Abstract
Flares are believed to derive their energy from localized nonpotential magnetic fields; this energy is somehow stored and initially released in the low corona. Therefore, knowledge of coronal conditions prior to flares is essential to our understanding of the flare process. The coronal plasma is constrained by the magnetic field and its characteristic emission is easily observed at soft X-ray wavelengths. Therefore, X-ray imagery is well suited for observing changes in emission influenced by nonpotential magnetic fields in the low corona. This study used soft X-ray images from the Skylab AS&E telescope to search for evidence of coronal preflare emission.
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Webb, D.F. (1980). X-Ray Evidence of Coronal Preflare Emission. In: Dryer, M., Tandberg-Hanssen, E. (eds) Solar and Interplanetary Dynamics. International Astronomical Union / Union Astronomique Internationale, vol 91. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-9100-2_28
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DOI: https://doi.org/10.1007/978-94-009-9100-2_28
Publisher Name: Springer, Dordrecht
Print ISBN: 978-90-277-1163-2
Online ISBN: 978-94-009-9100-2
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