title: 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 is approximately equal or > to 10 with the DECIGO or Big Bang Observer gravitational-wave observatories, assuming supermassive stars in the mass range 10(4)-10(6)M[symbol: see text]. The remnant is rapidly spinning with dimensionless spin a*=0.9. The surrounding accretion disk contains ~10% of the initial mass.
authors.affiliation: TAPIR, MC 350-17, California Institute of Technology, 1200 East California Boulevard, Pasadena, California 91125, USA.
authors.forename: C
authors.initials: C
authors.lastname: Reisswig
authors.forename: C D
authors.initials: CD
authors.lastname: Ott
authors.forename: E
authors.initials: E
authors.lastname: Abdikamalov
authors.forename: R
authors.initials: R
authors.lastname: Haas
authors.forename: P
authors.initials: P
authors.lastname: Mösta
authors.forename: E
authors.initials: E
authors.lastname: Schnetter