The velocity structure of the cometary H II regions G13.87+0.28, G32.80+ 0.19B, and G61,48+0.09B1

Details The velocity structure of the cometary H II regions G13.87+0.28, G32.80+ 0.19B, and G61,48+0.09B1 The velocity structure of the cometary H II regions G13.87+0.28, G32.80+ 0.19B, and G61,48+0.09B1

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...429..268g&link_type=abstract

The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 429, no. 1, p. 268-284

Astronomy and Astrophysics

Astronomy

37

Cometary Atmospheres, H Ii Regions, Kinematics, Molecular Clouds, Morphology, Radio Astronomy, Stellar Winds, Astronomical Models, Ionized Gases, Local Thermodynamic Equilibrium, Shock Waves

Scientific paper

We present H92 alpha radio recombination line and radio continuum observations toward three cometary-like H II regions, G13.87 + 0.28, G32.80 + 0.19B, and G61.48 + 0.09B1, with an angular resolution of approximately 2 arcsec. The kinematics (H92 alpha velocity and line-widths fields) and morphology (continuum maps) of the ionized gas from two of these sources, G32.80 + 0.19B and G61.48 + 0.09B1, are best explained by models in which the ionized gas is expanding in an anisotropic medium (champagne models), wheras that of G13.87 + 0.28 can be well explained in terms of a bow shock formed by the stellar wind of a massive star moving supersonically through a molecular cloud. As predicted theoretically, we find that at the frequency of the H92 alpha line (non-LTE) effects are significant, particularly for the compact, high emission measure H II regions we detected in the directed of two cometary regions.

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