OSU Navigation Bar

The Ohio State University University Libraries Knowledge Bank

Electron-Ion Recombination Rate Coefficients and Photoionization Cross Sections for Astrophysically Abundant Elements. V. Relativistic Calculations for Fe XXIV and Fe XXV for X-Ray Modeling

Please use this identifier to cite or link to this item: http://hdl.handle.net/1811/44618

Show full item record

Files Size Format View
apjs-rrc-fe24-fe26.pdf 621.9Kb PDF View/Open

Title: Electron-Ion Recombination Rate Coefficients and Photoionization Cross Sections for Astrophysically Abundant Elements. V. Relativistic Calculations for Fe XXIV and Fe XXV for X-Ray Modeling
Creators: Nahar, Sultana Nurun; Pradhan, Anil K.; Zhang, Hong Lin
Keywords: atomic data
atomic processes
line -- formation
X-rays -- general
Issue Date: 2001-03
Citation: Nahar, Sultana Nurun, Pradhan, Anil K., Zhang, Hong Lin. "Electron-Ion Recombination Rate Coefficients and Photoionization Cross Sections for Astrophysically Abundant Elements. V. Relativistic Calculations for Fe XXIV and Fe XXV for X-Ray Modeling," The Astrophysical Journal Supplement Series, v. 133, March, 2001, pp. 255-267.
DOI: 10.1086/319187
Abstract: Photoionization and recombination cross sections and rate coefficients are calculated for Li-like Fe XXIV and He-like Fe XXV using the Breit-Pauli R-matrix (BPRM) method. A complete set of total and level-specific parameters is obtained to enable X-ray photoionization and spectral modeling. The ab initio calculations for the unified (e + ion) recombination rate coefficients include both the nonresonant and the resonant recombination (radiative and dielectronic recombination, RR and DR, respectively) for (e + Fe XXV) → Fe XXIV and (e + Fe XXVI) → Fe XXV. The level-specific rates are computed for all fine-structure levels up to n = 10, enabling accurate computation of recombination-cascade matrices and effective rates for the X-ray lines. The total recombination rate coefficients for both Fe XXIV and Fe XXV differ considerably from the sum of RR and DR rates currently used to compute ionization fractions in astrophysical models. As the photoionization/recombination calculations are carried out using an identical eigenfunction expansion, the cross sections for both processes are theoretically self-consistent; the overall uncertainty is estimated to be about 10%-20%. All data for Fe XXIV and Fe XXV (and also for H-like Fe XXVI, included for completeness) are available electronically.
Description: Relevant data is available at: http://www.astronomy.ohio-state.edu/~nahar/nahar_radiativeatomicdata/index.html
ISSN: 0067-0049
URI: http://hdl.handle.net/1811/44618
Rights: © 2001. The American Astronomical Society. All rights reserved.
Bookmark and Share