Argon 1s(-2) Auger hypersatellites

The 1s(-2) Auger hypersatellite spectrum of argon is studied experimentally and theoretically. In total, three transitions to the final states 1s(-1)2p(-2)(S-2(e),D-2(e)) and 1s(-1)2s(-1)(S-1)2p(-1)(P-2(o)) are experimentally observed. The lifetime broadening of the 1s(-2) -> 1s(-1)2p(-2)(S-2(e),D-2(e)) states is determined to be 2.1(4) eV. For the used photon energy of h nu = 7500 eV a KK/K ionisation ratio of 2.5(3) x 10(-4) is derived. Generally, a good agreement between the experimental and present theoretical energy positions, linewidths, and intensities is obtained

The 1s → 2p resonance photoionization from the low-lying states of O

Thirty-state close-coupling calculations have been performed for the photoionization of O+ near the $1s\rightarrow2p$ resonance energy region from the terms belonging to the configurations of $1s^22s^22p^3$ and $1s^22s2p^4$. Total and partial photoionization cross-section and the contributions of the main ionization channels to the partial cross-section are calculated to obtain the resonance energies, autoionization widths and Auger branching ratios of the $1s\rightarrow2p$ core-excited states. The resonance oscillator strengths of the $1s\rightarrow2p$ transitions are also obtained by integrating the photoionization cross-section. The radiative widths of the $1s\rightarrow2p$ transitions can be obtained from the oscillator strengths. The results show that the radiative widths are generally three orders of magnitude smaller than the corresponding autoionization widths and therefore contributes little to the natural widths

Screening potential and continuum lowering in a dense plasma under solar-interior conditions

An accurate description of the screening potential induced by a hot, dense plasma is a fundamental problem in atomic physics and plasma physics, and it plays a pivotal role in the investigation of microscopic atomic processes and the determination of macroscopic physical properties, such as opacities and equations of state as well as nuclear fusion cross sections. Recent experimental studies show that currently available analytical models of plasma screening have difficulty in accurately describing the ionization-potential depression, which is directly determined by the screening potential. Here, we propose a consistent approach to determine the screening potential in dense plasmas under solar-interior conditions from the free-electron micro-space distribution. It is assumed that the screening potential for an ion embedded in a dense plasma is predominately determined by the free electrons in the plasma. The free-electron density is obtained by solving the ionization-equilibrium equation for an average-atom model to obtain the average degree of ionization of the plasma. The proposed model was validated by comparing the theoretically predicted ionization-potential depression of a solid-density Si plasma with recent experiments. Our approach was applied to investigate the screening potential and ionization-potential depression of Si plasmas under solar-interior conditions over a temperature range of 150–500 eV and an electron-density range of 5.88 × 1022–3.25 × 1024 cm−3. It can be easily incorporated into atomic-structure codes and used to investigate basic atomic processes, such as photoionization, electron-ion collisional excitation and ionization, and Auger decay, in a dense plasma