Evolution of a stellar cluster during the winds phase of massive stars

Details Evolution of a stellar cluster during the winds phase of massive stars Evolution of a stellar cluster during the winds phase of massive stars

Nov 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011hsa6.conf..392m&link_type=abstract

Highlights of Spanish Astrophysics VI, Proceedings of the IX Scientific Meeting of the Spanish Astronomical Society (SEA), held

Astronomy and Astrophysics

Astrophysics

Scientific paper

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 WRs 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 = Z_&sun; and an initial mass function (IMF) from Salpeter (1955, ApJ, 121, 161). This ejected mass is computed from the mass lost by the massive stars (M > 30 M_&sun;) 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.

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