Key points are not available for this paper at this time.
Since many or most galaxies have central massive black holes (BHs), mergers of galaxies can form massive binary black holes (BBHs). In this paper we study the evolution of massive BBHs in realistic galaxy models, using a generalization of techniques used to study tidal disruption rates around massive BHs. The evolution of BBHs depends on BH mass ratio and host galaxy type. BBHs with very low mass ratios (say, they are most likely to have merged in low-dispersion galaxies (line-of-sight velocity dispersion &90 km s 21 ) or in highly flattened or triaxial galaxies.
Qingjuan Yu (Thu,) studied this question.
Synapse has enriched 5 closely related papers on similar clinical questions. Consider them for comparative context: