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Understanding the fate of merging supermassive black holes

Manuela Campanelli

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Understanding the fate of merging supermassive black holes in galactic mergers, and the gravitational wave emission from this process, are important LISA science goals. To this end, we present results from numerical relativity simulations of binary black hole mergers using the so-called Lazarus approach to model gravitational radiation from these events. In particular, we focus here on some recent calculations of the final spin and recoil velocity of the remnant hole formed at the end of a binary black hole merger process, which may constrain the growth history of massive black holes at the core of galaxies and globular clusters.


PACS

04.70.Bw Classical black holes

04.30.Db Wave generation and sources

04.25.Nx Post-Newtonian approximation; perturbation theory; related approximations

97.80.Af Astrometric and interferometric binaries

04.25.D- Numerical relativity

98.62.Js Galactic nuclei (including black holes), circumnuclear matter, and bulges

MSC

83C35 Gravitational waves

83C57 Black holes

85A05 Galactic and stellar dynamics

83C25 Approximation procedures, weak fields

Subjects

Gravitation and cosmology

Astrophysics and astroparticles

Dates

Issue 10 (21 May 2005)

Received 14 November 2004, in final form 14 December 2004

Published 28 April 2005



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