Abstract
The influence of collisional-ionization and recombination processes on spectral line shapes in stellar atmospheres and in the hydrogen clouds in broad-line region of AGNs
Highlights
The processing of line spectra with radiative transfer calculations requires spectroscopic data as well as collisional data
These results cover the regions 2 ≤ n ≤ 20 and 4000 K < T ≤ 20000 K which are relevant for moderately ionized plasma layers in different environments
The fits are valid over the temperature range of 4000 K ≤ T ≤ 20000 K (see Mihajlov et al (2011a); Sreckovic et al (2018a); Sreckovic et al (2018b)). This enables the easy inclusion of these processes in the modeling the very dense parts of the clouds in active galactic nuclei (AGN) broad line region (BLR) and moderately ionized layers of the Sun and solar like stars
Summary
The processing of line spectra with radiative transfer calculations requires spectroscopic data as well as collisional data (e.g., cross sections, rate coefficients, atomic parameters, etc Baron & Hauschildt 1998; Mihajlov et al 2011a; Ignjatovic et al 2014; Sreckovic et al 2018a). If an atom is in a state of sufficiently high principal quantum number n it means that the valence electron is far from the ionic core, and such atom appears hydrogenic. It is commonly accepted to call such atoms as Rydberg atoms with electron excited into a high lying Rydberg state, with large principal quantum number. For Rydberg atoms even inelastic thermal collisions can be sufficiently energetic to lead to ionization reactions (Gnedin et al, 2009; Mihajlov et al, 2012). These types of reactions are collisional ionization processes of associative ionization and the non-associative ionization
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