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Energy dissipation of Alfven wave packets deformed by irregular magnetic fields in solar-coronal archesThe importance of field line geometry for shear Alfven wave dissipation in coronal arches is demonstrated. An eikonal formulation makes it possible to account for the complicated magnetic geometry typical in coronal loops. An interpretation of Alfven wave resonance is given in terms of gradient steepening, and dissipation efficiencies are studied for two configurations: the well-known slab model with a straight magnetic field, and a new model with stochastic field lines. It is shown that a large fraction of the Alfven wave energy flux can be effectively dissipated in the corona.
Document ID
19890035338
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Similon, Philippe L. (Cornell Univ. Ithaca, NY, United States)
Sudan, R. N. (Cornell University Ithaca, NY, United States)
Date Acquired
August 14, 2013
Publication Date
January 1, 1989
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 336
ISSN: 0004-637X
Subject Category
SOLAR PHYSICS
Funding Number(s)
CONTRACT_GRANT: NAGW-1006
Distribution Limits
Public
Copyright
Other