Astronomy and Astrophysics – Astrophysics
Scientific paper
2004-04-20
Astrophys.J. 615 (2004) 19
Astronomy and Astrophysics
Astrophysics
Accepted for publication in ApJ. 11 pages, 7 figures
Scientific paper
10.1086/424475
We investigate the expected gravitational wave emission from coalescing supermassive black hole (SMBH) binaries resulting from mergers of their host galaxies. When galaxies merge, the SMBHs in the host galaxies sink to the center of the new merged galaxy and form a binary system. We employ a semi-analytic model of galaxy and quasar formation based on the hierarchical clustering scenario to estimate the amplitude of the expected stochastic gravitational wave background owing to inspiraling SMBH binaries and bursts owing to the SMBH binary coalescence events. We find that the characteristic strain amplitude of the background radiation is $h_c(f) \sim 10^{-16} (f/1 \mu {\rm Hz})^{-2/3}$ for $f \lesssim 1 \mu {\rm Hz}$ just below the detection limit from measurements of the pulsar timing provided that SMBHs coalesce simultaneously when host galaxies merge. The main contribution to the total strain amplitude of the background radiation comes from SMBH coalescence events at $0
Enoki Motohiro
Inoue Kaiki T.
Nagashima Masahiro
Sugiyama Naoshi
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