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Nonlinear Evolution of the Parker Instability

Published online by Cambridge University Press:  03 August 2017

R. Matsumoto  and
K. Shibata
R. Matsumoto
Affiliation:
College of Arts and Sciences, Chiba University, Yayoi-cho, Chiba 260, Japan
K. Shibata
Affiliation:
Department of Earth Sciences, Aichi University of Education, Kariya, Aichi 448, Japan

Abstract

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Two-dimensional MHD simulations are performed to study the nonlinear evolution of the Parker instability in galactic gas disks. When the most unstable mode grows, magnetic field lines kink across the equatorial plane of the disk and thin spur-like structures are formed above dense regions in magnetic pockets. In low β (= ρgas/ρmag < 3) disks, shock waves are produced at the footpoint of magnetic loops, while in high β (> 3) disks, nonlinear oscillations are excited and the loop length increases with time up to λc ≃ (3.5β + 6)H, where H is the half-thickness of the disk.

Type
III. Theory and Modelling
Information
Symposium - International Astronomical Union , Volume 144: The Interstellar Disk-Halo Connection in Galaxies , 1991 , pp. 429 - 432
Copyright
Copyright © Kluwer 1991 

References

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