The Evolution of a Supermassive Retrograde Binary Embedded in an Accretion Disk

Baltic astronomy

article

P. B. Ivanov¹  J. C. B. Papaloizou²  S.-J. Paardekooper³  A. G. Polnarev³ 

[1] Astro Space Centre, P. N. Lebedev Physical Institute;University of Cambridge;Queen Mary University of London

关键词: accretion disks;    binaries;    hydrodynamics;    galaxies quasars supermassive black holes;    planet-disk interactions;   

DOI  :  10.1515/astro-2017-0216

来源: Institute of Theoretical Physics and Astronomy

【 摘 要 】

In this note we discuss the main results of a study of a massive binary with unequal mass ratio, q , embedded in an accretion disk, with its orbital rotation being opposed to that of the disk. When the mass ratio is sufficiently large, a gap opens in the disk, but the mechanism of gap formation is very different from the prograde case. Inward migration occurs on a timescale of t ev ~ M p / Ṁ , where M p is the mass of the less massive component (the perturber), and Ṁ is the accretion rate. When q ≪ 1, the accretion takes place mostly onto the more massive component, with the accretion rate onto the perturber being smaller than, or of order of, q 1/3 Ṁ . However, this rate increases when supermassive binary black holes are considered and gravitational wave emission is important. We estimate a typical duration of time for which the accretion onto the perturber and gravitational waves could be detected.

【 授权许可】

Unknown