Laboratory Studies of the Fe K Shell Emission

Peter Beiersdorfer

Lawrence Livermore National Laboratory
7000 East Ave, L-260
Livermore, CA 94550

The importance of the Fe K shell emission for astrophysics has been evident for many years. Data have typically been obtained with rather low-resolution solid-state detectors such as those used on ASCA or presently on Chandra. Next year's launch of ASTRO-E2 is expected to provide Fe K shell spectra with high-resolution (E/DE 1000). This will enable real spectroscopy of the Fe K lines and their use as diagnostics of such source parameters as temperature, ionization equilibrium, and electron density. In order to analyze Fe K shell data spectral models must be both complete and accurate. The Fe K shell spectrum has been studied in much detail on tokamaks and the Livermore electron beam ion traps. Laboratory data now include accurate line lists and identifications, even of several forbidden lines, electron-ion collision cross sections, innershell ionization phenomena and cross sections, dielectronic recombination resonance strengths, spectra produced by charge exchange recombination, electron beam polarization effects, resonance excitation, and radiative cascade contributions. These measurements have provided an assessment of the completeness and accuracy of the atomic data, and we will present results of such measurements.

This work was performed under the auspices of the U.S. DOE by UC-LLNL under contract W-7405-Eng-48 and support by NASA's Astronomy and Physics Research and Analysis Program under contract S-06553-G.