Coronal Mass Ejection Evolution in the Inner Heliosphere Geometry and Speed

Details Coronal Mass Ejection Evolution in the Inner Heliosphere Geometry and Speed Coronal Mass Ejection Evolution in the Inner Heliosphere Geometry and Speed

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh32a..04h&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH32A-04

Physics

2101 Coronal Mass Ejections (7513), 2126 Heliosphere/Interstellar Medium Interactions, 7513 Coronal Mass Ejections (2101), 7959 Models

Scientific paper

We present the results from two Coronal Mass Ejections (CMEs) which occurred in February 2003 and February 2004. They were tracked through LASCO within 30 R_\odot and then later as Interplanetary CMEs (ICMEs) through SMEI from 80-150 R_\odot. Both events were also associated with erupting filaments, followed by post-eruptive arcades which were observed by EIT, providing information on the three-dimensional (3D) direction of propagation. Assuming radial propagation, this allowed 3D reconstructions of the CME/ICME geometry, along with corrected (not sky plane projected) measurements of the distance-time (d-t) plots for each event out to ~0.5 AU. We present the results from an investigation of geometry evolution comparing CME/ICME images in LASCO and SMEI. The results show that the curvature becomes more sharply concave outward (i.e. the curvature is away from the Sun), suggesting that the ICME footprints remain fixed to the Sun even at 0.5 AU. We also present two models describing the evolution of the CME/ICMEs at large distances from the Sun and consider two drag models: Aerodynamic Drag and Snow Plow models. There was little difference between these, and their d-t profiles matched well with the SMEI data for the first event. The second event showed a net acceleration between the LASCO and SMEI fields of view and we find that we can match the data for this event well by introducing a driving Lorentz Force to the drag models. ICME mass almost doubled as a result of swept up solar wind material from the Snow Plow model. We discuss possible physical reasons for the difference between the speed evolutions for the two events.

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