Evolution of Galactic Field be Stars
| dc.creator | Zorec, Juan | |
| dc.creator | Fremat, Yves | |
| dc.creator | Cidale, Lydia | |
| dc.date | 2005-09-07 | |
| dc.date.accessioned | 2026-07-07T02:18:35Z | |
| dc.date.available | 2026-07-07T02:18:35Z | |
| dc.description | Galactic field Be stars were studied by taking into account the effects induced by the fast rotation on their fundamental parameters. Fractional ages $τ/τ\_{\rm MS}$ ($τ\_{\rm MS}$ = time spent in the MS) against stellar mass reveal that: a) Be stars spread over the whole interval $0<τ/τ\_{\rm MS}<1$; 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. | |
| dc.description | Societe Francaise d'Astronomie et d'Astrophysique, France (2005) | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0509169 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0509169 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/9539 | |
| dc.subject | Astrophysics | |
| dc.title | Evolution of Galactic Field be Stars | |
| dc.type | text |