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Simulations, Data Analysis and Algorithms

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Figure 8 | Computational Astrophysics and Cosmology

Figure 8

From: A new hybrid technique for modeling dense star clusters

Figure 8

BH Lagrange Radii and Binary BH Formation—The number of binary BHs and the Lagrange radii for all BHs during the early stages of cluster collapse for two example clusters. On the top, we show the number of BH binaries as a function of time in both RAPID and CMC. On the bottom, we show the radii enclosing 10% 50% and 90% of the BHs in the cluster for the two techniques. In both cases, as the cluster collapses, RAPID forms a binary through three-body encounters much earlier, halting the continued collapse of the cluster. CMC continues to collapse until its first binaries are formed several hundred dynamical times later

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