Black Hole Binary Mergers

Details Black Hole Binary Mergers Black Hole Binary Mergers

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005hia....13..339m&link_type=abstract

Highlights of Astronomy, Vol. 13, as presented at the XXVth General Assembly of the IAU - 2003 [Sydney, Australia, 13 - 26 July

Astronomy and Astrophysics

Astronomy

1

Scientific paper

In this talk I'll overview the current understanding of the evolution of massive black hole (MBH) binaries and triples in the center of the host stellar system based on direct N-body simulations.
When two MBHs are in the core of the host stellar system they easily form binaries since they sink to the center through dynamical friction. Since they are massive right from the beginning they are ""hard"" in the sense that the binding energy is much larger then the kinetic energy of stars in the core and therefore they continue to become more harder.
The question is whether the stellar dynamical effect can make the MBH binary hard enough that they can merge through gravitational wave radiation. So far theories and numerical simulations suggested otherwize since the hardening timescale becomes very long once ""loss cone"" is depleted. I'll present the result of recent simulations on this hardening timescale and discuss its implication on the formation history of massive black holes.

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