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A comprehensive set of UV and x-ray radiative transition rates for Fe XVI

Please use this identifier to cite or link to this item: http://hdl.handle.net/1811/45085

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Title: A comprehensive set of UV and x-ray radiative transition rates for Fe XVI
Creators: Nahar, Sultana Nurun; Eissner, W.; Sur, C.; Pradhan, A. K.
Issue Date: 2009
Citation: Nahar, Sultana Nurun, Eissner, W., Sur, C., Pradhan, A. K., "A comprehensive set of UV and x-ray radiative transition rates for Fe XVI," Physica Scripta, 79 (2009) 35401
DOI: 10.1088/0031-8949/79/03/035401
Abstract: Sodium-like Fe XVI is observed in collisionally ionized plasmas such as stellar coronae and coronal line regions of active galactic nuclei including black hole-accretion disc environments. Given its recombination edge from neon-like Fe XVII at ~25 Å, the Fe XVI bound-bound transitions lie in the soft x-ray and EUV (extreme ultraviolet) range. We present a comprehensive set of theoretical transition rates for radiative dipole allowed E1 transitions including fine structure for levels with nℓ(SLJ) ≤ 10, ℓ ≤ 9 using the relativistic Breit-Pauli R-matrix (BPRM) method. In addition, forbidden transitions of electric quadrupole (E2), electric octupole (E3), magnetic dipole (M1) and magnetic quadrupole (M2) type are presented for levels up to 5g(SLJ) from relativistic atomic structure calculations in the Breit-Pauli approximation using code SUPERSTRUCTURE. Some of the computed levels are autoionizing, and oscillator strengths among those are also provided. BPRM results have been benchmarked with the relativistic coupled cluster method and the atomic structure Dirac-Fock code GRASP. Levels computed with the electron collision BPRM codes in bound state mode were identified with a procedure based on the analysis of quantum defects and asymptotic wavefunctions. The total number of Fe XVI levels considered is 96, with 822 E1 transitions. Tabulated values are presented for the oscillator strengths f, line strengths S and Einstein radiative decay rates A. This extensive dataset should enable spectral modelings up to highly excited levels, including recombination-cascade matrices.
ISSN: 0031-8949
URI: http://hdl.handle.net/1811/45085
Rights: © The Royal Swedish Academy of Sciences
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