Gravitational waves from supermassive stars collapsing to a supermassive black hole

Shibata, Masaru; Sekiguchi, Y.; Uchida, Haruki; Umeda, Hideyuki

doi:10.1103/physrevd.94.021501

Cited by 43 publications

(54 citation statements)

References 42 publications

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“…[23]. We employ the original version of BSSN (Baumgarte-Shapiro-Shibata-Nakamura) formalism with a puncture gauge [31][32][33][34].…”

Section: A Calculation Of Gravitational Fieldmentioning

confidence: 99%

“…However, in its presence, the gravitational collapse of SMS cores could be observed. Our previous study [23] proposed that if a SMS core is rotating, gravitational waves associated with the quasi-normal mode ringdown are emitted during the black-hole formation and if it occurs at the cosmological redshift less than ≈ 3, the signal will be detectable by space laser interferometric detectors like LISA [24]. Other studies show that a collapsing SMS may be detectable as a gamma-ray burst or an ultra-luminous supernova if the formed black hole launches a relativistic jet during the collapse [25,26].…”

Section: Introductionmentioning

confidence: 98%

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Gravitational collapse of rotating supermassive stars including nuclear burning effects

et al. 2017

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Supermassive stars (SMSs) of mass 10 5 M are candidates for seeds of supermassive black holes found in the center of many massive galaxies. We simulate the gravitational collapse of a rigidly rotating SMS core including nuclear burning effects in axisymmetric numerical-relativity simulation. We find that for realistic initial conditions, the nuclear burning does not play an important role. After the collapse, a torus surrounding a rotating black hole is formed and a fraction of the torus material is ejected. We quantitatively study the relation between the properties of these objects and rotation. We find that if a SMS core is sufficiently rapidly rotating, the torus and outflow mass have approximately 6% and 1% of the initial mass, respectively. The typical average velocity and the total kinetic energy of the outflow are 0.2 c and 10 54−56 erg where c is the speed of light. Finally, we briefly discuss the possibility for observing the torus and outflow.

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“…[23]. We employ the original version of BSSN (Baumgarte-Shapiro-Shibata-Nakamura) formalism with a puncture gauge [31][32][33][34].…”

Section: A Calculation Of Gravitational Fieldmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

Gravitational collapse of rotating supermassive stars including nuclear burning effects

et al. 2017

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“…Montero et al [463] carried out simulations with detailed microphysics and hydrogen and helium burning, finding that a metallicity of 10 −3 is needed to cause thermonuclear explosion rather than black hole formation for mass-shedding supermassive stars of mass ∼ 5 × 10 5 M . Finally, Shibata and collaborators have included the deviation of Γ from 4/3 [464] and nuclear reactions [465], finding collapse outcomes similar to the Γ = 4/3 studies [461].…”

Section: B Massive Star Collapse In the Early Universementioning

confidence: 84%

Numerical relativity of compact binaries in the 21st century

Duez

Zlochower²

2018

Rep. Prog. Phys.

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We review the dramatic progress in the simulations of compact objects and compact-object binaries that has taken place in the first two decades of the twenty-first century. This includes simulations of the inspirals and violent mergers of binaries containing black holes and neutron stars, as well as simulations of black-hole formation through failed supernovae and high-mass neutron star-neutron star mergers. Modeling such events requires numerical integration of the field equations of general relativity in three spatial dimensions, coupled, in the case of neutron-star containing binaries, with increasingly sophisticated treatment of fluids, electromagnetic fields, and neutrino radiation. However, it was not until 2005 that accurate long-term evolutions of binaries containing black holes were even possible (Pretorius 2005 Phys. Rev. Lett. 95 121101, Campanelli et al 2006 Phys. Rev. Lett. 96 111101, Baker et al 2006 Phys. Rev. Lett. 96 111102). Since then, there has been an explosion of new results and insights into the physics of strongly-gravitating system. Particular emphasis has been placed on understanding the gravitational wave and electromagnetic signatures from these extreme events. And with the recent dramatic discoveries of gravitational waves from merging black holes by the Laser Interferometric Gravitational Wave Observatory and Virgo, and the subsequent discovery of both electromagnetic and gravitational wave signals from a merging neutron star-neutron star binary, numerical relativity became an indispensable tool for the new field of multimessenger astronomy.

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“…The uniqueness of the parameters characterizing the critical configuration implies that the subsequent evolution, namely the collapse to a black hole, as well as the gravitational wave signal emitted in the collapse, is unique as well. Numerical simulations have shown that this collapse will lead to a spinning black hole with mass M BH /M 0.9 and angular momentum J BH /M 2 BH 0.7, surrounded by a disk with mass M disk /M 0.1 (see, e.g., Liu et al 2007;Montero et al 2012;Shibata et al 2016a;Uchida et al 2017;Sun et al 2017Sun et al , 2018.…”

Section: Introductionmentioning

confidence: 99%

Maximally rotating supermassive stars at the onset of collapse: effects of gas pressure

Dennison

Baumgarte

Shapiro

2019

Monthly Notices of the Royal Astronomical Society

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The "direct collapse" scenario has emerged as a promising evolutionary track for the formation of supermassive black holes early in the Universe. In an idealized version of such a scenario, a uniformly rotating supermassive star spinning at the mass-shedding (Keplerian) limit collapses gravitationally after it reaches a critical configuration. Under the assumption that the gas is dominated by radiation pressure, this critical configuration is characterized by unique values of the dimensionless parameters J/M 2 and R p /M, where J is the angular momentum, R p the polar radius, and M the mass. Motivated by a previous perturbative treatment we adopt a fully nonlinear approach to evaluate the effects of gas pressure on these dimensionless parameters for a large range of masses. We find that gas pressure has a significant effect on the critical configuration even for stellar masses as large as M 10 6 M . We also calibrate two approximate treatments of the gas pressure perturbation in a comparison with the exact treatment, and find that one commonly used approximation in particular results in increasing deviations from the exact treatment as the mass decreases, and the effects of gas pressure increase. The other approximation, however, proves to be quite robust for all masses M 10 4 M . Approx. I, β = 0.001 MS J = 16.00 J = 16.50 J = 17.00 J = 17.50 J = 17.75 J = 18.00 J = 18.25 J = 18.42 J = 18.75 J = 19.00 Turn. Pt. Crit. Pt. 0.0 0.5 1.0 1.5 2.0 ×10 −8 4.50 4.51 4.52 4.53 4.54 4.55 Approx. II, β = 0.001 MS J = 16.00 J = 16.50 J = 17.00 J = 17.50 J = 17.75 J = 18.00 J = 18.25 J = 18.65 J = 18.75 J = 19.00 Turn. Pt. Crit. Pt. 0.0 0.5 1.0 1.5 2.0 ×10 −8 4.36 4.38 4.40 4.42 M Exact, β = 0.004 MS J = 14.00 J = 14.50 J = 15.00 J = 15.50 J = 16.00 J = 16.25 J = 16.50 J = 16.75 J = 18.00 J = 20.00 Turn. Pt. Crit. Pt. 0.0 0.5 1.0 1.5 2.0 ×10 −8 4.36 4.38 4.40 4.42 Approx. I, β = 0.004 MS J = 14.00 J = 14.50 J = 15.00 J = 15.50 J = 16.00 J = 16.25 J = 16.50 J = 16.75 J = 18.00 J = 20.00 Turn. Pt. Crit. Pt. 0.0 0.5 1.0 1.5 2.0 ×10 −8 4.42 4.44 4.46 4.48 Approx. II, β = 0.004 MS J = 14.00 J = 14.50 J = 15.00 J = 15.50 J = 16.00 J = 16.25 J = 16.50 J = 17.35 J = 18.00 J = 20.00 Turn. Pt. Crit. Pt. 0 2 4 6 ×10 −8 3.900 3.925 3.950 3.975 4.000 4.025 4.050 M Exact, β = 0.016 MS J = 8.00 J = 10.00 J = 10.50 J = 11.00 J = 11.50 J = 11.75 J = 12.00 J = 12.18 J = 16.00 J = 18.00 Turn. Pt. Crit. Pt. Approx. I, β = 0.016 MS J = 8.00 J = 10.00 J = 10.50 J = 11.00 J = 11.50 J = 11.75 J = 12.00 J = 12.10 J = 16.00 J = 18.00 Turn. Pt. Crit. Pt. Approx. II, β = 0.016 MS J = 8.00 J = 10.00 J = 10.50 J = 11.00 J = 11.50 J = 11.75 J = 12.00 J = 13.48 J = 16.00 J = 18.00 Turn. Pt. Crit. Pt. MS J = 6.00 J = 8.00 J = 8.25 J = 8.50 J = 8.75 J = 9.00 J = 9.25 J = 9.44 J = 11.00 J = 12.00 Turn. Pt. Crit. Pt. Approx. I, β = 0.028 MS J = 6.00 J = 8.00 J = 8.25 J = 8.50 J = 8.75 J = 9.00 J = 9.25 J = 9.26 J = 11.00 J = 12.00 Turn. Pt. Crit. Pt. Approx. II, β = 0.028 MS J = 6.00 J = 8.00 J = 8.25 J = 8.50 J = 8.75 J = 9.00 J = 9.25 J = 10.88 J = 11.00 J = ...

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Gravitational waves from supermassive stars collapsing to a supermassive black hole

Cited by 43 publications

References 42 publications

Gravitational collapse of rotating supermassive stars including nuclear burning effects

Gravitational collapse of rotating supermassive stars including nuclear burning effects

Numerical relativity of compact binaries in the 21st century

Maximally rotating supermassive stars at the onset of collapse: effects of gas pressure

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