Formation and Coalescence of Cosmological Supermassive Black Hole Binaries in Supermassive Star CollapseReport as inadecuate



 Formation and Coalescence of Cosmological Supermassive Black Hole Binaries in Supermassive Star Collapse


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We study the collapse of rapidly rotating supermassive stars that may have formed in the early Universe. By self-consistently simulating the dynamics from the onset of collapse using three-dimensional general-relativistic hydrodynamics with fully dynamical spacetime evolution, we show that seed perturbations in the progenitor can lead to the formation of a system of two high-spin supermassive black holes, which inspiral and merge under the emission of powerful gravitational radiation that could be observed at redshifts z>10 with the DECIGO or Big Bang Observer gravitational-wave observatories, assuming supermassive stars in the mass range 10^4-10^6 Msol. The remnant is rapidly spinning with dimensionless spin a^*=0.9. The surrounding accretion disk contains ~10% of the initial mass.



Author: C. Reisswig; C. D. Ott; E. Abdikamalov; R. Haas; P. Moesta; E. Schnetter

Source: https://archive.org/







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