Figure 5
From: A new hybrid technique for modeling dense star clusters
Dynamical Friction on a Single Particle (RAPID)—Similar to Fig. 4, but with the numerical results from RAPID. Here the agreement between theory and numerical experiment is somewhat diminished, particularly for the \(m_{\mathrm{{BH}}}/m_{\mathrm{{star}}} = 10\) case, where the different in inspiral times can be as high as 30%; however, the agreement improves considerably for more massive BHs