Symmetric Atom–Atom and Ion–Atom Processes in Stellar Atmospheres
Abstract
:1. Introduction
- the case of hydrogen, when and ,
- the case of helium, when and .
2. Chemi-Ionization and Chemi-Recombination Processes
2.1. Solar Atmosphere
2.2. Atmospheres of the DB White Dwarfs.
2.3. Chemi-Ionization Processes in Solar and DB White-Dwarf Atmospheres in the Presence of Mixing Channels
2.4. The Atmospheres of Late Type Dwarfs (M Red Dwarfs)
2.5. Influences of Chemi-Ionization/Recombination Processes on the Hydrogen Spectral Lines in the M Red Dwarf Atmosphere
3. Symmetric Ion–Atom Processes
3.1. Solar Atmosphere: Visible Wavelength Region
3.2. Solar Atmosphere: UV and VUV Wavelength Region
3.3. DB White Dwarf Atmospheres: Visible Wavelength Region
3.4. DB White Dwarf Atmospheres: UV and VUV Wavelength Region
4. Conclusions
Acknowledgments
Author Contributions
Conflicts of Interest
References
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Srećković, V.A.; Ignjatović, L.M.; Dimitrijević, M.S. Symmetric Atom–Atom and Ion–Atom Processes in Stellar Atmospheres. Atoms 2018, 6, 1. https://doi.org/10.3390/atoms6010001
Srećković VA, Ignjatović LM, Dimitrijević MS. Symmetric Atom–Atom and Ion–Atom Processes in Stellar Atmospheres. Atoms. 2018; 6(1):1. https://doi.org/10.3390/atoms6010001
Chicago/Turabian StyleSrećković, Vladimir A., Ljubinko M. Ignjatović, and Milan S. Dimitrijević. 2018. "Symmetric Atom–Atom and Ion–Atom Processes in Stellar Atmospheres" Atoms 6, no. 1: 1. https://doi.org/10.3390/atoms6010001