Zams Rotational Velocities of be Stars

Simple item page
dc.creatorZorec, Juan
dc.creatorMartayan, Christophe
dc.creatorFremat, Yves
dc.creatorHubert, Anne-Marie
dc.creatorFloquet, Michele
dc.date2005-09-07
dc.date.accessioned2026-07-07T02:18:35Z
dc.date.available2026-07-07T02:18:35Z
dc.descriptionWe show that Be stars belong to a high velocity tail of a single B-type star rotational velocity distribution in the main sequence (MS). We studied 127 galactic field Be stars and obtained their true equatorial velocity at the ZAMS using models of stellar evolution with rotation. There is a sharp mass-dependent cut in the ZAMS under which there is no Be star. Velocities above this cut follow a Gaussian-tail distribution. B stars with ZAMS rotational velocities lower than the cut probably cannot become Be.
dc.descriptionSociete Francaise d'Astronomie et d'Astrophysique, France (2005)
dc.identifierhttps://arxiv.org/abs/astro-ph/0509175
dc.identifierhttp://arxiv.org/abs/astro-ph/0509175
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/9543
dc.subjectAstrophysics
dc.titleZams Rotational Velocities of be Stars
dc.typetext

Files

Collections

arXiv