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As self-gravitating systems, dense star clusters exhibit a natural diffusionof energy from their innermost to outermost regions, which leads to a slow andsteady contraction of the core until it ultimately collapses under gravity.However, in spite of the natural tendency toward so-called "core collapse," theglobular clusters (GCs) in the Milky Way exhibit a well-observed bimodaldistribution in core radii separating the core-collapsed and non-core-collapsedclusters. This suggests an internal energy source is at work, delaying theonset of core collapse in many clusters. Primordial binary stars have beenthought for a long time to provide this energy source, but recent analyses havecast doubt upon the corresponding "binary-burning" mechanism as a viableexplanation. Over the past decade, a large amount of both observational andtheoretical work has suggested that many stellar-mass black holes (BHs) areretained in typical clusters today and that they play a dynamically-significantrole in these clusters throughout their entire lifetimes. Here we review ourlatest understanding of the formation and evolution of BH populations in GCsand demonstrate that, through their dynamical interaction with their hostcluster, BHs can naturally explain the distinction between core-collapsed andnon-core-collapsed clusters through a process we call "black hole burning."

The Role of "Black Hole Burning" in the Evolution of Dense Star Clusters