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A semi-analytic solution for the radial and vertical structure of accretion discs with a magnetic wind

Lookup NU author(s): Dr Christopher Campbell

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Abstract

A semi-analytic method is presented for solving for the radial and vertical structures of an accretion disc, with a magnetically channelled wind flowing from its surfaces. Both magnetic and turbulent viscous effects are taken into account, and the essential wind properties are related to the disc structure. The angular momentum removed by the wind plays a major part in driving the inflow through the disc, with photospheric temperatures being sufficient to generate the required wind mass flux. The magnetic field is generated by an αω-dynamo, but the method of solution should have application with other magnetic field sources. Self-consistent disc-wind solutions result, with rms turbulent Mach numbers which are in good agreement with those found in simulations of turbulence generated from magnetic shearing instabilities.

Publication metadata

Author(s): Campbell CG

Publication type: Review

Publication status: Published

Journal: Monthly Notices of the Royal Astronomical Society

Year: 2003

Volume: 345

Issue: 1

Pages: 123-143

ISSN (print): 0035-8711

ISSN (electronic): 1365-2966

URL: http://dx.doi.org/10.1046/j.1365-8711.2003.06926.x

DOI: 10.1046/j.1365-8711.2003.06926.x

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