Modeling CMEs in the Corona and Solar Wind

Details Modeling CMEs in the Corona and Solar Wind Modeling CMEs in the Corona and Solar Wind

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh22d..02l&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH22D-02

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7513 Coronal Mass Ejections, 7524 Magnetic Fields, 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields

Scientific paper

Coronal mass ejections (CMEs), immense eruptions of plasma and magnetic fields with velocities as high as 2000 km/s, are a major transient input of mass and energy into the solar wind. CMEs typically appear as loop-like features that disrupt helmet streamers in the solar corona. The interplanetary manifestation of CMEs is often, but not always, as flux ropes or magnetic clouds. In this talk we will review models of CMEs, from their initiation and evolution in the corona to their propagation in the inner heliosphere. We will discuss how "complexity" might arise in CMEs during their passage through interplanetary space, either due to interactions with the ambient solar wind or to collisions with other CMEs. Research supported by NASA and NSF.

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