Abstract
We model the kinematics and three-dimensional distribution of mass in a coronal mass ejection (CME) observed on 17 May 2008, using a comprehensive analysis of STEREO images of the CME. The CME is a surprisingly fast one for solar minimum, reaching velocities of up to 1120 km s−1. It can be followed continuously from inception all the way out to 1 AU. We find that the appearance of the CME can be modeled reasonably well as a combination of two distinct fronts that expand outward in a self-similar fashion. The model implies that STEREO-B is struck by the weaker of these two fronts on 19 May, and the in situ instruments on STEREO-B do see a weak density and magnetic field enhancement at the expected time.
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STEREO Science Results at Solar Minimum
Guest Editors: Eric R. Christian, Michael L. Kaiser, Therese A. Kucera, O.C. St Cyr.
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Wood, B.E., Howard, R.A., Thernisien, A. et al. Reconstructing the 3D Morphology of the 17 May 2008 CME. Sol Phys 259, 163–178 (2009). https://doi.org/10.1007/s11207-009-9391-0
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DOI: https://doi.org/10.1007/s11207-009-9391-0