Collapse of a Rotating Supermassive Star to a Supermassive Black Hole: Fully Relativistic Simulations | Zendy

Masaru Shibata | Zendy; Stuart L. Shapiro | Zendy

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Collapse of a Rotating Supermassive Star to a Supermassive Black Hole: Fully Relativistic Simulations

Author(s) -

Masaru Shibata,

Stuart L. Shapiro

Publication year - 2002

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/341516

Subject(s) - physics , supermassive black hole , astrophysics , intermediate mass black hole , spin flip , stellar black hole , black hole (networking) , rotating black hole , binary black hole , general relativity , classical mechanics , gravitational wave , accretion (finance) , galaxy , routing protocol , routing (electronic design automation) , computer science , link state routing protocol , computer network

We follow the collapse in axisymmetry of a uniformly rotating, supermassivestar (SMS) to a supermassive black hole (SMBH) in full general relativity. Theinitial SMS of arbitrary mass $M$ is marginally unstable to radial collapse androtates at the mass-shedding limit. The collapse proceeds homologously early onand results in the appearance of an apparent horizon at the center. Althoughour integration terminates before final equilibrium is achieved, we determinethat the final black hole will contain about 90% of the total mass of thesystem and have a spin parameter $J/M^2 \sim 0.75$. The remaining gas forms arotating disk about the nascent hole.Comment: 12 pages, to appear in ApJ

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