The evolution of very massive stars

Abstract

Core collapse of dense massive star clusters is unavoidable and this leads to the formation of massive objects, with a mass up to 1000 $\msun$ and even larger. When these objects become stars, stellar wind mass loss determines their evolution and final fate, and decides upon whether they form black holes (with normal mass or with intermediate mass) or explode as a pair instability supernova. In the present paper, we discuss the evolution of very massive stars and we present a convenient evolution recipe that can be implemented in a gravitational N-body code to study the dynamics of dense massive clusters.

16 pages, 4 figures, 2 tables. Accepted by ApJ

References in corpus (2)

• On the role of continuum-driven eruptions in the evolution of very massive stars and Population III stars
• The ecology of star clusters and intermediate mass black holes in the Galactic bulge

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