Abstract
Accretion onto supermassive black holes produces both the dramatic phenomena associated with active galactic nuclei and the underwhelming displays seen in the Galactic Center and most other nearby galaxies. I review selected aspects of the current theoretical understanding of black hole accretion, emphasizing the role of magnetohydrodynamic turbulence and gravitational instabilities in driving the actual accretion and the importance of the efficacy of cooling in determining the structure and observational appearance of the accretion flow. Ongoing investigations into the dynamics of the plunging region, the origin of variability in the accretion process, and the evolution of warped, twisted, or eccentric disks are summarized.
Partially supported by NASA and PPARC
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Armitage, P.J. (2004). Theory of Disk Accretion onto Supermassive Black Holes. In: Barger, A.J. (eds) Supermassive Black Holes in the Distant Universe. Astrophysics and Space Science Library, vol 308. Springer, Dordrecht. https://doi.org/10.1007/978-1-4020-2471-9_3
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