Volume 441, Number 1, October I 2005
|Page(s)||235 - 248|
|Section||Stellar structure and evolution|
|Published online||13 September 2005|
On the evolutionary status of Be stars
I. Field Be stars near the Sun
Institut d'Astrophysique de Paris, UMR 7095 CNRS-Université Pierre & Marie-Curie, 98bis Bd. Arago, 75014 Paris, France e-mail: email@example.com
2 Royal Observatory of Belgium, 3 Av. Circulaire, 1180 Bruxelles, Belgium
3 Facultad de Ciencias Astronómicas y Geofísicas, Universidad de La Plata, Paseo del Bosque S/N, 1900 La Plata, Argentina
4 Instituto de Astrofísica La Plata, CONICET, 1900 La Plata, Argentina
Accepted: 26 May 2005
A sample of 97 galactic field Be stars were studied by taking into account the effects induced by the fast rotation on their fundamental parameters. All program stars were observed in the BCD spectrophotometric system in order to minimize the perturbations produced by the circumstellar environment on the spectral photospheric signatures. This is one of the first attempts at determining stellar masses and ages by simultaneously using model atmospheres and evolutionary tracks, both calculated for rotating objects. The stellar ages (τ) normalized to the respective inferred time that each rotating star can spend in the main sequence phase () reveal a mass-dependent trend. This trend shows that: a) there are Be stars spread over the whole interval of the main sequence evolutionary phase; b) the distribution of points in the () diagram indicates that in massive stars () the Be phenomenon is present at smaller age ratios than for less massive stars (). This distribution can be due to: i) higher mass-loss rates in massive objets, which can act to reduce the surface fast rotation; ii) circulation time scales to transport angular momentum from the core to the surface, which are longer the lower the stellar mass.
Key words: stars: emission-line, Be / stars: evolution / stars: rotation / stars: fundamental parameters (classification, colors, luminosities, masses, radii, temperatures, etc.)
© ESO, 2005
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