The evolution of a supermassive retrograde binary embedded in an accretion disk
Abstract
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/(dot M), where M_p is the mass of the less massive component (the perturber), and dot M 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)M. 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.
Cite
@article{arxiv.1604.00946,
title = {The evolution of a supermassive retrograde binary embedded in an accretion disk},
author = {P. B. Ivanov and J. C. B. Papaloizou and S. -J. Paardekooper and A. G. Polnarev},
journal= {arXiv preprint arXiv:1604.00946},
year = {2018}
}
Comments
arXiv admin note: substantial text overlap with arXiv:1410.3250