Low Density Magnetic Structures (Cavities) in the Solar Corona

Details Low Density Magnetic Structures (Cavities) in the Solar Corona Low Density Magnetic Structures (Cavities) in the Solar Corona

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh41a..07f&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH41A-07

Physics

7509 Corona, 7513 Coronal Mass Ejections

Scientific paper

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.

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