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Time scales and efficiency of resonant absorption in periodically driven resistive plasmas

Published online by Cambridge University Press:  13 March 2009

Stefaan Poedts  and
Wolfgang Kerner
Stefaan Poedts
Affiliation:
Max-Planck-Institut für Plasmaphysik, Boltzmannstrasse 2, D-8046 Garching bei München, Germany
Wolfgang Kerner
Affiliation:
Max-Planck-Institut für Plasmaphysik, Boltzmannstrasse 2, D-8046 Garching bei München, Germany
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Abstract

The time scales and efficiency of plasma heating by resonant absorption of Alfvén waves are studied in the framework of linearized compressible and resistive magnetohydrodynamics. The configuration considered consists of a straight cylindrical axisymmetric plasma column surrounded by a vacuum region and a perfectly conducting shell. The plasma is excited periodically by an external source, located in the vacuum region. The temporal evolution of this driven system is simulated numerically. It is shown that the so-called ‘ideal quasi-modes’ (or ‘collective modes’) play a fundamental role in resonant absorption, and affect both the temporal evolution of the driven system and the efficiency of this heating mechanism considerably. The variation of the energetics in periodically driven resistive systems is analysed in detail for three different choices of the driving frequency, viz an arbitrary continuum frequency, the frequency of an ideal ‘quasi-mode’, and a discrete Alfvén wave frequency. The consequences for Alfvén wave heating of both laboratory plasmas and solar coronal loops are discussed.

Type
Research Article
Information
Journal of Plasma Physics , Volume 47 , Issue 1 , February 1992 , pp. 139 - 162
Copyright
Copyright © Cambridge University Press 1992

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References

REFERENCES

Appert, K., Gruber, R., Troyon, F. & Vaclavik, J. 1982 Plasma Phys. 24, 1147.CrossRefGoogle Scholar
Azevedo, C. A., de Assis, A. S., Shigueoka, H. & Sakanaka, P. H. 1990 Mechanisms of Chromospheric and Coronal Heating (ed. Ulmschneider, P., Priest, E. R. & Rosner, R.), p. 492. Springer.Google Scholar
Balet, B., Appert, K. & Vaclavik, J. 1982 Plasma Phys. 24, 1005.CrossRefGoogle Scholar
Goedbloed, J. P. 1984 Physica 12D, 107.Google Scholar
Grossmann, W. & Smith, R. A. 1988 Astrophys. J. 332, 476.CrossRefGoogle Scholar
Ionson, J. A. 1978 Astrophys. J. 226, 65.CrossRefGoogle Scholar
Kappraff, J. M. & Tataronis, J. A. 1977 J. Plasma Phys. 18, 209.CrossRefGoogle Scholar
Poedts, S., Goossens, M. & Kerner, W. 1989 a Solar Phys. 123, 83.CrossRefGoogle Scholar
Poedts, S., Goossens, M. & Kerner, W. 1990 Astrophys. J. 360, 279.CrossRefGoogle Scholar
Poedts, S. & Kerner, W. 1991 Phys. Rev. Lett. 66, 2871.CrossRefGoogle Scholar
Poedts, S., Kerner, W. & Goossens, M. 1989 b J. Plasma Phys. 42, 27.CrossRefGoogle Scholar
Priest, E. R. 1984 Solar Magnetohydrodynamics. Reidel.Google Scholar