Complexity of Coronal Mass Ejections in the Corona

Details Complexity of Coronal Mass Ejections in the Corona Complexity of Coronal Mass Ejections in the Corona

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh22d..06b&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH22D-06

Physics

7509 Corona, 7513 Coronal Mass Ejections

Scientific paper

Coronal mass ejections (CMEs) present a variety of morphologies and sizes as recorded in white light coronal images. Since magnetic flux is 'frozen' in to the plasma in the highly conducting corona, CME morphologies should be related to the topologies of the magnetic fields they contain. CMEs originating in sites containing complex or multi-polar fields may be expected to have more complex morphologies than CMEs originating in simple bipolar regions. In addition, CMEs may become more complex in appearance as they interact with the overlying corona and solar wind. An overview of CME morphologies will be presented, concentrating on CMEs believed to have occurred near the solar limb, where projection effects are minimized. The complexity of CME morphologies will be discussed in the context of their solar origins, their speeds, and their changing appearance at various heights, as the move outward through the corona.

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