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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 8.

Masses and spin alignments of BBHs produced through dynamical encounters (from 10 GC models generated with CMC) and through isolated binary evolution (from 5 × 104 stellar binaries evolved with COSMIC). On the top, we show the total masses of the BBHs, with the maximum mass from isolated binaries (89 M) being clearly visible. On the bottom, we show the distribution of spin–orbit misalignments for the BBHs as a function of total mass. While low-mass BBHs from the isolated binary population can experience significant misalignments from supernova natal kicks, this decreases as a function of mass, while the spin–orbit misalignments for dynamically formed binaries are isotropic irrespective of mass.

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