K-shell spectroscopy in hot plasmas: Stark effect, Breit interaction and QED corrections

Abstract

The broadening of lines by Stark effect is widely used for inferring electron density and temperature in plasmas. Stark-effect calculations often rely on atomic data (transition rates, energy levels,...) not always exhaustive and/or valid only for isolated atoms. In this work, we first present a recent development in the detailed opacity code SCO-RCG for K-shell spectroscopy. The approach is adapted from the work of Gilles and Peyrusse. Neglecting non-diagonal terms in dipolar and collision operators, the line profile is expressed as a sum of Voigt functions associated to the Stark components. The formalism relies on the use of parabolic coordinates and the relativistic fine structure of Lyman lines is included by diagonalizing the hamiltonian matrix associated to quantum states having the same principal quantum number n. The SCO-RCG code enables one to investigate plasma environment effects, the impact of the microfield distribution, the decoupling between electron and ion temperatures and the role of satellite lines (such as Li-like 1snℓn ′ ℓ ′ −1s 2 nℓ, Be-like, etc.). Atomic structure calculations have reached levels of accuracy which require evaluation of Breit interaction and many-electron quantum electro-dynamics (QED) contributions. Although much work was done for QED effects (self-energy and vacuum polarization) in hydrogenic atoms, the case of an arbitrary number of electrons is more complicated. Since exact analytic solutions do not exist, a number of heuristic methods have been used to approximate the screening of additional electrons in the self-energy part. We compare different ways of including such effects in atomic-structure codes (Slater-Condon, Multi-Configuration Dirac-Fock, etc.).

High Resolution Photoexcitation Measurements Exacerbate the Long-Standing Fe XVII Oscillator Strength Problem

“…Moreover, 3C and 3D with their, among many transitions, strong absorption and emission rates can also dominate the Planck and Rosseland mean opacity of hot plasmas [64][65][66]. Therefore, an accurate determination of their oscillator strengths may help elucidating the iron opacity issue [12,14,67], if, e.g., Rosseland mean opacity models [68,69] were found to use predicted oscillator strengths also in departure from experiments. Our result exposes in simplest dipole-allowed transitions of Fe XVII a far greater issue, namely, the persistent problems in the best approximations in use, and calls for renewed efforts in further developing the theory of many-electron systems.…”

Detailed opacity calculations for astrophysical applications

“…where Z eff takes into account screening by the other electrons. Such an approach is not as accurate as Welton's approach [104], but provides satisfactory results, when the effective charges are deduced from the average radius of the n j orbital [105]. We can see in Fig.…”

Detailed Opacity Calculations for Astrophysical Applications

“…Such an approach is not as accurate as Welton's approach [104], but provides satisfactory results, when the effective charges are deduced from the average radius of the n j orbital [105]. We can see in Figure 23 that the shift due to Breit and QED correction is of the order of 2 eV.…”