### 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 |

State | Published - Aug 20 2000 |

### Fingerprint

### Keywords

- Accretion, accretion disks
- Convection
- Hydrodynamics

### ASJC Scopus subject areas

- Space and Planetary Science

### Cite this

*Astrophysical Journal*,

*539*(2 PART 1), 809-814.

**Convection-dominated accretion flows.** / Quataert, Eliot; Gruzinov, Andrei.

Research output: Contribution to journal › Article

*Astrophysical Journal*, vol. 539, no. 2 PART 1, pp. 809-814.

}

TY - JOUR

T1 - Convection-dominated accretion flows

AU - Quataert, Eliot

AU - Gruzinov, Andrei

PY - 2000/8/20

Y1 - 2000/8/20

N2 - 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.

AB - 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.

KW - Accretion, accretion disks

KW - Convection

KW - Hydrodynamics

UR - http://www.scopus.com/inward/record.url?scp=0034691974&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=0034691974&partnerID=8YFLogxK

M3 - Article

VL - 539

SP - 809

EP - 814

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2 PART 1

ER -