Be stars and the IMF of young clusters

Details Be stars and the IMF of young clusters Be stars and the IMF of young clusters

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997agab...13..194g&link_type=abstract

Astronomische Gesellschaft Abstract Series, 13, 194

Astronomy and Astrophysics

Astronomy

1

Star Clusters, Initial Mass Function, Be Stars, Emission-Line Stars, Stellar Evolution, Statistical Methods

Scientific paper

Be stars are non-supergiant B stars with Balmer emission and infrared excess originating in circumstellar disks. The presence of Be stars in young clusters has been found to widen the main sequence (e.g., Grebel et al. 1996, Grebel 1997). On average, Be stars are intrinsically brighter than B stars of the same mass but without H alpha emission (Zorec & Briot 1991, 1997). The presence of Be stars thus changes the slope of the luminosity function of young clusters. IMF estimates based on luminosity functions consequently overestimate the number of massive stars in a cluster. In order to quantify this effect, we have carried out a variety of Monte-Carlo simulations. We present the resulting IMFs as a function of different Be star fractions, metallicities, and cluster ages based on our synthetic colour-magnitude diagrams, and compare them to IMFs of simulated clusters without Be stars.

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