Low density ionized gas in the inner Galaxy - Interpretation of recombination line observations at 325 MHz

Details Low density ionized gas in the inner Galaxy - Interpretation of recombination line observations at 325 MHz Low density ionized gas in the inner Galaxy - Interpretation of recombination line observations at 325 MHz

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985japa....6..203a&link_type=abstract

Journal of Astrophysics and Astronomy (ISSN 0250-6335), vol. 6, Dec. 1985, p. 203-226.

Astronomy and Astrophysics

Astrophysics

44

Astronomical Spectroscopy, Galactic Structure, Gas Density, Milky Way Galaxy, Rarefied Gases, Atomic Recombination, Electron Density (Concentration), Emission Spectra, H Ii Regions, Ionized Gases, Line Spectra, Nebulae

Scientific paper

The recent survey of the H 272α recombination line (324.99 MHz) in the direction of 34 H II regions, 12 SNRs and 6 regions of continuum minimum ("blank" regions) in the galactic plane is used to derive the properties of diffuse ionized gas in the inner Galaxy. The intensity of radio recombination lines at high frequencies is dominated by spontaneous emission in high-density gas and that at low frequencies by stimulated emission in low-density gas. The author has used this property to obtain the electron density in the gas in the direction of blank regions and SNRs, by combining the H 272α measurements with published data at higher frequencies. The derived properties of the gas are (1) electron density 0.5 - 6 cm-3, (2) electron temperature 3000 - 8000K and (3) emission measures 500 - 3000 pc cm-6. It is suggested that the low-frequency recombination lines arise in low-density envelopes of the observed H II regions.

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