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 language | English |
|---|---|
| Article number | 151101 |
| Journal | Physical Review Letters |
| Volume | 111 |
| Issue number | 15 |
| DOIs | |
| Publication status | Published - Oct 7 2013 |
| Externally published | Yes |
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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 journal › Article
}
TY - JOUR
T1 - Formation and coalescence of cosmological supermassive-black-hole binaries in supermassive-star collapse
AU - Reisswig, C.
AU - Ott, C. D.
AU - Abdikamalov, E.
AU - Haas, R.
AU - Mösta, P.
AU - Schnetter, E.
PY - 2013/10/7
Y1 - 2013/10/7
N2 - 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.
AB - 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.
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U2 - 10.1103/PhysRevLett.111.151101
DO - 10.1103/PhysRevLett.111.151101
M3 - Article
VL - 111
JO - Physical Review Letters
JF - Physical Review Letters
SN - 0031-9007
IS - 15
M1 - 151101
ER -