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Numerical Simulation of Twisted Solar Corona

Published online by Cambridge University Press:  08 February 2017

S. Parhi ,
B.P. Pandey ,
M. Goossens  and
G.S. Lakhina
S. Parhi
Affiliation:
Communications Research Laboratory, Tokyo 184, Japan
B.P. Pandey
Affiliation:
Indian Institute of Geomagnetism, Bombay 400 005, India
M. Goossens
Affiliation:
Katholieke Universiteit Leuven, Leuven, Belgium
G.S. Lakhina
Affiliation:
Indian Institute of Geomagnetism, Bombay 400 005, India

Extract

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The solar corona supports a variety of waves generated by convective upwelling motion in the photosphere. In order to explain the observed coronal temperature profile, resonant absorption of MHD waves by coronal plasma (Goossens et al, 1995) has been proposed as a possible candidate. The physical picture is that the footpoint motion in the photosphere constantly stirs the coronal plasma leading to the MHD wave generation which is then resonantly absorbed producing the enhanced heating of the corona. Here we consider the problem of MHD wave propagation in a twisted solar corona.

Type
VII. The Solar Atmosphere
Information
Symposium - International Astronomical Union , Volume 185: New Eyes to See Inside the Sun and Stars , 1998 , pp. 467 - 468
Copyright
Copyright © Kluwer 1998 

References

Goossens, M., Ruderman, M. and Hollweg, J. V.: 1995, Solar Phys., 157, 75.CrossRefGoogle Scholar
Parhi, S., De Bruyne, P., Murawski, K., Goossens, M. and DeVore, C. R.: 1996, Solar phys. 167, 181.Google Scholar
Parhi, S., Pandey, B. P., Goossens, M., Lakhina, G. S. and De Bruyne, P.: 1997, Astro. Space Sci., in press.Google Scholar