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Shear-induced instability and arch filament eruption - A magnetohydrodynamic (MHD) numerical simulationA situation wherein a bipolar magnetic field embedded in a stratified solar atmosphere undergoes symmetrical shear motion at the footpoints is investigated via a 2D (nonplanar) MHD simulation. It was found that the vertical plasma flow velocities grow exponentially, leading to a new type of global MHD instability. The growth rate increases almost linearly until it reaches the same order of magnitude as the Alfven speed. Then a nonlinear MHD instability occurs beyond this point. It was found that the central loops are pinched by opposing Lorentz forces, and the outer closed loops stretch upward with the vertically-rising mass flow. The nonlinear dynamical shearing instability is illustrated by a numerical example that is given for three different values of the plasma beta that span several orders of magnitude.
Document ID
19910063785
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Wu, S. T.
(Alabama Univ. Huntsville, AL, United States)
Song, M. T.
(Alabama, University Huntsville, United States)
Martens, P. C. H.
(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA; Lockheed Research Laboratories, Palo Alto CA, United States)
Dryer, M.
(NOAA, Space Environment Laboratory, Boulder CO, United States)
Date Acquired
August 14, 2013
Publication Date
August 1, 1991
Publication Information
Publication: Solar Physics
Volume: 134
ISSN: 0038-0938
Subject Category
Solar Physics
Accession Number
91A48408
Funding Number(s)
CONTRACT_GRANT: AF-AFOSR-88-0013
CONTRACT_GRANT: NAGW-9
CONTRACT_GRANT: NAGW-112
CONTRACT_GRANT: NOAA-50RANR7000104
Distribution Limits
Public
Copyright
Other

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