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B Star Rotational Velocities in h and χ Persei: A Probe of Initial Conditions during the Star Formation Epoch?
Projected rotational velocities (vsini) have been measured for 216 B0-B9stars in the rich, dense h and χ Persei double cluster and comparedwith the distribution of rotational velocities for a sample of fieldstars having comparable ages (t~12-15 Myr) and masses (M~4-15Msolar). For stars that are relatively little evolved fromtheir initial locations on the zero-age main sequence (ZAMS) (those withmasses M~4-5 Msolar), the mean vsini measured for the h andχ Per sample is slightly more than 2 times larger than the meandetermined for field stars of comparable mass, and the cluster and fieldvsini distributions differ with a high degree of significance. Forsomewhat more evolved stars with masses in the range 5-9Msolar, the mean vsini in h and χ Per is 1.5 times thatof the field; the vsini distributions differ as well, but with a lowerdegree of statistical significance. For stars that have evolvedsignificantly from the ZAMS and are approaching the hydrogen exhaustionphase (those with masses in the range 9-15 Msolar), thecluster and field star means and distributions are only slightlydifferent. We argue that both the higher rotation rates and the patternof rotation speeds as a function of mass that differentiatemain-sequence B stars in h and χ Per from their field analogs werelikely imprinted during the star formation process rather than a resultof angular momentum evolution over the 12-15 Myr cluster lifetime. Wespeculate that these differences may reflect the effects of the higheraccretion rates that theory suggests are characteristic of regions thatgive birth to dense clusters, namely, (1) higher initial rotationspeeds; (2) higher initial radii along the stellar birth line, resultingin greater spin-up between the birth line and the ZAMS; and (3) a morepronounced maximum in the birth line radius-mass relationship thatresults in differentially greater spin-up for stars that become mid- tolate-B stars on the ZAMS.
| Statistics of the Instability Strip of β Cephei Stars
We present a study of the β Cephei instability strip based on asample of 49 stars of this type. After deriving their effectivetemperatures and luminosities from their observed (B-V), (U-B) colorsand parallaxes we find their positions in the HR diagram to be mostlyconfined to the main sequence, and their masses to lie between 7Mȯ and 30 Mȯ. Their distribution on theHR diagram matches well with our previous theoretical instability stripwhich has an upper bound in the luminosity and rather tight boundariesin the effective temperature.
| Rotational Velocities of B Stars
We measured the projected rotational velocities of 1092 northern B starslisted in the Bright Star Catalogue (BSC) and calibrated them againstthe 1975 Slettebak et al. system. We found that the published values ofB dwarfs in the BSC average 27% higher than those standards. Only 0.3%of the stars have rotational velocities in excess of two-thirds of thebreakup velocities, and the mean velocity is only 25% of breakup,implying that impending breakup is not a significant factor in reducingrotational velocities. For the B8-B9.5 III-V stars the bimodaldistribution in V can be explained by a set of slowly rotating Ap starsand a set of rapidly rotating normal stars. For the B0-B5 III-V starsthat include very few peculiar stars, the distributions in V are notbimodal. Are the low rotational velocities of B stars due to theoccurrence of frequent low-mass companions, planets, or disks? Therotational velocities of giants originating from late B dwarfs areconsistent with their conservation of angular momentum in shells.However, we are puzzled by why the giants that originate from the earlyB dwarfs, despite having 3 times greater radii, have nearly the samerotational velocities. We find that all B-type primaries in binarieswith periods less than 2.4 days have synchronized rotational and orbitalmotions; those with periods between 2.4 and 5.0 days are rotating withina factor 2 of synchronization or are ``nearly synchronized.'' Thecorresponding period ranges for A-type stars are 4.9 and 10.5 days, ortwice as large. We found that the rotational velocities of the primariesare synchronized earlier than their orbits are circularized. The maximumorbital period for circularized B binaries is 1.5 days and for Abinaries is 2.5 days. For stars of various ages from 107.5 to1010.2 yr the maximum circularized periods are a smoothexponential function of age.
| Velocity Distribution of Stars in the Pup-CMa Association
The distribution of proper motions of stars in the Pup-CMa associationis presented. The stars' velocities are approximately parallel to eachother, which indicates that the stars are close together in space. Themutual distribution of stars and molecular clouds in the association isinterpreted as proof that the stars emerged from a single giganticprimordial molecular cloud (or several large clouds), destroyed byradiation and/or stellar wind coming from those stars. It is assumedthat part of that cloud is being dissipated, while part is being brokeninto several small clouds, which we are observing at present.
| 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 (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcar?J/A+A/367/521
| Surface abundances of light elements for a large sample of early B-type stars - I. Spectral observations of 123 stars; measurements of hydrogen and helium lines; infrared photometry
High-resolution spectral observations of 123 B0-B5 stars in the mainsequence evolutionary phase were obtained at two observatories, namelythe McDonald Observatory (McDO) and the Crimean AstrophysicalObservatory (CrAO). Accurate equivalent widths W of two Balmer lines,Hβ and Hγ, and ten Hei lines were obtained for all the stars,as well as of the Heiiλ4686 line for the hottest ones. A carefulanalysis of the measured equivalent widths was performed. It is shownthat there is a very good agreement between the W values derived fromthe McDO and CrAO spectra for 14 common stars. A comparison withpublished data leads to the conclusion that the W values measuredearlier by some authors for strong Hei lines are very likely to beunderestimated. Infrared photometric observations in the J, H, and Kbands were performed for 70 programme stars. All these data will be usedin other papers: in particular for the Teff and loggdetermination and for the He, C, N and O abundance analyses.
| The distribution of bright OB stars in the Canis Major-Puppis-Vela region of the Milky Way
The picture of the young stellar groups in the Canis Major-Puppis-Vela(215 deg
| B Stars as a Diagnostic of Star Formation at Low and High Redshift
We have extended the evolutionary synthesis models by Leitherer et al.by including a new library of B stars generated from the IUEhigh-dispersion spectra archive. We present the library and show how thestellar spectral properties vary according to luminosity classes andspectral types. We have generated synthetic UV spectra for prototypicalyoung stellar populations varying the IMF and the star formation law.Clear signs of age effects are seen in all models. The contribution of Bstars in the UV line spectrum is clearly detected, in particular forgreater ages when O stars have evolved. With the addition of the newlibrary we are able to investigate the fraction of stellar andinterstellar contributions and the variation in the spectral shapes ofintense lines. We have used our models to date the spectrum of the localsuper-star cluster NGC 1705-1. Photospheric lines of C III λ1247,Si III λ1417, and S V λ1502 were used as diagnostics todate the burst of NGC 1705-1 at 10 Myr. Interstellar lines are clearlyseen in the NGC 1705-1 spectrum. Broadening and blueshifts of severalresonance lines are stronger in the galaxy spectrum than in our modelsand are confirmed to be intrinsic of the galaxy. Si II λ1261 andAl II λ1671 were found to be pure interstellar lines with anaverage blueshift of 78 km s-1 owing to a directed outflow ofthe interstellar medium. We have selected the star-forming galaxy1512-cB58 as a first application of the new models to high-z galaxies.This galaxy is at z=2.723, it is gravitationally lensed, and its highsignal-to-noise ratio Keck spectrum shows features typical of localstarburst galaxies, such as NGC 1705-1. Models with continuous starformation were found to be more adequate for 1512-cB58 since there arespectral features typical of a composite stellar population of O and Bstars. A model with Z=0.4 Zsolar and an IMF with α=2.8reproduces the stellar features of the 1512-cB58 spectrum.
| Simultaneous photometry and spectroscopy of the Be star 28 (omega) CMa - I. Observational evidence of the periodic components of rapid variability
We analyse the periodic variability of the Be star 28 (omega) CMa. Thedata consist of 275 new He I 6678 line profiles of high spectral andtemporal resolution, and new Strömgren and Geneva photometry. Thephotometric analysis has been extended by including previously publisheddata to cover an interval of 16 yr. The principal spectroscopic periodof 1.37 d is confirmed by analysis of He I 6678 modes and moments. Thereis evidence to show that a single period is insufficient to explain thevariation in the line wings. In particular, the variation of the secondmoment, which samples the line wings, is best described when a secondperiod is included. The photometric data have been divided into 10 setsin which the time is sufficiently contiguous for period analysis. Thesesets have been smoothed to remove as well as possible the long-termirregular variations which are always present in Be stars. The residualshave then been analysed for coherent periodicities using severaltechniques. Evidence for one or the other of the two known spectroscopicperiods can be found in individual data sets. By an analysis in whichtwo periods are assumed, it is possible to recover both the principalspectroscopic period and the satellite period of 1.46 d. Unlike in theHe I 6678 line profiles, the latter period seems to be most oftenpresent in the light variations. The amplitude of the periodiccomponents of the light variation is only a few millimagnitudes, incontrast to the very large radial velocity amplitude. We find that thephotometric amplitudes of the two periodic components, and their ratio,vary smoothly on a time-scale of years. The amplitudes are larger inseasons when the mean brightness is higher.
| Determining the Physical Properties of the B Stars. I. Methodology and First Results
We describe a new approach to fitting the UV-to-optical spectra of Bstars to model atmospheres and present initial results. Using a sampleof lightly reddened stars, we demonstrate that the Kurucz modelatmospheres can produce excellent fits to either combined low-dispersionIUE and optical photometry or HST FOS spectrophotometry, as long as thefollowing conditions are fulfilled: (1) an extended grid of Kuruczmodels is employed; (2) the IUE NEWSIPS data are placed on the FOSabsolute flux system using the Massa & Fitzpatrick transformation;(3) and all of the model parameters and the effects of interstellarextinction are solved for simultaneously. When these steps are taken,the temperatures, gravities, abundances, and microturbulence velocitiesof lightly reddened B0-A0 V stars are determined to high precision. Wealso demonstrate that the same procedure can be used to fit the energydistributions of stars that are reddened by any UV extinction curve thatcan be expressed by the Fitzpatrick & Massa parameterization scheme.We present an initial set of results and verify our approach throughcomparisons with angular diameter measurements and the parametersderived for an eclipsing B-star binary. We demonstrate that themetallicity derived from the ATLAS9 fits to main-sequence B stars isessentially the Fe abundance. We find that a near zero microturbulencevelocity provides the best fit to all but the hottest or most luminousstars (where it may become a surrogate for atmospheric expansion) andthat the use of white dwarfs to calibrate UV spectrophotometry is valid.
| New OB-Association in Pup - CMA
Not Available
| UBV beta Database for Case-Hamburg Northern and Southern Luminous Stars
A database of photoelectric UBV beta photometry for stars listed in theCase-Hamburg northern and southern Milky Way luminous stars surveys hasbeen compiled from the original research literature. Consisting of over16,000 observations of some 7300 stars from over 500 sources, thisdatabase constitutes the most complete compilation of such photometryavailable for intrinsically luminous stars around the Galactic plane.Over 5000 stars listed in the Case-Hamburg surveys still lackfundamental photometric data.
| An extensive Delta a-photometric survey of southern B and A type bright stars
Photoelectric photometry of 803 southern BS objects in the Deltaa-system as detection tool for magnetic chemically peculiar (=CP2) starshas been carried out and compared to published spectral types. Thestatistical yield of such objects detected by both techniques ispractically the same. We show that there are several factors whichcontaminate the search for these stars, but this contamination is onlyof the order of 10% in both techniques. We find a smooth transition fromnormal to peculiar stars. Our sample exhibits the largest fraction ofCP2 stars at their bluest colour interval, i.e. 10% of all stars in thecolour range -0.19 <= B-V < -0.10 or -0.10 <= b-y < -0.05.No peculiar stars based on the Delta a-criterion were found at bluercolours. Towards the red side the fraction of CP2 stars drops to about3% for positive values of B-V or b-y with red limits roughlycorresponding to normal stars of spectral type A5. The photometricbehaviour of other peculiar stars: Am, HgMn, delta Del, lambda Boo, Heabnormal stars, as well as Be/shell stars and supergiants shows someslight, but definite deviations from normal stars. Spectroscopic andvisual binaries are not distinguished from normal stars in their Delta abehaviour. The results of this work justify larger statistical work(e.g. in open clusters) employing more time-saving photometric methods(CCD). \newpage Based on observations obtained at the European SouthernObservatory, La Silla, Chile. This research has made use of the Simbaddatabase, operated at CDS, Strasbourg, France. Table 2 is only availablein electronic form via anonymous ftp 130.79.128.5 orhttp://cdsweb.u-strasbg.fr/Abstract.html
| On the nature of the Be phenomenon. I. The case of omega Canis Majoris
The main purpose of this paper is to demonstrate the extreme complexityof the observed variations of Be stars on the example of a well-observedbright Be star omega CMa. A detailed analysis of all published radialvelocities and a representative set of photometric and spectralobservations of this star led to the following firm conclusions:\begin{itemize} At least three and possibly four different time scalesof variability of omega CMa, ranging from 1\D37 to more than 40 years,could be identified. The correct mean period of the RV and line-profilechanges is 1\D371906, not 1\D3667 as derived earlier. The brightness ofthe object and the strength of the Balmer emission vary in an apparentcycle of several thousands of days. The long-term brightness andemission-line changes can be understood as consequences of the formationand gradual dispersal of a gaseous envelope which is flattened and seenmore face-on than equator-on. During each episode, the envelope growsfrom an optically thick pseudophotosphere to a more extended andoptically thin envelope. Existence of much smaller episodes of lightbrightening which can have the same cause (though on a more limitedscale) has clearly been demonstrated. The amplitude of the 1\D37 RVcurve varies on a time scale somewhere between 10 and 300 d. Thefollowing conclusions are less certain and represent possiblealternatives to be tested by future, systematic and homogeneousobservations: \begin{itemize} Some evidence is presented that theamplitude of the 1\D372 RV variations, local mean RV and brightness ofthe object, prewhitened for the long-term changes, all vary on a timescale of about 35 d, possibly with a period of 34\D675. The O-Cdeviations of the local epochs of RV maxima from a linear ephemeris forthe 1\D372 period seem to be undergoing a slow and probably cyclicvariation in time, being shortest at times when the star is brightestand when a new Be envelope begins to grow. However, the same O-Cdeviations can also be reconciled with the 34\D675 period. Whatever thetrue timescale of the O-C deviations is, their behaviour can also besimulated as an interference of several periods, the second mostsignificant period being close to 1\D35. Several reasons are given whythe explanation in terms of one variable period appears more probable.With the help of both, real and artificial data it is demonstrated thatthe slow variation of the 1\D3719 period -- if unrecognized -- may bemisinterpreted for a multiperiodic variation with several close periodsbetween 1\D3 and 1\D45. This constitutes a methodological warning forthe period analyses of data on some \bn, Be and ``slowly pulsating" Bstars. The cause(s) of the variations with the 1\D37 (and 1\D345)period(s) and/or the 35 d cycle remain unexplained. It is obvious,however, that these three periods are not mutually independent. The34\D675 period may be either a real physical period or a beat periodbetween the 1\D372 and 1\D345 periods. In the former case, omega CMacould be a 34\D7 binary in an eccentric orbit and the periods twicelonger than the two periods near 1\D4 would represent the sidereal andsynodic rotational periods of the Be primary. Finally, some speculationsare offered in terms of a hierarchical multiple system of three or evenfour stars.
| A Radial Velocity Database for Stephenson-Sanduleak Southern Luminous Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....113..823R&db_key=AST
| 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.
| Average unreddened UV flux distributions of OB dwarfs
The average intrinsic flux distributions for early-type main-sequencestars are obtained from IUE low-dispersion spectra. The colour-excessdereddening method allows stars of various colour excesses to beincluded in the samples. The resulting spectra are free from allinterstellar extinction effects that correlate with E(B-V).
| A spectroscopic database for Stephenson-Sanduleak Southern Luminous Stars
A database of published spectral classifications for objects in theStepenson-Sanduleak Luminous Stars in the Southern Milky Way catalog hasbeen compiled from the literature. A total of 6182 classifications for2562 stars from 139 sources are incorporated.
| Far-Ultraviolet (912--1900 Angstrom ) Energy Distribution in Early-Type Main-Sequence Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJ...449..280C&db_key=AST
| Note on the radial velocities of 10 southern stars.
Echelle spectrograms of the stars HD 55857, 57219, 62623, 83058, 84400,86087, 86523, 89461, 90898, 96446 have been obtained in 1991 as part ofan investigation of stars previously classified as both chemicallypeculiar and high luminosity B and A stars. Radial velocity measurementsfor HD 83058, 84400 and 86087 are internally discordant and should berepeated. In the case of HD 55857, 57219, 62623 and 96466 the resultsare in fair agreement with earlier measurements but for HD 86523 ourresult is substantially different from the earlier ones. For HD 89461and 90898 no comparison with other sources was available. With nofurther observational opportunities in view (due to increasing demand ontelescopes), these preliminary results are presented here.
| SANTIAGO 91, a right ascension catalogue of 3387 stars (equinox J2000).
The positions in right ascension of 3387 stars belonging to the Santiago67 Catalogue, observed with the Repsold Meridian Circle at Cerro Calan,National Astronomical Observatory, during the period 1989 to 1994, aregiven. The average mean square error of a position, for the wholeCatalogue, is +/-0.009 s. The mean epoch of the catalogue is 1991.84.
| The distance to the Wolf-Rayet star HD 50896
We present high-resolution observations (R approximately equals105) of the interstellar Na I D lines in the spectra of 23stars which are close to HD 50896 on the plane of the sky, plus HD 50896itself. The results are parameterized by using simple cloud models. Weconfirm that HD 50896 lies beyond the cluster Cr 121 (which is in thesame line of sight), and estimate D approximately equals 1.8 kpc.
| An IUE survey of interstellar H I LY alpha absorption. 1: Column densities
We measure Galactic interstellar neutral hydrogen column densities byanalyzing archival interstellar Ly alpha absorption line data toward 554B2 and hotter stars observed at high resolution with the IUE satellite.This study more than doubles the number of lines of sight with measuresof N(H I) based on Ly alpha. We have included the scattered lightbackground correction algorithm of Bianchi and Bohlin in our datareduction. We use the correlation between the Balmer discontinuity(c1) index and the stellar Ly alpha absorption in order toassess the effects of stellar Ly alpha contamination. Approximately 40%of the B stars with measured (c1) index, exhibit seriousstellar Ly alpha contamination. One table contains the derived values ofthe interstellar N(H I) for 393 stars with at most small amounts ofstellar contamination. Another lists the observed values of total N(H I)for 161 stars with suspected stellar Ly alpha contamination and/oruncertain stellar parameters.
| An IUE survey of interstellar H I LY alpha absorption. 2: Interpretations
We present an analysis of interstellar neutral hydrogen column densitiesobtained from archival Ly alpha absorption line data toward the completesample of B2 and hotter stars observed at high spectral resolution withthe IUE satellite. The full sample includes 554 stars and more thandoubles the number of lines of sight previously observed. Many of the B2and B1.5 stars exhibit contamination from stellar Ly alpha absorption,and were excluded from the subsequent analysis. The final working sampleincludes 393 stars. We present statistical averages for a number ofquantities derived for the sample. The stars range in distance from 0.12to 11 kpc with an average distance of 2.1 kpc. Values for averagesight-line density range from 0.017 to 8.62 atoms cm-3, withan overall average of 0.23 atoms cm-3. Neutral hydrogen anddust are well correlated, with N(H I)/E(B - V) = 4.93 x 1021cm-2 mag-1, and N(H I)/E(Bump) = 2.17 x1021 cm-2 mag-1. There is an increasein the H I to dust ratios for the densest sight lines. Evidently, the HI to dust ratios in dense clouds are higher than in the lower densitymedium between the clouds and in interarm directions. The effect isprobably an indication of dust modification in the dense clouds. The H Ito dust ratios are approx. 17% smaller for the sight lines to O starscompared to the ratios found toward B stars. We have identified sightlines with anomalously large and small values of N(H I)/E(B - V) and H(HI)/E(Bump). Some of these sight lines are well-known examples ofpeculiar extinction (i.e., HD 147933 and HD 37061 (NU Ori)). Others areless well known and may provide important new examples of regions withhighly modified dust. The number of stars with anomalously low H I todust ratios is disproportionately larger than the number of stars withanomalously high H I to dust ratios. The distribution of the gas awayform the Galactic plane for the sample of objects is complex. For thesubset of 375 stars whose lines of sight have a statistically lowprobablility of intersecting a large cloud, the distribution may beroughly approximated by an exponential density distribution, with amidplane density of 0.366 atoms cm-3, a scale height of 195pc, and a random logarithmic scattering parameter sigma p of0.159 dex.
| Rnu-dependent optical and near-ultraviolet extinction
We have derived extinctions A(lambda)/A(V) at the wavelengths of theuvby filters for 22 stars, with a range of values of Rnu,from the sample of Cardelli, Clayton, & Mathis (1989, hereafterCCM). We have fit these extinctions, and also UBVRIJHKL, IUE and ANSextinction measurements, with linear relations A(lambda)/A/(V) =a+b/Rnu and fit a and b as a function of x(=1/lambda) withpolynomials to obtain an Rnu-dependent mean extinction law(A(x)/A(V) = a(x) + b(x)/Rnu)in the optical andnear-ultraviolet (1.1/micrometer less than or equal to 3.3/micrometer).This law is virtually identical to the CCM extinction law for largevalues of Rnu(Rnu approximately 5) but is slightlylower in the near-ultraviolet for smaller Rnu (Rnuapproximately 3). The extinction law presented here agrees much betterwith a high-resolution extinction curve for the diffuse interstellarmedium (Rnu approximately 3.1), presented by Bastiaansen(1992), than CCM. The deviations of individual extinction curves fromthe mean are dominated by observational errors. The wavelengthresolution of this work is not high enough to show evidence for oragainst the existence of very broad structure in optical extinctioncurves.
| The distribution of interstellar dust in the solar neighborhood
We surveyed the IRAS data base at the positions of the 1808 O6-B9.5stars in The Bright Star Catalog for extended objects with excessemission at 60 microns, indicating the presence of interstellar dust atthe location of the star. Within 400 pc the filling factor of theinterstellar medium, for dust clouds with a density greater than 0.5/cucm is 14.6 + or - 2.4%. Above a density of 1.0/cu cm, the densitydistribution function appears to follow a power law index - 1.25. Whenthe dust clouds are mapped onto the galactic plane, the sun appears tobe located in a low-density region of the interstellar medium of widthabout 60 pc extending at least 500 pc in the direction of longitudes 80deg - 260 deg, a feature we call the 'local trough'.
| The extraordinary early-type eclipsing binary HR 2680
Photometric observations of the HR 2680 (B5V) star using Stromgren-b andStromgren-uvby filters carried out in 1990 and 1991 are reported. It isfound that this star is a single-line spectroscopic binary showingpartial or annular eclipses with a period of 8.1 d. A light variationwith an amplitude of 0.03 mag can be seen outside eclipse which can beinterpreted as two oscillations, with approximate periods of about 1.19and 1.28 d, but the periods are not constant. It is suggested that thestar is a member of the 53 Per class of line-profile variables. Theextraordinary variability of HR 2680 outside eclipse makes this starunique. It is suggested that the star could be used as a test bed forstellar dynamics and nonradial pulsations.
| Ultraviolet and optical studies of binaries with luminous cool primaries and hot companions. IV - Further IUE detections
We have obtained IUE spectra for 31 middle and late-type giant andsupergiant stars whose TD-1 fluxes or ground-based spectra indicate thepresence of a hot component, or whose radial velocities indicate anunseen component. Stellar components earlier than type F1 were detectedin 22 cases. While 20 of the hot secondaries are seen weakly in opticalspectra, two are UV discoveries: HD 58134 and HD 183864. The hotcompanions are classified accurately by temperature class from theirfar-UV spectra. The interstellar extinction of each system and therelative luminosities of the components are derived from the UV andoptical fluxes, using a new grid of UV intrinsic colors for hot dwarfs.We find that many giant stars apparently have companions which are toohot and hence too luminous for consistency with the primary's spectralclassification.
| Longterm Photometry of Variables at ESO - Part Two - the Second Data Catalogue 1986-1990
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&AS..102...79S&db_key=AST
| Spectral synthesis in the ultraviolet. IV - A library of mean stellar groups
A library of mean UV stellar energy distributions is derived from IUEspectrophotometry of 218 stars. The spectra cover 1230-3200 A with aspectral resolution of about 6 A. They have been corrected forinterstellar extinction and converted to a common flux and wavelengthscale. Individual stars were combined into standard groups according totheir continuum colors, observed UV spectral morphology, MK luminosityclass, and metal abundance. The library consists of 56 groups: 21dwarf(V), 8 subgiant(IV), 16 giant(III), and supergiant(I + II) groups,covering O3-M4 spectral types. A metal-poor sequence is included,containing four dwarf and two giant groups, as is a metal-enhancedsequence with a single dwarf, subgiant, and giant group. Spectralindices characterizing the continuum and several strong absorptionfeatures are examined as temperature, luminosity, and abundancediagnostics. The library is intended to serve as a basis forinterpreting the composite UV spectra of a wide variety of stellarsystems, e.g., elliptical galaxies, starburst systems, and high-redshiftgalaxies.
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| Csillagkép: | Nagy Kutya |
| Rektaszcenzió: | 07h13m36.30s |
| Deklináció: | -27°21'23.0" |
| Vizuális fényesség: | 6.12 |
| Távolság: | 1587.302 parszek |
| RA sajátmozgás: | -3.6 |
| Dec sajátmozgás: | 4.3 |
| B-T magnitude: | 5.804 |
| V-T magnitude: | 6.062 |
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