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

Open Astronomy

卷:24

Ivanov P. B.¹  Polnarev A. G.²  Paardekooper S.-J.²  Papaloizou J. C. B.³ 

[1] Astro Space Centre, P. N. Lebedev Physical Institute, 84/32 Profsoyuznaya st., Moscow 117997, Russian Federation;

[2] Astronomy Unit, Queen Mary University of London, Mile end Road, London E14NS, United Kingdom of Great Britain and Northern Ireland;

[3] DAMTP, University of Cambridge, Wilberforce Road, Cambridge CB3 0WA, United Kingdom of Great Britain and Northern Ireland;

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

DOI  :  10.1515/astro-2017-0216

来源: DOAJ

【 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 tev ~ Mp/Ṁ, where Mp 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, q1/3Ṁ. 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