Radiative and Auger Decay Data for Modeling Nickel K Lines

Abstract

Radiative and Auger decay data have been calculated for modeling the K lines in ions of the nickel isonuclear sequence, from Ni + up to Ni 27+ . Level energies, transition wavelengths, radiative transition probabilities, and radiative and Auger widths have been determined using Cowan's Hartree-Fock with relativistic corrections ( HFR) method. Auger widths for the third-row ions ( Ni + YNi 10+ ) have been computed using single-configuration average (SCA) compact formulae. Results are compared with data sets computed with the AUTOSTRUCTURE and MCDF atomic structure codes and with available experimental and theoretical values, mainly in highly ionized ions and in the solid state.

Recent advances in the determination of atomic parameters for modeling K lines in cosmically abundant elements

“…We also note that the general agreement between our different Nickel Ni II-Ni XXVII [21] theoretical approaches seems to improve when increasing the nuclear charge. This is essentially due to the fact that the interaction between n = 2 and n = 3 configuration complexes (considered in our HFR model only) are more important for the lowest ionization stages.…”

Study of the many fluorescent lines and the absorption variability in GX 301−2 withXMM-Newton

“…8 due to the large flux of these lines. The residuals could be very well described with a broad Gaussian absorption (Palmeri et al 2008a). A Gaussian shaped line centered at that energy was used to model the residuals and improved the fit clearly.…”

“…To investigate the possibility of such a shift we froze the line energies of all measured elements to the values of their respective neutral line energy, with values taken from Palmeri et al (2008b) for S, Ar, and Ca, Kaastra & Mewe (1993) for Cr, Kallman et al (2004) for Fe, and Palmeri et al (2008a) for Ni. We then applied a gainshift kernel, shifting the model counts spectrum energy grid according to E new (c) = E old (c)/gainshift.…”

Atomic decay data for modeling the Al K lines

“…Following the work by Palmeri et al (2002Palmeri et al ( , 2003a, Bautista et al (2003Bautista et al ( , 2004, Mendoza et al (2004), and Kallman et al (2004) on the Fe K lines, by García et al (2005) on the K-shell photoabsorption of O ions, by Palmeri et al (2008a) on the Ne, Mg, Si, S, Ar, and Ca K lines, by Palmeri et al (2008b) on the Ni K lines, and our recent studies of the K-shell photoionization and photoabsorption of N, Ne, Mg, Si, Ar, and Ca (García et al 2009;Witthoeft et al 2009), we report new atomic data for the K-vacancy levels in the aluminum isonuclear sequence. The main goals are to improve the atomic database of the XSTAR modeling code and to prepare ionic targets (configuration expansions and orbitals) for the lengthy computations of the K-shell photoabsorption and…”