Abstract
Thermal energy must be continually supplied to the solar corona to maintain its 106 °K temperature. In the first part of this paper we review the efforts which have been made in the past twenty years to find a viable mechanism to explain coronal heating, with special emphasis on the conditions of applicability of the existing theories and on the possibility that coronal heating may be intimately linked to other manifestations of solar activity such as solar flares. The interplay of the different aspects of solar activity is discussed within the unifying framework of MHD turbulence.
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Einaudi, G., Velli, M. (1994). Coronal heating mechanisms. In: Belvedere, G., Rodonò, M., Simnett, G.M. (eds) Advances in Solar Physics. Lecture Notes in Physics, vol 432. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-58041-7_212
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DOI: https://doi.org/10.1007/3-540-58041-7_212
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