HEAD 2003 Meeting
Session 39. Laboratory Astrophysics II
Oral, Tuesday, March 25, 2003, 11:30am-12:10pm

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[39.03] Assessment of the Fluorescence and Auger Data Base used in Plasma Modeling

T. W. Gorczyca, C. N. Kodituwakku, K. T. Korista, O. Zatsarinny (Western Michigan University), N. R. Badnell (University of Strathclyde), E. Behar (Technion, Haifa), M. H. Chen (Lawrence Livermore National Laboratory), D. W. Savin (Columbia Astrophysics Laboratory)

Accurate fluorescence and Auger yields are crucial for the interpretation of spectra from X-ray photoionized plasmas (such as are found in X-ray binaries and active galactic nuclei) and for supernova remnants under conditions of non-equilibrium ionization. We have investigated the accuracy of the 1s-vacancy fluorescence and Auger data base of Kaastra & Mewe (1993, A&AS, 97, 443) resulting from the initial atomic physics calculations and the subsequent scaling along isoelectronic sequences. In particular, we have focused on the relatively simple Be-like and F-like 1s-vacancy sequences. We find that the earlier atomic physics calculations for the oscillator strengths and autoionization rates of singly-charged B II and Ne II are in sufficient agreement with our present calculations. However, the substantial charge dependence of these quantities along each isoelectronic sequence, the incorrect configuration averaging used for B II, and the neglect of relativistic effects (which become important at high-Z) all cast doubt on the reliability of the Kaastra & Mewe data for application to plasma modeling.

TWG, CNK, KTK, and OZ were supported by NASA Space Astrophysics Research and Analysis Program grant NAG5-10448. EB was supported by the Yigal-Alon Fellowship and by the GIF Foundation under grant #2028-1093.7/2001. The work of MHC was performed under the auspices of US Department of Energy by the University of California, Lawrence Livermore National Laboratory, Under Contract Number W-7405-ENG-48. DWS was supported in part by NASA Space Astrophysics Research and Analysis Program grant NAG5-5261 and NASA Solar Physics research, Analysis, and Suborbital Program grant NAG5-9581.

The author(s) of this abstract have provided an email address for comments about the abstract: gorczyca@wmich.edu

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