Monday, 7 January 2019
Hall 4 (Phoenix Convention Center - West and North Buildings)
There are several manifestations of coronal mass ejections (CMEs) in extreme ultraviolet imagery, including flares, coronal dimmings, filament eruptions, and large-scale propagating transients (waves). While none of these signatures can alone serve as a proxy for the definitive detection of a CME in the outer corona, a clearer picture of how these phenomena relate to the pre- and post-eruptive CME structure is beginning to emerge. We address advances in using these different inner coronal observational phenomena as diagnostics of a CME’s direction, energy, size, and magnetic footprint. Additionally, we discuss how to harness these new advances to support and improve forecasts of solar eruptions.
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