http://arxiv.org/abs/1606.07147
We derive the gravitational waveform from the collapse of a rapidly rotating supermassive star (SMS) core leading directly to a seed of a supermassive black hole (SMBH) in axisymmetric numerical-relativity simulations. We find that the peak strain amplitude of gravitational waves emitted during the black-hole formation is $\approx 5 \times 10^{-21}$ at the frequency $f \approx 5$\,mHz for an event at the cosmological redshift $z=3$, if the collapsing SMS core is in the hydrogen-burning phase. Such gravitational waves will be detectable by space laser interferometric detectors like eLISA with signal-to-noise ratio $\approx 10$, if the sensitivity is as high as LISA for $f=1$–10\,mHz. The detection of the gravitational-wave signal will provide a potential opportunity for testing the direct-collapse scenario for the formation of a seed of SMBHs.
M. Shibata, Y. Sekiguchi, H. Uchida, et. al.
Fri, 24 Jun 16
19/47
Comments: 5 pages, 3 figures, PRD accepted
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