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Advection-dominated Accretion: Underfed Black Holes and Neutron Stars

Ramesh Narayan, Insu Yi

The Astrophysical Journal, 1995

1,612 citations

Abstract

We describe new optically thin solutions for rotating accretion flows around black holes and neutron stars. These solutions are advection dominated, so that most of the viscously dissipated energy is advected radially with the flow. We model the accreting gas as a two-temperature plasma and include cooling by bremsstrahlung, synchrotron, and Comptonization. We obtain electron temperatures Te 108.5-1010 K. The new solutions are present only for mass accretion rates Mṡcrit less than a critical rate A crit which we calculate as a function of radius R and viscosity parameter α. For Mṡ < Mṡcrit we show that there are three equilibrium branches of solutions. One of the branches corresponds to a cool optically thick flow which is the well-known thin disk solution of Shakura & Sunyaev Another branch corresponds to a hot optically thin flow, discovered originally by Shapiro, Lightman, & Eardley (SLE). This solution is thermally unstable. The third branch corresponds to our new advection-dominated solution. This solution is hotter and more optically thin than the SLE solution but is viscously and thermally stable. It is related to the ion torus model of Rees et al. and may potentially explain the hard X-ray and γ-ray emission from X-ray binaries and active galactic nuclei. For Mṡ < Mṡcrit, our work suggests that an accretion flow can choose between two distinct states, namely, the thin disk solution and the new advection-dominated solution, both of which are apparently stable. We…

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