Bow shock models of ultracompact H II regions

Details Bow shock models of ultracompact H II regions Bow shock models of ultracompact H II regions

Mar 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...369..395m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 369, March 10, 1991, p. 395-409. Research supported by Alan and Dorothy Dav

Astronomy and Astrophysics

Astronomy

116

Astronomical Models, H Ii Regions, Molecular Clouds, Shock Wave Propagation, Stellar Winds, Astronomical Maps, Digital Simulation, Infrared Astronomy Satellite, Interstellar Matter, Milky Way Galaxy, Radiative Transfer

Scientific paper

This paper presents models of ultracompact H II regions as the bow shocks formed by massive stars, with strong stellar winds, moving supersonically through molecular clouds. The morphologies, sizes and brightnesses of observed objects match the models well. Plausible models are provided for the ultracompact H II regions G12.21 - 0.1, G29.96 - 0.02, G34.26 + 0.15, and G43.89 - 0.78. To do this, the equilibrium shape of the wind-blown shell is calculated, assuming momentum conservation. Then the shell is illuminated with ionizing radiation from the central star, radiative transfer for free-free emission through the shell is performed, and the resulting object is visualized at various angles for comparison with radio continuum maps. The model unifies most of the observed morphologies of ultracompact H II regions, excluding only those objects with spherical shells. Ram pressure confinement greatly lengthens the life of ultracompact H II regions, explaining the large number that exist in the Galaxy despite their low apparent kinematic ages.

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