Complexity Within Coronal Mass Ejections Observed in the Solar Wind

Details Complexity Within Coronal Mass Ejections Observed in the Solar Wind Complexity Within Coronal Mass Ejections Observed in the Solar Wind

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh22d..07g&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH22D-07

Physics

2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma

Scientific paper

The large majority of coronal mass ejections, CMEs, observed in the solar wind far from the Sun do not appear to be simple magnetic flux ropes and a relatively small fraction qualify as magnetic clouds as originally defined by the GSFC group. Further, not all CMEs or all portions of a given CME in the solar wind appear to be threaded by closed magnetic field lines despite the fact that CMEs appear to originate in closed field line regions in the solar corona. Moreover, some CMEs in the solar wind are compound events resulting from multiple ejections back at the Sun. This paper provides an overview of some of the complexities associated with CMEs in the solar wind far from the Sun and attempts to relate these complexities to the processes by which CMEs originate at the Sun and evolve within the heliosphere.

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