Black holes in radiation-dominated gas: an analogue of the Bondi accretion problem

Black holes, unlike other compact objects, are able to accrete matter more rapidly than their Eddington rate, | M_ E=L_ E/c²|⁠. Nevertheless, at such a high | M|⁠, radiation will probably be emitted by the in-falling gas in copious enough quantities to have a profound influence on the flow. To aid in understanding the nature of this influence, we study the steady flow, on to a stationary Schwarzschild black hole, of a uniform, non-relativistic gas in which radiation pressure swamps thermal pressure at infinity, and in which Thomson scattering provides the only radiation–gas couple. Asymptotic radiation pressure p∞ and matter density ρ∞ determine an asymptotic sound speed c∞, from which one can derive an accretion rate | M_ B| corresponding to the adiabatic flow of a |=4/3| gas. The actual accretion rate depends on the optical depth τB of a column of unperturbed gas spanning the Bondi radius, |rB=GM/c²_|⁠. If |B (2/3) (c/c_) |⁠, then the flow is adiabatic, and | M= M_ B|⁠. For a somewhat smaller τB, diffusion is efficient enough for the radiation to leak out of the gas as it moves towards the trans-sonic point. As a result, the sound speed decreases inwards in the subsonic region, while the density must increase steeply to maintain pressure balance. | M| may then exceed | M_ B| by a factor of up to | (2/3) (c/_ B c_) |⁠, although this effect can be limited by thermal pressure. Finally, for small enough τB the diffusion approximation breaks down, and radiation drag limits an otherwise thermally-determined | M|⁠. Our boundary conditions occur within super-massive | (M/M₁0²) | stars, and in the pre- and post-recombination universe. If a super-massive star of |M/M₅10⁵| happens to have a small | (M_ BH1 M_) | black hole passing through it on a bound orbit, it will capture and be swallowed by the hole, before it has a chance to ignite its nuclear fuel and blow itself apart. In any milieu where both small black holes and super-massive stars are likely to form (e. g. a dense star cluster), this may provide a natural mechanism for forming black holes in the mass range |10²-10⁵M_|⁠.