Possibility of detecting fine-structure lines of atomic hydrogen in H II regions

Details Possibility of detecting fine-structure lines of atomic hydrogen in H II regions Possibility of detecting fine-structure lines of atomic hydrogen in H II regions

Apr 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987pazh...13..285e&link_type=abstract

Pis'ma v Astronomicheskii Zhurnal (ISSN 0320-0108), vol. 13, April 1987, p. 285-295. In Russian. In Russian.

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Computational Astrophysics, Emission Spectra, Fine Structure, Hydrogen Atoms, Hydrogen Clouds, Line Spectra, Absorption Spectra, Brightness Temperature, Optical Thickness, Orion Nebula, Quantum Numbers, Thermodynamic Equilibrium

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The emission of hydrogen lines due to transitions between fine structure levels with small principal quantum number n is considered. The population of the fine structure levels with n = 2 is calculated. The 22S1/2 level is more populated than the 22P1/2 and 22P3/2 in H II regions because of its metastability. The product bβ, that is the ratio of the actual optical depth of the line to the thermal equilibrium value, gives a measure of the stimulated emission or enhanced absorption due to non-LTE effects and is very high. The line brightness temperature TL and the line-to-continuum ratio TL/TC are calculated for the Orion Nebula.

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