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

Shibata, Masaru; Shapiro, Stuart L.

doi:10.1086/341516

Cited by 193 publications

(197 citation statements)

References 25 publications

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“…However, a post-Newtonian calculation cannot follow the collapse into the strong-field regime and cannot rigorously address the outcome of the collapse. 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). They found that the final object is a Kerr-like black hole (spin parameter ≈0.75) containing 90% of the stellar mass.…”

Section: Gas-dynamical Processesmentioning

confidence: 99%

Formation of supermassive black holes

Volonteri

2010

Astron Astrophys Rev

781

707

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Evidence shows that massive black holes reside in most local galaxies. Studies have also established a number of relations between the MBH mass and properties of the host galaxy such as bulge mass and velocity dispersion. These results suggest that central MBHs, while much less massive than the host (∼ 0.1%), are linked to the evolution of galactic structure. In hierarchical cosmologies, a single big galaxy today can be traced back to the stage when it was split up in hundreds of smaller components. Did MBH seeds form with the same efficiency in small proto-galaxies, or did their formation had to await the buildup of substantial galaxies with deeper potential wells? I briefly review here some of the physical processes that are conducive to the evolution of the massive black hole population. I will discuss black hole formation processes for 'seed' black holes that are likely to place at early cosmic epochs, and possible observational tests of these scenarios.

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Section: Gas-dynamical Processesmentioning

confidence: 99%

Formation of supermassive black holes

Volonteri

2010

Astron Astrophys Rev

781

707

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“…The particular direct collapse scenario we address here requires the presence of large accretion rates of about ≥ 0.01 − 0.1 M ⊙ /yr (Begelman 2010;Hosokawa et al 2013;Schleicher et al 2013;Ferrara et al 2014). This is because such accretion rates are the main pre-requisite to rapidly build a supermassive star of about 10 4 − 10 5 M ⊙ , which would eventually collapse into a black hole retaining most of the star's mass (Baumgarte & Shapiro 1999;Shibata & Shapiro 2002). These large accretion rates can either be obtained through dynamical processes or thermodynamically, by keeping the gas warm (i.e, with a higher Jeans mass) to avoid fragmentation and star formation.…”

Section: Introductionmentioning

confidence: 99%

Assessing inflow rates in atomic cooling haloes: implications for direct collapse black holes

Latif

Volonteri

2015

Mon. Not. R. Astron. Soc.

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Supermassive black holes are not only common in the present-day galaxies, but billion solar masses black holes also powered z ≥ 6 quasars. One efficient way to form such black holes is the collapse of a massive primordial gas cloud into a so-called direct collapse black hole. The main requirement for this scenario is the presence of large accretion rates of ≥ 0.1 M ⊙ /yr to form a supermassive star. It is not yet clear how and under what conditions such accretion rates can be obtained. The prime aim of this work is to determine the mass accretion rates under non-isothermal collapse conditions. We perform high resolution cosmological simulations for three primordial halos of a few times 10 7 M ⊙ illuminated by an external UV flux, J 21 = 100 − 1000. We find that a rotationally supported structure of about parsec size is assembled, with an aspect ratio between 0.25−1 depending upon the thermodynamical properties. Rotational support, however, does not halt collapse, and mass inflow rates of ∼ 0.1 M ⊙ /yr can be obtained in the presence of even a moderate UV background flux of strength J 21 ≥ 100. To assess whether such large accretion rates can be maintained over longer time scales, we employed sink particles, confirming the persistence of accretion rates of ∼ 0.1 M ⊙ /yr. We propose that complete isothermal collapse and molecular hydrogen suppression may not always be necessary to form supermassive stars, precursors of black hole seeds. Sufficiently high inflow rates can be obtained for UV flux J 21 = 500 − 1000, at least for some cases. This value brings the estimate of the abundance of direct collapse black hole seeds closer to that high redshift quasars.

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“…There are, however, situations in which accretion disks with masses comparable to that of the central black hole can be formed. Examples include the collapse of rapidly rotating stars or supermassive stars [25], and neutron star merger (especially when the two neutron stars have unequal masses [2]). In these cases, the spacetime is dynamical and Einstein's equations for the metric must be evolved along with the MHD equations.…”

Section: Introductionmentioning

confidence: 99%

Relativistic magnetohydrodynamics in dynamical spacetimes: Numerical methods and tests

et al. 2005

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Many problems at the forefront of theoretical astrophysics require the treatment of magnetized fluids in dynamical, strongly curved spacetimes. Such problems include the origin of gamma-ray bursts, magnetic braking of differential rotation in nascent neutron stars arising from stellar core collapse or binary neutron star merger, the formation of jets and magnetized disks around newborn black holes, etc. To model these phenomena, all of which involve both general relativity (GR) and magnetohydrodynamics (MHD), we have developed a GRMHD code capable of evolving MHD fluids in dynamical spacetimes. Our code solves the Einstein-Maxwell-MHD system of coupled equations in axisymmetry and in full 3+1 dimensions. We evolve the metric by integrating the BSSN equations, and use a conservative, shock-capturing scheme to evolve the MHD equations. Our code gives accurate results in standard MHD code-test problems, including magnetized shocks and magnetized Bondi flow. To test our code's ability to evolve the MHD equations in a dynamical spacetime, we study the perturbations of a homogeneous, magnetized fluid excited by a gravitational plane wave, and we find good agreement between the analytic and numerical solutions.

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

Cited by 193 publications

References 25 publications

Formation of supermassive black holes

Formation of supermassive black holes

Assessing inflow rates in atomic cooling haloes: implications for direct collapse black holes

Relativistic magnetohydrodynamics in dynamical spacetimes: Numerical methods and tests

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