Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mnras.336..999c&link_type=abstract
Monthly Notice of the Royal Astronomical Society, Volume 336, Issue 3, pp. 999-1006.
Astronomy and Astrophysics
Astronomy
4
Accretion, Accretion Discs, Magnetic Fields, Mhd, Waves
Scientific paper
The standard method of finding the slow magnetosonic point in a magnetically influenced accretion disc wind flow is examined. This method uses the condition of vanishing effective gravity along the poloidal magnetic field, and corresponds to the merging of the slow magnetosonic and sonic points. It is shown that a necessary condition for the validity of such an approach is |Bφs/Bzs| < 1, where Bφs and Bzs are the azimuthal and vertical magnetic field components at the disc surface. The ratio B2φs/2μ0Pc, where Pc is the central gas pressure, must also be significantly less than unity. The nature of the local poloidal field geometry is shown to depend on the ratios h/ϖ0 and ϖ0/ϖA, where h is the disc semi-thickness and ϖ0 and ϖA are the distances of the footpoint of a field line and the Alfvén point from the rotation axis, respectively. The ratio |Bφs/Bzs| is also significant for the local field geometry, and its relation to the field source is discussed.
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