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Simulations, Data Analysis and Algorithms

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Figure 9 | Computational Astrophysics and Cosmology

Figure 9

From: A new hybrid technique for modeling dense star clusters

Figure 9

Number of Single and Binary BHs—The number of BHs retained in each cluster model over time. On the top, we show the total number of BHs present in each of the four clusters (including those in bound multiple systems) for the single NBODY6 model (in black), the 10 CMC models (in blue), and the 10 RAPID models (in red). In each case, the RAPID show better agreement with the NBODY6 model than the pure CMC models. In the second and third rows, we show the total number of BH binaries and BH triples (which cannot be produced in CMC) present in the NBODY6 model (in black) and a single RAPID model (in red) as a function of time. Although highly stochastic, the number of bound multiple systems shows good qualitative agreement between the two methods. As in Fig. 6, we show the mean and 1σ times when RAPID reverts to a pure MC approach with the white-dashed line and gray bands, respectively. For the middle and bottom rows, the white line indicated the reversion time for that run

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