Photoionization and Electron–Ion Recombination in Astrophysical Plasmas

Abstract

Photoionization and its inverse, electron–ion recombination, are key processes that influence many astrophysical plasmas (and gasses), and the diagnostics that we use to analyze the plasmas. In this review we provide a brief overview of the importance of photoionization and recombination in astrophysics. We highlight how the data needed for spectral analyses, and the required accuracy, varies considerably in different astrophysical environments. We then discuss photoionization processes, highlighting resonances in their cross-sections. Next we discuss radiative recombination, and low and high temperature dielectronic recombination. The possible suppression of low temperature dielectronic recombination (LTDR) and high temperature dielectronic recombination (HTDR) due to the radiation field and high densities is discussed. Finally we discuss a few astrophysical examples to highlight photoionization and recombination processes.

Current stage and future development of Belgrade collisional and radiative databases/datasets of importance for molecular dynamics

“…3), rate coefficients for non-local thermal equilibrium models and feed into models of various atmospheres, laboratory plasmas and are used in several technological applications. [68][69][70][71][72][73] The MolD database was developed in several stages. The first one, which was finished at the end of 2014, was distinguished by the development of a web interface, certain utility programs, and a service for all photodissociation data for hydrogen and helium molecular ions.…”

“…3), rate coefficients for non-local thermal equilibrium models and feed into models of various atmospheres, laboratory plasmas and are used in several technological applications. 68–73…”