ELECTRON IMPACT DISSOCIATION X (1)Sigma(+)(g) -˃ b (3)Sigma(+)(u) AND EXCITATIONS X (1)Sigma(+)(g) -˃ a (3)Sigma(+)(g) AND X (1)Sigma(+)(g) -˃ B (1)Sigma(+)(u) OF MOLECULAR HYDROGEN IN NONTHERMAL ASTROPHYSICAL PLASMAS
- Title
- ELECTRON IMPACT DISSOCIATION X (1)Sigma(+)(g) -˃ b (3)Sigma(+)(u) AND EXCITATIONS X (1)Sigma(+)(g) -˃ a (3)Sigma(+)(g) AND X (1)Sigma(+)(g) -˃ B (1)Sigma(+)(u) OF MOLECULAR HYDROGEN IN NONTHERMAL ASTROPHYSICAL PLASMAS
- Author
- 정영대
- Issue Date
- 2013-02
- Publisher
- IOP PUBLISHING LTD
- Citation
- The Astrophysical journal, Supplement series, 204, 2, 18
- Abstract
- We investigate the electronic transitions X 1Σ+ g → b 3Σ u +, X 1Σ+ g → a 3Σ g +, and X 1Σ+ g → B 1Σ u + of molecular hydrogen by studying electron impacts in astrophysical Lorentzian plasmas. Useful fitting formulae for the X 1Σ+ g → b 3Σ u +, X 1Σ+ g → a 3Σ g +, and X 1Σ+ g → B 1Σ u + excitation cross sections are employed in order to obtain the electronic excitation rate coefficients of H2 as functions of the spectral index and temperature. In low-temperature regions, it is found that the excitation rate coefficients $R_{b\,{}^3\Sigma _u^ + }$, $R_{a\,{}^3\Sigma _g^ + }$, and $R_{B\,{}^1\Sigma _u^ + }$ of H2 in non-Maxwellian plasmas are smaller than those in Maxwellian plasmas. However, in high-temperature regions, the excitation rate coefficients of H2 in non-Maxwellian plasmas are greater than those in Maxwellian plasmas. It is also shown that the X 1Σ+ g → b 3Σ u + excitation rate coefficient is the main contributor in low-temperature regions. In contrast, it is found that the X 1Σ+ g → B 1Σ u + electronic excitation is dominant in high-temperature regions.
- URI
- http://iopscience.iop.org/article/10.1088/0067-0049/204/2/18/meta
- DOI
- 10.1088/0067-0049/204/2/18
- Appears in Collections:
- GRADUATE SCHOOL[S](대학원) > ETC
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