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

By M. Shibata, Stuart L. Shapiro. 2002

169 citations recorded by the source corpus.

We follow the collapse in axisymmetry of a uniformly rotating, supermassive star (SMS) to a supermassive black hole in full general relativity. The initial SMS of arbitrary mass M is marginally unstable to radial collapse and rotates at the mass-shedding limit. The collapse proceeds homologously early on and results in the appearance of an apparent horizon at the center. Although our integration terminates before final equilibrium is achieved, we determine that the final black hole will contain about 90% of the total mass of the system and will have a spin parameter J/M2 ~ 0.75. The remaining gas forms a rotating disk about the nascent hole.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/001628db9808023778046013fe6ccc185efe6a8f

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Doing Science with eLISA: Astrophysics and Cosmology in the Millihertz Regime (2012, background): “The very massive quasi-star of about 105 M , burns hydrogen and helium in its core and once formed, the star collapses into a black hole when metallicity is below some threshold, as the alternative is its entire explosion (Montero et al., 2011, Shibata and Shapiro, 2002).”
Spin, Accretion, and the Cosmological Growth of Supermassive Black Holes (2004, background): “…for a black hole formed from the catastrophic collapse of a massive, radiation-dominated star spinning uniformly at the mass-shedding limit that has evolved to the onset of relativistic radial instability just prior to collapse (Shibata & Shapiro 2002; Shapiro & Shibata 2002; Shapiro 2004).”
Formation of supermassive black holes (2010, background): “The fate of a marginally unstable, maximally rotating SMS of arbitrary mass has been investigated numerically in full general relativity by Shibata and Shapiro (2002).”
Formation of Supermassive Black Hole Seeds (2016, background): “They may collapse via general relativistic (GR) instabilities into a DCBH while retaining ≥ 50% of their initial mass (Baumgarte & Shapiro 1999; Shibata & Shapiro 2002; Montero et al. 2012; Reisswig et al. 2013) or may evolve towards a ZAMS and later collapse into a massive BH (Ferrara et al. 2014).”
Quasi-stars: accreting black holes inside massive envelopes (2007, background): “…Begelman & Rees (1978) — which include instabilities in clusters of stars or stellar remnants, and the collapse of supermassive stars or massive discs — are still under consideration today (Umemura, Loeb & Turner 1993; Freitag, Gürkan & Rasio 2006; Shibata & Shapiro 2002; Lodato & Natarajan 2006).”
FORMATION OF PRIMORDIAL SUPERMASSIVE STARS BY RAPID MASS ACCRETION (2013, background): “The ultimate fate of an SMS, i.e., whether a star collapses to form a BH (e.g., Shibata & Shapiro 2002; Montero et al. 2012; Reisswig et al. 2013), explodes by thermo-nuclear burning (e.g., Whalen et al. 2012; Johnson et al. 2013b; Whalen et al. 2013a,b), or evolves into a “quasi-star” (Begelman et…”
Black hole formation from axion stars (2016, background): “Such an isolated star will collapse into a massive seed Kerr BH [78].”
Total and Jet Blandford-Znajek Power in the Presence of an Accretion Disk (2005, background): “M. Gilfanov, R. Sunyaev, & E. Churazov (Berlin: Springer), 381 Blandford, R. D., & Payne, D. G. 1982, MNRAS, 199, 883 Blandford, R. D., & Znajek, R. L. 1977, MNRAS, 179, 433 Broderick, A. E. 2005, MNRAS, 361, 955 De Villiers, J.-P., Hawley, J. F., Krolik, J. H., & Hirose, S. 2005, ApJ, 620, 878 Di M”
Black Hole Spin Evolution (2003, background): “Shibata & Shapiro (2002) followed the collapse of a marginally unstable supermassive star in full general relativity.”
STELLAR-MASS BLACK HOLE SPIN CONSTRAINTS FROM DISK REFLECTION AND CONTINUUM MODELING (2009, background): “Only considering the collapse event, a spin ofa ≃ 0.75 is expected (Shibata & Shapiro 2002); with additional considerations, a spin as high asa ≤ 0.93 may be possible (Gammie et al. 2004).”