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Coronal Heating Mechanism in the Presence of a Flow: A Numerical Approach

Published online by Cambridge University Press:  08 February 2017

S. Parhi  and
T. Tanaka
S. Parhi
Affiliation:
Communications Research Laboratory, Tokyo 184, Japan
T. Tanaka
Affiliation:
Communications Research Laboratory, Tokyo 184, Japan

Extract

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The solar corona is a hot, tenuous plasma permeated with the structured magnetic fields. A variety of waves is generated in the corona due to the convective upwelling motion in the photosphere. The excitation of MHD fluctuations is generated by the footpoint motion of the field lines in the photosphere. Resonant absorption of the Alfvén waves in an inhomogeneous plasma has been suggested as a means of driving current and plasma heating in the corona (Sakurai et al., 1991). We study this problem in the presence of flow.

Type
VII. The Solar Atmosphere
Information
Symposium - International Astronomical Union , Volume 185: New Eyes to See Inside the Sun and Stars , 1998 , pp. 469 - 470
Copyright
Copyright © Kluwer 1998 

References

Murawski, K., DeVore, C. R., Parhi, S. and Goossens, M.: 1996, Planet Space Sci. 44, 253.Google Scholar
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Sakurai, T., Goossens, M. and Hollweg, J. V.: 1991, Solar Phys. 133, 227.Google Scholar