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On the Evolution of Close Triple Stars That Produce Type IA Supernovae
Current observational estimates suggest that ~30% of all binary starsare in triple systems. In ~70% of these, the enclosed binary is closeenough that the primary in the binary can evolve to fill its Roche lobe.In ~10%-20%, the third, more distant component can evolve to fill itsRoche lobe, leading to configurations inaccessible to isolated binarystars. Triple stars are unstable if the ratio of the orbital period ofthe enclosed binary to the period of the third component exceeds acritical value. Hence, an increase in the orbital period of the binarydue to conservative mass transfer between components or to wind massloss from the binary can destabilize an initially stable triple system,causing it to decompose into a rapidly moving single star and an evolvedbinary recoiling in the opposite direction with a velocity largecompared with velocities typical of primordial binaries. To highlightthe different possibilities inherent in triple-star evolution, wediscuss qualitatively several possible scenarios whereby triple starswith component masses in the range 1-10 M_solar can evolve into Type Iasupernovae, which we assume to be explosions of merging carbon-oxygen oroxygen-neon white dwarfs of total mass larger than 1.4 M_solar. Beforequantitative predictions of the likelihood of these scenarios can bemade, it is necessary to determine the initial distribution of youngtriple stars over their masses and orbital separations and to calculatethe reaction of the enclosed binary to matter transferred to it by thethird component when it fills its Roche lobe or supports a strong wind.
| 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
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Pozíciós és asztrometriai adatok
| Csillagkép: | Eridánusz |
| Rektaszcenzió: | 03h15m31.76s |
| Deklináció: | -08°46'12.3" |
| Vizuális fényesség: | 6.617 |
| Távolság: | 196.85 parszek |
| RA sajátmozgás: | 9.9 |
| Dec sajátmozgás: | -12 |
| B-T magnitude: | 8.112 |
| V-T magnitude: | 6.741 |
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