Formation and coalescence of cosmological supermassive-black-hole binaries in supermassive-star collapse

C. Reisswig, C. D. Ott, E. Abdikamalov, R. Haas, P. Mösta, E. Schnetter

Research output: Contribution to journalArticle

40 Citations (Scopus)

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 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 za10 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.

Original languageEnglish
Article number151101
JournalPhysical Review Letters
Volume111
Issue number15
DOIs
Publication statusPublished - Oct 7 2013
Externally publishedYes

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supermassive stars
gravitational waves
coalescing
accretion disks
metal spinning
seeds
observatories
universe
hydrodynamics
perturbation

ASJC Scopus subject areas

  • Physics and Astronomy(all)

Cite this

Formation and coalescence of cosmological supermassive-black-hole binaries in supermassive-star collapse. / Reisswig, C.; Ott, C. D.; Abdikamalov, E.; Haas, R.; Mösta, P.; Schnetter, E.

In: Physical Review Letters, Vol. 111, No. 15, 151101, 07.10.2013.

Research output: Contribution to journalArticle

Reisswig, C. ; Ott, C. D. ; Abdikamalov, E. ; Haas, R. ; Mösta, P. ; Schnetter, E. / Formation and coalescence of cosmological supermassive-black-hole binaries in supermassive-star collapse. In: Physical Review Letters. 2013 ; Vol. 111, No. 15.
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