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Title:
Heating solar coronal holes
Authors:
Parker, E. N.
Affiliation:
AA(Chicago, University, IL)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 372, May 10, 1991, p. 719-727. (ApJ Homepage)
Publication Date:
05/1991
Category:
Solar Physics
Origin:
STI
NASA/STI Keywords:
Coronal Holes, Magnetohydrodynamic Waves, Radiative Transfer, Solar Wind, Convection Currents, Dissipation, Solar Magnetic Field
DOI:
10.1086/170015
Bibliographic Code:
1991ApJ...372..719P

Abstract

It has been shown that the coronal hole, and the associated high-speed stream in the solar wind, are powered by a heat input of the order of 500,000 ergs/sq cm s, with most of the heat injected in the first 1-2 solar radii, and perhaps 100,000 ergs/sq cm s introduced at distances of several solar radii to provide the high speed of the issuing solar wind. The traditional view has been that this energy is obtained from Alfven waves generated in the subphotospheric convection, which dissipate as they propagate outward, converting the wave energy into heat. This paper reviews the generation of waves and the known wave dissipation mechanisms, to show that the necessary Alfven waves are not produced under the conditions presently understood to exist in the sun, nor would such waves dissipate significantly in the first 1-2 solar radii if they existed. Wave dissipation occurs only over distances of the order of 5 solar radii or more.

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