CORRELATION BETWEEN CONCENTRATION PARAMETER AND BLACK HOLE SUBSYSTEMS IN GLOBULAR CLUSTERS
DOI:
https://doi.org/10.5281/zenodo.17462193Abstract
The dynamical evolution of globular clusters (GCs) is closely tied to the presence of black holes (BHs) in their centers. The concentration parameter, which measures the degree of stellar density toward the core, serves as a key diagnostic of a GC’s dynamical state. Understanding the correlation between this parameter and the physical characteristics of black hole subsystems (BHSs) is essential for tracing the evolutionary pathways of GCs. Observations and simulations over the past decades have demonstrated that both stellar-mass and intermediate-mass black holes (IMBHs) may significantly influence cluster dynamics (Gebhardt et al. 2005; Noyola et al. 2008; Arca Sedda et al. 2018). The discovery of BH candidates in Milky Way and extragalactic clusters (e.g., Maccarone et al. 2007; Strader et al. 2012) has challenged earlier assumptions that stellar-mass BHs cannot be retained within GCs due to dynamical ejection
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