Cme Propagation And Expansion In 3-d Space In The Heliosphere Based On Stereo/secchi Observations.

Details Cme Propagation And Expansion In 3-d Space In The Heliosphere Based On Stereo/secchi Observations. Cme Propagation And Expansion In 3-d Space In The Heliosphere Based On Stereo/secchi Observations.

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640615p&link_type=abstract

American Astronomical Society, AAS Meeting #216, #406.15; Bulletin of the American Astronomical Society, Vol. 41, p.882

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We report a study of kinematic and morphological evolution of CMEs by using STEREO/SECCHI observations to track in 3-D space a set of well observed events from the sun to a large distance in the heliosphere. The CME tracking is based on the Raytrace model (Thernisien et al 2006), which represents a CME as a 3-D flux rope like structure. This model is split into two parts having a where the upper portion is modeled as a semicircular and the lower portion as two straight legs. With this model the true 3-D location can be obtained. We are able to further calculate CME velocity, which is free of projection effect. In particular, the cross-section of CMEs, and thus the expansion speed can be found. For the 4 events studied, we find that their leading edge velocities eventually converge into a narrow range of 500 km/s to 700 km/s, while their initial velocities range from about 400 km/s to 1500 km/s. Their expansion velocities also converge into a narrow range between 75 km/s and 175 km/s. We also fit the data to a derived empirical formula that helps us compare the leading edge velocity profile for each event. We find that the deceleration of fast events and acceleration of slow events mainly occurs within 45 solar radii.

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