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D. W. Savin, S. M. Kahn (Columbia Astrophysics Laboratory), M. Grieser, J. Linkemann, R. Repnow, A. A. Saghiri, M. Schmitt, D. Schwalm, A. Wolf (Max Planck Institute for Nuclear Physics), T. Bartsch, A. Mueller, S. Schippers (University of Giessen), T. W. Gorczyca (Western Michigan University)
Accurate high temperature dielectronic recombination (DR) rate coefficients are needed to interpret solar spectroscopic data. We have shown experimentally that existing DR rates used for plamsa modeling can easily be wrong by factors of 2 or more. These errors affect our ability to derive reliable differential emission measures and chemical abundances. Accurate chemical abundances are particularly important for providing a means of connecting features in the chromosphere and corona with structure in the solar wind, for correctly applying many diagnostics such as X-ray band ratios used to derive electron temperatures, for reliable radiative cooling rates used to understand coronal heating, and for studying the physical processes involved in heating and accelerating the solar corona and solar wind (e.g., the FIP or first ionization potential effect). Here we will present our experimentally-derived high temperature rates for DR of Fe XIX to Fe XVII. We will also discuss our future plans.
The author(s) of this abstract have provided an email address for comments about the abstract: savin@astro.columbia.edu