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Coronal Heating: Theoretical Ideas

Published online by Cambridge University Press:  14 August 2015

Joseph V. Hollweg
Joseph V. Hollweg*
Affiliation:
Space Science Center, Institute for the Study of Earth, Oceans, and Space and Department of Physics, University of New Hampshire, Durham, NH 03824USA

Extract

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After four decades of study, the mechanisms for heating the corona are not understood. However, the development of the field is vigorous. A variety of new ideas have been proposed, and these new ideas have generated lively debate. The goal of this short review is to present a broad overview of the ideas currently under consideration.

It is now accepted that the solar magnetic field is the key ingredient. It is not known whether waves are important or not, but it is agreed that the magnetic (and possibly associated kinetic) energy must eventually appear in thin structures so that the (generally weak) dissipative processes can heat the plasma. This poses a problem of how the heat gets distributed throughout the corona.

Type
Joint Commission Meeting
Information
Highlights of Astronomy , Volume 8: Highlights of Astronomy. As presented at the XXth General Assembly of the IAU, 1988 , 1989 , pp. 517 - 520
Copyright
Copyright © Kluwer 1989

References

1. Golub, L., Maxson, C., Rosner, R., Serio, S., and Viana, G.S.: 1980, Ap.J., 238, pp. 343–348.CrossRefGoogle Scholar
2. Parker, E.N.: 1986, in Coronal and Prominence Plasmas, NASA-CP-2442, pp. 9–17.Google Scholar
3. Parker, E.N.: 1983, Ap.J., 264, pp. 642–647.CrossRefGoogle Scholar
4. van Ballegooijen, A.A.: 1985, Ap.J., 298, pp. 421–430.CrossRefGoogle Scholar
5. Antiochos, S.K.: 1988, Bull. Amer.Astron. Soc, 20, p. 681.Google Scholar
6. van Ballegooijen, A.A.: 1986, Ap. J., 311, pp. 1001–1014.CrossRefGoogle Scholar
7. Sturrock, P.A., and Uchida, Y.: 1981, Ap.J., 246, pp. 331–336.CrossRefGoogle Scholar
8. Heyvaerts, J., and Priest, E.R.: 1984, Astron. Astrophys, 137, p.63.Google Scholar
9. Dahlburg, R.B., Dahlburg, J.P., and Mariska, J.T.: 1988, Astron. Astrophys., in press.Google Scholar
10. Mikic, Z., Schnack, D.D., and van Hoven, G.: 1988, Ap.J., submitted.Google Scholar
11. Porter, J.G., and Moore, R.L.: 1987, NASA-Marshall preprint 87–146.Google Scholar
12. Koutchmy, S., Zugzda, Y.D., and Locans, V.: 1983, Astron. Astrophys., 120, p.185.Google Scholar
13. Davila, J.M.: 1987, Ap.J., 317, pp 514–521.CrossRefGoogle Scholar
14. Hollweg, J.V., and Yang, G.: 1988, J. Geophys. Res., 93, pp. 5423–5436.CrossRefGoogle Scholar
15. Hollweg, J.V., and Johnson, W.: 1988, J. Geophys. Res., in press.Google Scholar