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A post-CME current sheet (CS) is a common feature developed behind anerupting flux rope in CME models. Observationally, white light observationshave recorded many occurrences of a thin ray appearing behind a CME eruptionthat closely resembles a post-CME CS in its spatial correspondence andmorphology. UV and X-ray observations further strengthen this interpretation bythe observations of high temperature emission at locations consistent withmodel predictions. The next question then becomes whether the properties insidea post-CME CS predicted by a model agree with observed properties. In thiswork, we assume that the post-CME CS is a consequence of Petschek-likereconnection and that the observed ray-like structure is bounded by a pair ofslow mode shocks developed from the reconnection site. We performtime-dependent ionization calculations and model the UV line emission. We findthat such a model is consistent with SOHO/UVCS observations of the post-CME CS.The change of Fe XVIII emission in one event implies an inflow speed of ~10km/s and a corresponding reconnection rate of M_A ~ 0.01. We calculate theexpected X-ray emission for comparison with X-ray observations by Hinode/XRT,as well as the ionic charge states as would be measured in-situ at 1 AU. Wefind that the predicted count rate for Hinode/XRT agree with what was observedin a post-CME CS on April 9, 2008, and the predicted ionic charge states areconsistent with high ionization states commonly measured in the interplanetaryCMEs. The model results depend strongly on the physical parameters in theambient corona, namely the coronal magnetic field, the electron density andtemperature during the CME event. It is crucial to obtain these ambient coronalparameters and as many facets of the CS properties as possible by observationalmeans so that the post-CME current sheet models can be scrutinized moreeffectively.

Modeling UV and X-Ray Emission in a Post-CME Current Sheet