HR: 17:30h
AN: SH24A-07    [Abstracts]
TI: Using global MHD simulations to relate the Three-Part Structure of CMEs to in situ observations
AU: * Riley, P
EM: pete.riley@saic.com
AF: SAIC, 10260 Campus Point Dr., MS X1B, San Diego, CA 92121 United States
AU: Linker, J A
EM: jon.linker@saic.com
AF: SAIC, 10260 Campus Point Dr., MS X1B, San Diego, CA 92121 United States
AU: Mikic, Z
EM: zoran.mikic@saic.com
AF: SAIC, 10260 Campus Point Dr., MS X1B, San Diego, CA 92121 United States
AU: Odstrcil, D
EM: dusan.odstrcil@noaa.gov
AF: NOAA/SEC, 325 Broadway, Boulder, CO 80305 United States
AU: Webb, D F
EM: david.webb@hanscom.af.mil
AF: AFRL/VSBXS, 29 Randolf Rd, Hanscom AFB, MA 01731 United States
AU: Zurbuchen, T H
EM: thomasz@umich.edu
AF: University of Michigan, 2455 Hayward St., Ann Arbor, MI 48109 United States
AB: The classic three-part structure of Coronal mass ejections (CMEs) observed in white light observations consisting of a bright front, cavity, and dense core has generally been interpreted as swept-up material, magnetic flux rope, and prominence/filamentary material. Usually, however, there is no clear relationship between these observations and in situ observations of CMEs, or magnetic clouds, in particular. In this study we use a coupled coronal and heliospheric MHD model to relate these disparate observations. The simulations, while idealized, reproduce many of the features found in solar observations, and suggest that the spacecraft's trajectory through the CME plays a dominant role in the type of signatures observed. To track these features through the heliosphere, we use an ensemble of tracer particles. We also exploit the mapping of these tracer particles to explore how compositional profiles associated with the CME evolve as they move away from the Sun.
DE: 7513 Coronal mass ejections
DE: 7823 Ionization processes
DE: 7835 Magnetic reconnection
DE: 7843 Numerical simulation studies
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting