2018/05/18 by Shu-Xu Yi, K. S. Cheng, Ronald E. Taam
Physics and Astronomy · #Accretion (finance) #Active galactic nucleus #Angular momentum #Astrophysical Phenomena and Observations #Binary black hole #Black hole (networking) #Gamma-ray bursts and supernovae #Gravitational wave #Intermediate-mass black hole #Pulsars and Gravitational Waves Research #Stellar mass #Supermassive black hole #astro-ph.HE
paper · pdf · doi:10.3847/2041-8213/aac649
Accepted for publication in ApJL
arxiv created 2018/05/18 · openalex created_date 2018/06/01 · openalex publication_date 2018/06/01 · arxiv updated 2018/06/13 · openalex updated_date 2026/08/06
Abstract Among the four black hole (BH) binary merger events detected by the Laser Interferometer Gravitational-Wave Observatory (LIGO), six progenitor BHs have masses greater than 20 M ⊙ . The existence of such massive BHs suggests that extreme metal-poor stars are the progenitors. An alternative possibility, that a pair of stellar mass BHs each with mass ∼7 M ⊙ increases to >20 M ⊙ via accretion from a disk surrounding a supermassive BH (SMBH) in an active galactic nucleus (AGN), is considered. The growth of mass of the binary and the transfer of orbital angular momentum to the disk accelerates the merger. Based on the recent numerical work of Tang et al., it is found that, in the disk of a low-mass AGN with mass ∼10 6 M ⊙ and Eddington ratio >0.01, the mass of an individual BH in the binary can grow to >20 M ⊙ before coalescence, provided that accretion takes place at a rate more than 10 times the Eddington value. This mechanism predicts a new class of gravitational wave (GW) sources involving the merger of two extreme Kerr black holes associated with AGNs and a possible electromagnetic wave counterpart.