SECCHI View of CME Dynamics: Observations and Theory

Details SECCHI View of CME Dynamics: Observations and Theory SECCHI View of CME Dynamics: Observations and Theory

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp43a..03k&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SP43A-03

Physics

7513 Coronal Mass Ejections (2101)

Scientific paper

LASCO observations in the region of 2--30 Rs established that CMEs can be understood as erupting magnetic flux ropes based on comparison with LASCO/EIT observations (Chen et al. 1997; Thernisien et al. 2006) and that the observed dynamics in this regime can be correctly described by the erupting flux rope (EFR) model (Chen 1996). Beyond 30 Rs, however, CME morphology and dynamics have not been observed previously, and the EFR model has not been directly compared with data. In this paper, we use LASCO and SECCHI data to examine the evolution of CME morphology and quantitatively test the EFR model against the observed CME dynamics below 2 Rs and beyond 30 Rs. The main topics of this study are (1) the evolution of CME magnetic geometry and (2) forces responsible for acceleration and propagation through the inner corona and interplanetary space. These issues are integrally related because the 3D configuration of magnetic field determines the driving Lorentz force (J × B). We present analysis of two events, CMEs on May 15, 2007 and January 2, 2008 and show that the calculated dynamics closely match the observed dynamics of these CMEs throughout the FOVs of the LASCO and SECCHI telescopes. This suggests that the EFR model correctly captures the essential macroscopic physics of the observed CME dynamics extending to nearly 1 AU.
Chen, J. 1996, JGR, 101, 27499. Chen, J. et al. 1997, ApJ, 490, L191. Thernisien, A., Howard, R. A., and Vourlidas, A. 2006, ApJ, 652, 763.
Work supported by ONR and NASA.

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