Comparison of MHD Simulations of CME Evolution and Structure with Coronagraph Observations

Details Comparison of MHD Simulations of CME Evolution and Structure with Coronagraph Observations Comparison of MHD Simulations of CME Evolution and Structure with Coronagraph Observations

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh11a..07m&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH11A-07

Physics

7509 Corona, 7513 Coronal Mass Ejections (2101), 7519 Flares, 7524 Magnetic Fields, 7531 Prominence Eruptions

Scientific paper

Coronal mass ejections (CMEs) expel significant amounts of plasma into interplanetary space producing large-scale variations in density that are manifest in coronagraph images. A limitation of these images is that they present two-dimensional projections of three-dimensional structures that are challenging to interpret. The circumstances are even more complex when CMEs are observed at large elongation and the location of preferential scattering is significantly curved. To address the interpretation of such coronagraph images, we examine the Thomson-scattered white-light appearance of 3D MHD simulations of CMEs to identify and reproduce features observed by LASCO and SECCHI coronagraphs. We find close quantitative comparison with LASCO observations and produce shapes at large elongations as seen by SECCHI. We find evidence of shock propagation, magnetic clouds, CME pancaking, and complex time evolution as CMEs propagate at large elongation past the Thomson sphere. A key point is to determine how the 3-D structure of CMEs is affected by propagation through a structured solar wind.

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