Convection in radiatively inefficient black hole accretion flows

Details Convection in radiatively inefficient black hole accretion flows Convection in radiatively inefficient black hole accretion flows

2001-02-28

arxiv.org/abs/astro-ph/0102482v1

Astronomy and Astrophysics

Astrophysics

12 pages, 4 figures, invited plenary review at the 20th Texas Symposium on Relativistic Astrophysics, Austin, Texas, 2000, eds

Scientific paper

10.1063/1.1419633

Recent numerical simulations of radiatively inefficient accretion flows onto compact objects have shown that convection is a general feature in such flows. Dissipation of rotational and gravitational energies in the accretion flows results in inward increase of entropy and development of efficient convective motions. Convection-dominated accretion flows (CDAFs) have a structure that is modified significantly in comparison with the canonical advection-dominated and Bondi-like accretion flows. The flows are characterized by the flattened radial density profiles, ~R^{-1/2}, and have reduced mass accretion rates. Convection transports outward a significant amount of the released binding energy of the accretion flow. We discuss basic dynamical and observational properties of ADAFs using numerical models and self-similar analytical solutions.

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