2006/11/03 by Carlos F. Sopuerta, Nicolás Yunes, Nicolas Yunes +1 · 59 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Binary black hole #Black hole (networking) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Gravitational wave #Intermediate-mass black hole #Pulsars and Gravitational Waves Research #Recoil #Stellar black hole #Supermassive black hole #astro-ph #gr-qc
paper · pdf · doi:10.1086/512067
published in The Astrophysical Journal 656(1), L9-L12 (IOP Publishing) · 6 pages, 3 figures
arxiv created 2006/11/03 · openalex publication_date 2007/01/12 · arxiv updated 2011/02/11 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The formation and growth of supermassive black holes is a key issue to unveil the secrets of galaxy formation. In particular, the gravitational recoil produced in the merger of unequal mass black hole binaries could have a number of astrophysical implications, such as the ejection of black holes from the host galaxy or globular cluster. We present estimates of the recoil velocity that include the effect of small eccentricities. The approach is especially suited for the last stage of the merger, where most of the emission of linear momentum in gravitational waves takes place. Supplementing our estimates with post-Newtonian approximations, we obtain lower and upper bounds that constrain previous recoil velocities estimates, as well as a best estimate that agrees with numerical simulations in the quasi-circular case. For eccentricities e ≤ 0.1, the maximum recoil is found for a mass ratio of M 1 / M 2 ~ 0.38 with velocities in the range 79-216 km s -1 (1 + e ) and a best estimate of 167 km s -1 (1 + e ).