Formation of rapidly rotating dynamic black holes

Motoyuki Saijo*

*この研究の対応する著者

研究成果: Conference contribution

抄録

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.

本文言語English
ホスト出版物のタイトルProceedings of the 19th Workshop on General Relativity and Gravitation in Japan, JGRG 2009
ページ299-302
ページ数4
出版ステータスPublished - 2009
外部発表はい
イベント19th Workshop on General Relativity and Gravitation in Japan, JGRG 2009 - Tokyo
継続期間: 2009 11月 302009 12月 4

Other

Other19th Workshop on General Relativity and Gravitation in Japan, JGRG 2009
CityTokyo
Period09/11/3009/12/4

ASJC Scopus subject areas

  • 原子分子物理学および光学

フィンガープリント

「Formation of rapidly rotating dynamic black holes」の研究トピックを掘り下げます。これらがまとまってユニークなフィンガープリントを構成します。

引用スタイル