The Collisional Atomic Processes of Rydberg Hydrogen and Helium Atoms: Astrophysical Relevance

Abstract

Abstract:Elementary processes in astrophysical environments traditionally attract researchers' attention. We present the data needed for the inclusion of the specific atomic collisional processes in the investigation of the optical and kinetic properties of weakly ionized stellar atmosphere layers. The first type of processes are collisional ionisation (chemi-ionization) processes, and the second ones are excitation and de-excitation (i.e., (n − n )-mixing processes). We give the rate coefficients of the aforementioned processes for the conditions that exist in the solar photosphere, the atmosphere of DB white dwarfs, M-type red dwarfs, etc.

Databases for collisional and radiative processes in small molecules needed for spectroscopy use in astrophysics

“…The database is hosted at the Belgrade Astronomical Observatory, http://servo.aob.rs (Jevremović et al, 2009). The corresponding data are important for exploring the dense molecular clouds in the interstellar medium (ISM), surfaces of small bodies and satellites in our Solar System, modeling of different stellar atmospheres (see the papers Srećković et al 2018;Vujčić et al 2015). Collections of such data sets are as well important for the early Universe chemistry and also for understanding the molecular origins of life (Tielens, 2013;Mason et al, 2014).…”

“…from Srećković et al 2017a) and its role in exploring of the interstellar medium, the early Universe chemistry as well as the modeling of different stellar atmospheres (see e.g. Coppola et al, 2013;Babb, 2015;Srećković et al, 2018).…”

Dynamic Instability of Rydberg Atomic Complexes

“…Figure 3). The further development of the Fermi approach [45][46][47], the so-called dipole resonance ionization (DRI), has found wide application in the solution of a diverse range of problems (see, for example, the review [13]) from the broadening and shift of spectral lines to the balance of ionization processes in the solar photosphere (see, for example, [25,48]).…”

“…A fundamental contribution to "Rydberg Physics" was made by Fermi [44], who proposed considering the quasimolecular formation of A * * 2 as a structure that consists of two positively charged atomic cores A + , a quasi-free Rydberg electron (RE) e − nl in the Keplerian orbit, and the generalized valence electron e − (see Figure 3). The further development of the Fermi approach [45][46][47], the so-called dipole resonance ionization (DRI), has found wide application in the solution of a diverse range of problems (see, for example, the review [13]) from the broadening and shift of spectral lines to the balance of ionization processes in the solar photosphere (see, for example, [25,48]).…”

Photoionization of the alkali molecular ions in geo-cosmical plasmas

“…For the helium-rich white dwarf atmospheres A designate He(1s 2 ) and B H(1s), and eventually oxygen or carbon (Ignjatović et al, 2009;Mihajlov et al, 2013). Recently, Srećković et al (2017Srećković et al ( , 2018 show the importance of including the symmetric processes (1) with A = H(1s) in the solar atmosphere models like Fontenla et al (2006). Also, for modeling the DB white dwarf atmospheres results for case A = He(1s 2 ) have been used (Koester, 2010).…”