Magnetohydrodynamical winds from an accretion disk - Driving by the magnetic pressure and tension of toroidal magnetic fields

Details Magnetohydrodynamical winds from an accretion disk - Driving by the magnetic pressure and tension of toroidal magnetic fields Magnetohydrodynamical winds from an accretion disk - Driving by the magnetic pressure and tension of toroidal magnetic fields

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990pasj...42..793f&link_type=abstract

Astronomical Society of Japan, Publications (ISSN 0004-6264), vol. 42, no. 6, 1990, p. 793-817.

Astronomy and Astrophysics

Astronomy

11

Accretion Disks, Active Galactic Nuclei, Magnetic Field Configurations, Magnetohydrodynamics, Radio Jets (Astronomy), Buoyancy, Equations Of Motion, Magnetohydrodynamic Flow, Stream Functions (Fluids), Toroids

Scientific paper

Magnetohydrodynamical (MHD) equations are determined to describe the MHD winds and jets from a thin, rotating accretion disk. The equations are developed in terms of orthogonal curvilinear coordinates with axes parallel and perpendicular to the streamlines. The MHD model, which studies only the toroidal magnetic fields, shows that the magnetic pressure and tension of the fields can accelerate steady rotating MHD jets. The properties of MHD winds in the cold limit are discussed for several streamline configurations. In diverging streamlines, the magnetic tension suppresses acceleration of the flow; vertical streamlines, the magnetic pressure drives steady jets where the speed approaches the disk's rotational speed. A case where the streamlines converge on the rotation axis is also discussed, and the general properties of toroidal fields are given. The interval g(2) between adjacent streamlines can be properly evaluated because the equations are considered in streamline coordinates.

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