Formation and Coalescence of Cosmological Supermassive-Black-Hole Binaries in Supermassive-Star Collapse
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 z≳10 with the DECIGO or Big Bang Observer gravitational-wave observatories, assuming supermassive stars in the mass range 10^4–10^6M⊙. The remnant is rapidly spinning with dimensionless spin a*=0.9. The surrounding accretion disk contains ∼10% of the initial mass.
Additional Information
© 2013 American Physical Society. Received 29 April 2013; published 7 October 2013. We acknowledge helpful discussions with Volker Bromm, Sterl Phinney, Michele Vallisneri, and members of our Simulating eXtreme Spacetimes (SXS) collaboration (http://www.black-holes.org). This research is partially supported by NSF Grants No. PHY-1151197, No. AST-1212170, No. PHY-1212460, and No. OCI-0905046, by the Alfred P. Sloan Foundation, and by the Sherman Fairchild Foundation. C. R. acknowledges support by NASA through Einstein Postdoctoral Fellowship Grant No. PF2-130099 given by the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under Contract No. NAS8-03060. R.H. acknowledges support by the Natural Sciences and Engineering Council of Canada. The simulations were performed on the Caltech compute cluster Zwicky (NSF MRI Grant No. PHY-0960291), on supercomputers of the NSF XSEDE network under computer time allocation TG-PHY100033, on machines of the Louisiana Optical Network Initiative under Grant No. loni_numrel08, and at the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.Attached Files
Published - PhysRevLett.111.151101.pdf
Submitted - 1304.7787v2.pdf
Supplemental Material - H_conv.pdf
Supplemental Material - README.TXT
Supplemental Material - SMSFragmentPaperSuppl.bbl
Supplemental Material - SMSFragmentPaperSuppl.pdf
Supplemental Material - SMSFragmentPaperSuppl.tex
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Additional details
- Eprint ID
- 42268
- Resolver ID
- CaltechAUTHORS:20131106-100213472
- NSF
- PHY-1151197
- NSF
- AST-1212170
- NSF
- PHY-1212460
- NSF
- OCI-0905046
- Alfred P. Sloan Foundation
- Sherman Fairchild Foundation
- NASA Einstein Postdoctoral Fellowship
- PF2-130099
- NASA
- NAS8-03060
- Natural Sciences and Engineering Council of Canada
- NSF MRI
- PHY-0960291
- NSF XSEDE
- TG-PHY100033
- Louisiana Optical Network Initiative
- loni_numrel08
- National Energy Research Scientific Computing Center (NERSC)
- Department of Energy (DOE) Office of Science
- DE-AC02-05CH11231
- Created
-
2013-11-06Created from EPrint's datestamp field
- Updated
-
2021-11-10Created from EPrint's last_modified field
- Caltech groups
- TAPIR