|Statistical Constraints for Astrometric Binaries with Nonlinear Motion|
Useful constraints on the orbits and mass ratios of astrometric binariesin the Hipparcos catalog are derived from the measured proper motiondifferences of Hipparcos and Tycho-2 (Δμ), accelerations ofproper motions (μ˙), and second derivatives of proper motions(μ̈). It is shown how, in some cases, statistical bounds can beestimated for the masses of the secondary components. Two catalogs ofastrometric binaries are generated, one of binaries with significantproper motion differences and the other of binaries with significantaccelerations of their proper motions. Mathematical relations betweenthe astrometric observables Δμ, μ˙, and μ̈ andthe orbital elements are derived in the appendices. We find a remarkabledifference between the distribution of spectral types of stars withlarge accelerations but small proper motion differences and that ofstars with large proper motion differences but insignificantaccelerations. The spectral type distribution for the former sample ofbinaries is the same as the general distribution of all stars in theHipparcos catalog, whereas the latter sample is clearly dominated bysolar-type stars, with an obvious dearth of blue stars. We point outthat the latter set includes mostly binaries with long periods (longerthan about 6 yr).
|Shocked Clouds in the Vela Supernova Remnant|
Unusually strong high-excitation C I has been detected in 11 lines ofsight through the Vela supernova remnant (SNR) by means of UV absorptionline studies of IUE data. Most of these lines of sight lie near thewestern edge of the bright X-ray region of the SNR in a spatiallydistinct band approximately 1° by 4° oriented approximatelynorth-south. The high-excitation C I (denoted C I* and C I**) isinterpreted as evidence of a complex of shocked dense clouds interactingwith the SNR, because of the high pressures indicated in this region. Tofurther analyze the properties of this region of enhanced C I* and CI**, we present new HIRES-processed IRAS data of the entire Vela SNR. Atemperature map calculated from the HIRES IRAS data, based on atwo-component dust model, reveals the signature of hot dust at severallocations in the SNR. The hot dust is anticorrelated spatially withX-ray emission, as would be expected for a dusty medium interacting witha shock wave. The regions of hot dust are strongly correlated withoptical filaments, supporting a scenario of dense clouds interior to theSNR that have been shocked and are now cooling behind the supernovablast wave. With few exceptions, the lines of sight to the stronghigh-excitation C I pass through regions of hot dust and opticalfilaments. Possible mechanisms for the production of the unexpectedlylarge columns of high-excitation C I are discussed. Dense clouds on theback western hemisphere of the remnant may explain the relatively lowX-ray emission in the western portion of the Vela SNR due to the slowerforward shock velocity in regions where the shock has encountered thedense clouds. An alternate explanation for the presence of ground-stateand excited-state neutrals, as well as ionized species, along the sameline of sight is a magnetic precursor that heats and compresses the gasahead of the shock.
|Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics|
The Catalogue, available at the Centre de Données Stellaires deStrasbourg, consists of 13 573 records concerning the results obtainedfrom different methods for 7778 stars, reported in the literature. Thefollowing data are listed for each star: identifications, apparentmagnitude, spectral type, apparent diameter in arcsec, absolute radiusin solar units, method of determination, reference, remarks. Commentsand statistics obtained from CADARS are given. The Catalogue isavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (220.127.116.11) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcar?J/A+A/367/521
|Spectroscopy and Time Variability of Absorption Lines in the Direction of the Vela Supernova Remnant|
We present high-resolution (R~75,000), high signal-to-noise (S/N~100) CaII λ3933.663 and Na I λλ5889.951, 5895.924 spectraof 68 stars in the direction of the Vela supernova remnant. The spectracomprise the most complete high-resolution, high S/N optical survey ofearly-type stars in this region of the sky. A subset of the sight lineshas been observed at multiple epochs, 1993/1994 and 1996. Of the 13stars observed twice, seven have spectra revealing changes in theequivalent width and/or velocity structure of lines, most of which arisefrom remnant gas. Such time variability has been reported previously forthe sight lines toward HD 72089 and HD 72997 by Danks & Sembach andfor HD 72127 by Hobbs and coworkers. We have confirmed the ongoing timevariability of these spectra and present new evidence of variability inthe spectra of HD 73658, HD 74455, HD 75309, and HD 75821. We havetabulated Na I and Ca II absorption-line information for the sight linesin our sample to serve as a benchmark for further investigations of thedynamics and evolution of the Vela SNR. Based on observations obtainedat the European Southern Observatory, La Silla, Chile.
|The ROSAT all-sky survey catalogue of optically bright OB-type stars.|
For the detailed statistical analysis of the X-ray emission of hot starswe selected all stars of spectral type O and B listed in the Yale BrightStar Catalogue and searched for them in the ROSAT All-Sky Survey. Inthis paper we describe the selection and preparation of the data andpresent a compilation of the derived X-ray data for a complete sample ofbright OB stars.
|Tests of the Pulsation and Starspot Models for the Periodic Be-Stars|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995MNRAS.277.1547B&db_key=AST
|Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.|
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
|A search for rapid photometric variations in southern Be and BN stars|
Fifteen Be, 5 Bn, and 1 B stars were monitored during 10 nights inMarch-April 1988 by means of photoelectric ubvy photometry. At least 80percent of the Be stars were found variable. Tentative periods between0.3 and 4.3 days were derived for 13 stars of this entire sample. In allcases, the stars are bluest when brightest. Variations in B0-B5e starsare, in average, of larger amplitude than in B5-B9e stars. Bn starsshow, in general, variations of smaller amplitude than Be stars. Theseresults are discussed in terms of the current models on short-termphotometric variability. In addition, from the observed perioddistribution the existence of intrinsically slow Be rotators arededuced. The rotation of slightly displaced poles of a weak globaldipolar magnetic field is proposed as being responsible for the rapidperiodic light variations.
|Radial velocities in three fields along the southern galactic equator|
A list of radial velocities for 764 stars is given for three fields inthe Vela-Carina region of the galaxy. They were obtained from GPO-platestaken at La Silla and reduced following Fehrenbach's method.Slit-spectra were collected with the 152 cm-spectrographic telescope atLa Silla, to derive an accurate radial velocity for a sufficient numberof calibration stars: out of the 29 stars, 26 had no formerly publishedvalue. The global motions of 10 to 14 km/s can be considered as normalon the basis of galactic rotation. Some stars, however, show highvelocities, and are therefore marked with one or two asterisks in thetable.
|Carbon and nitrogen in B2 to A2 main-sequence stars|
Carbon abundances are derived from the C II resonance doublet at 1335 Ain 108 main-sequence stars between 9000 and 21000 K from IUE archivaldata. Only alpha Leo and psi sq 2 Aqr are strongly carbon deficient(factors 14 and 50, resp.). The N I lines at 1493 and 1495 A weremeasured in 28 sharp-lined stars below 16500 K. Nitrogen anomalies arefound in 5 stars, but seem uncorrelated to the C abundances. Fourmechanisms for the depletion of carbon are discussed, but none issatisfactory.
|The local system of early type stars - Spatial extent and kinematics|
Published uvby and H-beta photometric data and proper motions arecompiled and analyzed to characterize the structure and kinematics ofthe bright early-type O-A0 stars in the solar vicinity, with a focus onthe Gould belt. The selection and calibration techniques are explained,and the data are presented in extensive tables and graphs and discussedin detail. The Gould belt stars of age less than 20 Myr are shown togive belt inclination 19 deg to the Galactic plane and node-lineorientation in the direction of Galactic rotation, while the symmetricaldistribution about the Galactic plane and kinematic properties (purecircular differential rotation) of the belt stars over 60 Myr oldresemble those of fainter nonbelt stars of all ages. The unresolveddiscrepancy between the expansion observed in the youngest nearby starsand the predictions of simple models of expansion from a point isattributed to the inhomogeneous distribution of interstellar matter.
|Interstellar gas in the GUM Nebula|
A survey of the interstellar gas near the Gum Nebula by opticalobservation of 67 stars at Ca II, 42 stars at Na I, and 14 stars in theUV with the Copernicus satellite provided radial velocities and columndensities for all resolved absorption components. Velocity dispersionsfor gas in the Gum Nebula are not significantly larger than in thegeneral interstellar medium; the ionization structure is predominantlythat of an H II region with moderately high ionization. Denser, morehighly ionized clouds are concentrated toward the Gum Nebula; theseclouds do not show the anomalously high ionization observed in the Velaremnant clouds.
|The VELA star cloud. I - NGC 2547, TR 10, the Gamma Velorum system, and bright stars|
The first results of an intermediate-band, large-scale photometricsurvey of the Vela star cloud are discussed. Attention is given to theluminosity and reddening, as well as the apparent or proper motions ofall the CPD stars near NGC 2547, the brightest stars in Trumpler 10, arandom selection of stars in the region of Gamma Velorum, and the HRstars. The similarity of the Alpha Persei cluster with the clusters inthe Vela sheet is shown, and it is found that the Vela sheet, at leastover the region surveyed, is nearly perpendicular to the line of sight.The probability is demonstrated that a thin sheet of coeval (2.5 x 10 tothe 7th yr) stars, some 425 pc distant and with a similar metalabundance, lies in front of a dense dark cloud.
|A catalogue of stellar spectrophotometric data|
A list of 378 sets of stellar energy distributions for 356 stars basedon photoelectric spectrophotometry is presented. Data from eight sourceshave been transformed to the Hayes-Latham calibration of Alpha Lyrae.The procedure follows that of Breger (1976) and the present list extendsprevious data, especially for stars of earliest and intermediatespectral types.
|Prediction of spectral classification from photometric observations - Application of the UVBY beta photometry and the MK spectra classification. II - General case|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1980A&A....85...93M&db_key=AST
|Prediction of spectral classification from photometric observations-application to the UVBY beta photometry and the MK spectral classification. I - Prediction assuming a luminosity class|
An algorithm based on multiple stepwise and isotonic regressions isdeveloped for the prediction of spectral classification from photometricdata. The prediction assumes a luminosity class with reference touvbybeta photometry and the MK spectral classification. The precisionattained is about 90 percent and 80 percent probability of being withinone spectral subtype respectively for luminosity groups I and V and forluminosity groups III and IV. A list of stars for which discrepanciesappear between photometry and spectral classification is given.
|Ultraviolet absorption lines associated with the VELA supernova remnant|
Two stars behind the Vela supernova remnant and two stars offset fromthe remnant have been observed with the UV spectrometer aboard theCopernicus satellite. Over 200 interstellar atomic and molecularabsorption features between 1000 and 1400 A have been identified andmeasured for radial velocity and equivalent width. In many cases,additional information was obtained by studying the detailed shapes ofthe recorded profiles. Most of the stars show several absorptioncomponents, with clouds of the highest radial velocity appearing in thespectra of stars behind the remnant. For each component, columndensities were derived using velocity dispersion parameters whichyielded the most self-consistent results. Qualitatively, the gas towardthe remnant exhibits a number of unusual properties, when compared withnormal interstellar material. First, abnormally high radial velocitieswere evident. Second, the degree of ionization of some elementssuggested the existence of ionizing processes significantly more potentthan those found in general regions of space. Finally, an investigationof electron densities shows that much of the gas, especially that athigh velocity, must exist in the form of relatively thin sheets orfilaments. If cosmic abundances prevail, the column densities ofhigh-velocity excited material suggest that H-alpha emission measurescould be as large as 100 sq cm/cu pc.
|Measurements of neutral-hydrogen absorption in the spectra of five pulsars and parameters of the GUM Nebula|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975A&A....40...27G&db_key=AST
|New kinematical data for bright southern OB-stars|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1972A&AS....5..129L&db_key=AST
|Interstellar Gas in the Direction of the VELA Pulsar|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971ApJ...170..289W&db_key=AST
|Four-color and H-beta photometry for bright B-type stars in the southern hemisphere.|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971AJ.....76..621C&db_key=AST
|MK Spectral Types for Bright Southern OB Stars|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1969ApJ...157..313H&db_key=AST
|A Photometric Investigation of the SCORPlO-CENTAURUS Association|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1968ApJS...15..459G&db_key=AST
|A Survey of Southern Be Stars|
|The Scorpio-Centaurus Association: II. Spectral types and luminosities of 220 O, B and a stars|
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1961MNRAS.122..325M&db_key=AST