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Small scale MHD wave processes in the solar atmosphere and solar windSolar wind observations suggesting wave-particle interactions via ion-cyclotron resonances are reviewed. The required power at high frequencies is presumably supplied via a turbulent cascade. Tu's (1987) model, which considers a turbulent cascade explicitly, is outlined. In the solar atmosphere, resonance absorption is considered. The meanings of the cusp and Alfven resonances are discussed, and it is shown how energy gets pumped into small scales. It is shown that resonance absorption can heat the corona and spicules in a manner consistent with observations, if turbulence provides an eddy viscosity.
Document ID
19880007225
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Hollweg, Joseph V.
(New Hampshire Univ. Durham, NH, United States)
Date Acquired
September 5, 2013
Publication Date
August 1, 1987
Publication Information
Publication: ESA, Proceedings of the 21st ESLAB Symposium on Small Scale Plasma Processes in the Solar Chromosphere(Corona, Interplanetary Medium and Planetary Magnetospheres
Subject Category
Solar Physics
Accession Number
88N16608
Funding Number(s)
CONTRACT_GRANT: NAGW-76
CONTRACT_GRANT: NSG-7411
Distribution Limits
Public
Copyright
Other

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