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2018MNRAS.481..153O - Mon. Not. R. Astron. Soc., 481, 153-163 (2018/November-3)

Very massive stars in not so massive clusters.

OH S. and KROUPA P.

Abstract (from CDS):

Very young star clusters in the Milky Way exhibit a well-defined relation between their maximum stellar mass, mmax, and their mass in stars, Mecl. A recent study shows that the young intermediate-mass star cluster VVV CL041 possibly hosts a ≳80 M star, WR62-2, which appears to violate the existence of the mmax-Mecl relation since the mass of the star is almost two times higher than that expected from the relation. By performing direct N-body calculations with the same mass as the cluster VVV CL041 (≃3000 M), we study whether such a very massive star can be formed via dynamically induced stellar collisions in a binary-rich star cluster that initially follows the mmax-Mecl relation. Eight out of 100 clusters form a star more massive than 80 M through multiple stellar collisions. This suggests that the VVV CL041 cluster may have become an outlier of the relation because of its early-dynamical evolution, even if the cluster followed the relation at birth. We find that more than half of our model clusters host a merger product as its most massive member within the first 5 Myr of cluster evolution. Thus, the existence of stars more massive than the mmax-Mecl relation in some young clusters is expected due to dynamical processes despite the validity of the mmax-Mecl relation. We briefly discuss evolution of binary populations in our model.

Abstract Copyright: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): methods: numerical - stars: kinematics and dynamics - stars: massive - open clusters and associations: general - open clusters and associations: individual: VVV CL041 - galaxies: star clusters: general

Simbad objects: 10

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2020.09.19-18:41:33

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