Accretion Onto “Seed” Black Holes in the First Galaxies

Milosavljević, Miloš; Bromm, Volker; Couch, Sean M.; Oh, S. Peng

doi:10.1088/0004-637x/698/1/766

Cited by 172 publications

(156 citation statements)

References 113 publications

(142 reference statements)

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“…Radiative feedback has been found to limit accretion onto stellar-mass black holes in spherical and clumpy accretion flows (Milosavljević et al 2009). This applies to the dark-remnant accretion phase, because we have assumed spherical accretion in Sect.…”

Section: Limitations Of Dark-remnant Accretion Through Local Radiativmentioning

confidence: 99%

Superbubble dynamics in globular cluster infancy

Krause

Charbonnel

Decressin

et al. 2013

A&A

139

155

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Context. The self-enrichment scenario for globular clusters (GC) requires large amounts of residual gas after the initial formation of the first stellar generation. Recently, we found that supernovae may not be able to expel that gas, as required to explain their presentday gas-free state, and suggested that a sudden accretion onto the dark remnants at a stage when type II supernovae have ceased may plausibly lead to fast gas expulsion. Aims. Here, we explore the consequences of these results for the self-enrichment scenario via fast-rotating massive stars (FRMS). Methods. We analysed the interaction of FRMS with the intra-cluster medium (ICM), in particular where, when, and how the second generation of stars may form. From the results, we developed a timeline of the first ≈40 Myr of GC evolution. Results. Our previous results imply three phases during which the ICM is in a fundamentally different state, namely the wind bubble phase (lasting 3.5 to 8.8 Myr), the supernova phase (lasting 26.2 to 31.5 Myr), and the dark remnant accretion phase (lasting 0.1 to 4 Myr): (i) Quickly after the first-generation massive stars have formed, stellar wind bubbles compress the ICM into thin filaments. No stars may form in the normal way during this phase because of the high Lyman-Werner flux density. If the first-generation massive stars have equatorial ejections however, as we proposed in the FRMS scenario, accretion may resume in the shadow of the equatorial ejecta. The second-generation stars may then form due to gravitational instability in these disc, which are fed by both the FRMS ejecta and pristine gas. (ii) In the supernova phase the ICM develops strong turbulence, with characteristic velocities below the escape velocity. The gas does not accrete either onto the stars or onto the dark remnants in this phase because of the high gas velocities. The strong mass loss associated with the transformation of the FRMS into dark remnants then leads to the removal of the secondgeneration stars from the immediate vicinity of the dark remnants. (iii) When the supernovae have ceased, turbulence quickly decays, and the gas can once more accrete, now onto the dark remnants. As discussed previously, this may release sufficient energy to unbind the gas, and may happen fast enough so that a large fraction of less tightly bound first-generation stars are lost. Conclusions. Studying the FRMS scenario for the self-enrichment of GCs in detail reveals the important role of the physics of the ICM for our understanding of the formation and early evolution of GCs. Depending on the level of mass segregation, this sets constraints on the orbital properties of the stars, in particular high orbital eccentricities, which likely has implications on the GC formation scenario.

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Section: Limitations Of Dark-remnant Accretion Through Local Radiativmentioning

confidence: 99%

Superbubble dynamics in globular cluster infancy

Krause

Charbonnel

Decressin

et al. 2013

A&A

139

155

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“…Population III (or Pop III) stars were also the first great nucleosynthetic engines of the universe, expelling large quantities of the heavy EACOA Fellow, E-mail: ken.chen@nao.ac.jp elements needed for the later formation of planets and life (e.g., Bromm et al 2003;Kitayama & Yoshida 2005;Greif et al 2007;Karlsson et al 2013). They may also be the origins of the supermassive black holes found in most massive galaxies today (e.g., Volonteri et al 2003;Milosavljević et al 2009;Alvarez et al 2009;Park & Ricotti 2011;Johnson et al 2012;Agarwal et al 2012;Johnson et al 2013;Latif et al 2013;Johnson et al 2014;Smidt et al 2016;Woods et al 2016;Hammerlé et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Low-energy Population III supernovae and the origin of extremely metal-poor stars

Chen

Heger

Whalen

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Some ancient, dim, metal-poor stars may have formed in the ashes of the first supernovae. If their chemical abundances can be reconciled with the elemental yields of specific Pop III explosions, they could reveal the properties of primordial stars. But multidimensional simulations of such explosions are required to predict their yields because dynamical instabilities can dredge material up from deep in the ejecta that would otherwise be predicted to fall back onto the central remnant and be lost in one-dimensional (1D) models. We have performed two-dimensional (2D) numerical simulations of two low-energy Pop III supernovae, a 12.4 M explosion and a 60 M explosion, and find that they produce elemental yields that are a good fit to those measured in the most iron-poor star discovered to date, SMSS J031300.36-670839.3 (J031300). Fallback onto the compact remnant in these weak explosions accounts for the lack of measurable iron in J031300 and its low iron-group abundances in general. Our 2D explosions produce higher abundances of heavy elements (atomic number Z > 20) than their 1D counterparts due to dredge-up by fluid instabilities. Since almost no 56 Ni is ejected by these weak SNe, their low luminosities will prevent their detection in the near infrared with the James Webb Space Telescope and future 30-meter telescopes on the ground. The only evidence that they ever occurred will be in the fossil abundance record.

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“…In this context Madau et al (2004) and Ricotti & Ostriker (2004) have suggested that a smaller fraction of ionizing photons were provided by primordial black holes of intermediate mass ("miniquasars", at z > 10) accreting by Bondi-Hoyle from the surrounding gas. However, feedback from Bondi-Hoyle accretion to solitary black holes significantly suppresses both any further inflow (Alvarez et al 2009;Milosavljevic et al 2009) and the consequent injection of radiation and high-energy particles to the surrounding medium.…”

Section: Introductionmentioning

confidence: 99%

Stellar black holes at the dawn of the universe

Mirabel

Dijkstra

Laurent

et al. 2011

A&A

252

292

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Context. It is well established that between 380 000 and 1 billion years after the Big Bang the Inter Galactic Medium (IGM) underwent a "phase transformation" from cold and fully neutral to warm (≈10 4 K) and ionized. Whether this phase transformation was fully driven and completed by photoionization by young hot stars is a question of topical interest in cosmology. Aims. We propose here that besides the ultraviolet radiation from massive stars, feedback from accreting black holes in high-mass X-ray binaries (BH-HMXBs) was an additional, important source of heating and reionization of the IGM in regions of low gas density at large distances from star-forming galaxies. Methods. We use current theoretical models on the formation and evolution of primitive massive stars of low metallicity, and the observations of compact stellar remnants in the near and distant universe, to infer that a significant fraction of the first generations of massive stars end up as BH-HMXBs. Results. The total number of energetic ionizing photons from an accreting stellar black hole in an HMXB is comparable to the total number of ionizing photons of its progenitor star. However, the X-ray photons emitted by the accreting black hole are capable of producing several secondary ionizations and the ionizing power of the resulting black hole could be greater than that of its progenitor. Feedback by the large populations of BH-HMXBs heats the IGM to temperatures of ≈10 4 K and maintains it ionized on large distance scales. Conclusions. BH-HMXBs determine the early thermal history of the universe and maintain it as ionized over large volumes of space in regions of low density. This has a direct impact on the properties of the faintest galaxies at high redshifts, the smallest dwarf galaxies in the local universe, and on the existing and future surveys at radio wavelengths of atomic hydrogen in the early universe.

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Accretion Onto “Seed” Black Holes in the First Galaxies

Cited by 172 publications

References 113 publications

Superbubble dynamics in globular cluster infancy

Superbubble dynamics in globular cluster infancy

Low-energy Population III supernovae and the origin of extremely metal-poor stars

Stellar black holes at the dawn of the universe

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