Authors: Bence Kocsis, Abraham Loeb (Harvard)
Date: 3 Mar 2008
Abstract: Mergers of supermassive black hole binaries release peak power of up to ~10ˆ57 erg/s in gravitational waves (GWs). As the GWs propagate through ambient gas, they induce shear and a small fraction of their power is dissipated through viscosity. The dissipated heat appears as electromagnetic (EM) radiation, providing a prompt EM counterpart to the GW signal. For thin accretion disks, the GW heating rate exceeds the accretion power at distances farther than 10ˆ3 Schwarzschild radii, independently of the accretion rate and viscosity coefficient.
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