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Pulkovo compilation of radial velocities for 35495 stars in a common system.
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| 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.
| Radial velocity measurements. IV - Ground-based accompaniment to the HIPPARCOS observation program
The paper presents 396 radial velocities of stars distributed in 19fields of 4 x 4 degrees. The study employs the Fehrenbach objectiveprism method and the same measuring technique used in a previous paper(Fehrenbach et al., 1987).
| Is the Be star HR 9070 actually pulsating?
New photometric observations on the short-period Be variable HR 9070 arepresented which show that the light maxima can be predicted by a givenephemeris. Analysis using a 0.3-day period or a double-wave 0.6-dayperiod curve results in the same rms error, hence equal probabilities.Spectrography suggests large RV discontinuities in the components ofH-alpha, superimposed on smooth variations possibly correlated with theshortest period. Depending on the actual solution, pulsation or rotationmay be invoked. The shortest periodic Be stars show periods longer thanthe classical Beta CMa pulsating variables, so unusual pulsation modesshould be considered. If rotation of a star with spots on its surfaceaccounts for the variations, an exclusion mechanism between Beta CMa andBe phenomena must exist, probably as a function of rotation.
| Errata in Magnitudes of Stars in AGK3
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| Takýmyýldýz: | Zincirli Prenses |
| Sað Açýklýk: | 00h09m27.58s |
| Yükselim: | +46°23'16.4" |
| Görünürdeki Parlaklýk: | 7.16 |
| Uzaklýk: | 201.613 parsek |
| özdevim Sað Açýklýk: | 9.7 |
| özdevim Yükselim: | -12.2 |
| B-T magnitude: | 7.2 |
| V-T magnitude: | 7.164 |
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