HR: 08:25h
AN: SH21A-02    [Abstracts]
TI: Solar Mass Ejection Imager (SMEI) Solar Wind 3-D Analysis of the January 20, 2005 CME
AU: * Jackson, B V
EM: bvjackson@ucsd.edu
AF: CASS, University of California at San Diego, LaJolla, CA 92093 United States
AU: Buffington, A
EM: abuffington@ucsd.edu
AF: CASS, University of California at San Diego, LaJolla, CA 92093 United States
AU: Hick, P P
EM: pphick@ucsd.edu
AF: CASS, University of California at San Diego, LaJolla, CA 92093 United States
AU: Yu, Y
EM: yyu@cs.ucsd.edu
AF: CASS, University of California at San Diego, LaJolla, CA 92093 United States
AU: Webb, D
EM: david.webb@hanscom.af.mil
AF: ISR, Boston College, Chestnut Hill, MA 02467 United States
AB: The Solar Mass Ejection Imager (SMEI) has observed the inner heliospheric response in white light from over 200 CMEs. One of these, on January 20, 2005, produced one of the largest Solar Energetic Particle events ever recorded. We show SMEI orbital difference images and the 3D solar wind reconstruction of this well-observed CME, and demonstrate how we can track its outward motion from approximately 20 deg. from the Sun until it vanishes in the SMEI field of view in the direction of the Ulysses spacecraft. Our 3D reconstruction technique is used to obtain perspective views from outward-flowing solar wind as observed from Earth by iteratively fitting a kinematic solar wind density model using the SMEI white light observations. This 3D modeling technique permits us to separate the heliospheric response in SMEI from background noise, and to estimate the 3D structure and transient heliospheric components of the CME and its speed and mass. We then determine the total energy of the CME that can be used as input to determine the total energy output of the event. More information about the spatial extent and energetics of this CME event can be determined by measurements in-situ from the Ulysses spacecraft that was beyond 5 AU and about 35 degrees west of Earth. Ulysses first detected an extremely fast CME response at the spacecraft 7 days following the event on the Sun and the transient flow continued for several days. The SMEI 3D reconstruction shows the event as it passes Earth to the west and helps to disentangle the CME structure. This will allow a better understanding of which portions of the CME intersect Ulysses, and the 3D trajectories of several CMEs observed earlier in coronagraph and SMEI data.
UR: http://cass185.ucsd.edu/smei/smei.html
DE: 2101 Coronal mass ejections (7513)
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 2114 Energetic particles (7514)
DE: 7513 Coronal mass ejections (2101)
DE: 7514 Energetic particles (2114)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005