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MHD Models of Galactic Center Lobes, Shells, and Filaments

Published online by Cambridge University Press:  19 July 2016

Kazunari Shibata  and
Ryoji Matsumoto
Kazunari Shibata
Affiliation:
1 Department of Earth Sciences, Aichi University of Education, Kariya, Aichi 448, Japan
Ryoji Matsumoto
Affiliation:
2 College of Art Sciences, Chiba University, Chiba 260, Japan

Abstract

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Magnetohydrodynamic (MHD) mechanisms producing radio lobes, shells, and filaments in the Galactic center as well as in the gas disk of the Galaxy are studied by using two-dimensional MHD code: (a) the explosion in a magnetized disk, (b) the interaction of a rotating disk with vertical fields, and (c) the nonlinear Parker instability in toroidal magnetic fields in a disk. In all cases, dense shells or filaments are created along magnetic field lines in a transient state, in contrast to the quasi-equilibrium filaments perpendicular to magnetic fields.

Type
7. Magnetic Fields in Galactic Nuclei
Information
Symposium - International Astronomical Union , Volume 140: Galactic and Intergalactic Magnetic Fields , 1990 , pp. 379 - 380
Copyright
Copyright © Kluwer 1990 

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