Abstract
Chromospheres and coronae owe their existence to mechanical heating. In the present work the mechanisms which are thought to provide steady mechanical heating are reviewed. These mechanisms can be classified as hydrodynamical- and magnetic heating mechanisms and each of these can be subdivided further on basis of the fluctuation frequency. Rapid fluctuations generated by the turbulence in the convection zones lead to acoustic waves and to mhd waves (AC-mechanisms), slow fluctuations to pulsational waves and to stressed fields with current sheets (DC-mechanisms).
Solar and stellar observations, as well as acoustic and mhd wave generation rate computations on basis of convection zone models and a Kolmogorov-type energy spectrum representation for the turbulence, provide great progress towards the understanding of the complete dependence of the chromospheres and coronae on the properties of the underlying stars.
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Ulmschneider, P. (1998). Heating of chromospheres and coronae. In: Vial, J.C., Bocchialini, K., Boumier, P. (eds) Space Solar Physics. Lecture Notes in Physics, vol 507. Springer, Berlin, Heidelberg. https://doi.org/10.1007/BFb0106917
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DOI: https://doi.org/10.1007/BFb0106917
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