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D.W. Savin (Columbia Astrophysics Laboratory), T. Bartsch (University of Giessen), M.H. Chen (Lawrence Livermore National Laboratory), T.W. Gorczyca (Western Michigan University), M. Grieser (Max Planck Institute for Nuclear Physics), S.M. Kahn (Columbia Astrophysics Laboratory), J. Linkemann (Max Planck Institute for Nuclear Physics), A. Mueller (University of Giessen), R. Repnow, A.A. Saghiri (Max Planck Institute for Nuclear Physics), S. Schippers (University of Giessen), M. Schmitt, D. Schwalm, A. Wolf (Max Planck Institute for Nuclear Physics)
Accurate high temperature dielectronic recombination (DR) rate coefficients are needed to interpret cosmic X-ray spectra. 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 of X-ray sources such as stellar coronae, galaxies, clusters of galaxies, the interstellar medium, and supernova remnants. 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.
This research is supported by the NASA High Energy Astrophysics X-Ray Astronomy Research and Analysis and NASA Solar Physics Research, Analysis, and Suborbital programs, by a NATO Collaborative Research Grant, and by the German Federal Minister for Education, Science, Research, and Technology (BMBF). Work at Lawrence Livermore National Laboratory was performed under the auspices of the US Department of Energy.