Generation and maintenance of bisymmetric spiral magnetic fields in disk galaxies in differential rotation

Details Generation and maintenance of bisymmetric spiral magnetic fields in disk galaxies in differential rotation Generation and maintenance of bisymmetric spiral magnetic fields in disk galaxies in differential rotation

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ppcn.conf..375s&link_type=abstract

In ESA, Fourth International Toki Conference on Plasma Physics and Controlled Nuclear Fusion p 375-378 (SEE N94-22624 05-75)

Physics

Plasma Physics

Dynamo Theory, Galactic Rotation, Interstellar Magnetic Fields, Magnetic Field Configurations, Magnetohydrodynamics, Spiral Galaxies, Disk Galaxies, Plasma Dynamics

Scientific paper

The approximate dynamo equation, which yields asymptotic solutions for the large scale bisymmetric spiral (BSS) magnetic fields rotating rigidly over a large area of the galactic disk, is derived. The vertical thickness and the dynamo strength of the gaseous disk which are necessary to generate and sustain the BSS magnetic fields is determined. The globally BSS magnetic fields which propagate over the disk as a wave without being twisted more tightly are reproduced. A poloidal field configuration is theoretically predicted in the halo around the disk, and is observed in the edge-on galaxy NGC4631. Mathematical methods for the galactic dynamo are shown to be equivalent. Those methods give different growth rates between the BSS and the axisymmetric spiral (ASS) magnetic fields in the disk. Magnetohydrodynamical excitation is discussed between the BSS magnetic fields and the two armed spiral density waves.

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