New capabilities for studying the Sun allow us to image for the first time the magnetic Kelvin–Helmholtz (KH) instability developing at the surface of a fast coronal mass ejecta (CME) less than 150 Mm above the solar surface. We conduct a detailed observational investigation of this phenomenon, observed off the east solar limb on 2010 November 3, in the EUV with SDO/AIA. In conjunction with STEREO-B/EUVI, we derive the CME source surface position. We ascertain the timing and early evolution of the CME outflow leading to the instability onset. We perform image and spectral analysis, exploring the CME plasma structuring and its parabolic flow pattern. As we evaluate and validate the consistency of the observations with theoretical considerations and predictions, we take the view that the ejecta layer corresponds to a reconnection outflow layer surrounding the erupting flux rope, accounting for the timing, high temperature (∼11.6 MK), and high flow shear (∼680 km s−1) on the unstable CME northern flank and for the observed asymmetry between the CME flanks. From the irregular evolution of the CME flow pattern, we infer a shear gradient consistent with expected spatial flow variations across the KH-unstable flank. The KH phenomenon observed is tied to the first stage of a linked flare–CME event.
The Astrophysical Journal
American Astronomical Society
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Scholarly Commons Citation
Foullon, C., Verwichte, E., Nykyri, K., Aschwanden, M. J., & Hannah, I. G. (2013). Kelvin-Helmholtz Instability of the CME Reconnection Outflow Layer in the Low Corona. The Astrophysical Journal, 767(2). https://doi.org/10.1008/0004-637X/767/2/170