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dc.contributor.author | Reisswig, C. | |
dc.contributor.author | Ott, C. D. | |
dc.contributor.author | Abdikamalov, Ernazar | |
dc.contributor.author | Haas, R. | |
dc.contributor.author | Mosta, P. | |
dc.contributor.author | Schnetter, E. | |
dc.date.accessioned | 2015-12-22T06:03:27Z | |
dc.date.available | 2015-12-22T06:03:27Z | |
dc.date.issued | 2013-09-20 | |
dc.identifier.citation | Reisswig C., Ott C. D., Abdikamalov Ernazar, Haas R., Mosta P., Schnetter E.; 2013; Formation and Coalescence of Cosmological Supermassive Black Hole Binaries in Supermassive Star Collapse; http://arxiv.org/find/all/1/all:+abdikamalov/0/1/0/all/0/1 | ru_RU |
dc.identifier.uri | http://nur.nu.edu.kz/handle/123456789/924 | |
dc.description.abstract | 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 threedimensional 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 104-106M. The remnant is rapidly spinning with dimensionless spin a = 0:9. The surrounding accretion disk contains 10% of the initial mass. | ru_RU |
dc.language.iso | en | ru_RU |
dc.subject | Research Subject Categories::NATURAL SCIENCES::Physics | ru_RU |
dc.subject | supermassive black holes | ru_RU |
dc.title | Formation and Coalescence of Cosmological Supermassive Black Hole Binaries in Supermassive Star Collapse | ru_RU |
dc.type | Article | ru_RU |