Line formation in H II regions during the champagne phase

Details Line formation in H II regions during the champagne phase Line formation in H II regions during the champagne phase

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...138..325y&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 138, no. 2, Sept. 1984, p. 325-332. Research supported by the Universitaets-St

Astronomy and Astrophysics

Astronomy

48

Astronomical Spectroscopy, H Ii Regions, H Lines, Line Shape, Doppler Effect, Electron Density (Concentration), Forbidden Transitions, Frequency Shift, Ion Production Rates, Molecular Clouds, Radio Astronomy

Scientific paper

Line transfer calculations are presented for interpreting complex velocity fields in H II regions detected by radio telescopes. Consideration is focused on hydrogen and forbidden oxygen lines which exhibit an emissivity proportional to the square of the electron density inside the H II region and zero outside. Account is taken of factors such as the ionization rate, recombination, absorption by dust, opacity and the extinction coefficient. Spectral intensity arrays are generated for specific view angles of the champagne phase. Doppler shifts are obtained for intensities in various positions around the central star of the H II region. Typical features of a champagne flow are concluded to be a Doppler shift of no more than 5 km/sec for the ionized gas relative to the outer surface of the ionized cloud, ionized matter flowing away from the molecular cloud, velocity differences of up to 4 km/sec of various components of the nebula, and greater complexity occurring mostly in the low density-bounded periphery of the H II regions.

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