Cometary and bipolar ultracompact HII regions

Details Cometary and bipolar ultracompact HII regions Cometary and bipolar ultracompact HII regions

Jul 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.298...33r&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 298, Issue 1, pp. 33-41.

Astronomy and Astrophysics

Astronomy

23

Hydrodynamics, Shock Waves, Stars: Mass-Loss, Hii Regions, Ism: Structure

Scientific paper

Mass-loaded models can explain how a cometary morphology, ultracompact HII region can arise around a stationary star. The star is located in a density gradient in the mass-loading sources. Continuous mass-loss from the clumps embedded in the ionized gas allows the region to remain compact. The wind and radiation field from the central star set up a fully supersonic flow that is bounded by a recombination front. We develop the models further by calculating the velocity and density structure in detail for a variety of viewing angles, mass-loading laws and density scaleheights. The results are compared with observational work, and the agreements and differences are highlighted. We extend this model to show how a massive star located in a dense molecular ridge can give rise to a bipolar or ring morphology, depending on the viewing angle.

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