Can Direct Collapse Black Holes Launch Gamma-Ray Bursts and Grow to Supermassive Black Holes?

Matsumoto, Tatsuya; Nakauchi, Daisuke; Ioka, Kunihito; Heger, Alexander; Nakamura, Takashi

doi:10.1088/0004-637x/810/1/64

Cited by 48 publications

(51 citation statements)

References 74 publications

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“…[28] (see Eqs. (25)(26)(27) for this reference). We also simulated the gravitational collapse including the effect of the rpprocess as test calculations and found that the rp-process affects only weakly the gravitational collapse because this process becomes efficient only in the very dense and hot region.…”

Section: Equation Of Statementioning

confidence: 99%

“…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: 99%

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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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Section: Equation Of Statementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Gravitational collapse of rotating supermassive stars including nuclear burning effects

et al. 2017

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“…Thus we conclude that it will be difficult for Pop-III HNRs to dominantly contribute to the observed high-energy backgrounds unless the explosion energy is E Pop−III 10 53 erg. On the other hand, the explosion energy for supermassive stars at very-high-redshifts could be larger than ∼ 10 55 erg (Matsumoto et al 2015). Note that the relative ratio of the neutrino fluxes contributed by the high and low redshift components are largely uncertain.…”

Section: Discussionmentioning

confidence: 99%

Revisiting the Contributions of Supernova and Hypernova Remnants to the Diffuse High-Energy Backgrounds: Constraints on Very High Redshift Injection

Xiao

Mészáros

Murase

et al. 2016

ApJ

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Star-forming and starburst galaxies are considered as one of the viable candidate sources of the high-energy cosmic neutrino background detected in IceCube. We revisit contributions of supernova remnants (SNRs) and hypernova remnants (HNRs) in such galaxies to the diffuse high-energy neutrino and gamma-ray backgrounds, in light of the latest Fermi data above 50 GeV. We also take into account possible time dependent effects of the cosmic-ray (CR) acceleration during the SNR evolution. CRs accelerated by the SNR shocks can produce high-energy neutrinos up to ∼ 100 TeV energies, but CRs from HNRs can extend the spectrum up to PeV energies. We show that, only if HNRs are dominant over SNRs, the diffuse neutrino background above 100 TeV can be explained without contradicting the gamma-ray data. However, the neutrino data around 30 TeV remain unexplained, which might suggest a different population of gamma-ray dark CR sources. We also consider possible contributions of Pop-III HNRs up to z 10, and show that they are not constrained by the gamma-ray data, and thus could contribute to the diffuse high-energy backgrounds if their explosion energy reaches E POP−III ∼ a few × 10 53 erg. More conservatively, our results suggest that the explosion energy of POP-III HNRs is E POP−III 7 × 10 53 erg.

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“…It is difficult to understand how these early SMBHs formed over such short time-scales, and there are open issues with various plausible scenarios (e.g., Dijkstra et al 2008;Mayer et al 2010;Inayoshi & Omukai 2012;Tanaka & Li 2014;Matsumoto et al 2015). The presence of massive BH seed candidates (10 5 M⊙ at z > 6), possibly direct collapse black holes, in a bright Lyman-α emitter at z = 6.6 have been recently suggested (Smith, Bromm & Loeb 2016;Pacucci et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Quasar outflows at z ≥ 6: the impact on the host galaxies

Barai

Gallerani

Pallottini

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We investigate quasar outflows at z 6 by performing zoom-in cosmological hydrodynamical simulations. By employing the SPH code GADGET-3, we zoom in the 2R 200 region around a 2×1012 M ⊙ halo at z = 6, inside a (500 Mpc) 3 comoving volume. We compare the results of our AGN runs with a control simulation in which only stellar/SN feedback is considered. Seeding 10 5 M ⊙ BHs at the centers of 10 9 M ⊙ halos, we find the following results. BHs accrete gas at the Eddington rate over z = 9 − 6. At z = 6, our most-massive BH has grown to M BH = 4 × 10 9 M ⊙ . Fast (v r > 1000 km/s), powerful (Ṁ out ∼ 2000M ⊙ /yr) outflows of shock-heated low-density gas form at z ∼ 7, and propagate up to hundreds kpc. Star-formation is quenched over z = 8 − 6, and the total SFR (SFR surface density near the galaxy center) is reduced by a factor of 5 (1000). We analyse the relative contribution of multiple physical process: (i) disrupting cosmic filamentary cold gas inflows, (ii) reducing central gas density, (iii) ejecting gas outside the galaxy; and find that AGN feedback has the following effects at z = 6. The inflowing gas mass fraction is reduced by ∼ 12%, the high-density gas fraction is lowered by ∼ 13%, and ∼ 20% of the gas outflows at a speed larger than the escape velocity (500 km/s). We conclude that quasar-host galaxies at z 6 are accreting non-negligible amount of cosmic gas, nevertheless AGN feedback quenches their star formation dominantly by powerful outflows ejecting gas out of the host galaxy halo.

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Can Direct Collapse Black Holes Launch Gamma-Ray Bursts and Grow to Supermassive Black Holes?

Cited by 48 publications

References 74 publications

Gravitational collapse of rotating supermassive stars including nuclear burning effects

Gravitational collapse of rotating supermassive stars including nuclear burning effects

Revisiting the Contributions of Supernova and Hypernova Remnants to the Diffuse High-Energy Backgrounds: Constraints on Very High Redshift Injection

Quasar outflows at z ≥ 6: the impact on the host galaxies

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