Abstract
We investigate the formation of rapidly rotating dynamic black hole through gravitational collapse of rotating relativistic stars by means of 3+1 hydrodynamic simulations in general relativity. We succeed in producing a dynamic black hole of a = 0.98M through the collapse of differentially rotating supermassive stars, and find the following three issues. Firstly, the estimated ratio of the mass between the black hole and the surrounding disk from the equilibrium star is roughly the same as the results from numerical simulation. This suggests that the picture of axisymmetric collapse is adequate, in the absence of nonaxisymmetric instabilities, to illustrate the final state of the collapse. Secondly, quasi-periodic gravitational waves continue to be emitted after the quasinormal mode frequency has decayed. Finally, when the newly formed black hole is almost extreme Kerr, the amplitude of the quasi-periodic oscillation is enhanced during the late stages of the evolution. Geometrical features, shock waves, and instabilities of the fluid are suggested as a cause of this amplification behaviour. This alternative scenario for the collapse of differentially rotating supermassive stars might be observable by LISA.
| Original language | English |
|---|---|
| Title of host publication | Proceedings of the 19th Workshop on General Relativity and Gravitation in Japan, JGRG 2009 |
| Pages | 299-302 |
| Number of pages | 4 |
| Publication status | Published - 2009 |
| Externally published | Yes |
| Event | 19th Workshop on General Relativity and Gravitation in Japan, JGRG 2009 - Tokyo Duration: 2009 Nov 30 → 2009 Dec 4 |
Other
| Other | 19th Workshop on General Relativity and Gravitation in Japan, JGRG 2009 |
|---|---|
| City | Tokyo |
| Period | 09/11/30 → 09/12/4 |
Fingerprint
ASJC Scopus subject areas
- Atomic and Molecular Physics, and Optics
Cite this
Formation of rapidly rotating dynamic black holes. / Saijo, Motoyuki.
Proceedings of the 19th Workshop on General Relativity and Gravitation in Japan, JGRG 2009. 2009. p. 299-302.Research output: Chapter in Book/Report/Conference proceeding › Conference contribution
}
TY - GEN
T1 - Formation of rapidly rotating dynamic black holes
AU - Saijo, Motoyuki
PY - 2009
Y1 - 2009
N2 - We investigate the formation of rapidly rotating dynamic black hole through gravitational collapse of rotating relativistic stars by means of 3+1 hydrodynamic simulations in general relativity. We succeed in producing a dynamic black hole of a = 0.98M through the collapse of differentially rotating supermassive stars, and find the following three issues. Firstly, the estimated ratio of the mass between the black hole and the surrounding disk from the equilibrium star is roughly the same as the results from numerical simulation. This suggests that the picture of axisymmetric collapse is adequate, in the absence of nonaxisymmetric instabilities, to illustrate the final state of the collapse. Secondly, quasi-periodic gravitational waves continue to be emitted after the quasinormal mode frequency has decayed. Finally, when the newly formed black hole is almost extreme Kerr, the amplitude of the quasi-periodic oscillation is enhanced during the late stages of the evolution. Geometrical features, shock waves, and instabilities of the fluid are suggested as a cause of this amplification behaviour. This alternative scenario for the collapse of differentially rotating supermassive stars might be observable by LISA.
AB - We investigate the formation of rapidly rotating dynamic black hole through gravitational collapse of rotating relativistic stars by means of 3+1 hydrodynamic simulations in general relativity. We succeed in producing a dynamic black hole of a = 0.98M through the collapse of differentially rotating supermassive stars, and find the following three issues. Firstly, the estimated ratio of the mass between the black hole and the surrounding disk from the equilibrium star is roughly the same as the results from numerical simulation. This suggests that the picture of axisymmetric collapse is adequate, in the absence of nonaxisymmetric instabilities, to illustrate the final state of the collapse. Secondly, quasi-periodic gravitational waves continue to be emitted after the quasinormal mode frequency has decayed. Finally, when the newly formed black hole is almost extreme Kerr, the amplitude of the quasi-periodic oscillation is enhanced during the late stages of the evolution. Geometrical features, shock waves, and instabilities of the fluid are suggested as a cause of this amplification behaviour. This alternative scenario for the collapse of differentially rotating supermassive stars might be observable by LISA.
UR - http://www.scopus.com/inward/record.url?scp=84887463129&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84887463129&partnerID=8YFLogxK
M3 - Conference contribution
AN - SCOPUS:84887463129
SP - 299
EP - 302
BT - Proceedings of the 19th Workshop on General Relativity and Gravitation in Japan, JGRG 2009
ER -