Image Details

Choose export citation format:

Modeling Dense Star Clusters in the Milky Way and beyond with the Cluster Monte Carlo Code

  • Authors: Carl L. Rodriguez, Newlin C. Weatherford, Scott C. Coughlin, Pau Amaro-Seoane, Katelyn Breivik, Sourav Chatterjee, Giacomo Fragione, Fulya Kıroğlu, Kyle Kremer, Nicholas Z. Rui, Claire S. Ye, Michael Zevin, and Frederic A. Rasio

2022 The Astrophysical Journal Supplement Series 258 22.

  • Provider: AAS Journals

Caption: Figure 3.

The density profile of the Plummer sphere with 108 particles near core collapse as a function of radius. Both quantities are calculated in terms of the initial virial radius and the initial density of objects within that radius. We show the densities from three separate snapshots, whose time is given in terms of the initial half-mass relaxation time. During the last moments of the cluster’s evolution, the inner regions rapidly converge to the ρr−2.23 power law expected from Fokker–Planck calculations (Cohn 1980), showing self-similar behavior over more than 15 orders of magnitude in density.

Other Images in This Article
Copyright and Terms & Conditions

Additional terms of reuse