The radio recombination line spectrum of Orion A - Observations and analysis

Details The radio recombination line spectrum of Orion A - Observations and analysis The radio recombination line spectrum of Orion A - Observations and analysis

Oct 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...201..134l&link_type=abstract

Astrophysical Journal, vol. 201, Oct. 1, 1975, pt. 1, p. 134-150.

Other

41

H Lines, Hydrogen Recombinations, Nebulae, Radiative Recombination, Radio Spectra, Spectral Line Width, Astronomical Models, Data Reduction, Electron Density (Concentration), Line Shape, Orion Constellation

Scientific paper

On the basis of a large body of radio observations of Orion A, it is shown that temperature and density can be derived from the ratio of peak recombination line intensity to the intensity in the adjacent continuum and from the line width of the hydrogen radio recombination lines. It is demonstrated that the intensity ratio and the line width can be accurately determined in the low-frequency observations even when erroneous baselines are used, that a density gradient must exist in the nebula, and that the isothermal models cannot reproduce the observed line strengths, i.e., the densest parts of the nebula must be somewhat cooler than the surrounding gas.

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