Statistics – Computation
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...212.0314g&link_type=abstract
American Astronomical Society, AAS Meeting #212, #3.14; Bulletin of the American Astronomical Society, Vol. 40, p.186
Statistics
Computation
Scientific paper
Standard methods for determining temperatures and densities of high-temperature astrophysical plasmas involve the modeling of the optically thin far-UV and X-ray emission lines of multiply charged atomic ions. Their presence in relatively low concentration can strongly influence the energy and ionization balance evaluations that require detailed knowledge of many elementary radiative and collisional processes, such as dielectronic recombination (DR). DR is the dominant electron-ion recombination mechanism in cosmic plasmas, and to complement existing experimental/theoretical data we have undertaken new, methodical, state-of-the-art calculations of DR rate coefficients (Badnell et. al. A&A 2003) using AUTOSTRUCTURE, a comprehensive suite of atomic structure and collision codes. A significant portion of our efforts is directed at providing reliable DR data for argon-like ions, mainly through various in-depth investigations, and we will present the latest results for Ni XI. Recent astrophysical interests in Ni XI ions range from SXR spectra analysis of the bright nearby F-type star Procyon (Raassen et. al. A&A 2002) or Alpha Centauri's corona by Chandra-LETGS (Raassen et. al. A&A. 2003), to improved modeling of the Sun's EUV irradiance, to derivation of element abundances using a set of F-K dwarfs sampled from the young open cluster IC 4665 (Shen et. al. ApJ 2005). Computations of atomic data for Ni XI, as a potentially valuable diagnostic tool, are scarce in the literature and our multi-configuration Breit-Pauli calculations represent a significant improvement over outdated DR data. Maxwellian DR rate coefficients for Ni XI, resolved into 3-3 and 3-4 core-excitations and covering typical photoionized and electron-collisional plasma temperature ranges, will be presented in a convenient functional form for ease of implementation into plasma modeling codes.
This work was funded in part by NASA (APRA), NASA (SHP) SR&T and UK PPARC grants.
Badnell Nigel R.
Gorczyca Tom
Nikolić Danko
Savin Daniel Wolf
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