Free access article

Issue A&A Volume 424, Number 2, September III 2004 Page(s) 379 - 387 Section Astrophysical processes DOI 10.1051/0004-6361:20040538

A&A 424, 379-387 (2004)
DOI: 10.1051/0004-6361:20040538

A model for quasi-spherical magnetized accretion flow

M. Shadmehri

Department of Physics, School of Science, Ferdowsi University, Mashhad, Iran
    e-mail: mshadmehri@science1.um.ac.ir

(Received 29 March 2004 / Accepted 11 May 2004 )

Abstract
A model for axisymmetric magnetized accretion flow is proposed. The dominant mechanism of energy dissipation is assumed to be the magnetic diffusivity due to turbulence in the accretion flow. In analogy to the advection-dominated accretion flow (ADAF) solutions, a constant fraction of the resistively dissipated energy is stored in the accreting gas and the rest is radiated. We first introduce the general self-similar solutions which describe a resistive and nonrotating flow with purely poloidal magnetic field. The radial dependence of physical quantities is identical to that in viscous ADAF solutions. Although the main focus of this study is on nonrotating magnetized accretion flow, for rotating flow with both poloidal and toroidal components of magnetic field we find a radial scaling of solutions similar to the nonrotating case. We show that the accretion and the rotation velocities are both below the Keplerian rate, irrespective of the amount of cooling. We show that the set of equations is reduced to one second order differential equation for a nonrotating flow. The geometrical shape of the disk changes depending on the fraction of the resistively dissipated energy which is stored in the accreting gas. However, there is a hot low-density gas above the disk in almost all cases. The net accretion rate is calculated for a set of illustrative parameters.

Key words: accretion, accretion disks -- magnetohydrodynamics (MHD)

© ESO 2004

What is OpenURL?