UVCS Observations of CMEs from October-November 2003 Flares

Details UVCS Observations of CMEs from October-November 2003 Flares UVCS Observations of CMEs from October-November 2003 Flares

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh51a..03r&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SH51A-03

Other

7513 Coronal Mass Ejections, 7549 Ultraviolet Emissions

Scientific paper

UVCS observed the CMEs associated with several of the powerful flares in late October and early November of 2003. While some of the observations were compromised by high particle background, useful observations of at least six events were obtained. In general, these events resemble the CMEs associated with X-class flares observed in 2002, in that low ionization spectral lines that dominate most UV spectra of CMEs are nearly absent. On the other hand, the [Fe XVIII] line formed at 65 MK is rarely seen in CMEs, but it is detected in many of these events. We discuss whether this means that no cool prominence material is ejected, or that the prominence material is heated so strongly that all the plasma reaches a high ionization state.

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