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Wave Energy Dissipation in the Solar Atmosphere

Published online by Cambridge University Press:  19 July 2016

Zhou Aihua
Zhou Aihua*
Affiliation:
(Purple Mountain Observatory, Academia Sinica, Nanjing, P.R.C.)

Abstract

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There are two regions of rapid dissipation when Alfvén waves propagate from the transition region to the corona. They occur respectively in a range of several hundred kilometers above the base of the transition region and in the corona at about 1-3Ro. The heating of the atmosphere by wave dissipation could be one order of magnitude larger than heat conduction in the coronal part with a lower temperature and density and stronger magnetic field. Wave heating could also become more important when the magnetic field divergence becomes stronger.

Type
VI. Chromospheric and Coronal Heating
Information
Symposium - International Astronomical Union , Volume 142: Basic Plasma Processes on the Sun , 1990 , pp. 266 - 267
Copyright
Copyright © Kluwer 1990 

References

1. Zhou, A H et al (1988), Chinese Journal of Space Science, 8, 81.Google Scholar
2. Zhou, A H et al (1989), Adv. Space Res. 9pp (4) 33.Google Scholar
3. Jacques, S A (1977), Ap. J. 215, 942.Google Scholar
4. Li, X Q et al (1984), Solar Phys., 91, 289.Google Scholar
5. Vanbeveren, D and De Loore, C (1976), Solar Phys., 50, 99.Google Scholar
6. Rosner, R and Tucker, W H (1978) Ap. J. 220, 643.Google Scholar
7. Kaplan, S A and Tsytovich, V N (1973) Plasma Astrophysics, Pergamon, Oxford, P. 25.Google Scholar
8. Zhou, A H (1990), to be published.Google Scholar