On the Origins of Coronal Mass Ejections during Solar Minimum using STEREO Observations

Details On the Origins of Coronal Mass Ejections during Solar Minimum using STEREO Observations On the Origins of Coronal Mass Ejections during Solar Minimum using STEREO Observations

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh43a..08l&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SH43A-08

Other

7509 Corona, 7513 Coronal Mass Ejections (2101), 7524 Magnetic Fields, 7529 Photosphere

Scientific paper

This study addresses the question of the origins of CMEs at the current solar minimum. It is a common consensus that it should be straight forward to track a CME from its source to 1AU during solar quiet times when the solar wind and IMF structure is less complex and fewer CMEs and other coronal activity occur. In reality, total of 1249 CMEs from January to October 2007 are reported on the LASCO CME catalog. Only ~23% (292) CMEs are wider than 30deg and ~2% (28) CMEs wider than 90deg from L1 view point. Most CMEs in the catalog are narrow or jet-like and are classified as poor events. Majority of the CMEs are slow with only one event over 1000km/s. But it has not been an easy task to relate a CME to its source during this period. Using an appropriate set of events and images from three viewing angles from STEREO A/B and SOHO at L1, we determine the sources of the CMEs and their locations on the Sun and in the large scale coronal field. Among other issues, we discuss the implications of our results to CME generation/origin, specifically, whether CMEs always originate from photospheric magnetic neutral lines? Whether some CMEs originate higher in the corona with no signature on the solar disk?

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