Evolution of Galactic Field be Stars

Details Evolution of Galactic Field be Stars Evolution of Galactic Field be Stars

2005-09-07

arxiv.org/abs/astro-ph/0509169v1

Astronomy and Astrophysics

Astrophysics

Societe Francaise d'Astronomie et d'Astrophysique, France (2005)

Scientific paper

Galactic field Be stars were studied by taking into account the effects induced by the fast rotation on their fundamental parameters. Fractional ages $\tau/\tau\_{\rm MS}$ ($\tau\_{\rm MS}$ = time spent in the MS) against stellar mass reveal that: a) Be stars spread over the whole interval $0<\tau/\tau\_{\rm MS}<1$; b) the Be phenomenon in massive stars ($M>12M\_{\odot}$) is present at smaller age ratios than for less massive stars ($M<12M\_{\odot}$); c) there is a lack of Be stars with $M<7M\_{\odot}$ in the first half of the MS. Low mass fast rotators ($M<7M\_{\odot}$), called Bn stars, could be "becoming" Be stars.

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