Low Density Magnetic Structures (Cavities) in the Solar Corona
Abstract
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.
- Publication:
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AGU Fall Meeting Abstracts
- Pub Date:
- December 2003
- Bibcode:
- 2003AGUFMSH41A..07F
- Keywords:
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- 7509 Corona;
- 7513 Coronal mass ejections