Small-scale inviscid accretion discs around black holes
arXiv:astro-ph/0006351 · doi:10.1046/j.1365-8711.2001.04133.x
Abstract
Gas falling quasi-spherically onto a black hole forms an inner accretion disc if its specific angular momentum exceeds $\lmin\sim r_gc$ where is the Schwarzschild radius. The standard disc model assumes $l\gg\lmin$. We argue that, in many black-hole sources, accretion flows have angular momenta just above the threshold for disc formation, $l\simgt\lmin$, and assess the accretion mechanism in this regime. In a range $\lmin<l<\lcr$, a small-scale disc forms in which gas spirals fast into the black hole without any help of horizontal viscous stresses. Such an `inviscid' disc, however, interacts inelastically with the feeding infall. The disc-infall interaction determines the dynamics and luminosity of the accretion flow. The inviscid disc radius can be as large as , and the energy release peaks at . The disc emits a Comptonized X-ray spectrum with a break at keV. This accretion regime is likely to take place in wind-fed X-ray binaries and is also possible in active galactic nuclei.
10 pages, accepted to MNRAS
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