Formation of the First Supermassive Black Holes

Bromm, Volker; Loeb, Abraham

doi:10.1086/377529

Cited by 776 publications

(899 citation statements)

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“…The coherence between the near-IR and X-ray emissions would be strong for the PBHs because of the larger value of T max than for DCBHs. This mode of evolution, inevitable if PBHs make up the DM, may influence adjacent star formation and DCBH collapse and evolution as discussed, e.g., in Bromm & Loeb (2003), Agarwal et al (2012), and Yue et al (2014).…”

Section: Discussionmentioning

confidence: 98%

Ligo Gravitational Wave Detection, Primordial Black Holes, and the Near-Ir Cosmic Infrared Background Anisotropies

Kashlinsky

2016

ApJL

187

168

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LIGOʼs discovery of a gravitational wave from two merging black holes (BHs) of similar masses rekindled suggestions that primordial BHs (PBHs) make up the dark matter (DM). If so, PBHs would add a Poissonian isocurvature density fluctuation component to the inflation-produced adiabatic density fluctuations. For LIGOʼs BH parameters, this extra component would dominate the small-scale power responsible for collapse of early DM halos at z  10, where first luminous sources formed. We quantify the resultant increase in high-z abundances of collapsed halos that are suitable for producing the first generation of stars and luminous sources. The significantly increased abundance of the early halos would naturally explain the observed source-subtracted near-IR cosmic infrared background (CIB) fluctuations, which cannot be accounted for by known galaxy populations. For LIGOʼs BH parameters, this increase is such that the observed CIB fluctuation levels at 2-5 μm can be produced if only a tiny fraction of baryons in the collapsed DM halos forms luminous sources. Gas accretion onto these PBHs in collapsed halos, where first stars should also form, would straightforwardly account for the observed high coherence between the CIB and unresolved cosmic X-ray background in soft X-rays. We discuss modifications possibly required in the processes of first star formation if LIGO-type BHs indeed make up the bulk or all of DM. The arguments are valid only if the PBHs make up all, or at least most, of DM, but at the same time the mechanism appears inevitable if DM is made of PBHs.

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Section: Discussionmentioning

confidence: 98%

Ligo Gravitational Wave Detection, Primordial Black Holes, and the Near-Ir Cosmic Infrared Background Anisotropies

Kashlinsky

2016

ApJL

187

168

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“…One is remnant BHs of massive Population III (Pop III) stars with ∼ 100 M (Madau & Rees 2001;Haiman & Loeb 2001;Schneider et al 2002;Islam, Taylor & Silk 2003;Volonteri, Haardt & Madau 2003;Tanaka & Haiman 2009). Second, the socalled direct collapse model (Loeb & Rasio 1994;Oh & Haiman 2002;Bromm & Loeb 2003;Begelman, Volonteri & Rees 2006;Lodato & Natarajan 2006;Shang, Bryan & 2014). When the BH is fed by sufficiently strong gas flows, and the emergent luminosity increases, radiative feedback is likely to affect gas dynamics.…”

Section: Introductionmentioning

confidence: 99%

Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity

Sakurai

Inayoshi

Haiman

2016

Mon. Not. R. Astron. Soc.

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We perform one-dimensional radiation hydrodynamical simulations to solve accretion flows onto massive black holes (BHs) with a very high rate. Assuming that photon trapping limits the luminosity emerging from the central region to L L Edd , Inayoshi, Haiman & Ostriker (2016) have shown that an accretion flow settles to a "hyper-Eddington" solution, with a steady and isothermal (T 8000 K) Bondi profile reaching 5000 times the Eddington accretion rateṀ Edd ≡ L Edd /c 2 . Here we address the possibility that gas accreting with finite angular momentum forms a bright nuclear accretion disc, with a luminosity exceeding the Eddington limit (1 L/L Edd 100). Combining our simulations with an analytic model, we find that a transition to steady hyper-Eddington accretion still occurs, as long as the luminosity remains below L/L Edd 35 (M BH /10 4 M ) 3/2 (n ∞ /10 5 cm −3 )(T ∞ /10 4 K) −3/2 (r /10 14 cm) −1/2 , where n ∞ and T ∞ are the density and temperature of the ambient gas, and r is the radius of the photosphere, at which radiation emerges. If the luminosity exceeds this value, accretion becomes episodic. Our results can be accurately recovered in a toy model of an optically thick spherical shell, driven by radiation force into a collapsing medium. When the central source is dimmer than the above critical value, the expansion of the shell is halted and reversed by ram pressure of the collapsing medium, and by shell's weight. Our results imply that rapid, unimpeded hyper-Eddington accretion is possible even if the luminosity of the central source far exceeds the Eddington limit, and can be either steady or strongly episodic.

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“…Numerical simulations indicate that stars of mass ∼ 10 6 M ⊙ could have formed at the centers of early dwarf galaxies that were barely able to cool their gas through transitions of atomic hydrogen, having T vir ∼ 10 4 K and no H 2 molecules (which were suppressed by a Lyman-Werner background, Bromm and Loeb 2003;Dijkstra et al 2008;Regan and Haehnelt 2009). Such systems have a total mass that is several orders of magnitude higher than the earliest Jeans-mass condensations.…”

Section: Seeds Of Supermassive Black Holesmentioning

confidence: 99%

Menus for Feeding Black Holes

Kocsis¹,

Loeb²

2013

The Physics of Accretion Onto Black Holes

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Black holes are the ultimate prisons of the Universe, regions of spacetime where the enormous gravity prohibits matter or even light to escape to infinity. Yet, matter falling toward the black holes may shine spectacularly, generating the strongest source of radiation. These sources provide us with astrophysical laboratories of extreme physical conditions that cannot be realized on Earth. This chapter offers a review of the basic menus for feeding matter onto black holes and discusses their observational implications.Keywords Black holes · black hole binaries · Accretion and accretion disks · Plasmas -astrophysical PACS 04.70.Bw · 04.25.dg · 97.60.Lf · 98.62.Mw · 95.30.Qd

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Formation of the First Supermassive Black Holes

Cited by 776 publications

References 79 publications

Ligo Gravitational Wave Detection, Primordial Black Holes, and the Near-Ir Cosmic Infrared Background Anisotropies

Ligo Gravitational Wave Detection, Primordial Black Holes, and the Near-Ir Cosmic Infrared Background Anisotropies

Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity

Menus for Feeding Black Holes

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