Ultra-Low Frequency Gravitational Radiation from Massive Black Hole Binaries
Abstract
For massive black hole binaries produced in galactic mergers, we examine the possibility of inspiral induced by interaction with field stars. We model the evolution of such binaries for a range of galaxy core and binary parameters, using numerical results from the literature to compute the binary's energy and angular momentum loss rates due to stellar encounters and including the effect of back-action on the field stars. We find that only a small fraction of binary systems can merge within a Hubble time via unassisted stellar dynamics. External perturbations may, however, cause efficient inspiral. Averaging over a population of central black holes and galaxy mergers, we compute the expected background of gravitational radiation with periods Pw ~ 1-10 yr. Comparison with sensitivities from millisecond pulsar timing suggests that the strongest sources may be detectable with modest improvements to present experiments.
Keywords
Cite
@article{arxiv.astro-ph/9412038,
title = {Ultra-Low Frequency Gravitational Radiation from Massive Black Hole Binaries},
author = {Mohan Rajagopal and Roger W. Romani},
journal= {arXiv preprint arXiv:astro-ph/9412038},
year = {2010}
}
Comments
To appear in Ap.J., June 1995; corrections to merger frequency formulae, updated figures; latex, 15 pages with 5 eps figures. POSTSCRIPT VERSION at http://geminga.stanford.edu/users/mohan/bhgw_pp.ps