Abstract
Abstract We present the results of realistic N-body modelling of massive star clusters in the Magellanic Clouds, aimed at investigating a dynamical origin for the radius–age trend observed in these systems. We find that stellar-mass black holes, formed in the supernova explosions of the most massive cluster stars, can constitute a dynamically important population. If a significant ensemble is retained (here we assume complete retention), these objects rapidly form a dense core where interactions are common, resulting in the scattering of black holes into the cluster halo, and the ejection of black holes from the cluster. These two processes heat the stellar component, resulting in prolonged core expansion of a magnitude matching the observations. Significant core evolution is also observed in Magellanic Cloud clusters at early times. We find that this does not result from the action of black holes, but can be reproduced by the effects of mass-loss due to rapid stellar evolution in a primordially mass-segregated cluster.
Highlights
Globular clusters are central to a wide variety of astrophysical research, ranging from star formation, stellar and binary star evolution, and stellar dynamics, through to galaxy formation and evolution, and cosmology
We demonstrate that a cluster which retains its black holes (BHs) undergoes dramatic core expansion for most of its lifetime, in contrast to a cluster with no BHs, which proceeds towards core collapse
Expansion is induced via heating due to a BH population
Summary
Globular clusters are central to a wide variety of astrophysical research, ranging from star formation, stellar and binary star evolution, and stellar dynamics, through to galaxy formation and evolution, and cosmology. To directly observe cluster evolution, we must switch our attention to the Magellanic Clouds (LMC/SMC), which both possess extensive systems of star clusters with masses comparable to the Galactic globulars, but crucially of all ages: 106 τ 1010 yr. These systems are of fundamental importance because they are the nearest places we can observe snapshots of all phases of cluster development. We show that primordial MSeg has an important effect on the early evolution of a cluster, when mass-loss due to stellar evolution is severe
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Schedule a callMore From: Monthly Notices of the Royal Astronomical Society: Letters
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