Physics – Atomic Physics
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.1837g&link_type=abstract
American Astronomical Society, HEAD meeting #9, #18.37; Bulletin of the American Astronomical Society, Vol. 38, p.387
Physics
Atomic Physics
Scientific paper
The interpretation of cosmic spectra relies on a vast sea of atomic data which are not readily obtainable from analytic expressions or simple calculations. Rather, their evaluation typically requires state-of-the-art atomic physics calculations, with the inclusion of weaker effects (spin-orbit and configuration interactions, relaxation, Auger broadening, etc.), to achieve the level of accuracy needed for use by astrophysicists. Our research program is focused on calculating data for three important atomic processes, 1) dielectronic recombination (DR), 2) inner-shell photoabsorption, and 3) fluorescence and Auger decay of inner-shell vacancy states. Our DR work has produced rate coefficients for all H-like through Na-like ions up to nuclear charge Z=30. Present work is focused on the more challenging third-row isoelectronic sequences, such as M-shell iron ions which are responsible for X-ray absorption in active galactic nuclei. K-shell photoabsorption cross sections for all oxygen and neon ions will also be presented and compared to existing experimental measurements. These newly computed data have already been used in conjunction with observed X-ray spectra to infer elemental abundances in the ISM. We also present new fluorescence yields for all second-row K-shell-vacancy isoelectronic sequences, where the inclusion of higher-order effects frequently give results that differ considerably from the currently recommended data, and where we show in particular the inadequacy of the commonly-used configuration-averaged approximation.
This work is supported in part by the NASA APRA program.
Badnell Nigel R.
Dumitriu Ioana
Fu Jian
Gorczyca Tom
Hasoglu M. F.
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