Electromagnetic Emission from the Last Hours of Merging Supermassive Black Holes

Details Electromagnetic Emission from the Last Hours of Merging Supermassive Black Holes Electromagnetic Emission from the Last Hours of Merging Supermassive Black Holes

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21743215b&link_type=abstract

American Astronomical Society, AAS Meeting #217, #432.15; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Synergistic electromagnetic (EM) and gravitational wave (GW) observations from the coalescence of supermassive black holes (SBHs), considered to be the next observational frontier, will shed light on galaxy assembly and SBH growth. Computational modeling of the dynamics and accretion processes in this last evolutionary stage of SBH binaries is central to understanding the conditions under which EM emission accompanies GWs. On scales smaller than 0.01 pc for a 107 Msun binary, gravitational wave emission determines the orbital dynamics of SBH binaries and therefore EM emissions can only be studied within the context of fully relativistic simulations. We present results from fully general relativistic hydrodynamics simulations of the late inspiral and merger of SBH binaries within astrophysically relevant gaseous environments including circumbinary disks and hot, radiatively inefficient accretion flows. We find that the observability and characteristics of EM signatures are intricately connected to the physical properties of the binary and its environment. For instance, a sudden drop in EM luminosity will not only signal the merger of the SBHs but also the presence of hot, radiatively inefficient accretion flows, whereas dramatic changes in spectral emission lines close to the coalescence may signal the presence of a circumbinary disk.

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