SUPER-CRITICAL GROWTH OF MASSIVE BLACK HOLES FROM STELLAR-MASS SEEDS

By P. Madau, F. Haardt, M. Dotti. 2014

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We consider super-critical accretion with angular momentum onto stellar-mass black holes as a possible mechanism for growing billion-solar-mass black holes from light seeds at early times. We use the radiatively inefficient “slim disk” solution—advective, optically thick flows that generalize the standard geometrically thin disk model—to show how mildly super-Eddington intermittent accretion may significantly ease the problem of assembling the first massive black holes when the universe was less than 0.8 Gyr old. Because of the low radiative efficiencies of slim disks around non-rotating as well as rapidly rotating black holes, the mass e-folding timescale in this regime is nearly independent of the spin parameter. The conditions that may lead to super-critical growth in the early universe are briefly discussed.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/9df38000ce9cdb88ed6b3d0cf472890a2467663a

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Citations in the corpus

Physical Properties of 15 Quasars at z ≳ 6.5 (2017, background): “…Devecchi & Volonteri 2009), or the rapid growth of stellar-mass seeds via episodes of super-Eddington, radiatively inefficient accretion (e.g., Madau et al. 2014, Alexander & Natarajan 2014, Pacucci et al. 2015, Volonteri et al. 2016, Lupi et al. 2016, Pezzulli et al. 2016, Begelman &…”
Science with the space-based interferometer eLISA. III: probing the expansion of the universe using gravitational wave standard sirens (2016, background): “2 for light seeds (so as to allow for mildly super-Eddington accretion [105]).”
Formation of Supermassive Black Hole Seeds (2016, background): “There is a growing consensus that the stellar mass BHs require various episodes of super Eddington accretion to reach a billion solar masses by z ≥ 6 (Madau et al. 2014; Volonteri et al. 2015; Pacucci et al. 2015; Inayoshi et al. 2015a).”
Selection bias in dynamically measured supermassive black hole samples: its consequences and the quest for the most fundamental relation (2016, background): “…et al. 2015; Wu et al. 2015), alleviates th need to invoke very massive seeds (e.g., Alexander & Natarajan 2014; c© 2016 RAS, MNRAS000, 1– 20 Madau et al. 2014; Lupi et al. 2015), and it may also add some empirical evidence towards the existence of intermediate-mass black holes (e.g.,…”
A GLOBAL THREE-DIMENSIONAL RADIATION MAGNETO-HYDRODYNAMIC SIMULATION OF SUPER-EDDINGTON ACCRETION DISKS (2014, background): “The existence of ∼ 2 × 109 solar mass black hole only at 0.78 Gyr after big bang (Mortlock et al. 2011) also implies that black holes can grow with an accretion rate larger than ṀEdd (Madau et al. 2014; Volonteri & Silk 2014).”
Observational evidence for intermediate-mass black holes (2017, background): “The short phases of super-Eddington growth, followed by longer periods of quiescence, expected to occur in IMBHs (e.g., Volonteri & Rees 2005; Madau et al. 2014; Pezzulli et al. 2016) could also decrease the probability of detecting accreting BHs (Pezzulli et al. 2017).”
Titans of the early Universe: The Prato statement on the origin of the first supermassive black holes (2018, background): “Several works (Alexander & Natarajan 2014; Madau et al. 2014; Volonteri, Silk, & Dubus 2015) have predicted the occurrence of largely super-Eddington accretion episodes at high redshift.”
SUBARU HIGH-z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND BRIGHT GALAXIES AT 5.7 < z < 6.9 (2016, unknown): “…λ−1Edd ln ( MBH MBH,0 ) =0.043 ln ( MBH MBH,0 ) Gyr, where tEdd = 0.44µ −1 e Gyr is the Eddington timescale, µe is the mean molecular weight per electron, ǫ is the radiative efficiency, and λEdd is the Eddington ratio (Shapiro 2005; Madau et al. 2014); here we assume that λEdd is constant in time.”