The Collapse of Differentially Rotating Supermassive Stars: Conformally Flat Simulations

Abstract

We investigate the gravitational collapse of rapidly rotating relativistic supermassive stars by means of a 3+1 hydrodynamical simulations in conformally flat spacetime of general relativity. We study the evolution of differentially rotating supermassive stars of $q\equiv J/M^2\sim 1$ ($J$ is the angular momentum and $M$ is the gravitational mass of the star) from the onset of radial instability at $R/M\sim 65$ ($R$ is the circumferential radius of the star) to the point where the conformally flat approximation breaks down. We find that the collapse of the star of $q\gtrsim 1$, a radially unstable differentially rotating star form a black hole of $q\lesssim 1$. The main reason to prevent formation of a black hole of $q\gtrsim 1$ is that quite a large amount of angular momentum stays at the surface. We also find that most of the mass density collapses coherently to form a supermassive black hole with no appreciable disk nor bar. In the absence of nonaxisymmetric deformation, the collapse of differentially rotating supermassive stars from the onset of radial instability are the promising sources of burst and quasinormal ringing waves in the Laser Interferometer Space Antenna.

arXiv comment15 pages, 14 figures included, uses emulateapj.cls (included). Accepted for publication in The Astrophysical Journal

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• Formation and Coalescence of Cosmological Supermassive Black Hole Binaries in Supermassive Star Collapse
• Formation of the first stars and black holes
• Features of Accretion-phase Gravitational-wave Emission from Two-dimensional Rotating Core-collapse Supernovae
• Magnetorotational Collapse of Supermassive Stars: Black Hole Formation, Gravitational Waves and Jets
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• Non-axisymmetric instability and fragmentation of general relativistic quasi-toroidal stars
• Collapse of differentially rotating supermassive stars: Post black hole formation
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• Dynamical bar instability in a relativistic rotational core collapse
• On the accuracy of the IWM-CFC approximation in differentially rotating relativistic stars
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• An estimate of the gravitational-wave background from the observed cosmological distribution of quasars
• Gravitational-wave asteroseismology with f-modes from neutron star binaries at the merger phase