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 |