The S-cone luminance input depends on the level of M-cone adaptation

Ripamonti, Caterina; Crowther, Elizabeth; Stockman, Andrew

doi:10.1167/8.6.956

Cited by 1 publication

(1 citation statement)

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“…The impact of the radiation field produced near the event horizon on the accretion flow and on the state of the interstellar medium of the protogalaxy and that of the intergalactic medium (e.g., Dijkstra et al 2004;Kuhlen & Madau 2005;Zaroubi et al 2007; Thomas & Zaroubi 2008;Ripamonti et al 2008;Spaans & Meijerink 2008) is sensitive to the shape of the spectral energy distribution (SED) of the central source. The SEDs of rapidly accreting low-mass massive black holes (M BH ∼ 10 5 − 10 6 M ) exhibit significantly larger X-ray (2 keV) to optical spectral ratios than the AGN containing more massive rapidly accreting black holes (Greene & Ho 2007), as is expected if a fraction of the radiation is produced in a geometrically thin disk.…”

Section: Introductionmentioning

confidence: 99%

Accretion Onto “Seed” Black Holes in the First Galaxies

Milosavljević

Bromm

Couch

et al. 2009

ApJ

172

153

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The validity of the hypothesis that the massive black holes in high redshift quasars grew from stellar-sized "seeds" is contingent on a seed's ability to double its mass every few ten million years. This requires that the seed accrete at approximately the Eddington-limited rate. In the specific case of radiatively efficient quasiradial accretion in a metal-poor protogalactic medium, for which the Bondi accretion rate is often prescribed in cosmological simulations of massive black hole formation, we examine the effects of the radiation emitted near the black hole's event horizon on the structure of the surrounding gas flow. We find that photoheating and radiation pressure from photoionization significantly reduce the steady-state accretion rate and potentially render the quasiradial accretion flow unsteady and inefficient. The time-averaged accretion rate is always a small fraction of the "Bondi" accretion rate calculated ignoring radiative feedback. The pressure of Lyα photons trapped near the H II region surrounding the black hole may further attenuate the inflow. These results suggest that an alternative to quasiradial, radiatively efficient Bondi-like accretion should be sought to explain the rapid growth of quasar-progenitor seed black holes.

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