Abstract
Coronal mass ejections provide a gateway to understanding the physics of energy release and conversion in the solar corona. While it is generally accepted that the energy required to power a CME is contained in the pre-eruption coronal magnetic field, the pre-CME state of that field and the conditions leading up to the release of the magnetic energy are still not entirely clear. Recent studies point to various phenomena which are common to many, if not all, CME events, suggesting that there may be identifiable characteristics of the pre-CME corona which signal the impending eruption. However, determining whether these phenomena are necessary or even sufficient has yet to be achieved. In this paper we attempt to summarize the state of the solar corona and its evolution in the build up to a CME.
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Alexander, D. An Introduction to the Pre-CME Corona. Space Sci Rev 123, 81–92 (2006). https://doi.org/10.1007/s11214-006-9013-1
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DOI: https://doi.org/10.1007/s11214-006-9013-1