Stellar Collapse (Astrophysics and Space Science Library)

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Sign up for new issue notifications. 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.

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.

This object, together with the handful of bright Sloan Digital Sky Survey SDSS quasars at redshift z 6 Fan , sets some of the tightest constraints on models for the formation and growth of massive black holes MBHs at early epochs. The challenge provided by the existence of billion-solar-mass black holes at the end of the reionization epoch is easily described see, e.

The characteristic e -folding timescale t acc for mass growth is then. The third condition requires radiative efficiencies that are below those expected for thin disk accretion onto rapidly spinning Kerr black holes 0. Over the last decade, a number of alternatives to the above picture have been proposed.

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Questions remain about the idealized conditions needed in these models to avoid fragmentation, dissipate angular momentum, and drive gas toward the center of protogalaxies at extremely high rates. In this Letter we discuss super-critical i. Evidence for near-Eddington or super-Eddington flows has been accumulating in recent years. Super-critical accretion onto stellar-mass black holes has been invoked to explain the nature of the ultraluminous X-ray sources e.

In this regime, viscosity-generated heat does not have sufficient time to be radiated away, and is instead advected into the hole. The shorter mass e -folding timescales and the decreased radiative efficiencies that characterize these flows make them ideal for feeding and growing MBHs out of stellar-mass seeds at early times. The Shakura—Sunyaev treatment of accretion onto a black hole via a thin disk posits a radiatively efficient flow where all the heat generated by viscosity at a given radius is immediately radiated away.

It is a local model, described by algebraic equations, valid at any particular radial location in the disk, independently of the physical conditions at different radii. Scientific Detectors for Astronomy by P. Multiwavelength Cosmology by Manolis Plionis. Future Perspectives by Pascale Ehrenfreund. Solar and Space Weather Radiophysics: How does the Galaxy work?: Albany's Dudley Observatory, by George Wise. Nonequilibrium Phenomena in Plasmas: Recollections of "Tucson Operations" by M.

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Scientific Detectors for Astronomy by Jenna E. Astrophysical Disks by Aleksey M. Solar Journey by Priscilla C. Plasma Astrophysics, Part I: Fundamentals and Practice by Boris V. Organizations and Strategies in Astronomy 7 by Andre Heck. Sirius Matters by Noah Brosch. The Science of Solar System Ices: The First Woman in Radio Astronomy: Ruby Payne-Scott by W. Fundamental Questions of Practical Cosmology: Exploring the Realm of Galaxies by Yurij Baryshev. Nanodust in the Solar System: Show only see all Show only. Amounts shown in italicised text are for items listed in currency other than Euros and are approximate conversions to Euros based upon Bloomberg's conversion rates.

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