Collapse of differentially rotating relativistic stars: Post black hole formation stage

Motoyuki Saijo, Ian Hawke

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Abstract

We investigate the collapse of differentially rotating supermassive stars (SMSs) by means of 3+1 hydrodynamic simulations in general relativity. We particularly focus on the onset of collapse to understand the final outcome of collapsing SMSs. We find that the estimated ratio between the black hole (BH) and the surrounding disk from the equilibrium star is roughly the same as the results from numerical simulation. This statement suggests that the picture of axisymmetric collapse is adequate in the absence of nonaxisymmetric instabilities for illustrating the final state of the collapse. We also find that when the newly formed BH is almost an extreme Kerr, a corotation resonance can be triggered by the oscillation of a BH. In this case, nonaxisymmetric instabilities are triggered by corotation resonance and make a significant difference in the gravitational waveforms. This alternative scenario for the collapse of differentially rotating SMSs might be observable by LISA.

Original languageEnglish
Title of host publicationProceedings of the 17th Workshop on General Relativity and Gravitation in Japan, JGRG 2007
Pages228-232
Number of pages5
Publication statusPublished - 2007
Externally publishedYes
Event17th Workshop on General Relativity and Gravitation in Japan, JGRG 2007 - Nagoya
Duration: 2007 Dec 32007 Dec 7

Other

Other17th Workshop on General Relativity and Gravitation in Japan, JGRG 2007
CityNagoya
Period07/12/307/12/7

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ASJC Scopus subject areas

  • Atomic and Molecular Physics, and Optics

Cite this

Saijo, M., & Hawke, I. (2007). Collapse of differentially rotating relativistic stars: Post black hole formation stage. In Proceedings of the 17th Workshop on General Relativity and Gravitation in Japan, JGRG 2007 (pp. 228-232)