Pre-mainsequence stellar evolution in N-body models

Abstract

We provide a set of analytic fits to the radii of pre-mainsequence stars in the mass range 0.1 < M/Msun < 8.0. We incorporate the formulae in N-body cluster models for evolution from the beginning of pre-main sequence. In models with 1,000 stars and high initial cluster densities, pre-mainsequence evolution causes roughly twice the number of collisions between stars than in similar models with evolution begun only from the zero-age main sequence. The collisions are often all part of a runaway sequence that creates one relatively massive star.

8 pages, 4 figures, accepted by PASA

References in corpus (3)

• The Early Expansion of Cluster Cores
• Collisional formation of very massive stars in dense clusters
• The role of stellar collisions for the formation of massive stars

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