Black holes in globular clusters

Abstract

Dynamical evolution in star clusters naturally creates an environment in which interactions among massive stars, binaries, and compact remnants are common. Young clusters may temporarily contain a significant population of stellar black holes, and close encounters and physical collisions among stars in dense cluster cores may lead to the formation of very massive stars and high-mass black holes via runaway merging. Numerical simulations suggest runaway masses in the range commonly cited for intermediate-mass black holes. While our understanding of black hole formation and retention has improved greatly in recent years, substantial uncertainties remain in both the physics of the runaway merger process and the evolution of very massive stars. Direct and indirect observational evidence have been reported for massive black holes in globular clusters, although here too interpretations remain controversial. I examine critically some details of the processes possibly leading to massive black holes in present-day globular clusters, and discuss some observational constraints on the various theoretical scenarios. Introduction Black holes are natural products of stellar evolution in massive stars, and may also result from dynamical interactions in dense stellar systems, such as star clusters and galactic nuclei. They can significantly influence the dynamics of their parent cluster, and may also have important observational consequences, via their x-ray emission, the production of gravitational radiation, and their effect on the structural properties of the system in which they reside. Globular clusters offer particularly rich environments for the production of black holes in statistically significant numbers. Direct evidence for black holes in globulars is scarce, although several independent lines of investigation now hint at their presence.