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Alfven wave trapping, network microflaring, and heating in solar coronal holesFresh evidence that much of the heating in coronal holes is provided by Alfven waves is presented. This evidence comes from examining the reflection of Alfven waves in an isothermal hydrostatic model coronal hole with an open magnetic field. Reflection occurs if the wavelength is as long as the order of the scale height of the Alfven velocity. For Alfven waves with periods of about 5 min, and for realistic density, magnetic field strength, and magnetic field spreading in the model, the waves are reflected back down within the model hole if the coronal temperature is only slightly less than 1.0 x 10 to the 6th K, but are not reflected and escape out the top of the model if the coronal temperature is only slightly greater than 1.0 x 10 to the 6th K. Because the spectrum of Alfven waves in real coronal holes is expected to peak around 5 min and the temperature is observed to be close to 1.0 x 10 to the 6th K, the sensitive temperature dependence of the trapping suggests that the temperature in coronal holes is regulated by heating by the trapped Alfven waves.
Document ID
19910065888
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Moore, R. L.
(NASA Marshall Space Flight Center Huntsville, AL, United States)
Suess, S. T.
(NASA Marshall Space Flight Center Huntsville, AL, United States)
Musielak, Z. E.
(Alabama, University Huntsville, United States)
An, C.-H.
(Applied Research, Inc. Huntsville, AL, United States)
Date Acquired
August 14, 2013
Publication Date
September 1, 1991
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 378
ISSN: 0004-637X
Subject Category
Solar Physics
Accession Number
91A50511
Distribution Limits
Public
Copyright
Other

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