Electron-Ion Recombination Rate Coefficients and Photoionization Cross Sections for Astrophysically Abundant Elements. X. Ne VIII and Ne IX for Ultraviolet and X-Ray Modeling

Details Electron-Ion Recombination Rate Coefficients and Photoionization Cross Sections for Astrophysically Abundant Elements. X. Ne VIII and Ne IX for Ultraviolet and X-Ray Modeling Electron-Ion Recombination Rate Coefficients and Photoionization Cross Sections for Astrophysically Abundant Elements. X. Ne VIII and Ne IX for Ultraviolet and X-Ray Modeling

Feb 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006apjs..162..417n&link_type=abstract

The Astrophysical Journal Supplement Series, Volume 162, Issue 2, pp. 417-427.

Astronomy and Astrophysics

Astronomy

7

Atomic Data, Atomic Processes, Line: Formation, X-Rays: General

Scientific paper

Results are presented for the inverse processes of photoionization and electron-ion recombination of (hν+Ne VIII<-->Ne IX+e) and (hν+Ne IX<-->Ne X+e) using the self-consistent unified method. The method employs an identical wave function expansion for both photoionization and recombination, and it includes both radiative and dielectronic recombination. Total, as well as level-specific, photoionization cross sections, σPI(E nSLJ), and recombination rate coefficients, αR(T nSLJ), are presented for all fine-structure levels up to n<=10. These correspond to a total of 98 bound fine-structure levels of Ne VIII with 1/2<=J<=17/2, and 178 bound levels of Ne IX with 0<=J<=10. Total recombination cross sections and rates as functions of electron energy are also presented. The coupled channel wave function expansions for the core ions include 17 levels of Ne IX and 16 levels of Ne X. Relativistic fine structure is considered through the Breit-Pauli R-matrix (BPRM) method. The photoionization and recombination cross sections include important atomic effects such as radiation damping, channel coupling, and interference and should be of definitive accuracy. Level-specific σPI(nSLJ) and αR(T nSLJ) are calculated for the first time. In addition, we describe the applicability of these comprehensive data sets to not only ionization balance and recombination-cascade models for astrophysical and laboratory plasmas, but also to (1) models of UV and X-ray lines in He-like ions from C V to Ne IX involving the 2 3Po0,1,2-->2 3S1 allowed triplet transitions in the UV, and 2(1Po1, 3Po1,2, 3S1)-->1 1S0 allowed, intercombination, and forbidden transitions in the X-ray, and (2) calculation of dielectronic satellite intensities from the highly resolved resonances in the unified recombination cross sections of He-like and Li-like ions through straightforward integration over a Maxwellian or other electron distribution functions.

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