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Lookup NU author(s): Dr Christopher Campbell
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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 \B-phis/B-zs\ < 1, where B-phi s and B-zs are the azimuthal and vertical magnetic field components at the disc surface. The ratio B-phi s(2)/2mu(0)P(c), where P-c 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/(omega) over bar (0) and (omega) over bar (0)/(omega) over bar (A), where h is the disc semi-thickness and (omega) over bar (0) and (omega) over bar (A) are the distances of the footpoint of a field line and the Alfven point from the rotation axis, respectively. The ratio \B-phis/B-zs\ is also significant for the local field geometry, and its relation to the field source is discussed.
Author(s): Campbell CG
Publication type: Article
Publication status: Published
Journal: Monthly Notices of the Royal Astronomical Society
Year: 2002
Volume: 336
Issue: 3
Pages: 999-1006
ISSN (print): 0035-8711
ISSN (electronic): 1365-2966
Publisher: Wiley-Blackwell Publishing Ltd.
URL: http://dx.doi.org/10.1046/j.1365-8711.2002.05836.x
DOI: 10.1046/j.1365-8711.2002.05836.x
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