AAS 207th Meeting, 8-12 January 2006
Session 111 Solar Activity
Poster, Wednesday, 9:20am-6:30pm, January 11, 2006, Exhibit Hall

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[111.08] 3D CME Mass and Energy From Solar Mass Ejection Imager (SMEI) and Interplanetary Scintillation (IPS) Data

B.V. Jackson, A. Buffington, P.P. Hick, Y. Yu (CASS/UCSD)

White-light Thomson scattering observations from the Solar Mass Ejection Imager (SMEI) have recorded the inner heliospheric response to several hundred CMEs including the halo CMEs of May 28, 2003 and October 28, 2003, and numerous other heliospheric structures. We show the extent of several well-observed CMEs in SMEI observations, and measure these events from their first observations in SMEI approximately 20 degrees from the solar disk until they vanish in the SMEI field of view. Several portions of large CMEs can be observed in the interplanetary medium associated with the initial coronal response and the underlying erupting prominence structure observed by the LASCO coronagraphs and other instruments. To enhance the images and understand the outward propagation of these structures we use a 3D reconstruction technique that obtains perspective views from outward-flowing solar wind as observed from Earth, iteratively fitting a kinematic solar wind density model to the SMEI white light observations and, when available, also to the Solar-Terrestrial Environment Laboratory (STELab), Japan interplanetary scintillation (IPS) velocity data. This 3D modeling technique allows separating the heliospheric response in SMEI from background noise, and estimating the 3D structure of the CME and its mass. Pixel-to-pixel 3D comparison with the IPS velocity structure gives the outward flow kinetic energy for these events.

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