Reconstructing the 3D Morphology of the 17 May 2008 CME

Details Reconstructing the 3D Morphology of the 17 May 2008 CME Reconstructing the 3D Morphology of the 17 May 2008 CME

Oct 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009soph..259..163w&link_type=abstract

Solar Physics, Volume 259, Issue 1-2, pp. 163-178

Physics

14

Coronal Mass Ejections, Initiation And Propagation, Coronal Mass Ejections, Interplanetary

Scientific paper

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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