Interpretation of radio recombination line emission from G 0.7-0.0

Details Interpretation of radio recombination line emission from G 0.7-0.0 Interpretation of radio recombination line emission from G 0.7-0.0

Dec 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976a%26a....53..165s&link_type=abstract

Astronomy and Astrophysics, vol. 53, no. 2, Dec. 1976, p. 165-174.

Astronomy and Astrophysics

Astronomy

13

Abundance, Emission Spectra, Galactic Nuclei, Helium Ions, Hydrogen Clouds, Milky Way Galaxy, Radio Astronomy, Hydrogen Ions, Interstellar Masers, Ion Recombination, Line Spectra, Nonequilibrium Conditions, Radio Spectra

Scientific paper

Available radio continuum and hydrogen recombination-line observations of G 0.7-0.0 (Sgr B2) are summarized, and a four-component model of the source is proposed. The peak flux densities predicted by this model are compared with observed values, the model is found to represent the observations well, and it is concluded that the continuum flux density can be represented by a superposition of optically thin and partially opaque thermal components. Parameters of the source components are determined along with various line-to-continuum and He(+)-to-H(+) ratios. The observations are compared with predictions based on the 'geometric effect' and 'external maser' hypotheses. It is shown that neither hypothesis can fully account for all the observations, the geometric effect could probably explain most of them, and an external maser is apparently inconsistent with available data.

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