Vertical Structure of a Magnetic Accretion Disk

Details Vertical Structure of a Magnetic Accretion Disk Vertical Structure of a Magnetic Accretion Disk

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982pthph..68..541h&link_type=abstract

Progress of Theoretical Physics, Vol. 68, No. 2, pp. 541-553

Physics

1

Scientific paper

The vertical equation of a magnetic disk is solved on the approximation that the disk is geometrically thin, and its whole structure is investigated. The solutions are obtained in the form that we can apply them not only to an accretion flow, but also to a stellar wind. The disk is determined by the values of a thickness parameter of the disk δ (≪ 1) and the ratio ζ (>1) of the corotation radius rc to the Alfvén one ra. It is found that the magnetic disk consisting of a perfectly conductive plasma can exist in the super-Alfvénic region by [ 1 + δ3/(2 ζ3-1)5/2 < r/ra < ζ3/δ2/3. ] For a small ζ (˜ O(1)), there occur the sudden concentration of stream lines and a large density gradient in the super-Alfvénic region (r > ra), even if δ ≪ 1. Therefore, it is necessary that the corotation radius is much larger than the Alfvén one (ζ ≫ 1) in order to obtain stable magnetic disks in the super-Alfvénic region.

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