Figure 4 from Modeling Dense Star Clusters in the Milky Way and beyond with the Cluster Monte Carlo Code

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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 4.

The total energy of the two Plummer sphere models (including the energy of ejected particles) over time. The sharp downturn at the end arises from the reduction of the time step near core collapse to better resolve the dense central regions of the cluster.

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