Abstract
The magnetized, million-degree solar corona evolves in cycles of about eleven years, in dynamical response to newly generated magnetic fluxes emerging from below to eventually reverse the global magnetic polarity. Over the larger scales, the corona does not erupt violentiy all the time Violent events like the flares and episodic ejections of material into mass — planetary space occur frequently, several times a day. but they often originate in long-lived magnetic structures which form continually tnrougholly the solar cycle. in this paper, the creation, stability, and eventual eruption of these structures are discussed from basic principles, drawing on recer, advances in observation and theory. A global view is offered in which different pieces of observation relate physically, with distinct roles for the conservation of magnetic helicity and the releases of magnetic energy dissipated and ordered forms.
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Low, B.C. (1996). Magnetohydrodynamic Processes in the Solar Corona: Flares, Coronal Mass Ejections and Magnetic Helicity. In: Tsinganos, K.C. (eds) Solar and Astrophysical Magnetohydrodynamic Flows. NATO ASI Series, vol 481. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0265-7_7
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