HR: 09:45h
AN: SH41A-07    [PDF]
TI: Low Density Magnetic Structures (Cavities) in the Solar Corona
AU: * Foster, D
EM: dafoster@ucar.edu
AF: National Center for Atmospheric Research, 3450 Mitchell Lane, Boulder, CO 80301 United States
AU: Gibson, S
EM: sgibson@ucar.edu
AF: National Center for Atmospheric Research, 3450 Mitchell Lane, Boulder, CO 80301 United States
AU: Burkepile, J
EM: iguana@ucar.edu
AF: National Center for Atmospheric Research, 3450 Mitchell Lane, Boulder, CO 80301 United States
AB: Some helmet streamers in the low corona contain a density depleted region known as a cavity. Cavities form over magnetic polarity inversion lines, often referred to as filament channels, which frequently contain prominences. CMEs often erupt from helmet streamers, and are well associated with erupting prominences. The most common CME morpholgy is the well known loop cavity. Models have been proposed that identify these coronal cavities as low coronal manifestations of twisted magnetic flux ropes, which are then ejected into the solar wind as part of a CME. In order to begin to understand the magnetic structure of coronal cavities, this poster will first examine the frequency of quiescent cavities in the corona using white light observations from the Mark IV coronameter and eclipse photographs.
DE: 7509 Corona
DE: 7513 Coronal mass ejections
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting