Évolution d'un amas stellaire pendant la phase de vent stellaire des étoiles massives
Departamento de Inverstigacion Básica, CIEMAT, Madrid
We study the evolution of the elemental abundances of He, C, N y O of a stellar cluster during the first 20 Myr by taking into account the contribution of the WR's stars. In order to do that, we calculate the ejected mass and the proportion of the different chemical elements in the stellar cluster with solar initial abundance Z=Zsun and an initial mass function (IMF) from Salpeter(1955). This ejected mass is computed from the mass lost by the massive stars (M>30 Msun) during their winds phase, mainly for WR stars. To this, we add the ejections of elements due to massive stars dying as SN type II. Finally we may compare the effects of both contributions on the final abundances and analyze the impact of the WR over the evolution of the cluster.
|Friday, 4 March 2011
|Pavillon Alexandre-Vachon, local 1661