Physics
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh24a..07r&link_type=abstract
American Geophysical Union, Fall Meeting 2004, abstract #SH24A-07
Physics
7513 Coronal Mass Ejections, 7823 Ionization Processes, 7835 Magnetic Reconnection, 7843 Numerical Simulation Studies
Scientific paper
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.
Linker Jon A.
Mikic Zoran
Odstrcil Dusan
Riley Pete
Webb David F.
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