+ molecular ion. C1 OAK RIDGE NATL LAB, DIV PHYS, OAK RIDGE, TN 37831 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOLEC PHYS, CAMBRIDGE, MA 02138 USA. RP UNIV LOUISVILLE, DEPT PHYS, LOUISVILLE, KY 40292 USA. NR 36 TC 7 Z9 7 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0040-5744 J9 THEOR CHIM ACTA JI Theor. Chim. Acta PD OCT PY 1991 VL 80 IS 4-5 BP 245 EP 255 DI 10.1007/BF01117412 PG 11 WC Chemistry, Physical SC Chemistry GA GM733 UT WOS:A1991GM73300002 ER PT J AU SMITH, PL YOSHINO, K PARKINSON, WH ITO, K STARK, G AF SMITH, PL YOSHINO, K PARKINSON, WH ITO, K STARK, G TI HIGH-RESOLUTION, VUV (147-201-NM) PHOTOABSORPTION CROSS-SECTIONS FOR C2H2 AT 195-K AND 295-K SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article; Proceedings Paper CT 2ND INTERNATIONAL CONF ON LABORATORY RESEARCH FOR PLANETARY ATMOSPHERES ( 2ND ICLRPA ) CY OCT 21, 1990 CL UNIV VIRGINIA CHARLOTTESVILLE, CHARLOTTESVILLE, VA SP NASA, GODDARD SPACE FLIGHT CTR, UNIV MARYLAND, UNIV TENNESSEE, UNIV VIRGINIA HO UNIV VIRGINIA CHARLOTTESVILLE ID VIBRATION-ROTATION CONSTANTS; X BAND SYSTEM; UPPER-ATMOSPHERE; SPECTROSCOPIC FACILITY; WAVELENGTH BANDS; ACETYLENE; ULTRAVIOLET; TEMPERATURE; SPECTRUM; URANUS AB Acetylene, C2H2, plays an important role in the photochemistry of the atmospheres of the giant planets, in part because of its strong absorption features in the 145-200 nm region where there is significant solar flux. Accurate photoabsorption cross section data at the temperatures of planetary atmospheres are required for interpretation of observations and for reliable photochemical models. We have measured the photoabsorption cross sections of acetylene at 195 and 295 K in the wavelength range 147-201 nm. (The 295 K measurements extend to 137 nm.) The high-resolution spectrometers employed had instrumental bandwidths smaller than those used in previous measurements and therefore produced cross sections that are less influenced by instrumental effects. Our results indicate that hot bands make small but significant contributions to the room temperature absorption spectrum of C2H2. Photochemical models of planetary atmospheres should employ cross sections measured at the temperatures of these atmospheres. C1 NATL LAB HIGH ENERGY PHYS,PHOTON FACTORY,TSUKUBA,IBARAKI 305,JAPAN. WELLESLEY COLL,DEPT PHYS,WELLESLEY,MA 02181. RP SMITH, PL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 22 TC 34 Z9 34 U1 3 U2 7 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 SEP 25 PY 1991 VL 96 IS E2 BP 17529 EP 17533 DI 10.1029/91JE01739 PG 5 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA GJ255 UT WOS:A1991GJ25500014 ER PT J AU BRODIE, JP HUCHRA, JP AF BRODIE, JP HUCHRA, JP TI EXTRAGALACTIC GLOBULAR-CLUSTERS .3. METALLICITY COMPARISONS AND ANOMALIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE CLUSTERS - GLOBULAR; GALAXIES - STELLAR CONTENT; STARS - ABUNDANCES ID SPECTRAL-ENERGY-DISTRIBUTIONS; EARLY-TYPE GALAXIES; ELLIPTICAL GALAXIES; STELLAR POPULATIONS; INFRARED PHOTOMETRY; IRREGULAR GALAXIES; RADIAL-VELOCITY; DWARF GALAXIES; VIRGO CLUSTER; M31 AB Using a method based on the strengths of six absorption line indices measured in integrated spectra, we have derived metallicities for 22 globular clusters associated with the Sc galaxy, M33, 10 globular clusters associated with the giant elliptical galaxy, M87, eight globular clusters associated with the Sb(r)I-II galaxy, M81, and three globular clusters associated with the Fornax dwarf elliptical galaxy. In addition, we have derived mean metallicities for 38 bright galaxies, mostly ellipticals, 29 dwarf elliptical galaxies in the Virgo cluster, 10 dwarf elliptical galaxies in the Fornax cluster and four local group dwarf galaxies. Comparing these results with metallicities we previously derived for 149 clusters in M31 and with the Milky Way cluster metallicities, we show that the mean metallicity of a cluster system is linearly related to the luminosity of the parent galaxy. A similar relationship is suggested between galaxy metallicity and luminosity for the bright and dwarf galaxies, although metallicity is not the only parameter differentiating the spectroscopic properties of galaxies. The slope of the relationship between the mean metallicity of a cluster system and parent galaxy luminosity is very similar to the slope of the relationship between galaxy metallicity and luminosity, but there is an offset in the sense that the clusters are more metal poor. Investigation of the distribution of 12 different line strength indices versus metallicity for clusters and galaxies shows a remarkable uniformity in abundance characteristics among these diverse populations. The only apparent abundance anomalies are in the strengths of cyanogen (4170 angstrom) and the Ca II H and K lines, both of which are enhanced in M31 globular clusters. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP BRODIE, JP (reprint author), UNIV CALIF SANTA CRUZ,LICK OBSERV,UNIV CALIF OBSERV,SANTA CRUZ,CA 95064, USA. NR 64 TC 205 Z9 207 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 1991 VL 379 IS 1 BP 157 EP 167 DI 10.1086/170492 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GF749 UT WOS:A1991GF74900014 ER PT J AU LEES, JF KNAPP, GR RUPEN, MP PHILLIPS, TG AF LEES, JF KNAPP, GR RUPEN, MP PHILLIPS, TG TI MOLECULAR GAS IN ELLIPTIC GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES - INTERSTELLAR MATTER; INTERSTELLAR - ABUNDANCES; INTERSTELLAR - MOLECULES ID ULTRAVIOLET-EXCESS GALAXIES; H-I OBSERVATIONS; NEUTRAL-HYDROGEN CONTENT; POWERFUL RADIO GALAXIES; EMISSION-LINE GALAXIES; COMPACT DWARF GALAXIES; X-RAY-PROPERTIES; STAR-FORMATION; SEYFERT-GALAXIES; GALACTIC NUCLEI AB Observations of 24 early-type galaxies, mostly far-infrared (FIR)-bright ellipticals, in the CO-12(2-1) emission line resulted in 10 detections including eight out of the 20 ellipticals. Eight of these galaxies have not previously been detected. A search of the literature reveals a total of 17 elliptical galaxies, including our eight detections, with observed molecular gas, as well as 27 upper limits. Thus, our study almost doubles the number of elliptical galaxies detected in CO emission. The detected ellipticals have typical molecular gas masses of about 10(7)-10(8) M., similar to their H I masses, and an approximately power-law distribution of M(H)2/L(B) (in contrast to the Gaussian distribution for later type galaxies), extending to much lower values than for the spirals. The lenticular galaxies have CO properties intermediate between the elliptical and spiral systems. The 27 early-type galaxies which are detected in both molecular and atomic gas have the same mean ratio of molecular to atomic gas mass as later type spirals (albeit with a larger dispersion), similar ratios of H-alpha luminosity and FIR luminosity to molecular gas mass, and identical FIR colors. Thus, these (mostly FIR-bright) ellipticals seem to have global interstellar medium properties similar to those in late-type galaxies, but on a much smaller scale. A comparison of the properties of those ellipticals which have been detected in CO with the undetected galaxies indicates that the molecular gas may occur preferentialy in the bluer, lower luminosity dwarf ellipticals, which have more than twice the detection rate of the brighter galaxies. Both the detected and undetected ellipticals are at the same mean distance; however, it may be more difficult to detect gas in bright galaxies because of their larger line widths. Further study of the bright ellipticals is needed to verify this conclusion. The detected ellipticals also tend to be much brighter in the far-infrared, implying the presence of cold dust and/or star formation associated with the molecular gas. Our high detection rate, and the power-law distribution of M(H)2/L(B), implies that most FIR-bright ellipticals probably contain a molecular interstellar medium. For those ellipticals in which molecular gas is detected, the lack of correlation between the molecular gas mass and the blue luminosity argues for an external origin for this gas. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. CALTECH, DOWNS LAB PHYS, PASADENA, CA 91125 USA. RP LEES, JF (reprint author), PRINCETON UNIV OBSERV, PEYTON HALL, PRINCETON, NJ 08544 USA. NR 258 TC 123 Z9 123 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 SEP 20 PY 1991 VL 379 IS 1 BP 177 EP 215 DI 10.1086/170494 PN 1 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GF749 UT WOS:A1991GF74900016 ER PT J AU BARSONY, M SCHOMBERT, JM KISHALAS, K AF BARSONY, M SCHOMBERT, JM KISHALAS, K TI THE LKH-ALPHA 101 INFRARED CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE CLUSTERS - OPEN; INFRARED - SOURCES; STARS - BE; STARS - BROWN DWARFS; STARS - INDIVIDUAL (LKH-ALPHA-101); STARS - PRE-MAIN-SEQUENCE ID OPHIUCHI DARK CLOUD; RHO-OPHIUCHI; STARS; DISTRIBUTIONS; DISCOVERY; CORE AB An 8' x 12' area, corresponding to a 1.9 x 2.8 pc field centered on the Herbig Ae/Be star, LkH-alpha 101, has been mapped in the near-infrared J and K (1.2 and 2.2-mu-m) bandpasses at 1''.35 pixel-1 resolution using IRIM on the KPNO 1.3 m telescope. We report the discovery of an embedded cluster of more than 100 young stellar objects within this area. We estimate our completeness limits to be 16.5 mag at J and 14.5 mag at K, although sources as faint as K = 16.0 and J = 17.5 were detected. We have identified four types of cluster members, defined by their location in the K versus J-K color magnitude diagram: (1) accreting protostars (the Class I sources of Lada and Wilking, which are the sources with J-K > 4), (2) probable accreting protostars (sources with 3 < J-K < 4), (3) embedded, low-mass, pre-main-sequence (PMS) stars younger than 10(6) yr (sources with K < 13.4 and 2 < J-K < 3), and (4) young (almost-equal-to 10(6) yr), embedded, brown dwarf candidates (sources with K > 13.4 and 2 < J-K < 3). According to this classification scheme, the embedded cluster population of the LkH-alpha 101 cloud core consists of 16 Class I sources, 39 probable Class I sources, 40 young, embedded, low-mass, PMS stars, and 46 young, embedded, brown dwarf candidates. Only eight of the latter have J counterparts. From the relative numbers of sources of each type, we estimate an upper limit for the accreting protostar phase of 4 x 10(5) yr. The spatial distribution of the sources in the cloud core is highly nonuniform, such that the youngest sources are the most centrally concentrated. In keeping with this trend, it appears that the most massive star of the cluster, LkH-alpha 101, is probably the youngest. There is also a hint of mass segregation in the cluster, such that almost-equal-to 58% of the brown dwarf candidate sources are concentrated in 17% of the observed area. The star formation efficiency (SFE) in the central 2' x 2' of this cluster is almost-equal-to 18%. In the densest parts of the cluster, the observed stellar density places a limit of 1 star per almost-equal-to (2.7 x 10(17) cm)3 for the initial volume of gas which can eventually form a star. This volume corresponds to initial masses of 0.045, 0.45, and 4.5 M. for uniform densities of rho-H2 = 10(3), 10(4), and 10(5) cm-3, respectively. We find an upper limit of 4 x 10(5) yr for the protostellar collapse phase in this cluster and infall rates of 1.1 x 10(-7), 1.1 x 10(-6), and 1.1 x 10(-5) M. yr-1, corresponding to the above-quoted stellar masses if the collapse time is assumed independent of the final stellar mass. C1 UNIV MICHIGAN, DEPT ASTRON, ANN ARBOR, MI 48109 USA. UNIV MICHIGAN, DEPT ASTRON, ANN ARBOR, MI 48109 USA. KITT PEAK NATL OBSERV, NATL OPT ASTRON OBSERV, TUCSON, AZ 85726 USA. RP BARSONY, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, MS-78, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 35 TC 40 Z9 40 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 SEP 20 PY 1991 VL 379 IS 1 BP 221 EP 231 DI 10.1086/170496 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GF749 UT WOS:A1991GF74900018 ER PT J AU NARAYAN, R PIRAN, T SHEMI, A AF NARAYAN, R PIRAN, T SHEMI, A TI NEUTRON-STAR AND BLACK-HOLE BINARIES IN THE GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE BLACK HOLES; GAMMA-RAYS, BURSTS; GRAVITATION; PULSARS; STARS, BINARIES; STARS, COLLPASED ID X-RAY BINARIES; RADIO PULSARS; ORIGIN AB We present a statistical analysis of the number and birthdate of double neutron star (NS-NS) binaries. We estimate that there are approximately 10(4.5)z0 such systems in the Galaxy, with a birthrate approximately 10(-5)z0 yr-1, where z0 (kpc) is their scale height; we expect z0 approximately few kpc. We find that mergers of NS-NS binaries through gravitational radiation losses should be occurring roughly once a year in galaxies within 200/h Mpc. Also, we estimate that one out of approximately 10(2)/z0 massive stars in close binaries ends up in a NS-NS system. Progenitor stars more massive than approximately 50 M. probably form black holes (BHs). We estimate that the number and formation rate of BH-NS binaries in the Galaxy are comparable to the corresponding estimates for NS-NS binaries, and we predict that a BH-NS binary is likely to be discovered in pulsar surveys. Such an object may be an even better general relativistic laboratory than PSR 1913 + 16 or PSR 1534 + 12. BH-NS binaries may also be strong sources of gravitational radiation. C1 HEBREW UNIV JERUSALEM,RACAH INST PHYS,JERUSALEM,ISRAEL. TEL AVIV UNIV,DEPT PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL. RP NARAYAN, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 30 TC 293 Z9 294 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 SEP 20 PY 1991 VL 379 IS 1 BP L17 EP L20 DI 10.1086/186143 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GF750 UT WOS:A1991GF75000004 ER PT J AU ELVIS, M GIOMMI, P WILKES, BJ MCDOWELL, J AF ELVIS, M GIOMMI, P WILKES, BJ MCDOWELL, J TI PERSISTENCE AND CHANGE IN THE SOFT-X-RAY SPECTRUM OF THE QUASAR PG 1211+143 SO ASTROPHYSICAL JOURNAL LA English DT Article DE QUASARS; X-RAYS, SOURCES; X-RAYS, SPECTRA ID VARIABILITY; EXCESS; AGN; EMISSION; HOT AB Two Einstein and three EXOSAT observations of PG 1211 + 143 over a 6 year baseline show that strong steep-spectrum low-energy X-ray emission is a persistent feature of this quasar. EXOSAT observations of PG 1211 + 143 detected a factor of 2.3 increase in its steep soft X-ray (C-band) flux in 18 days. The bulk of the soft X-ray emission of PG 1211 + 143 therefore comes from a region less than 5 x 10(16) cm across. In another (quasar rest frame) interval of 193 days the soft X-rays decreased by a factor of 3.7. Either an intrinsic emission variation or an increase of N(H) from 3.4 to 7.6 x 10(20) atoms cm-2 could produce the same change. In the same time interval the hard (2-10 keV) X-rays decreased by a factor 1.6 +/- 0.05. This suggests a connection between the two energy regimes and argues against variable absorption causing the soft X-ray variations. In order to decrease in luminosity so rapidly a thermal source in PG 1211 + 143 would have to be optically thick to both electron scattering and free-bound absorption. The same argument applies to six of the seven other rapidly variable soft excesses reported in the literature, which suggests that optically thin thermal models are ruled out in general. C1 EUROPEAN SPACE TECHNOL CTR,EXOSAT OBSERV,2200 AG NOORDWIJK,NETHERLANDS. RP ELVIS, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI giommi, paolo/0000-0002-2265-5003; Wilkes, Belinda/0000-0003-1809-2364 NR 45 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 SEP 10 PY 1991 VL 378 IS 2 BP 537 EP 542 DI 10.1086/170454 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GD781 UT WOS:A1991GD78100010 ER PT J AU MARKEVITCH, M BLUMENTHAL, GR FORMAN, W JONES, C SUNYAEV, RA AF MARKEVITCH, M BLUMENTHAL, GR FORMAN, W JONES, C SUNYAEV, RA TI DO CLUSTERS OF GALAXIES AFFECT THE SPECTRUM OF THE MICROWAVE BACKGROUND SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMIC BACKGROUND RADIATION; COSMOLOGY; GALAXIES, CLUSTERING ID HOT AB Motivated by recent COBE limits on the spectral distortions in the cosmic microwave background radiation, we calculate the distortion, averaged over the sky, due to the Compton scattering of background photons with electrons in the hot gas in clusters of galaxies. Using an existing sample of X-ray clusters, various values of the density parameter OMEGA, and plausible models for cluster evolution (or lack thereof), we generate Monte Carlo realizations of the microwave sky. The spatial structure of these simulations shows a network of discrete sources whose properties can be a strong function of both evolution and OMEGA. The amount of spectral distortion in the models is greatest for models characterized by self-similar cluster evolution in an open universe and is within an order of magnitude of the current upper limits. Thus, improved observational sensitivity must inevitably detect some deviation from a blackbody spectrum. C1 UNIV CALIF SANTA CRUZ,LICK OBSERV,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064. ACAD SCI USSR,INST SPACE RES,MOSCOW 117810,USSR. RP MARKEVITCH, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 18 TC 23 Z9 23 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 SEP 10 PY 1991 VL 378 IS 2 BP L33 EP L36 DI 10.1086/186135 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GD782 UT WOS:A1991GD78200001 ER PT J AU SCOTT, TC DALGARNO, A MORGAN, JD AF SCOTT, TC DALGARNO, A MORGAN, JD TI EXCHANGE ENERGY OF H2+ CALCULATED FROM POLARIZATION PERTURBATION-THEORY AND THE HOLSTEIN-HERRING METHOD SO PHYSICAL REVIEW LETTERS LA English DT Article ID GROUND-STATE-ENERGY; 1/R EXPANSION; HYDROGEN; ASYMPTOTICS; BEHAVIOR; CURVES; ATOMS; TERMS; H-2+ AB Tang, Toennies, and Yiu have shown that unsymmetrized Rayleigh-Schrodinger perturbation theory can be used to calculate the leading terms in the ground-state exchange energy of H-2+ using the method of Holstein and Herring. We clarify this seemingly puzzling result by showing that their approximation to the polarization wave function is exactly the leading term of the Herring-Holstein function. We also show that a generalization of their method yields the leading asymptotic exchange energy terms for excited states, thereby suggesting the existence of a general underlying property and the applicability of the method to many-electron systems. C1 UNIV DELAWARE,DEPT PHYS & ASTRON,NEWARK,DE 19716. RP SCOTT, TC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 27 TC 28 Z9 28 U1 0 U2 7 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 SEP 9 PY 1991 VL 67 IS 11 BP 1419 EP 1422 DI 10.1103/PhysRevLett.67.1419 PG 4 WC Physics, Multidisciplinary SC Physics GA GD965 UT WOS:A1991GD96500013 ER PT J AU WORL, R AF WORL, R TI OIL AGE ESKIMOS - JORGENSEN,JG SO AMERICAN ANTHROPOLOGIST LA English DT Book Review RP WORL, R (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 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 1991 VL 93 IS 3 BP 745 EP 746 DI 10.1525/aa.1991.93.3.02a00640 PG 2 WC Anthropology SC Anthropology GA GF761 UT WOS:A1991GF76100063 ER PT J AU KEENLEYSIDE, A MANN, R AF KEENLEYSIDE, A MANN, R TI A RARE FORM OF METATARSAL SYNOSTOSIS SO AMERICAN JOURNAL OF ROENTGENOLOGY LA English DT Letter C1 SMITHSONIAN INST,WASHINGTON,DC 20560. RP KEENLEYSIDE, A (reprint author), MCMASTER UNIV,HAMILTON L8S 4L9,ONTARIO,CANADA. NR 4 TC 1 Z9 1 U1 0 U2 0 PU AMER ROENTGEN RAY SOC PI RESTON PA 1891 PRESTON WHITE DR SUBSCRIPTION FULFILLMENT, RESTON, VA 22091 SN 0361-803X J9 AM J ROENTGENOL JI Am. J. Roentgenol. PD SEP PY 1991 VL 157 IS 3 BP 648 EP 648 PG 1 WC Radiology, Nuclear Medicine & Medical Imaging SC Radiology, Nuclear Medicine & Medical Imaging GA GB719 UT WOS:A1991GB71900050 PM 1872256 ER PT J AU DUNN, PJ GRICE, JD CRIDDLE, A STANLEY, C AF DUNN, PJ GRICE, JD CRIDDLE, A STANLEY, C TI CIANCIULLIITE, A NEW MAGNESIUM MANGANESE ZINC HYDROXIDE FROM FRANKLIN, NEW-JERSEY SO AMERICAN MINERALOGIST LA English DT Article AB Cianciulliite, Mn(Mg,Mn)2Zn2(OH)10.2-4H2O, is a new species from Franklin, New Jersey. It is monoclinic, C2/m, with a = 15.47(2), b = 6.369(6), c = 5.576(6) angstrom, beta = 101.29(9)-degrees, Z = 2, and D(calc) = 2.87 g/cm3. It is dark reddish brown, occurs in flattened crystals, shows perfect cleavage on {100}, and has highly contrasting, form-selective lusters, pearly to dull on {100} and vitreous on other forms. C1 CANADIAN MUSEUM NAT,MINERAL SCI SECT,OTTAWA K1P 6P4,ONTARIO,CANADA. BRITISH MUSEUM NAT HIST,DEPT MINERAL,LONDON SW7 5BD,ENGLAND. RP DUNN, PJ (reprint author), SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560, USA. OI Stanley, Christopher/0000-0002-6015-5210 NR 2 TC 1 Z9 1 U1 0 U2 2 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 SEP-OCT PY 1991 VL 76 IS 9-10 BP 1708 EP 1710 PG 3 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA GL397 UT WOS:A1991GL39700025 ER PT J AU GRICE, JD DUNN, PJ AF GRICE, JD DUNN, PJ TI THE CRYSTAL-STRUCTURE OF CIANCIULLIITE, MN(MG,MN)2ZN2(OH)10.2-4H2O SO AMERICAN MINERALOGIST LA English DT Article ID TODOROKITE BUSERITE PROBLEM; MARINE MANGANESE NODULES; MINERALOGY AB The new species cianciulliite, Mn(Mg,Mn)2Zn2(OH)10.2-4H2O, is monoclinic, C2/m, with a = 15.405(3), b = 6.344(1), c = 5.562(2) angstrom, beta = 101.23(2)-degrees, V = 533.2 angstrom3, and Z = 2. The crystal structure was solved by direct methods and refined to R = 4.0% using 675 observed X-ray diffractions. Solution of the structure was essential in determining the correct chemical composition of cianciulliite. The atomic arrangement consists of two discrete (100) layers, a brucite-type layer and an H2O layer. The brucite-type layer is formed of Mn and Mg octahedra, with the octahedral holes capped by ZnO4 tetrahedra. The apical OH of the Zn tetrahedra are H bonded to the H2O layer. The H2O layer readily loses H2O during microprobe and X-ray analysis. C1 SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560. RP GRICE, JD (reprint author), CANADIAN MUSEUM NAT,MINERAL SCI SECT,OTTAWA K1P 6P4,ONTARIO,CANADA. NR 10 TC 4 Z9 4 U1 1 U2 1 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 SEP-OCT PY 1991 VL 76 IS 9-10 BP 1711 EP 1714 PG 4 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA GL397 UT WOS:A1991GL39700026 ER PT J AU EMMONS, LH AF EMMONS, LH TI FRUGIVORY IN TREESHREWS (TUPAIA) SO AMERICAN NATURALIST LA English DT Article ID FOOD AB Four species of treeshrews (Tupaia spp.) studied in the field in Sabah, Malaysia, show intense frugivory concentrated on small, soft, bird-dispersed fruits. Observations of a wild individual and captives of two species show that treeshrews reject indigestible fibers and other parts of fruits before swallowing the pulp. Transit times of fruit through the gut are rapid and body-size dependent, with mean times to first defecation of marker dye of 20 min (range, 13-29 min) for Tupaia minor (almost-equal-to 60 g mass), and 57 min (range, 38-73 min) for Tupaia tana (220 g mass). The intestine of Tupaia species consists of a long small intestine, rudimentary or no cecum, and a greatly reduced, narrow, smooth colon. The fruit-processing method, rapid food transit time, and gut morphology of treeshrews resemble those of frugivorous bats but are unlike those of small primates. RP EMMONS, LH (reprint author), SMITHSONIAN INST, DIV MAMMALS, WASHINGTON, DC 20560 USA. NR 20 TC 19 Z9 19 U1 1 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 EI 1537-5323 J9 AM NAT JI Am. Nat. PD SEP PY 1991 VL 138 IS 3 BP 642 EP 649 DI 10.1086/285239 PG 8 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA GL946 UT WOS:A1991GL94600006 ER PT J AU PETERSEN, CW AF PETERSEN, CW TI SEX ALLOCATION IN HERMAPHRODITIC SEA BASSES SO AMERICAN NATURALIST LA English DT Article ID CORAL-REEF FISH; SERRANUS-FASCIATUS; REPRODUCTIVE EFFORT; MATING SYSTEM; STRATEGIES; EVOLUTION; BEHAVIOR; SUCCESS; PLANTS; GENDER AB Local mate competition theory has emphasized the importance of sperm competition in determining individual patterns of sex allocation in outcrossing hermaphrodites. In this article I develop a more general model of local mate competition that incorporates fertilization efficiency. I use this model to predict interspecific differences in sex allocation. These predictions are tested by using dry weights of male and female gonadal tissue from six species of hermaphroditic sea basses. In all four paired comparisons, when two of the three factors presumed to determine sex allocation patterns are relatively constant, the shift in sex allocation between species is correctly predicted. Neither levels of sperm competition nor the expected effects of spawning behavior on fertilization efficiency can account for all of the differences in sex allocation, although sperm competition does correctly predict the most differences in sex allocation. Overall, the interspecific differences are predicted by either the level of sperm competition or by factors affecting fertilization efficiency. A broader view of local mate competition that includes aspects of sperm competition and the dynamics of fertilization should ultimately provide more accurate predictions of sex allocation in hermaphroditic organisms. C1 SMITHSONIAN TROP RES INST,APO,MIAMI,FL 34002. NR 39 TC 68 Z9 68 U1 2 U2 9 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0003-0147 J9 AM NAT JI Am. Nat. PD SEP PY 1991 VL 138 IS 3 BP 650 EP 667 DI 10.1086/285240 PG 18 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA GL946 UT WOS:A1991GL94600007 ER PT J AU FORESTA, M AF FORESTA, M TI TRACING THE LINE + EXPERIMENTAL PHOTOGRAPHY OF THE 1920S AND THE 1930S - ART AND PHOTOGRAPHY IN THE AGE OF CONTACT SO APERTURE LA English DT Article RP FORESTA, M (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER ART,WASHINGTON,DC 20560, USA. NR 21 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 FAL PY 1991 IS 125 BP 16 EP 23 PG 8 WC Art SC Art GA HA321 UT WOS:A1991HA32100005 ER PT J AU ARMANDROFF, TE MASSEY, P AF ARMANDROFF, TE MASSEY, P TI WOLF-RAYET STARS IN LOCAL GROUP GALAXIES - NUMBERS AND SPECTRAL PROPERTIES SO ASTRONOMICAL JOURNAL LA English DT Article ID LARGE MAGELLANIC CLOUD; H-II REGIONS; MASSIVE STARS; SUPERNOVA-REMNANTS; STELLAR CONTENT; HOT STARS; OPTICAL SPECTROPHOTOMETRY; ABUNDANCE GRADIENT; O STARS; M33 AB A large number of spectra have been obtained of Wolf-Rayet (WR) candidates found by CCD surveys in regions of M31, M33, NGC 6822, and IC 1613. Using these newly acquired data as well as published work, we attempt to answer the questions posed at the beginning of our survey project concerning the relative population of WR stars in these galaxies, what correlation exists between metallicity and WC/WN ratio, and whether the stellar wind properties of these stars vary from system to system. We continue to find that extragalactic WR stars are readily classifiable into spectral types found in the Galaxy and Magellanic Clouds, although the latest WC types (WC8 and WC9) have so far been found only in the inner part of the Milky Way. We find two examples of intermediate WN/WC objects in M31, similar to those known in the Galaxy and LMC. Equivalent widths and full widths at half maximum are measured for the strongest emission lines to see how the stellar wind properties compare between galaxies. We find that the M33 and M31 WN stars are like those of the Galaxy and LMC, while the WN stars of NGC 6822 have weaker lines and are more like the WN stars found in the SMC. The WC stars in M33 and M31 are peculiar in that stars with narrow and strong lines are lacking. An examination of the available data on Galactic stars reveals that the WC stars with both narrow and strong lines are preferentially found in the inner part of the Milky Way along with the WC8 and WC9 stars which are missing in M33 and M31. We find that both M33 and the Galaxy show a clear change from their inner to outer regions in the distribution of WC stars in the line-strength, line-width diagram, in the sense that the stars with the strongest and broadest lines are found in the outer regions; no such change with galactocentric distance is found for the M31 WC stars. We suggest that changing metallicity is at least partially responsible for this effect. Between the inner and outer samples in the Milky Way and in M33 there is a strong change in metallicity, while the metallicity gradient in M31 is much weaker. However, some parameter(s) other than metallicity must also be acting. WC/WN ratios and WR number densities are also calculated from our data. We find that the WC/WN ratio is not a monotonic function of metallicity, in disagreement with theoretical predictions. The solar neighborhood, M33, and M31 have WC/WN ratios that agree within the errors despite their different metallicities, while the LMC and the regions surveyed in M33 have similar metallicities but very different WC/WN ratios. The WR surface density is similar in the SMC, NGC 6822, and IC1613, but is a factor of 2 higher in the LMC. The solar neighborhood and M33 have similar WR surface densities, while the most active regions in M33 have a WR surface density that is a factor of 6 higher than the most active regions in M31. C1 UNIV ARIZONA,MULTIPLE MIRROR TELESCOPE OBSERV,TUCSON,AZ 85721. SMITHSONIAN INST,MULTIPLE MIRROR TELESCOPE OBSERV,WASHINGTON,DC 20560. RP ARMANDROFF, TE (reprint author), NATL OPT ASTRON OBSERV,KITT PEAK NATL OBSERV,POB 26732,TUCSON,AZ 85726, USA. NR 57 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 SEP PY 1991 VL 102 IS 3 BP 927 EP 950 DI 10.1086/115924 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GD160 UT WOS:A1991GD16000011 ER PT J AU WILNER, DJ LADA, CJ AF WILNER, DJ LADA, CJ TI THE LUMINOSITY FUNCTION OF THE YOUNG CLUSTER NGC-2362 SO ASTRONOMICAL JOURNAL LA English DT Article ID STARS AB We construct the I band luminosity function of the young open cluster NGC 2362 from CCD photometric observations which are complete to a limiting magnitude of 17.6. After empirically correcting for the presence of background field stars, we find the cluster luminosity function to be significantly deficient in low luminosity stars compared to the luminosity function derived from the Salpeter IMF. Although it is impossible to entirely dismiss systematic uncertainties in our correction for field stars, artificial star tests confirm that the deficiency in the cluster luminosity function is not due to observational incompleteness at faint magnitudes. If the observed luminosity function is representative of the luminosity function of the entire cluster, then our observations provide strong evidence that the IMF varies on the scale of individual open clusters. However, our data does not allow us to rule out the existence of an outer halo of low luminosity stars that could account for this deficit. We also find marginal evidence for a dip in the observed luminosity function at magnitudes corresponding to ZAMS spectral types mid-A to mid-F, a characteristic that has been observed in at least one other cluster of similar age. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP WILNER, DJ (reprint author), UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720, USA. NR 23 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 SEP PY 1991 VL 102 IS 3 BP 1050 EP 1055 DI 10.1086/115931 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GD160 UT WOS:A1991GD16000018 ER PT J AU ANTHONYTWAROG, BJ HEIM, EA TWAROG, BA CALDWELL, N AF ANTHONYTWAROG, BJ HEIM, EA TWAROG, BA CALDWELL, N TI A BV PHOTOGRAPHIC AND CCD ANALYSIS OF THE INTERMEDIATE-AGE OPEN CLUSTER NGC-3680 SO ASTRONOMICAL JOURNAL LA English DT Article ID ROSSELAND OPACITY TABLES; THEORETICAL ISOCHRONES; BETA PHOTOMETRY; GALACTIC DISK; MASS STARS; NGC 3680; OLD; ABUNDANCE; POPULATION; EVOLUTION AB New photoelectric and CCD data on the BV system have been obtained in the open cluster, NGC 3680, and used to calibrate a photographic survey of over 490 stars down to V = 17.6 in the field of the cluster. The cluster color-magnitude diagram exhibits a well populated red giant clump, but effectively has no red giant branch. The turnoff region has a sharp cutoff at (B - V) = 0.4, with a red hook and a large amount of scatter, consistent with the explanation of a significant binary population. Comparison with model field star counts for this region of the sky demonstrates that the cluster main sequence is, at best, poorly populated below V = 14.0 (M(v) = 4.0). Adopting E(B - V) = 0.05, [Fe/H] = 0.1, and (m - M) = 10.0, the standard isochrones of VandenBerg [ApJS, 58, 711 (1985)] produce an age of 1.9 +/- 0.5 x 10(9) yr, but appear unable to match the morphology of the turnoff region. The discrepancy is removed when the comparison is made to isochrones which include convective overshoot. An approximate transformation relation between the respective age scales leads to an age of 4.5 x 10(9) yr for NGC 3680 on a system where the Hyades is 1.2 x 10(9) yr old and M67 is between 6 and 7 x 10(9) yr old. Comparison to the color-magnitude diagrams of clusters of similar metallicity indicates that NGC 3680 is intermediate in age to the Hyades and IC 4651, but only slightly younger than IC 4651, consistent with the color distribution of the red giants. The comparisons to both theory and observation imply that the distance modulus for the cluster needs to be increased to (m - M) = 10.3. C1 CERRO TOLOLO INTERAMER OBSERV,LA SERENA,CHILE. SMITHSONIAN INST,FL WHIPPLE OBSERV,AMADO,AZ 85645. NATL OPT ASTRON OBSERV,CERRO TOLOLO INTER AMER OBSERV,LA SERENA,CHILE. RP ANTHONYTWAROG, BJ (reprint author), UNIV KANSAS,DEPT PHYS & ASTRON,LAWRENCE,KS 66045, USA. NR 42 TC 38 Z9 38 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 1991 VL 102 IS 3 BP 1056 EP 1069 DI 10.1086/115932 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GD160 UT WOS:A1991GD16000019 ER PT J AU LUU, J AF LUU, J TI CCD PHOTOMETRY AND SPECTROSCOPY OF THE OUTER JOVIAN-SATELLITES SO ASTRONOMICAL JOURNAL LA English DT Article ID 4 TROJAN ASTEROIDS; SPECTRA; SHAPES AB We present new charge-coupled device (CCD) photometry and spectroscopy of the eight outer Jovian satellites obtained from November 1987 to February 1989. The photometry consists of light curves for J7-J12, plus BVRI colors for J6, J8-J13. Spectroscopic data include reflectance spectra for J6, J8-J11. The satellites are spectrally diverse, with reflectivity gradients ranging from neutral (0.4% +/- 0.1%/10(3) angstrom) to red (12% +/- 1%/10(3) angstrom). The satellites thus resemble a mixture of C- and D-type asteroids. Similarities between the satellites and Trojan asteroids (diverse colors, low albedos) are consistent with the hypothesis that these two groups of objects share a common origin [Kuiper, Vistas in Astronomy, 2, 1631 (1956)]. However, the satellites seem to have less extreme shapes than the Trojans, perhaps due to the longer amount of time they spent in the proto-Jupiter nebula. Physical properties of the satellites are generally consistent with, but do not prove, the capture origin theory [Pollack et al., Icarus, 37, 587 (1979)]. RP LUU, J (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, MS 52, CAMBRIDGE, MA 02138 USA. NR 33 TC 24 Z9 24 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 1991 VL 102 IS 3 BP 1213 EP 1225 DI 10.1086/115949 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GD160 UT WOS:A1991GD16000036 ER PT J AU BIEMONT, E BAUDOUX, M KURUCZ, RL ANSBACHER, W PINNINGTON, EH AF BIEMONT, E BAUDOUX, M KURUCZ, RL ANSBACHER, W PINNINGTON, EH TI THE SOLAR ABUNDANCE OF IRON - A FINAL WORD SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ATOMIC AND MOLECULAR DATA; SUN, ABUNDANCES ID FE-II LINES; OSCILLATOR-STRENGTHS; RADIATIVE LIFETIMES; LASER EXCITATION; ENERGY-LEVELS; SPECTRUM; BEAM; SUN; MODEL AB New accurate radiative lifetimes have been measured by a laser-induced-fluorescence technique for 12 selected levels of Fe+ of astrophysical interest. These new results combined with recent theoretical transition probabilities provide another contribution in order to try to solve the controversy raised during the last months concerning the content of iron in the sun. The abundance value, A(Fe) = 7.54 +/- 0.03, obtained from an extensive sample of Fe II lines, supports the "low" value of the iron abundance, in agreement with the meteoritic result. C1 UNIV MONS, FAC SCI, B-7000 MONS, BELGIUM. UNIV ALBERTA, DEPT PHYS, EDMONTON T6G 2J1, ALBERTA, CANADA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP UNIV LIEGE, INST ASTROPHYS, B-4000 COINTE OUGREE, BELGIUM. NR 41 TC 277 Z9 277 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 1991 VL 249 IS 2 BP 539 EP 544 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GJ844 UT WOS:A1991GJ84400039 ER PT J AU LEIBUNDGUT, B TAMMANN, GA CADONAU, R CERRITO, D AF LEIBUNDGUT, B TAMMANN, GA CADONAU, R CERRITO, D TI SUPERNOVA STUDIES .7. AN ATLAS OF LIGHT CURVES OF SUPERNOVAE TYPE-I SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article DE SUPERNOVAE AND SUPERNOVA REMNANTS; GENERAL; SUPERNOVAE AND SUPERNOVA REMNANTS; INDIVIDUAL ID ABSOLUTE-MAGNITUDE; PHOTOMETRY; GALAXIES; CATALOG AB We present an atlas of optical light and color curves of 75 supernovae type I. Fits to templet light and color curves provide the epochs of maximum as well as the magnitudes and colors at maximum. C1 UNIV BASEL,INST ASTRON,CH-4102 BINNINGEN,SWITZERLAND. EUROPEAN SO OBSERV,W-8046 GARCHING,GERMANY. RP LEIBUNDGUT, B (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 43 TC 114 Z9 114 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 SEP PY 1991 VL 89 IS 3 BP 537 EP 579 PG 43 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GC354 UT WOS:A1991GC35400007 ER PT J AU KENT, SM DAME, TM FAZIO, G AF KENT, SM DAME, TM FAZIO, G TI GALACTIC STRUCTURE FROM THE SPACELAB INFRARED TELESCOPE .2. LUMINOSITY MODELS OF THE MILKY-WAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, STRUCTURE; GALAXIES, THE GALAXY; INFRARED, SOURCES; INTERSTELLAR, MATTER ID ON SPIRAL GALAXIES; SURFACE PHOTOMETRY; 3-DIMENSIONAL DISTRIBUTION; RADIAL-DISTRIBUTION; MOLECULAR CLOUDS; CO SURVEY; H-I; DISK; LIGHT; BULGE AB The three-dimensional luminosity distribution of the Milky Way has been determined from a 2.4-mu-m map of the northern Galactic plane. The radial surface brightness profile of the disk has an exponential scale length of 3.0 kpc (assuming R0 = 8 kpc). The vertical distribution of light follows the law exp (-\z\/h(z)) more closely than a canonical sech2 profile. In the solar neighborhood, the scale height h(z) is approximately 247 pc (assuming R0 = 8 kpc), in agreement with star counts perpendicular to the Galactic plane. The scale height is not constant with radius but decreases to approximately 165 pc at R = 5 kpc. To first order, the bulge can be represented by an oblate spheroid with an axis ratio b/a = 0.61 and again, an exponential luminosity profile. The 2.2-mu-m/12-mu-m flux ratio for the bulge is typical of other dust-free spheroidal systems. Luminosity fluctuations along the galactic plane are found to be caused chiefly by variations in the line-of-sight extinction. These fluctuations can be reproduced quantitatively by a detailed model for the dust distribution and allow an approximate calibration of the dust/gas ratio in regions of high (10 mag at V) optical depth. RP KENT, SM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MAIL STOP 20,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 53 TC 307 Z9 309 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 SEP 1 PY 1991 VL 378 IS 1 BP 131 EP 138 DI 10.1086/170413 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GC363 UT WOS:A1991GC36300014 ER PT J AU NARAYAN, R AF NARAYAN, R TI GRAVITATIONAL LENSING, TIME-DELAY, AND ANGULAR DIAMETER DISTANCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY; DARK MATTER; GALAXIES, DISTANCES; GRAVITATIONAL LENSES ID FERMAT PRINCIPLE; IMAGES; LENSES AB Combining a model of the mass distribution in the gravitational lens Q0957 + 561 with measurements of the velocity dispersion of the primary lensing galaxy and the time delay between the two images, the Hubble constant has been recently estimated to be H0 = 37 +/- 14 km s-1 Mpc-1. The result depends weakly on the assumed value of q0 and may have systematic errors due to nonuniqueness of the model. It is shown here that the quantity that is most directly measured using a gravitational lens system is not H0 but rather the angular diameter distance d(OL) from the observer to the lens. The determination of d(OL) requires neither a knowledge of the distance to the source nor any cosmological assumption other than local isotropy and homogeneity transverse to the line of sight, again with possible systematic effects. In the case of Q0957 + 561, where the lens is at a redshift of z(L) = 0.36, the result is d(OL) = 1700 +/- 600 Mpc. If the mass distribution of the cluster surrounding the primary lens in Q0957 + 561 can be determined through independent observations, then it may be possible to estimate both H0 and q0. RP NARAYAN, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 22 TC 28 Z9 28 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 1991 VL 378 IS 1 BP L5 EP L9 DI 10.1086/186129 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GC364 UT WOS:A1991GC36400002 ER PT J AU ROGERS, RD FIELD, GB AF ROGERS, RD FIELD, GB TI A COMPTON REFLECTION MODEL FOR THE COSMIC X-RAY AND GAMMA-RAY BACKGROUNDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMIC BACKGROUND RADIATION; GAMMA-RAYS, GENERAL; X-RAYS, SOURCES ID SEYFERT-GALAXIES; COLD MATTER; ELECTRONS; NUCLEI AB We calculate the gamma-ray spectrum of an AGN in the Compton reflection model and consider the contribution of such sources to the cosmic gamma-ray background. The spectrum is composed of three parts: an X-ray power law, a broad hump from almost-equal-to 10 to 120 keV due to reprocessing of the power-law X-ray spectrum by cold gas, and gamma rays which are due to the inverse-Compton scattering of X-rays. We compute the contribution of such sources to the cosmic gamma-ray background and find that they provide an excellent fit to the entire background spectrum from 3 keV to 10 MeV. We derive constraints on the physical conditions in these sources based on our results and consider the possibility of observing such sources with GRO. RP ROGERS, RD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MAIL STOP 10,CAMBRIDGE,MA 02138, USA. NR 27 TC 11 Z9 11 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 1991 VL 378 IS 1 BP L17 EP L20 DI 10.1086/186131 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GC364 UT WOS:A1991GC36400004 ER PT J AU WAGNER, RH AF WAGNER, RH TI THE USE OF EXTRAPAIR COPULATIONS FOR MATE APPRAISAL BY RAZORBILLS, ALCA-TORDA SO BEHAVIORAL ECOLOGY LA English DT Article AB Razorbills (Alca torda) engaged in extrapair copulations (EPCs) during two phases of their breeding cycle when fertilization of eggs was not possible, suggesting that EPCs provide nongenetic benefits. Females actively pursued extrapair mountings after they completed egg laying, the first monogamous species reported to do so. Mountings were performed in mating arenas outside of the breeding colony, where attendance by postlaying females indicated that they sought encounters with extrapair males while their mates were incubating. Postlaying females always successfully resisted insemination yet positioned themselves to receive mountings. These findings support the hypothesis that resistance to insemination is a ploy used by females to appraise males. At the end of the breeding cycle, when males escorted the fledgling to sea, females remained at the colony where they consorted and sometimes copulated with other males. Nonfertilizable extrapair copulations may serve two social functions for razorbills: female appraisal of males for future fertilizable EPCs and the appraisal and acquisition of new mates by both sexes. RP WAGNER, RH (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008, USA. NR 0 TC 50 Z9 50 U1 0 U2 5 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 1991 VL 2 IS 3 BP 198 EP 203 DI 10.1093/beheco/2.3.198 PG 6 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA GU433 UT WOS:A1991GU43300002 ER PT J AU CAMARGO, JMF ROUBIK, DW AF CAMARGO, JMF ROUBIK, DW TI SYSTEMATICS AND BIONOMICS OF THE APOID OBLIGATE NECROPHAGES - THE TRIGONA-HYPOGEA GROUP (HYMENOPTERA, APIDAE, MELIPONINAE) SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE OBLIGATE NECROPHAGY; STINGLESS BEES; BEE NESTS; CARRION; TRIGONA; TROPICAL FORESTS ID STINGLESS BEES; PROVISIONS; NEST C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP CAMARGO, JMF (reprint author), UNIV SAO PAULO,FAC FILOSOFIA CIENCIAS & LETRAS RIBEIRAO PRETO,DEPT BIOL,BR-14049 RIBEIRAO PRETO,SP,BRAZIL. NR 35 TC 38 Z9 40 U1 2 U2 3 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD SEP PY 1991 VL 44 IS 1 BP 13 EP 39 DI 10.1111/j.1095-8312.1991.tb00604.x PG 27 WC Evolutionary Biology SC Evolutionary Biology GA GK232 UT WOS:A1991GK23200002 ER PT J AU LEMAITRE, R AF LEMAITRE, R TI TO THE MEMORY OF VOSS,GILBERT,L. - PORTUNUS-VOSSI, A RARE NEW SPECIES OF SWIMMING CRAB (DECAPODA, BRACHYURA, PORTUNIDAE) FROM THE WEST-COAST OF FLORIDA SO BULLETIN OF MARINE SCIENCE LA English DT Article; Proceedings Paper CT GILBERT L VOSS INTERNATIONAL SYMP AT THE 1990 ANNUAL MEETING OF THE AMERICAN MALACOLOGICAL UNION CY JUN 03-07, 1990 CL MARINE BIOL LAB, WOODS HOLE, MA SP AMER MALACOL UNION, CEPHALOPOD INT ADVISORY COUNCIL HO MARINE BIOL LAB AB A new species of swimming crab, Portunus vossi, is described from the west coat of Florida. The new species resembles Portunus ordwayi (Stimpson), but can be differentiated by the shape of the frontal teeth, the armature of the merus of the swimming leg, and the absence of iridescence on the chelae. The material of the new species was collected using a triangle dredge during environmental studies of the southwest Florida shelf ecosystem. The new species is apparently rare, or because of its possible burrowing behavior, has previously escaped more conventional sampling methods, such as otter trawls. RP LEMAITRE, R (reprint author), SMITHSONIAN OCEANOG SORTING CTR,NATL MUSEUM NAT HIST,WASHINGTON,DC 20560, USA. NR 7 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 1991 VL 49 IS 1-2 BP 546 EP 551 PG 6 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA HC568 UT WOS:A1991HC56800046 ER PT J AU OFTEDAL, OT BOWEN, WD WIDDOWSON, EM BONESS, DJ AF OFTEDAL, OT BOWEN, WD WIDDOWSON, EM BONESS, DJ TI THE PRENATAL MOLT AND ITS ECOLOGICAL SIGNIFICANCE IN HOODED AND HARBOR SEALS SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Note ID CYSTOPHORA-CRISTATA; PUPS AB Hooded and harbor seals are unique among true seals (family Phocidae) in that the lanugo (fetal pelage) is typically shed in utero. Shedding had occurred in all newborn hooded seals examined off the Labrador coast (n = 62) and in 94% of newborn harbor seals on Sable Island, Nova Scotia (n = 110), although in one-fifth of the latter the molt was incomplete. In hooded seals the shed hair in the amniotic sac was organized into tightly woven disks, whereas in harbor seals the shed hair formed a loose mat with no evident structure. We examined hair masses in the intestines of pups of both species but could find no evidence that the intestines were involved in hair disk formation. We argue that fetal shedding, like prenatal blubber deposition, is an adaptation enabling newborn pups to enter cold water without adverse consequences. This ability allows the use of pupping substrates that are unstable or regularly inundated with water. C1 FISHERIES & OCEANS CANADA,BEDFORD INST OCEANOG,DIV MARINE FISH,DARTMOUTH B2Y 4A2,NS,CANADA. UNIV CAMBRIDGE,DEPT MED,CAMBRIDGE,ENGLAND. RP OFTEDAL, OT (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008, USA. RI Bowen, William/D-2758-2012 NR 28 TC 24 Z9 24 U1 0 U2 7 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 1991 VL 69 IS 9 BP 2489 EP 2493 DI 10.1139/z91-351 PG 5 WC Zoology SC Zoology GA GX853 UT WOS:A1991GX85300032 ER PT J AU GRADWOHL, J GREENBERG, R AF GRADWOHL, J GREENBERG, R TI FORESTS IN A WARMING WORLD - A TIME FOR NEW POLICIES - COMMENT SO CLIMATIC CHANGE LA English DT Editorial Material C1 SMITHSONIAN RES CTR,MIGRATORY BIRD PROGRAM,EDGEWATER,MD 21037. RP GRADWOHL, J (reprint author), SMITHSONIAN INST,OFF ENVIRONM AWARENESS,RIPLEY CTR 3123,WASHINGTON,DC 20560, USA. NR 11 TC 2 Z9 2 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0165-0009 J9 CLIMATIC CHANGE JI Clim. Change PD SEP PY 1991 VL 19 IS 1-2 BP 253 EP 256 DI 10.1007/BF00142234 PG 4 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA GH182 UT WOS:A1991GH18200027 ER PT J AU JAMIESON, MJ DU, ML AF JAMIESON, MJ DU, ML TI LOG-DERIVATIVE METHODS BASED ON LINEAR 2-STEP INTEGRATION FORMULAS SO COMPUTER PHYSICS COMMUNICATIONS LA English DT Article ID SCATTERING; COLLISIONS AB Single- and multi-channel propagators for the log-derivative and a simple modification of it are derived from the linear two-step formulae of Hartree and Numerov. Their stabilities are briefly discussed. Their use is illustrated in a single-channel eigenvalue problem and in a multi-channel scattering problem. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. ACAD SINICA,INST THEORET PHYS,BEIJING 100080,PEOPLES R CHINA. NR 18 TC 3 Z9 3 U1 1 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0010-4655 J9 COMPUT PHYS COMMUN JI Comput. Phys. Commun. PD SEP-OCT PY 1991 VL 66 IS 2-3 BP 150 EP 156 DI 10.1016/0010-4655(91)90063-Q PG 7 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA GH799 UT WOS:A1991GH79900002 ER PT J AU ERWIN, TL AF ERWIN, TL TI HOW MANY SPECIES ARE THERE - REVISITED SO CONSERVATION BIOLOGY LA English DT Editorial Material RP ERWIN, TL (reprint author), SMITHSONIAN INST,DEPT ENTOMOL,WASHINGTON,DC 20560, USA. NR 0 TC 69 Z9 76 U1 1 U2 20 PU BLACKWELL SCIENCE INC PI CAMBRIDGE PA 238 MAIN ST, CAMBRIDGE, MA 02142 SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD SEP PY 1991 VL 5 IS 3 BP 330 EP 333 DI 10.1111/j.1523-1739.1991.tb00145.x PG 4 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA GC702 UT WOS:A1991GC70200011 ER PT J AU SCHWARTZ, JJ RAND, AS AF SCHWARTZ, JJ RAND, AS TI THE CONSEQUENCES FOR COMMUNICATION OF CALL OVERLAP IN THE TUNGARA FROG, A NEOTROPICAL ANURAN WITH A FREQUENCY-MODULATED CALL SO ETHOLOGY LA English DT Article ID COMPLEX VOCAL REPERTOIRE; ACOUSTIC INTERFERENCE; AUDITORY-NERVE; TREEFROGS; BEHAVIOR; SYSTEM; BAT; RECOGNITION; AMPHIBIANS; INTENSITY AB We presented male tungara frogs, Physalaemus pustulosus, with call-triggered computer-synthesized whines that either did or did not overlap the frogs' own frequency-modulated whines in time. When the stimulus was nonoverlapping, males added a high proportion of chuck notes to their calls. When the stimulus was overlapping, males responded with either no or only small increases in chucking. This suggests they have difficulty detecting whines while vocalizing. When female tungara frogs were given a choice between alternating whines and out-of-phase overlapping whines they did not discriminate The result with males was similar to that previously obtained with species of frogs that have amplitude-modulated advertisement callS (SCHWARTZ 1987a), the result with females was different. We discuss our findings in relation to peripheral processing of spectral and temporal information in the anuran auditory system. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP SCHWARTZ, JJ (reprint author), UNIV CONNECTICUT,DEPT ECOL & EVOLUTIONARY BIOL,BOX U-43,STORRS,CT 06269, USA. NR 40 TC 14 Z9 15 U1 1 U2 1 PU BLACKWELL WISSENSCHAFTS-VERLAG GMBH PI BERLIN PA KURFURSTENDAMM 57, D-10707 BERLIN, GERMANY SN 0179-1613 J9 ETHOLOGY JI Ethology PD SEP PY 1991 VL 89 IS 1 BP 73 EP 83 PG 11 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA GT819 UT WOS:A1991GT81900005 ER PT J AU PISANO, DA AF PISANO, DA TI TECHNICAL WORKERS IN AN ADVANCED SOCIETY - THE WORK, CAREERS, AND POLITICS OF FRENCH ENGINEERS - CRAWFORD,S SO ISIS LA English DT Book Review RP PISANO, DA (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 CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0021-1753 J9 ISIS JI Isis PD SEP PY 1991 VL 82 IS 313 BP 598 EP 598 DI 10.1086/355906 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA GJ379 UT WOS:A1991GJ37900080 ER PT J AU SEITEL, P AF SEITEL, P TI MAGIC, KNOWLEDGE, AND IRONY IN SCHOLARY EXCHANGE - A COMMENT ON CANTWELL,ROBERT OBSERVATIONS ON THE FESTIVAL-OF-AMERICAN-FOLKLIFE SO JOURNAL OF AMERICAN FOLKLORE LA English DT Note RP SEITEL, P (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 2 TC 2 Z9 2 U1 0 U2 0 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 SN 0021-8715 J9 J AM FOLKLORE JI J. Am. Folk. PD FAL PY 1991 VL 104 IS 414 BP 495 EP 496 DI 10.2307/541552 PG 2 WC Folklore SC Arts & Humanities - Other Topics GA GM761 UT WOS:A1991GM76100004 ER PT J AU HENSON, PM SCHORZMAN, TA AF HENSON, PM SCHORZMAN, TA TI VIDEOHISTORY - FOCUSING ON THE AMERICAN PAST SO JOURNAL OF AMERICAN HISTORY LA English DT Article ID ORAL-HISTORY RP HENSON, PM (reprint author), SMITHSONIAN INST,ORAL HIST,WASHINGTON,DC 20560, USA. NR 40 TC 3 Z9 3 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 1991 VL 78 IS 2 BP 618 EP 627 DI 10.2307/2079539 PG 10 WC History SC History GA GF124 UT WOS:A1991GF12400010 ER PT J AU YENER, KA SAYRE, EV JOEL, EC OZBAL, H BARNES, IL BRILL, RH AF YENER, KA SAYRE, EV JOEL, EC OZBAL, H BARNES, IL BRILL, RH TI STABLE LEAD ISOTOPE STUDIES OF CENTRAL TAURUS ORE SOURCES AND RELATED ARTIFACTS FROM EASTERN MEDITERRANEAN CHALCOLITHIC AND BRONZE-AGE SITES SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE LEAD ISOTOPES; METALS; ARTIFACTS; CENTRAL TAURUS; EASTERN MEDITERRANEAN; CHALCOLITHIC; BRONZE AGE ID BOLKARDAG C1 BOGAZICI UNIV,FAC ARTS & SCI,ISTANBUL,TURKEY. NATL INST STAND & TECHNOL,GAITHERSBURG,MD 20899. CORNING MUSEUM GLASS,CORNING,NY 14830. RP YENER, KA (reprint author), SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560, USA. NR 108 TC 54 Z9 55 U1 0 U2 6 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD SEP PY 1991 VL 18 IS 5 BP 541 EP 577 DI 10.1016/0305-4403(91)90053-R PG 37 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA GG018 UT WOS:A1991GG01800003 ER PT J AU DUDLEY, R AF DUDLEY, R TI BIOMECHANICS OF FLIGHT IN NEOTROPICAL BUTTERFLIES - AERODYNAMICS AND MECHANICAL POWER REQUIREMENTS SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE BUTTERFLY; FLIGHT; AERODYNAMICS; LIFT COEFFICIENT; MECHANICAL POWER; BIOMECHANICS ID HOVERING INSECT FLIGHT; TERRESTRIAL LOCOMOTION; ENERGY CHANGES; BODY SIZE; KINEMATICS; ENERGETICS; MUSCLE; SPEED; LIFT; BUMBLEBEES AB A quasi-steady aerodynamic analysis of forward flight was performed on 15 species of neotropical butterflies for which kinematic and morphological data were available. Mean lift coefficients required for flight typically exceeded maximum values obtained on insect wings under conditions of steady flow, thereby implicating unsteady aerodynamic mechanisms even during fast forward flight of some butterflies. The downstroke produced vertical forces on average 18% in excess of those necessary to support the body weight through the wingbeat, while the upstroke contributed minimal or negative vertical force. Estimated effective angles of incidence (alpha-r') of the wings averaged 39-degrees during the downstroke and -22-degrees during the upstroke; spanwise variation in alpha-r' was greater than the average difference between half-strokes. Total mechanical power requirements of forward flight averaged 12.5 W kg-1, for the case of perfect elastic storage of wing inertial energy, and 20.2 W kg-1, assuming zero elastic energy storage. Energetic costs of the erratic trajectories during forward flight increased mechanical power requirements by an average of 43%, assuming perfect elastic storage. Fluctuations in horizontal kinetic energy of the center of mass were principally responsible for this dramatic increase. When comparing different species, total mechanical power increased linearly with forward airspeed (assuming perfect elastic energy storage of inertial energy) and scaled with mass0.26. If no elastic energy storage was assumed, mechanical power was independent of airspeed and was proportional to mass0.36. Estimated metabolic rates during flight averaged 22 and 36 ml O2 g-1 h-1, for the cases of perfect and zero elastic storage, respectively. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 48 TC 34 Z9 39 U1 2 U2 11 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE, CAMBS, ENGLAND CB4 4DL SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD SEP PY 1991 VL 159 BP 335 EP 357 PG 23 WC Biology SC Life Sciences & Biomedicine - Other Topics GA GD870 UT WOS:A1991GD87000019 ER PT J AU DURDEN, LA AF DURDEN, LA TI A NEW SPECIES AND AN ANNOTATED WORLD LIST OF THE SUCKING LOUSE GENUS NEOHAEMATOPINUS (ANOPLURA, POLYPLACIDAE) SO JOURNAL OF MEDICAL ENTOMOLOGY LA English DT Article DE INSECTA; NEOHAEMATOPINUS; NEW SPECIES; WORLD LIST ID SULAWESI AB A new species of sucking louse, Neohaematopinus sundasciuri, collected from the tree squirrel, Sundasciurus juvencus, is described from Palawan Island, Philippines. An updated world list of the genus Neohaematopinus is presented; this documents descriptive citations, known hosts, and geographical distributions with interpretive annotations for each of the 32 species now included in the genus. The geographical distribution of Neohaematopinus sciuri and N. sciurinus are discussed. C1 SMITHSONIAN INST,CTR MUSUEM SUPPORT,DEPT ENTOMOL,WASHINGTON,DC 20560. NR 20 TC 4 Z9 4 U1 0 U2 0 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 SN 0022-2585 J9 J MED ENTOMOL JI J. Med. Entomol. PD SEP PY 1991 VL 28 IS 5 BP 694 EP 700 PG 7 WC Entomology; Veterinary Sciences SC Entomology; Veterinary Sciences GA GG448 UT WOS:A1991GG44800021 PM 1941938 ER PT J AU SCHIEWE, MC FITZ, TA BROWN, JL STUART, LD WILDT, DE AF SCHIEWE, MC FITZ, TA BROWN, JL STUART, LD WILDT, DE TI RELATIONSHIP OF ESTRUS SYNCHRONIZATION METHOD, CIRCULATING HORMONES, LUTEINIZING-HORMONE AND PROSTAGLANDIN-F2-ALPHA RECEPTORS AND LUTEAL PROGESTERONE CONCENTRATION TO PREMATURE LUTEAL REGRESSION IN SUPEROVULATED SHEEP SO JOURNAL OF REPRODUCTION AND FERTILITY LA English DT Article DE SHEEP; SUPEROVULATION; PREMATURE LUTEAL REGRESSION; PROSTAGLANDIN F2-ALPHA; RECEPTOR ID OVINE CORPUS-LUTEUM; ESTROUS-CYCLE; CORPORA-LUTEA; CELL-TYPES; MORPHOMETRIC ANALYSIS; SUPER-OVULATION; EARLY-PREGNANCY; LIFE-SPAN; EWES; GOATS AB Ewes were treated with exogenous follicle-stimulating hormone (FSH) and oestrus was synchronized using either a dual prostaglandin F-2-alpha (PGF-2-alpha) injection regimen or pessaries impregnated with medroxy progesterone acetate (MAP). Natural cycling ewes served as controls. After oestrus or AI (Day 0), corpora lutea (CL) were enucleated surgically from the left and right ovaries on Days 3 and 6, respectively. The incidence of premature luteolysis was related (P < 0.05) to PGF-2-alpha treatment and occurred in 7 of 8 ewes compared with 0 of 4 controls and 1 of 8 MAP-exposed females. Sheep with regressing CL had lower circulating and intraluteal progesterone concentrations and fewer total and small dissociated luteal cells on Day 3 than gonadotrophin-treated counterparts with normal CL. Progesterone concentration in the serum and luteal tissue was higher (P < 0.05) in gonadotrophin-treated ewes with normal CL than in the controls; but luteinizing hormone (LH) receptors/cell were not different on Days 3 and 6. There were no apparent differences in the temporal patterns of circulating oestradiol-17-beta, FSH and LH. High progesterone in gonadotrophin-treated ewes with normal CL coincided with an increase in total luteal mass and numbers of cells, which were primarily reflected in more small luteal cells than in control ewes. Gonadotrophin-treated ewes with regressing CL on Day 3 tended (P < 0.10) to have fewer small luteal cells and fewer (P < 0.05) low-affinity PGF-2-alpha binding sites than sheep with normal CL. By Day 6, luteal integrity and cell viability was absent in ewes with prematurely regressed CL. These data demonstrate that (i) the incidence of premature luteal regression is highly correlated with the use of PGF-2-alpha; (ii) this abnormal luteal tissue is functionally competent for 2-3 days after ovulation, but deteriorates rapidly thereafter and (iii) luteal-dysfunctioning ewes experience a reduction in numbers of small luteal cells without a significant change in luteal mass by Day 3 and, overall, have fewer low-affinity PGF-2-alpha binding sites. C1 NIH,NATL CTR RES RESOURCES,VET RESOURCES PROGRAM,BETHESDA,MD 20892. UNIFORMED SERV UNIV HLTH SCI,BETHESDA,MD 20814. RP SCHIEWE, MC (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 40 TC 23 Z9 25 U1 1 U2 2 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 SEP PY 1991 VL 93 IS 1 BP 19 EP 30 PG 12 WC Reproductive Biology SC Reproductive Biology GA GG006 UT WOS:A1991GG00600005 PM 1920289 ER PT J AU JORDAN, TE CORRELL, DL MIKLAS, J WELLER, DE AF JORDAN, TE CORRELL, DL MIKLAS, J WELLER, DE TI LONG-TERM TRENDS IN ESTUARINE NUTRIENTS AND CHLOROPHYLL, AND SHORT-TERM EFFECTS OF VARIATION IN WATERSHED DISCHARGE SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article ID UPPER CHESAPEAKE BAY; RIVER; PHYTOPLANKTON; ENRICHMENT; QUALITY; PLANTS; ALGAE AB For up to 18 yr we monitored salinity and the concentrations of nutrients, organic matter, plant pigments, and suspended particles in the Rhode River (a subestuary of Chesapeake Bay, USA) to examine long-term trends and relationships to watershed discharges. There was no clear evidence of increasing eutrophication. Chlorophyll concentration did not show a long-term trend, although pheopigments increased. Total suspended particles and forms of P, N, and C showed either a decrease or no trend, except for dissolved ammonium, which increased slightly in one segment of the estuary. The largest and most consistent trend was a decrease in dissolved organic N. We also analyzed correlations between watershed flow and concentrations at weekly and seasonal time scales, resolving the different influences of the Susquehanna River and local watersheds. In some cases, nitrate was positively correlated with either local or Susquehanna flow depending on season, location in the estuary, and time scale. At both weekly and seasonal time scales, chlorophyll was positively correlated with Susquehanna flow in spring in one segment of the estuary. At the seasonal time scale, chlorophyll in summer was correlated with Susquehanna flow of the previous spring. These results and the pattern of fluctuation in the ratio of dissolved inorganic N:P support the hypothesis that chlorophyll concentrations in spring are controlled by nitrate inputs from the Susquehanna, while in summer they are controlled by the regeneration of inorganic N from organic matter produced in the spring. RP JORDAN, TE (reprint author), SMITHSONIAN ENVIRONM RES CTR, EDGEWATER, MD 21037 USA. OI Weller, Donald/0000-0002-7629-5437 NR 50 TC 73 Z9 73 U1 1 U2 4 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD SEP PY 1991 VL 75 IS 2-3 BP 121 EP 132 PG 12 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA GG435 UT WOS:A1991GG43500002 ER PT J AU SEWELL, MC AF SEWELL, MC TI SEEDS OF CHANGE - 500 YEARS OF ENCOUNTER AND EXCHANGE SO MUSEUM NEWS LA English DT Art Exhibit Review RP SEWELL, MC (reprint author), SMITHSONIAN INST,TRAVELING EXHIBIT SERVICE,WASHINGTON,DC 20560, USA. NR 1 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 SEP-OCT PY 1991 VL 70 IS 5 BP 38 EP 42 PG 5 WC Art SC Art GA GD001 UT WOS:A1991GD00100013 ER PT J AU ALPERT, YL AF ALPERT, YL TI ON SOME ELECTROMAGNETIC PHENOMENA IN THE TETHER MAGNETOPLASMA CLOUD SO NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA C-GEOPHYSICS AND SPACE PHYSICS LA English DT Article DE PHYSICS OF THE IONOSPHERE AB The tethered satellite system (TSS) will be accompanied by a variety of electromagnetic phenomena. An independent interconnected formation, a <> (TMC), moving in space along the orbit of TSS, at an altitude of about 300 km, will be created. This time-dependent cloud will be a very complicated inhomogeneous formation including electromagnetic oscillations and waves of different type. Some of these waves will be observed on the Earth's surface. Rarefied regions of the magnetoplasma behind, and dense regions in front of the shuttle orbiter (SO) and the subsatellite (SS) will arise. The neutral nitrogen beam ejected by the thruster becomes an ion beam on the day-light part of the orbit. Its energy is much greater than the local thermal energy. Instabilities of different kind as well as diffusion and recombination effects are expected to accompany the interaction of these beams with the surrounding plasma. The electron beams will produce other types of instabilities. By the electrons precessing along the magnetic-field lines, a current (5.10(3) V, 0.5A) should be induced in the 20th km length conducting tether. It will be closed at the bottom of the ionosphere. This huge magnetic loop, so-called <> (PL), should accompany the tether system along its orbit. The length of this <> (TEMT) is about 200 km, its magnetic moment will be about 10(13) A.cm2. Alfven waves and nonlinear effects of heating type may be produced by this loop along the magnetic-field lines. <> of hot plasma may accompany the tether system. RP ALPERT, YL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 0 TC 1 Z9 1 U1 0 U2 1 PU EDITRICE COMPOSITORI BOLOGNA PI BOLOGNA PA VIA STALINGRADO 97/2, I-40128 BOLOGNA, ITALY SN 0390-5551 J9 NUOVO CIMENTO C JI Nuovo Cimento Soc. Ital. Fis. C-Geophys. Space Phys. PD SEP-OCT PY 1991 VL 14 IS 5 BP 501 EP 522 DI 10.1007/BF02509201 PG 22 GA GN628 UT WOS:A1991GN62800007 ER PT J AU NILSSON, AE JOHANSSON, S KURUCZ, RL AF NILSSON, AE JOHANSSON, S KURUCZ, RL TI THE SPECTRUM OF SINGLY IONIZED-YTTRIUM, Y-II SO PHYSICA SCRIPTA LA English DT Article ID STRENGTHS AB Hollow-cathode spectra of yttrium have been registered in the wavelength region 1000-48 800 angstrom. Resonant charge transfer reactions in the light source favour the excitation of Y II, where 174 new levels have been established by means of 1284 newly classified lines. Altogether we report 1521 lines between 235 levels in Y II. The ground complex (4d + 5s)2 is now completely known and a number of Rydberg series have been extended. The new levels belong to the 4dnl (nl = 7s, 8s, 9s, 6p, 7p, 4d, 5d, 6d, 7d, 8d, 4f, 5f, 6f, 7f, 5g) and 5snl (nl = 7s, 8s, 6p, 6d, 4f, 5f) configurations. Eigenvector compositions, based on parametric calculations including configuration interaction, are given for all levels. The ionization limit has been determined to 98 590 +/- 5 cm-1. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP NILSSON, AE (reprint author), UNIV LUND,DEPT PHYS,SOLVEGATAN 14,S-22362 LUND,SWEDEN. NR 21 TC 53 Z9 54 U1 0 U2 2 PU ROYAL SWEDISH ACAD SCIENCES PI STOCKHOLM PA PUBL DEPT BOX 50005, S-104 05 STOCKHOLM, SWEDEN SN 0281-1847 J9 PHYS SCRIPTA JI Phys. Scr. PD SEP PY 1991 VL 44 IS 3 BP 226 EP 257 DI 10.1088/0031-8949/44/3/003 PG 32 WC Physics, Multidisciplinary SC Physics GA GB828 UT WOS:A1991GB82800003 ER PT J AU RONCIN, JY LAUNAY, F SUBTIL, JL YOSHINO, K AF RONCIN, JY LAUNAY, F SUBTIL, JL YOSHINO, K TI NEW EMISSION BANDS IN THE HIGH-RESOLUTION SPECTRUM OF MOLECULAR NITROGEN BETWEEN 107.7 AND 124.2 NM SO PLANETARY AND SPACE SCIENCE LA English DT Article ID EXTREME ULTRAVIOLET OBSERVATIONS; ELECTRON-IMPACT; N-2; EUV; PREDISSOCIATION; ENCOUNTER; SATURN; STATE AB The vacuum ultraviolet emission spectrum of molecular nitrogen, produced by a low pressure discharge, is investigated at high spectral resolution from 107.7 to 124.2nm. Band origins are reported for the 103 bands rotationally analyzed. C1 OBSERV PARIS,CNRS,URA 812,SECT MEUDON,F-92195 MEUDON,FRANCE. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP RONCIN, JY (reprint author), CNRS,URA 842,TRAITEMENT SIGNAL & INSTRUMENTAT,23 RUE DR P MICHELON,F-42023 ST ETIENNE,FRANCE. NR 15 TC 13 Z9 13 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD SEP PY 1991 VL 39 IS 9 BP 1301 EP 1304 DI 10.1016/0032-0633(91)90045-C PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GM922 UT WOS:A1991GM92200011 ER PT J AU ADAMS, RMC AF ADAMS, RMC TI MUSEUMS BEYOND TREASURES AND TRADITIONS SO PROCEEDINGS OF THE AMERICAN PHILOSOPHICAL SOCIETY LA English DT Article RP ADAMS, RMC (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 5 TC 0 Z9 0 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 1991 VL 135 IS 3 BP 332 EP 338 PG 7 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA GL809 UT WOS:A1991GL80900002 ER PT J AU HERKEN, G AF HERKEN, G TI DAYS OF CHALLENGE, YEARS OF CHANGE - A TECHNICAL HISTORY OF THE PACIFIC-MISSILE-TEST-CENTER - PACIFIC-MISSILE-TEST-CENTER SO PUBLIC HISTORIAN LA English DT Book Review RP HERKEN, G (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 1991 VL 13 IS 4 BP 45 EP 47 PG 3 WC History SC History GA GU150 UT WOS:A1991GU15000006 ER PT J AU KIRSHNER, RP AF KIRSHNER, RP TI EXPLODING STARS AND THE EXPANDING UNIVERSE SO QUARTERLY JOURNAL OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article ID LARGE MAGELLANIC CLOUD; SUPERNOVA; SN-1987A; DISTANCE AB Supernovae are exploding stars: after as little as ten million years of preparation, a single star can shine as brightly as 10 billion suns for a few weeks. Supernovae come in two broad classes - one that provides a 'custom yardstick' to measure the distances to individual galaxies and another that offers standard candles that can be detected a third of the way across the universe. Techniques are being developed to use these stellar beacons to gauge the age of the Universe and the geometry of space. Definitive answers are not in yet, but they are within our grasp and supernovae may soon become a central element of the cosmological quest. RP KIRSHNER, RP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 20 TC 0 Z9 0 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8738 J9 Q J ROY ASTRON SOC JI Q. J. R. Astron. Soc. PD SEP PY 1991 VL 32 IS 3 BP 233 EP 244 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GD504 UT WOS:A1991GD50400003 ER PT J AU ADAMS, RMC AF ADAMS, RMC TI SMITHSONIAN HORIZONS SO SMITHSONIAN LA English DT Editorial Material RP ADAMS, RMC (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD SEP PY 1991 VL 22 IS 6 BP 10 EP 10 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA GC763 UT WOS:A1991GC76300001 ER PT J AU HINES, AH SMITH, LD AF HINES, AH SMITH, LD TI CRUSTACEAN SEXUAL BIOLOGY - BAUER,RT, MARTIN,JW SO SCIENCE LA English DT Book Review RP HINES, AH (reprint author), SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037, USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD AUG 30 PY 1991 VL 253 IS 5023 BP 1045 EP 1046 DI 10.1126/science.253.5023.1045-a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA GC982 UT WOS:A1991GC98200053 PM 17775355 ER PT J AU GREGORY, B AF GREGORY, B TI CLASSICAL RECORDS SO NATURE LA English DT Letter RP GREGORY, B (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,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 AUG 29 PY 1991 VL 352 IS 6338 BP 763 EP 763 DI 10.1038/352763a0 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA GC964 UT WOS:A1991GC96400036 ER PT J AU SNOW, AA SPIRA, TP AF SNOW, AA SPIRA, TP TI POLLEN VIGOR AND THE POTENTIAL FOR SEXUAL SELECTION IN PLANTS SO NATURE LA English DT Article ID MULTIPLE PATERNITY; RAPHANUS-SATIVUS; WILD RADISH; TUBE GROWTH; CONSEQUENCES; POLLINATIONS; CARRYOVER; SUCCESS AB DISCOVERING whether paternal fecundity varies within populations is crucial for evaluating whether male-male competition and/or female choice can lead to sexual selection 1-3. In natural populations of plants, pollinators often deposit mixtures of 'surplus' pollen from several individuals onto receptive stigmas 4-7. Therefore within-flower competition among pollen-tubes for ovules could lead to nonrandom paternal success. We found that pollen competition was common in populations of wild rose mallow (Hibiscus moscheutos). Co-occurring individuals often differed in mean pollen-tube growth rates, and this trait was correlated with the number of seeds the plants sired when pollen mixtures were applied to stigmas. Differences between pairs of individuals in pollen-tube growth rates were consistent across maternal plants, suggesting that sexual selection can occur. This unexpected variation in pollen vigour could lead to nonrandom fertilization whenever pollen-tubes compete for access to ovules. C1 GEORGIA SO UNIV,DEPT BIOL,STATESBORO,GA 30460. SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. RP SNOW, AA (reprint author), OHIO STATE UNIV,DEPT PLANT BIOL,COLUMBUS,OH 43210, USA. NR 28 TC 155 Z9 156 U1 5 U2 27 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD AUG 29 PY 1991 VL 352 IS 6338 BP 796 EP 797 DI 10.1038/352796a0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA GC964 UT WOS:A1991GC96400057 ER PT J AU WATTERS, TR AF WATTERS, TR TI ORIGIN OF PERIODICALLY SPACED WRINKLE RIDGES ON THE THARSIS PLATEAU OF MARS SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LITHOSPHERIC STRESS; OCEANIC LITHOSPHERE; TERRESTRIAL PLANETS; REGION; WATER; SERENITATIS; THICKNESS; EVOLUTION; HISTORY; CRISIUM AB Ridged plains are a major geologic unit on Mars and are a predominant unit on the Tharsis Plateau, a region that has undergone uplift, extension, and extensive shield and flood volcanism. These units, probably flood volcanic in origin, are characterized by landforms classed as wrinkle ridges. Wrinkle ridges are interpreted to be folds, resulting from buckling followed by reverse to thrust faulting (flexure-fracture). A prominent characteristic of many of the wrinkle ridges on Mars, particularly those in the Tharsis ridge system, is the periodic nature of their spacing. The periodic spacing has been evaluated in six major provinces on the Tharsis Plateau with regions further divided into domains based largely on variation in ridge orientation. The average spacing of the Tharsis ridges, based on 2934 measurements, is 30 km. In an effort to account for the periodic nature of the wrinkle ridges, the ridged plains material is modeled as both a single member and a multilayer with frictionless contacts that has buckled at a critical wavelength of folding. Free slip between layers is assumed based on the possible existence of mechanically weak interbeds in the ridged plains sequence separating groups of flows. The near-surface mechanical structure in the area of ridged plains is approximately by a strong layer or layers overlying a weak megaregolith of finite thickness overlying a strong basement. Buckling of the ridged plains is assumed to be decoupled from the basement by the weak megaregolith. Decoupling is enhanced if the megaregolith were water- or ice-rich at the time of deformation. The rheologic behavior of the ridged plains and megaregolith is approximated by a linear elastic and linear viscous material. The models are examined for a range in (1) the strength contrast between the ridged plains material and the underlying megaregolith; (2) thickness of the ridged plains materials; (3) thickness of the megaregolith; and (4) number of layers. The elastic model can explain the observed ridge spacing only if the ridged plains are relatively thick (greater-than-or-equal-to 2400 m) with multiple layers (n > 1) and relatively high contrast in Young's modulus (E/E0 greater-than-or-equal-to 100). The high E/E0 required is possible only if the megaregolith was water-rich at the time of deformation. Over the same range in values of the parameters, viscous buckling is much less restricted. The viscous model can explain the observed ridge spacing over a wide range in ridged plains thickness (250 m to several kilometers), megaregolith thickness, number of layers (n = 1 to 8) and contrasts in viscosity (eta/eta-0 greater-than-or-equal-to 10). In addition, viscous buckling is viable if the megaregolith were dry, water-rich or ice-rich at the time of deformation. The absence of folds with a cross-sectional geometry in the shape of a sinusoid (anticline-syncline pairs) may be the result of initial deformation of the ridged plains material into low-amplitude folds (in infinitesimal strain) followed by plastic yielding in the cores of the anticlines (in finite strain). Initial elastic or viscous buckling, coupled with plastic yielding confined to the hinge area followed by the development of reverse to thrust faulting, could account for the asymmetric fold geometry of many of the wrinkle ridges. RP WATTERS, TR (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,CTR EARTH & PLANETARY STUDIES,WASHINGTON,DC 20560, USA. NR 81 TC 57 Z9 57 U1 1 U2 5 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 AUG 25 PY 1991 VL 96 IS E1 BP 15599 EP 15616 DI 10.1029/91JE01402 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA GH507 UT WOS:A1991GH50700005 ER PT J AU VACANTI, G CAWLEY, MF COLOMBO, E FEGAN, DJ HILLAS, AM KWOK, PW LANG, MJ LAMB, RC LEWIS, DA MACOMB, DJ OFLAHERTY, KS REYNOLDS, PT WEEKES, TC AF VACANTI, G CAWLEY, MF COLOMBO, E FEGAN, DJ HILLAS, AM KWOK, PW LANG, MJ LAMB, RC LEWIS, DA MACOMB, DJ OFLAHERTY, KS REYNOLDS, PT WEEKES, TC TI GAMMA-RAY OBSERVATIONS OF THE CRAB-NEBULA AT TEV ENERGIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GAMMA-RAYS, GENERAL; NEBULAE, CRAB NEBULA; PULSARS; RADIATION MECHANISMS ID PULSAR; EMISSION AB The Crab Nebula was observed in TeV gamma rays with the Whipple Observatory high-resolution atmospheric Cherenkov camera and a signal was detected at the 20-sigma-level. The energy spectrum derived has the form N(E) x dE = 2.5 x 10(-10) (E/0.4 TeV)-2.4 +/- 0.3 photons cm-2 s-1 TeV-1 between 0.4 and 4 TeV. There is no evidence for the pulsar periodicity, and the flux is steady on a monthly time scale. If this signal is used to optimize the technique for gamma-ray detection, then a flux one-tenth that of the Crab can be detected at the 3-sigma-level in 60 hr of integration time. For an on-axis source the angular resolution is shown to be +/- 0.-degrees-1. C1 IOWA STATE UNIV SCI & TECHNOL,DEPT PHYS,AMES,IA 50011. ST PATRICKS COLL,DEPT PHYS,MAYNOOTH,KILDARE,IRELAND. HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,CAMBRIDGE,MA 02138. NATL UNIV IRELAND UNIV COLL DUBLIN,DEPT PHYS,DUBLIN 4,IRELAND. UNIV LEEDS,DEPT PHYS,LEEDS LS2 9JT,W YORKSHIRE,ENGLAND. OI Lang, Mark/0000-0003-4641-4201 NR 43 TC 161 Z9 161 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 20 PY 1991 VL 377 IS 2 BP 467 EP 479 DI 10.1086/170376 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GA594 UT WOS:A1991GA59400012 ER PT J AU GOMEZ, Y RODRIGUEZ, LF GARAY, G MORAN, JM AF GOMEZ, Y RODRIGUEZ, LF GARAY, G MORAN, JM TI THE DENSE MOLECULAR ENVELOPE AROUND THE COMPACT-H-II REGION-G5.89-0.39 (W28 A2) SO ASTROPHYSICAL JOURNAL LA English DT Article DE INTERSTELLAR, MOLECULES; NEBULAE, H-II REGIONS; RADIO SOURCES, LINES; STARS, FORMATION ID GALACTIC PLANE; STAR FORMATION; REGIONS; AMMONIA; EMISSION; NEBULA; DUST AB We present VLA observations of ammonia in the (J, K) = (2, 2) and (3, 3) inversion transitions toward the compact H II region G5.89-0.39. These observations reveal the presence of a massive (approximately 30 M. and hot (approximately 90 K) molecular envelope that is clumpy and probably undergoing expansion. We also detect overheated or inverted (3, 3) ammonia emission in front of the H II region. The radio continuum map shows bipolar protuberances, suggesting that the ionized gas is flowing out through openings in the molecular envelope. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CHILE,DEPT ASTRON,SANTIAGO,CHILE. RI Garay, Guido/H-8840-2013 OI Garay, Guido/0000-0003-1649-7958 NR 27 TC 27 Z9 27 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 20 PY 1991 VL 377 IS 2 BP 519 EP 525 DI 10.1086/170381 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GA594 UT WOS:A1991GA59400017 ER PT J AU MENTEN, KM MELNICK, GJ AF MENTEN, KM MELNICK, GJ TI 321-GHZ SUBMILLIMETER WATER MASERS AROUND EVOLVED STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE MASERS; STARS, CIRCUMSTELLAR SHELLS; STARS, LATE-TYPE; STARS, LONG-PERIOD VARIABLES ID MASS-LOSS RATES; CIRCUMSTELLAR ENVELOPES; SIO MASERS; H2O MASERS; EMISSION; LINES; GHZ AB We have observed the 321 GHz 10(29) --> 9(36) transition of water vapor toward a sample of oxygen-rich late-type stars, all of which show maser emission in the well-studied 22 GHz 6(16) --> 5(23) line of water. The 321 GHz line is detected toward eight Mira variables, two semiregulars, and the supergiant VY CMa and most likely shows maser action in all cases. For one star, two 321 GHz spectra taken 2 months apart show clear signs of variability. Spectra of the 22 GHz water line were taken almost simultaneously with the 321 GHz spectra. Although the emission in both transitions is observed at similar velocities, the 22 GHz spectra in general look quite different from the 321 GHz spectra: 22 GHz emission features are observed at velocities that do not show detectable 321 GHz emission, and vice versa. For most stars the luminosity in the 22 GHz line is comparable to or smaller than the 321 GHz luminosity, which is difficult to understand if the masers in both lines are saturated, equally beamed, and H-2-H2O collisions are primarily responsible for populating the H2O energy levels. For Mira variables there may be a correlation between the 22 to 321 GHz luminosity ratio and the mass-loss rate. We present arguments that suggest that the maser lines from the nu-2 vibrationally excited state of H2O that have recently been detected toward VY CMa do not arise from the same part of the circumstellar envelope as the 22 and 321 GHz masers, but rather from the hot, very high density region close to the stellar photosphere that gives rise to SiO masers. RP MENTEN, KM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 45 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 AUG 20 PY 1991 VL 377 IS 2 BP 647 EP 656 DI 10.1086/170392 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GA594 UT WOS:A1991GA59400028 ER PT J AU FONTENLA, JM AVRETT, EH LOESER, R AF FONTENLA, JM AVRETT, EH LOESER, R TI ENERGY-BALANCE IN THE SOLAR TRANSITION REGION .2. EFFECTS OF PRESSURE AND ENERGY INPUT ON HYDROSTATIC MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE DIFFUSION; LINE FORMATION; RADIATIVE TRANSFER; SUN, ATMOSPHERE; SUN, TRANSITION REGION ID LOOP RADIATIVE HYDRODYNAMICS; COLLISION STRENGTHS; PHYSICAL-PROPERTIES; CHROMOSPHERE; CORONA; PLAGE AB In this paper we address the question of how energy is radiated by hydrogen lines and continua hydrostatic energy-balance models of the transition region between the solar chromosphere and corona. Our models assume that mechanical or magnetic energy is dissipated in the hot corona and is then transported toward the chromosphere down the steep temperature gradient of the transition region. This model can be applied to the lower portions of magnetic flux tubes in which the temperature varies from chromospheric to coronal values. and to either open field or loop models. The basic difference between our calculations and those of other authors is that our theoretical hydrostatic energy-balance models properly take into account the diffusion of hydrogen atoms and ions. Diffusion, which was introduced in a previous paper, arises naturally due to the concentration and temperature gradients and is characterized by the ambipolar diffusion velocity. The diffusion effects are used in both the statistical equilibrium and energy balance equations and, as shown earlier. give order of magnitude agreement between calculations and the observations of the hydrogen Lyman continuum and Lyman lines in the average quiet Sun. The present paper describes various models constructed for the transition regions that correspond to different features of the solar atmosphere. Our calculations give the magnitude and distribution of energy radiated by the lower transition region after being transported down from the corona. Wc find that our models not only explain the average quiet Sun but also the entire range of variability of the Ly-alpha lines. We describe the relations between the downward energy flux, the pressure of the transition region, and the different hydrogen emissions. We show how the usual optically thin radiative loss curve can be modified to give agreement with our detailed calculations. and the extent to which this method can be used for estimating the actual radiative losses. Also, we show how the usual emission measure method can be modified to treat the Ly-alpha line emission, and we discuss the limitations of the emission measure approach. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP UNIV ALABAMA, CSPAR, HUNTSVILLE, AL 35899 USA. NR 31 TC 107 Z9 107 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 AUG 20 PY 1991 VL 377 IS 2 BP 712 EP 725 DI 10.1086/170399 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GA594 UT WOS:A1991GA59400035 ER PT J AU AKERLOF, CW CAWLEY, MF CHANTELL, M FEGAN, DJ HARRIS, K HILLAS, AM JENNINGS, DG LAMB, RC LAWRENCE, MA LANG, MJ LEWIS, DA MEYER, DI MOHANTY, G OFLAHERTY, KS PUNCH, M REYNOLDS, PT SCHUBNELL, MS WEEKES, TC WHITAKER, T AF AKERLOF, CW CAWLEY, MF CHANTELL, M FEGAN, DJ HARRIS, K HILLAS, AM JENNINGS, DG LAMB, RC LAWRENCE, MA LANG, MJ LEWIS, DA MEYER, DI MOHANTY, G OFLAHERTY, KS PUNCH, M REYNOLDS, PT SCHUBNELL, MS WEEKES, TC WHITAKER, T TI LOCATING VERY-HIGH-ENERGY GAMMA-RAY SOURCES WITH ARCMINUTE ACCURACY SO ASTROPHYSICAL JOURNAL LA English DT Article DE GAMMA-RAYS, GENERAL; INSTRUMENTS; NEBULAE, CRAB NEBULA; STARS, INDIVIDUAL (GEMINGA) AB The angular accuracy of gamma-ray detectors is intrinsically limited by the physical processes involved in photon detection. Although a number of pointlike sources were detected by the COS B satellite, only two have been unambiguously identified by time signature with counterparts at longer wavelengths. By taking advantage of the extended longitudinal structure of VHE gamma-ray showers, measurements in the TeV energy range can pin-point source coordinates to arcminute accuracy. This has now been demonstrated with new data analysis procedures applied to observations of the Crab Nebula using Cherenkov air shower imaging techniques. With two telescopes in coincidence, the individual event circular probable error will be 0-degrees.13. The half-cone angle of the field of view is effectively 1-degrees. C1 ST PATRICKS COLL,DEPT PHYS,MAYNOOTH,KILDARE,IRELAND. HARVARD SMITHSONIAN CTR ASTROPHYS,FRED LAWRENCE WHIPPLE OBSERV,AMADO,AZ 85645. NATL UNIV IRELAND UNIV COLL DUBLIN,DEPT PHYS,DUBLIN 4,IRELAND. UNIV LEEDS,DEPT PHYS,LEEDS LS2 9JT,W YORKSHIRE,ENGLAND. IOWA STATE UNIV SCI & TECHNOL,DEPT PHYS & ASTRON,AMES,IA 50011. RP AKERLOF, CW (reprint author), UNIV MICHIGAN,RANDALL LAB PHYS,ANN ARBOR,MI 48109, USA. NR 10 TC 49 Z9 53 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 1991 VL 377 IS 2 BP L97 EP L100 DI 10.1086/186125 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GA595 UT WOS:A1991GA59500008 ER PT J AU COOKSY, AL DRUCKER, S FAEDER, J GOTTLIEB, CA KLEMPERER, W AF COOKSY, AL DRUCKER, S FAEDER, J GOTTLIEB, CA KLEMPERER, W TI HIGH-RESOLUTION SPECTRUM OF THE V = 1 PI STATE OF ARHCN SO JOURNAL OF CHEMICAL PHYSICS LA English DT Note ID AR-HCN; MICROWAVE; SPECTROSCOPY C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. HARVARD SMITHSONIAN CTR ASTROPHYS,DIV APPL SCI,CAMBRIDGE,MA 02138. RP COOKSY, AL (reprint author), HARVARD UNIV,DEPT CHEM,CAMBRIDGE,MA 02138, USA. NR 12 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 AUG 15 PY 1991 VL 95 IS 4 BP 3017 EP 3019 DI 10.1063/1.460906 PG 3 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA GA108 UT WOS:A1991GA10800089 ER PT J AU FALCO, EE WAMBSGANSS, J SCHNEIDER, P AF FALCO, EE WAMBSGANSS, J SCHNEIDER, P TI THE ROLE OF MICROLENSING IN ESTIMATES OF THE RELATIVE-TIME DELAY FOR THE GRAVITATIONAL IMAGES OF Q0957+561 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article ID LENS; SYSTEM; STARS; EVENT AB We present a study of the effects of individual stars in the gravitational lens that forms the images A and B of the QSO Q0957 + 561. Our main result is evidence that it is very unlikely that microlensing effects dominate the observed fluctuations of the images. Therefore, the measured (but uncertain) correlation between the light curves of the images is likely due to intrinsic luminosity variations at the source, rather than to propagation effects at the lens. We find, however, that the disagreement between magnification estimates at optical and radio wavelengths is a strong indicator of microlensing. Thus, estimates for the time delay for A and B, DELTA-tau-BA, should be obtained for spectral bands that are least affected by microlensing, i.e., the largest emission regions in the QSO. However, we still lack a general method to separate intrinsic and microlensing fluctuations to obtain estimates of DELTA-tau-BA. We also highlight several problems associated with cross-correlating the unevenly sampled light curves of images A and B. Recent estimates for DELTA-tau-BA are different for the two available optical data sets, and they depend strongly on the method used to cross-correlate the light curves. From simulated model data, we single out a reliable method for cross-correlation in the present situation. We also propose a method that yields simultaneous estimates for the time delay for an image pair and for their magnification ratio at optical wavelengths. C1 MAX PLANCK INST PHYS & ASTROPHYS, W-8046 GARCHING, GERMANY. RP FALCO, EE (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 24 TC 17 Z9 17 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 AUG 15 PY 1991 VL 251 IS 4 BP 698 EP 706 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA GA797 UT WOS:A1991GA79700016 ER PT J AU BARTSCHAT, K MCLAUGHLIN, BM HOVERSTEN, RA AF BARTSCHAT, K MCLAUGHLIN, BM HOVERSTEN, RA TI PHOTOIONIZATION AND EXCITATION OF ATOMIC BARIUM FROM THE (6S6P)1P10 STATE SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID 2-STEP OPTOGALVANIC SPECTROSCOPY; AUTOIONIZING SERIES; GENERAL PROGRAM; NEUTRAL BARIUM; EVEN LEVELS; BA; PHOTOIONISATION; RESONANCES; LIMIT; J=1 AB A previous Breit-Pauli R-matrix calculation for photoionization of the excited initial state (6s6p)P-1(1)o of atomic barium (Bartschat and McLaughlin 1990) has been extended over a wide range of energies and various final ionic states. The complicated resonance structure was fully resolved and has been analysed in terms of quantum defect theory. While the agreement of this fully ab initio calculation with other recent theoretical and experimental work is quite satisfactory, the use of a semi-empirical core potential may be necessary to further improve the agreement between experimental and theoretical resonance positions. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. RP BARTSCHAT, K (reprint author), DRAKE UNIV,DEPT PHYS & ASTRON,DES MOINES,IA 50311, USA. RI Bartschat, Klaus/I-2527-2012 NR 28 TC 19 Z9 19 U1 0 U2 0 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 AUG 14 PY 1991 VL 24 IS 15 BP 3359 EP 3371 DI 10.1088/0953-4075/24/15/007 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA GB596 UT WOS:A1991GB59600007 ER PT J AU REGOS, E GELLER, MJ AF REGOS, E GELLER, MJ TI THE EVOLUTION OF VOID-FILLED COSMOLOGICAL STRUCTURES SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY; GALAXIES, CLUSTERING; GALAXIES, REDSHIFTS; NUMERICAL METHODS ID EINSTEIN-DESITTER UNIVERSE; LARGE-SCALE STRUCTURE; EXPANDING UNIVERSE; SUPERCLUSTER; SIMULATIONS; GALAXIES; MATTER; HOLES; SLICE AB We simulate the growth and evolution of voids in the large-scale distribution of galaxies. For arbitrary value of the cosmological density parameter-OMEGA, we examine one-, two-, and three-dimensional models. In these models void-filled cosmological structures evolve from a high number density of shallow initial voids with unspecified origin. The growth rate of a void decreases significantly at the cosmic time corresponding to OMEGA = 0.5. In models constructed in two and three dimensions, suitable initial conditions lead to cellular structure with faceted voids similar to those observed in redshift surveys. These structures form for OMEGA less-than-or-equal-to 0.4. The matter compressed to planes flows more rapidly toward the condensations at the intersections than one would expect for spherical infall. The rms peculiar streaming velocities for void diameters of 5000 km s-1 are on the order of 1000 km s-1 OMEGA-0.6. If OMEGA is large, the appearance of voids and walls in redshift space can be very different from their appearance in real space when the adjacent voids differ significantly in size; voids and walls can masquerade for each other. The maximum size of a three-dimensional void that can be misidentified in redshift space is 1/5 OMEGA-0.6 relative to its neighbors. The three-dimensional models indicate that the redshift maps are a rather good guide to the structure in real space. For the 5000 km s-1 maximum void size in the CfA survey, structures in redshift space on scales less than 1000 km s-1 are uncertain if OMEGA = 1. For smaller OMEGA, the scale for such severe distortion is smaller. A first approximation to the differential outflow velocity of an undisturbed wall (between identified voids) in three dimensions is upsilon-out approximately H0(d1 - d2)1/10-OMEGA-0.6, where d1 and d2 are the diameters of the adjacent voids along the direction perpendicular to the wall. It should be possible, in future three-dimensional simulations, to test or improve this estimate. Then measurement of the outflow velocities of walls could limit the value of OMEGA-0. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. EOTVOS LORAND UNIV, H-1364 BUDAPEST 5, HUNGARY. RP REGOS, E (reprint author), UNIV CALIF SANTA CRUZ, INST PARTICLE PHYS, SANTA CRUZ, CA 95064 USA. NR 31 TC 42 Z9 42 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 10 PY 1991 VL 377 IS 1 BP 14 EP 28 DI 10.1086/170332 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA FZ463 UT WOS:A1991FZ46300003 ER PT J AU VELUSAMY, T BECKER, RH SEWARD, FD AF VELUSAMY, T BECKER, RH SEWARD, FD TI G33.6+0.1 - A SHELL TYPE SUPERNOVA REMNANT WITH UNUSUAL STRUCTURE SO ASTRONOMICAL JOURNAL LA English DT Article ID X-RAY OBSERVATIONS; NOVA REMNANTS; RADIO AB The morphology of Supernova Remnant G33.6 + 0.1 (Kes 79) has been studied in the x rays with Einstein and in the radio wavelengths using the VLA. Multifrequency high resolution observations of the VLA at 327, 1500, and 5000 MHz are used to study the radio spectrum and polarization. The radio emission shows well formed outer shell structure and very bright central emission. Although the overall distribution of spectral index (approximately -0.6 to -0.75) is consistent with that of shell type remnants, the bright filamentary emission along the "inner ring" has relatively flatter spectrum (alpha approximately -0.4). Both radio and x rays show strong central emission; existence of a plerion near the center cannot be ruled out. The x-ray image does not show the characteristic limb brightening for shell type SNRs. The x ray and radio morphology may be understood in terms of very thick shell and the bright central emission as due to reverse shock. C1 UNIV CALIF DAVIS,DEPT PHYS,DAVIS,CA 95616. UNIV CALIF LAWRENCE LIVERMORE NATL LAB,IGPP,LIVERMORE,CA 94550. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP VELUSAMY, T (reprint author), TIFR,CTR RADIO ASTRON,POST BOX 8,UDHAGAMANDALAM 643001,INDIA. NR 20 TC 19 Z9 19 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 1991 VL 102 IS 2 BP 676 EP 682 DI 10.1086/115901 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA FY255 UT WOS:A1991FY25500018 ER PT J AU SCHWARTZ, DA BRADT, HV REMILLARD, RA TUOHY, IR AF SCHWARTZ, DA BRADT, HV REMILLARD, RA TUOHY, IR TI THE X-RAY COOLING FLOW IN THE CLUSTER OF GALAXIES AROUND PKS-2354-35 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERING; GALAXIES, INDIVIDUAL (PK-2354-350); GALAXIES, INTERGALACTIC MEDIUM; GALAXIES, X-RAYS ID EINSTEIN SATELLITE; PERSEUS CLUSTER; RICH CLUSTERS; CATALOG; GAS; MORPHOLOGY; ACCRETION; DYNAMICS; EMISSION; MASS AB A position measured with the HEAO 1 Scanning Modulation collimator suggested the group of galaxies surrounding the radio galaxy PKS 2354-35 as the identification of the bright, hard X-ray source 4U 0009-33 = 3A 2356-341 = 1H 2355-350. We confirm this identification with measurements of the position and spatial extent using the EXOSAT CMA detector. It shows centrally condensed X-ray emission which is distinctly asymmetric, with a core radius approximately 7'.3 in a roughly N-S direction and approximately 2'.5 in the E-W direction. A serendipitous Einstein IPC detection confirms the shape of this extent. The EXOSAT ME data are fitted by a thermal bremsstrahlung spectrum with a temperature of 3.7 +/- 0.7 keV. Previously, PKS 2354-35 had been found to be a cD galaxy in a small group at redshift 0.048. At this distance the 2-6 keV X-ray luminosity is 1.6 x 10(44) ergs s-1. Our own optical observations reveal strong, narrow (< 1000 km s-1) emission lines of [O II] and [N II] with luminosities approximately 10(41) ergs s-1. Archival radio observations from the partially completed VLA discovered a 35" long, jetlike component, nearly aligned with the major axis of the X-ray distribution. The high-frequency radio spectrum of the total source is very steep, with a special index of 1.6 in the 1.4-5 GHz band. From the X-ray observations we deduce a strong accretion flow. The luminosity and core radius imply a central density at least 8 x 10(-3) cm-3. The central cooling time is no longer than 5 x 10(9) yr, and the mass accretion rate can be estimated roughly as 320 M. yr-1. C1 MIT,DEPT PHYS,CAMBRIDGE,MA 02139. MIT,CTR SPACE RES,CAMBRIDGE,MA 02139. BRITISH AEROSP AUSTRALIA,SALISBURY 5108,SOUTH AFRICA. AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,WODEN,ACT 2606,AUSTRALIA. RP SCHWARTZ, DA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MAIL STOP 3,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 45 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 AUG 1 PY 1991 VL 376 IS 2 BP 424 EP 429 DI 10.1086/170291 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA FY359 UT WOS:A1991FY35900004 ER PT J AU MYERS, PC FULLER, GA GOODMAN, AA BENSON, PJ AF MYERS, PC FULLER, GA GOODMAN, AA BENSON, PJ TI DENSE CORES IN DARK CLOUDS .6. SHAPES SO ASTROPHYSICAL JOURNAL LA English DT Article DE INTERSTELLAR, MOLECULES; NEBULAE, STRUCTURE; STARS, FORMATION ID ROTATING ISOTHERMAL CLOUDS; STAR FORMATION; MOLECULAR CLOUD; NONHOMOLOGOUS CONTRACTION; AMMONIA OBSERVATIONS; CYLINDRICAL CLOUDS; INTERCLOUD MEDIUM; EQUILIBRIA; TAURUS; FRAGMENTATION AB Forty-eight line intensity maps of 16 dense cores in dark clouds are compared, based on observations in the 13 mm line of NH3 and in the 3 mm lines of CS and (CO)-O-18. The core maps have mean FWHM size 0.15 pc (NH3), 0.27 pc (CS), and 0.36 pc ((CO)-O-18). From line to line, the maps are similar in their position on the sky, in their axial ratio 0.5-0.6, and in the alignment of their long axes, usually within 20-degrees. Elongation is thus a common characteristic of dense cores. Therefore, cores are not generally in isolated equilibrium between self-gravity and isotropic random motions. Elongation is evident in cores with and without stars, so it precedes, rather than follows, star formation. The typical observed axial ratio can arise from identical oblate spheroids, if they are highly flattened, with axial ratio less than 0.1-0.3, or from prolate spheroids, if they are modestly elongated, with axial ratio 0.4-0.5. Six of the 16 cores are likely to be prolate because they align with, and are integral parts of, more extended structures seen in obscuration and/or CO line emission. The 10 other cores have less certain three-dimensional shape. Their elongation cannot generally arise from rotational flattening, because they lack the necessary velocity shift in magnitude, direction, or both. Their line widths, column densities, and sizes are equally consistent with virial equilibrium models of spheres, magnetized or rotating oblate spheroids, and finite segments of infinitely long prolate cylinders. The prevalence of prolate cores suggests that initial conditions for low-mass star formation should in some cases include prolate geometry. Prolate cores cannot be described by isolated equilibrium models, so models of prolate environments, and the development of prolate fragments, may be an important part of their description. C1 WELLESLEY COLL,WHITIN OBSERV,DEPT ASTRON,WELLESLEY,MA 02181. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. RP MYERS, PC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MAIL STOP 42,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 50 TC 235 Z9 235 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 AUG 1 PY 1991 VL 376 IS 2 BP 561 EP 572 DI 10.1086/170305 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA FY359 UT WOS:A1991FY35900018 ER PT J AU SOKER, N AF SOKER, N TI NONLINEAR INSTABILITY OF THE ACCRETION LINE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION; HYDRODYNAMICS; INSTABILITIES ID INHOMOGENEOUS-MEDIUM; ANGULAR-MOMENTUM; FLOW; GRADIENT AB We study the instability of the flow along the accretion line in the two-dimensional Bondi-Hoyle-Lyttleton type accretion flow. By means of numerical simulations we explore the nonlinear regime of the instability, thus extending a previous work that dealt with the linear regime using the WKB approximation. In contrast to the behavior in the linear regime, in the nonlinear regime the radial and tangential modes are coupled. The radial instability, which manifests itself as large density and velocity variations on short distances, grows far beyond the linear regime. The tangential instability, on the other hand, stays in the linear regime and is dominant by long-wavelength perturbations. This results from both the influence of the radial instability and the incoming material (the material accreted onto the accretion line). RP SOKER, N (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MAIL STOP 15,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 17 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 AUG 1 PY 1991 VL 376 IS 2 BP 750 EP 756 DI 10.1086/170322 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA FY359 UT WOS:A1991FY35900035 ER PT J AU HERANT, M PARDO, F SPILLER, E GOLUB, L AF HERANT, M PARDO, F SPILLER, E GOLUB, L TI FLARES OBSERVED BY THE NORMAL INCIDENCE X-RAY TELESCOPE ON 1989 SEPTEMBER 11 SO ASTROPHYSICAL JOURNAL LA English DT Article DE SUN, FLARES; SUN, X-RAYS ID SPECTRUM; EVENTS AB We report observations of two solar flares seen in soft X-rays during a sounding rocket flight of the Normal Incidence X-ray Telescope (NIXT) payload on 1989 September 11. The rocket was launched at the onset of a two-ribbon event which reached a maximum intensity of C5 (GOES classification) slightly before the start of our X-ray observations. The flare in X-rays consists primarily of a single bright loop crossing the neutral line and having its footpoints at the southern ends of the ribbons; this loop accounts for more than two-thirds of the emission and is shown to have an electron density of approximately 6 x 10(10) cm-3 at a temperature of approximately 6 x 10(6) K. However, within the remainder of each of the flare ribbons, we also observe complicated coronal structure which although energetically less important is clearly interacting with the main flare loop. A second event in an active region at the limb began during the flight: its most striking feature is a strong correlation with H-alpha images taken at the same time, which indicates the coexistence of chromospheric and coronal temperature material in close proximity. We give possible interpretations of this phenomenon as either a sheath of X-ray emitting material surrounding the H-alpha ejection or as an admixture of hot and cool magnetic flux tubes, each ejecting the material which they contain. C1 IBM CORP,THOMAS J WATSON RES CTR,YORKTOWN HTS,NY 10598. HARVARD UNIV,DEPT ASTRON,CAMBRIDGE,MA 02138. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP HERANT, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 14 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 AUG 1 PY 1991 VL 376 IS 2 BP 797 EP & DI 10.1086/170328 PN 1 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA FY359 UT WOS:A1991FY35900041 ER PT J AU DEWDNEY, PE COSTAIN, CH MCHARDY, I WILLIS, AG HARRIS, DE STERN, CP AF DEWDNEY, PE COSTAIN, CH MCHARDY, I WILLIS, AG HARRIS, DE STERN, CP TI AN X-RAY AND RADIO STUDY OF STEEP-SPECTRUM RADIO-SOURCES .2. 4 FIELDS FROM A 22 MHZ POLAR-CAP SURVEY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE GALAXIES, CLUSTERING; GALAXIES, X-RAYS; RADIO SOURCES, GENERAL; RADIO SOURCES, IDENTIFICATIONS; RADIO SOURCES, SPECTRA ID MEDIUM-SENSITIVITY SURVEY; CLUSTERS; GALAXIES AB Four fields containing radio sources with spectral indices greater than unity at low frequencies have been observed over a wide range of radio wavelengths and at X-ray wavelengths. For most of the steep-spectrum sources no optical identifications have been found to the detection limit of the Palomar Schmidt prints, even with the positional precision of approximately 1" from VLA maps. This implies that the associated galaxies or clusters lie at a great distance. X-ray emission was not detected from any of the steep-spectrum radio sources. In one case, an extended source appears to be a radio halo in an uncataloged cluster of galaxies at a redshift of 0.125, and we suggest that this object is a promising candidate for the detection of inverse Compton X-rays, since it is not a high-luminosity source of thermal X-rays. C1 UNIV OXFORD,DEPT ASTROPHYS,OXFORD OX1 3RH,ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP DEWDNEY, PE (reprint author), NATL RES COUNCIL CANADA,DOMINION RADIO ASTRON OBSERV,BOX 248,PENTICTON V2A 6K3,BC,CANADA. NR 15 TC 8 Z9 8 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 AUG PY 1991 VL 76 IS 4 BP 1055 EP 1066 DI 10.1086/191590 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA FZ247 UT WOS:A1991FZ24700002 ER PT J AU VRTILEK, SD MCCLINTOCK, JE SEWARD, FD KAHN, SM WARGELIN, BJ AF VRTILEK, SD MCCLINTOCK, JE SEWARD, FD KAHN, SM WARGELIN, BJ TI THE EINSTEIN OBJECTIVE GRATING SPECTROMETER SURVEY OF GALACTIC BINARY-X-RAY SOURCES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE X-RAYS, BINARIES; X-RAYS, SPECTRA ID EMISSION-LINES; CYGNUS X-2; SPECTRAL VARIABILITY; SCORPIUS X-1; SPECTROSCOPY; ABSORPTION; MODELS; HERCULES-X-1; RADIATION; PLASMA AB The results of observations of 22 bright Galactic X-ray point sources taken with the Objective Grating Spectrometer (OGS) of the Einstein Observatory are presented. In most cases simultaneous observations with the Monitor Proportional Counter (MPC) are available also. By combining the high spectral resolution data from the OGS (E/DELTA-E = 31[E(keV)]-1 over the range 0.2-1.5 keV), which effectively constrain column densities, with the higher energy range data from the MPC (1-20 keV), which serve to constrain continuum temperatures, the most reliable measurements to date of X-ray column densities to these sources have been derived. The measured column densities range from N(H) = 4.0 x 10(19) to 5.0 x 10(23) cm-2. The extinction A-upsilon-X-ray implied by measured N(H) is always greater than or approximately equal to optically measured A-upsilon-opt; in addition, for several sources where multiple observations exist, the column density varies as a function of orbital phase. These results are consistent with the idea that some of the objects have a component of column density intrinsic to the source in addition to an interstellar component. The K-edge absorption due to oxygen is clearly detected in 10 of the sources, and the Fe L and Ne K edges are detected in a few. X-ray line emission is detected unambiguously in 11 of the sources and marginally in another four; the line features observed suggest that the emitting material spans a large range in temperature and ionization state. Neither models with excitation by photoionization nor those with excitation by collisions can reproduce the relative intensities of the features. However, features that can be associated with one or the other mechanisms are observed simultaneously; since X-ray binaries are not spatially resolved, it is probable that emission originating in a collisionally excited (coronal) region and emission from a photoionized region excited directly by the central source are combined in the spectra that we have obtained. Future missions with higher energy resolution and sensitivity will greatly facilitate measurement of line velocities as a function of binary phase, enabling disentanglement of the line emission regions. An atlas of the raw count spectrum and photon spectrum of each observation is presented. C1 UNIV CALIF BERKELEY, DEPT PHYS, BERKELEY, CA 94720 USA. RP VRTILEK, SD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 64 TC 56 Z9 56 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 1991 VL 76 IS 4 BP 1127 EP 1167 DI 10.1086/191594 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA FZ247 UT WOS:A1991FZ24700006 ER PT J AU LUBIN, YD AF LUBIN, YD TI PATTERNS OF VARIATION IN FEMALE-BIASED COLONY SEX-RATIOS IN A SOCIAL SPIDER SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE BIASED SEX RATIO; SOCIAL SPIDERS; ACHAEARANEA-WAU; COLONY DEMOGRAPHY ID ACHAEARANEA-WAU THERIDIIDAE; ANELOSIMUS-EXIMIUS ARANEAE; WASP NASONIA-VITRIPENNIS; PARASITIC WASP; GENETIC-VARIATION; EVOLUTION; BEHAVIOR; COMPETITION; SELECTION; MODEL C1 SMITHSONIAN TROP RES INST, BALBOA, PANAMA. RI Lubin, Yael/F-1382-2012 OI Lubin, Yael/0000-0003-3876-1668 NR 41 TC 20 Z9 21 U1 0 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD AUG PY 1991 VL 43 IS 4 BP 297 EP 311 DI 10.1111/j.1095-8312.1991.tb00601.x PG 15 WC Evolutionary Biology SC Evolutionary Biology GA GE580 UT WOS:A1991GE58000005 ER PT J AU GOLDWIRTH, DS PIRAN, T AF GOLDWIRTH, DS PIRAN, T TI ENTROPY, INFLATION AND THE ARROW OF TIME SO CLASSICAL AND QUANTUM GRAVITY LA English DT Letter ID SCALAR FIELD; ASYMMETRY; UNIVERSE AB One of the motivations for the introduction of inflation was to explain the large entropy of the observed universe. Penrose has recently pointed out that the entropy of the observable universe is small when compared with the maximal possible entropy. We show that this phenomenon is also a natural consequence of inflation. furthermore, inflation is generic in the expanding phase but exceedingly unlikely in the collapsing phase. This introduces an asymmetry in the evolution of the universe which resembles to a large extent the asymmetry that appears in the growth of entropy and it might be related to the question of the arrow of time. C1 HEBREW UNIV JERUSALEM,RACAH INST PHYS,JERUSALEM,ISRAEL. RP GOLDWIRTH, DS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 18 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TECHNO HOUSE, REDCLIFFE WAY, BRISTOL, ENGLAND BS1 6NX SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD AUG PY 1991 VL 8 IS 8 BP L155 EP L160 DI 10.1088/0264-9381/8/8/001 PG 6 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA GA656 UT WOS:A1991GA65600001 ER PT J AU BEEHLER, BM SWABY, RJ AF BEEHLER, BM SWABY, RJ TI PHYLOGENY AND BIOGEOGRAPHY OF THE PTILORIS RIFLEBIRDS (AVES, PARADISAEIDAE) SO CONDOR LA English DT Article DE SYSTEMATICS; BIOGEOGRAPHY; PTILORIS; PARADISAEIDAE; RIFLEBIRDS ID BIRDS AB We performed a phylogenetic and biogeographic study of the riflebird genus Ptiloris (Paradisaeidae). Our analysis, which includes sonograms documenting intertaxonomic variation in male advertisement vocalizations and a reassessment of key morphological characters, indicates that (1) the genus includes two distinct clades (P. victoriae/paradiseus and the P. magnificus complex); (2) within the P. magnificus complex, the eastern Papuan form may constitute a heretofore unrecognized sibling species; and (3) the biogeography of Ptiloris provides additional confirming evidence that the Torres Strait has been of minor importance as a biogeographic barrier for Australo-Papuan rainforest birds. RP BEEHLER, BM (reprint author), SMITHSONIAN INST,NHB ROOM 336,WASHINGTON,DC 20560, USA. NR 28 TC 6 Z9 6 U1 4 U2 12 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 AUG PY 1991 VL 93 IS 3 BP 738 EP 745 DI 10.2307/1368206 PG 8 WC Ornithology SC Zoology GA GG626 UT WOS:A1991GG62600028 ER EF