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Paper: Simulations of Electromagnetic Signals from Black Hole Mergers
Volume: 453, Advances in Computational Astrophysics: Methods, Tools, and Outcome
Page: 195
Authors: Lodato, G.
Abstract: The coalescence of supermassive black hole binaries is one of the primary sources of gravitational wave emission, that can be detected by forthcoming interferometers, such as LISA. However, a proper spatial localization and physical characterization of the GW source requires additional informations, that might come in the electromagnetic domain. Such ‘electromagnetic counterparts’ result from hydrodynamical processes occuring in the gas surrounding the merging black hole binary and include: a luminous flare from the accretion of remnant gas within the binary orbit during the merger proper; a prompt afterglow from the shock induced in the circumbinary disc due to the black hole kick and mass loss; a late afterglow resulting from the viscous refilling of the inner disc. Here, I briefly discuss the various aspects of this problem, which have often been modeled with high-resolution numerical simulations.
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