An accretion disc model with a magnetic wind and turbulent viscosity

Details An accretion disc model with a magnetic wind and turbulent viscosity An accretion disc model with a magnetic wind and turbulent viscosity

Sep 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000mnras.317..501c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 317, Issue 3, pp. 501-527.

Astronomy and Astrophysics

Astronomy

16

Accretion, Accretion Discs, Magnetic Fields, Mhd, Turbulence, Ism: Jets And Outflows

Scientific paper

A model is presented for an accretion disc with turbulent viscosity and a magnetically influenced wind. The magnetic field is generated by a dynamo in the disc, involving the turbulence and radial shear. Disc-wind solutions are found for which the wind mass flux is sufficient to play a major part in driving an imposed steady inflow, but small enough for most material to be accreted on to the central object. Constraints arise for the magnetic Reynolds and Prandtl numbers in terms of the turbulent Mach number and vertical length-scale of the disc's horizontal magnetic field. It is shown that the imposition of a stellar boundary condition enhances the wind mass flux in the very inner region of the disc and may result in jet formation.

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