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Contribution to the study of composite spectra - IX. Spectroscopic orbital elements of 10 systems*
We present the results of a radial-velocity study of 10 spectroscopicbinaries with composite spectra that were observed at Observatoire deHaute-Provence with the CORAVEL instrument. Those systems, including acool, evolved, primary and a hot secondary of type B or A, were found tobe spectroscopic binaries. We computed their orbital elements for thefirst time. For three systems, the large mass function implies i~90°, with the possibility of eclipses. Mean angular separations arevery small (a<= 0.010 arcsec), which makes those systems resolvableonly with multi-pupil large interferometers.
| Spectral Classification of the Hot Components of a Large Sample of Stars with Composite Spectra, and Implication for the Absolute Magnitudes of the Cool Supergiant Components.
A sample of 135 stars with composite spectra has been observed in thenear-UV spectral region with the Aurélie spectrograph at theObservatoire de Haute-Provence. Using the spectral classifications ofthe cool components previously determined with near infrared spectra, weobtained reliable spectral types of the hot components of the samplesystems. The hot components were isolated by the subtraction methodusing MK standards as surrogates of the cool components. We also derivedthe visual magnitude differences between the components usingWillstrop's normalized stellar flux ratios. We propose a photometricmodel for each of these systems on the basis of our spectroscopic dataand the Hipparcos data. We bring to light a discrepancy for the Gsupergiant primaries between the visual absolute magnitudes deduced fromHipparcos parallaxes and those tabulated by Schmidt-Kaler for the GIbstars: we propose a scale of Mv-values for these stars incomposite systems. By way of statistics, about 75% of the hot componentsare dwarf or subgiant stars, and 25% should be giants. The distributionin spectral types is as follows: 41% of B-type components, 57% of typeA, and 2% of type F; 68% of the hot components have a spectral type inthe range B7 to A2. The distribution of the ΔMv-valuesshows a maximum near 0.75 mag.
| Spectral classifications in the near infrared of stars with composite spectra. III. Study of a sample of 137 objects with the Aurelie spectrograph
We provide spectral classifications for a sample of 137 stars mentionedas having composite spectra. The classifications were carried out on 33Angstroms /mm spectra in the region 8370 - 8870 Angstroms. Of these 137objects, 115 correspond in the infrared to cool stars (G, K or M) ofluminosity classes III, II and I; for 22 stars, we find only hot spectraof types B, A, F or Am, so that they do not fulfil our definition ofcomposite spectra. We detect four new Am stars, and one Am star (HD70826) turns out to be a composite spectrum object. As in Paper II, thecool components of composite spectra show a strong concentration in thevicinity of G8III. Based upon observations carried out at Observatoirede Haute-Provence (OHP).
| Environments of active close binaries. II. GK Hydrae and TY Pyxidis.
High-resolution spectroscopic observations were obtained for twoeclipsing active close binary systems, GK Hydrae and TY Pyxidis. For GKHya excess emission was observed in the Balmer lines and Mg I b lineswhile TY Pyx showed excess emission in the Balmer lines and Ca iiH&K lines. The emission from GK Hya arises from a global phenomenonassociated solely with the secondary component. The lack of significantHe I D_3_ excess absorption and an analysis of the flux ratio in theBalmer lines suggest that the emission originates in prominence-likematerial seen off the limb of the star. A marginal broad excessabsorption band centered around the Balmer emission peaks may be causedby this material absorbing the stellar continuum against the disk withhigh (350km/s) line-of-sight turbulent velocities. The inference thatplage-like regions and associated star-spots are not substantial on thisstar is in agreement with the lack of spot modulation in the photometriclight curve. For TY Pyx the majority of the Hβ excess and a largerproportion of the Ca ii core emission could be attributed to a globalphenomenon on the primary. Analysis suggests that very large volumes areresponsible for the emission, however, there is no observationalevidence for the existence of discrete extended structures around TYPyx.
| 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.
| Catalog of Indidual Radial Velocities, 0h-12h, Measured by Astronomers of the Mount Wilson Observatory
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1970ApJS...19..387A&db_key=AST
| Spectral Classification of the Late Component of Stars with Composite Spectra
Not Available
| Radial Velocities of 360 Stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1952ApJ...115..157W&db_key=AST
| A survey of stars with composite spectra.
Not Available
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Pozíciós és asztrometriai adatok
| Csillagkép: | Egyszarvú |
| Rektaszcenzió: | 07h13m44.56s |
| Deklináció: | -05°09'19.9" |
| Vizuális fényesség: | 7.281 |
| Távolság: | 10000000 parszek |
| RA sajátmozgás: | -1.6 |
| Dec sajátmozgás: | -0.1 |
| B-T magnitude: | 8.336 |
| V-T magnitude: | 7.369 |
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