## Abstract

Nonradiating advection-dominated accretion flows are convectively unstable in the radial direction. We calculate the two-dimensional (r-θ) structure of such flows assuming that (1) convection transports angular momentum inward, opposite to normal viscosity, and (2) viscous transport by other mechanisms (e.g., magnetic fields) is weak (α ≪ 1). Under such conditions convection dominates the dynamics of the accretion flow and leads to a steady state structure that is marginally stable to convection. We show that the marginally stable flow has a constant temperature and rotational velocity on spherical shells, a net flux of energy from small to large radii, zero net accretion rate, and a radial density profile of ρ ∝ r^{-1/2}, flatter than the ρ ∝ r^{-3/2} profile characteristic of spherical accretion flows. This solution accurately describes the full two-dimensional structure of recent axisymmetric numerical simulations of advection-dominated accretion flows.

Original language | English (US) |
---|---|

Pages (from-to) | 809-814 |

Number of pages | 6 |

Journal | Astrophysical Journal |

Volume | 539 |

Issue number | 2 PART 1 |

DOIs | |

State | Published - Aug 20 2000 |

## All Science Journal Classification (ASJC) codes

- Astronomy and Astrophysics
- Space and Planetary Science

## Keywords

- Accretion, accretion disks
- Convection
- Hydrodynamics