Abstract
The mechanical (nonradiative) energy that is responsible for the solar chromosphere and corona is generated in the subphotospheric layers and propagates into the outer layers where it is dissipated. The propagating energy probably carries momentum as well as energy. Also, because the energy source is mechanical it is expected to be associated with temporal and spatial fluctuations of physical variables. It is logical to assume, therefore, that the transport of mechanical energy and momentum will produce local fluctuations in intensity and velocity and possibly in magnetic field strength. Solar fine structure, at least in part, is the observational manifestation of such processes. The dissipation process, of course, may involve intermediate phenomena that influence the fine structure, and, in turn, the fine structure undoubtedly influences the energy propagation. In any case, the nature of the propagating energy and its dissipation is undoubtedly imprinted in the fine structure.
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Athay, R.G. (1985). Chromospheric Fine Structure. In: Sturrock, P.A., Holzer, T.E., Mihalas, D.M., Ulrich, R.K. (eds) Physics of the Sun. Geophysics and Astrophysics Monographs, vol 25. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-9636-2_2
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