HR: 08:50h
AN: SH41C-04    [Abstracts]
TI: Physical Properties in the Post-CME Current Sheet
AU: * Ko, Y
EM: yko@cfa.harvard.edu
AF: Harvard-Smithsonian Center for Astrophysics, 60 Garden Steet, MS-50, Cambridge, MA 02138, United States
AU: Raymond, J C
EM: jraymond@cfa.harvard.edu
AF: Harvard-Smithsonian Center for Astrophysics, 60 Garden Steet, MS-50, Cambridge, MA 02138, United States
AB: Post-CME current sheet is a common feature associated with solar eruptions as inferred by CME models. Magnetic reconnection within the current sheet should produce observational signatures, such as heated plasma, bursty outflows and accelerations, that can be used to test various models. Thin ray-like features in the corona appeared shortly after the eruption have been observed by white light coronagraphs on SMM, SOHO/LASCO and MLSO/MK4. They are believed to be the observational evidence of the post-CME current sheet. Spectroscopic observations from SOHO/UVCS also supports its existence by the observations of highly ionized emission lines that exist co-spatially with those features observed in white light. We present the first attempt to model the time-dependent density, temperature and ionic charge state evolution following the magnetic reconnection within a post-CME current sheet, and discuss the observational consequences implied from our results.
DE: 2164 Solar wind plasma
DE: 7509 Corona
DE: 7513 Coronal mass ejections (2101)
DE: 7526 Magnetic reconnection (2723, 7835)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting