Physics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh41c08g&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SH41C-08
Physics
7509 Corona, 7513 Coronal Mass Ejections, 7524 Magnetic Fields, 7531 Prominence Eruptions
Scientific paper
Physical models admitting a range of magnetic topologies within a coronal mass ejection (CME) will be compared to observations. The nature of CME magnetic fields and their relationships with their plasma distributions are largely unknown, because coronal magnetic fields are not directly observed and the three-dimensional (3D) morphology of the CME can, at best, be inferred from CME density and temperature structures observed as projections onto the plane of the sky. Important insights can be obtained from the relationship between CMEs observed at the solar limb and those observed projected on the solar disk. To study this relationship an MHD model of the 3-D CME is required. This was carried out using a 3-D analytically exact MHD model which treats the CME magnetic field as a spheromak-type flux rope magnetic field pushing its way out of a global open magnetic field (Gibson and Low, ApJ, 493, 460, 1998 & JGR, 105, 18187, 2000). This model shows that such observed white-light limb features as three-part CMEs and U-shaped ``disconnected'' regions, and on-disk structures such as twin dimmings (also referred to as transient coronal holes), and sigmoidal filaments and X-ray loops can be self-consistently explained in terms of the same 3D magnetic morphology and plasma structure viewed in different projections. Further development in this work, including variations of the original model to allow for a greater variety of admissible magnetic topologies, will be reported.
Gibson Sarah Elizabeth
Low B.
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