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Annual Review of Astronomy and Astrophysics

Volume 57, 2019

Star Clusters Across Cosmic Time

Abstract

Star clusters stand at the intersection of much of modern astrophysics: the ISM, gravitational dynamics, stellar evolution, and cosmology. Here, we review observations and theoretical models for the formation, evolution, and eventual disruption of star clusters. Current literature suggests a picture of this life cycle including the following several phases:

  • ▪  Clusters form in hierarchically structured, accreting molecular clouds that convert gas into stars at a low rate per dynamical time until feedback disperses the gas.
  • ▪  The densest parts of the hierarchy resist gas removal long enough to reach high star-formation efficiency, becoming dynamically relaxed and well mixed. These remain bound after gas removal.
  • ▪  In the first ∼100 Myr after gas removal, clusters disperse moderately fast, through a combination of mass loss and tidal shocks by dense molecular structures in the star-forming environment.
  • ▪  After ∼100 Myr, clusters lose mass via two-body relaxation and shocks by giant molecular clouds, processes that preferentially affect low-mass clusters and cause a turnover in the cluster mass function to appear on ∼1–10-Gyr timescales.
  • ▪  Even after dispersal, some clusters remain coherent and thus detectable in chemical or action space for multiple galactic orbits.
In the next decade, a new generation of space– and adaptive optics–assisted ground-based telescopes will enable us to test and refine this picture.

Keyword(s): globular clusters, open clusters and associations, star clusters, star formation, stellar abundances
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2019-08-18
2024-04-20
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Annual Review of Astronomy and Astrophysics 57, 227 (2019); https://doi.org/10.1146/annurev-astro-091918-104430
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