Figure 1 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 1.

Schematic diagram of the Hénon method. The cumulative velocity change due to many two-body encounters in a realistic cluster can be calculated given the average local mass, velocity, and density of stars with Equation (9). In Hénon’s method, this is reduced to a single encounter between nearest-neighbor particles, where the deflection angle is chosen to reproduce the statistical predictions using Equation (12).

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