Discussion of papers on structure and dynamics of HII regions:
How to get a particular bibtex entry:
e.g., http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1978A%26A....70..769I&data_type=BIBTEX
How to get a load of bibtex entries
http://adsabs.harvard.edu/cgi-bin/abs_connect?author=henney,+w.&data_type=BIBTEX
A Study of Bright Rims in Diffuse Nebulae
1956BAN....13...77P.pdf
This talks about bright rims in 34 HII regions. They typically have density contrasts of 7 to 23 wrt the mean density of the region. He has little maps of them all and classifies their appearance. More convex rims tend to be closer to the ionizing star.
This is more-or-less consistent with our models, in which concavity tends to increase with time. Interestingly, he suggests that the evolutionary sequence is the opposite.
HII Regions and CO Clouds: The Blister Model
1978A+A____70__769I.pdf
Compares radio observations of CO clouds and HII regions and concludes that they are all "blister flows" - seems to be the first occurrence in literature of this term. His main line of evidence is radio morphology (core-halo structure) and the mean blueshift of 5 km/s between ionized and molecular gas for optically visible regions. For obscured regions he gets no net velocity shift, suggesting they are obscured by unrelated material along the line of sight rather (otherwise they should show a net redshift).
Evolution of Diffuse Nebulae
1969ARA+A___7___67M.pdf
The Time Evolution of a Globule Immersed in an HII Region
1977A&A....54..517T.pdf
Similar to Bertoldi, but earlier.
The gas dynamics of H II regions. I - The champagne model
1979A&A....71...59T
The original paper, with a 1-d plane-parallel density discontinuity.
The gas dynamics of H II regions. II - Two-dimensional axisymmetric calculations
1979ApJ...233...85B
The gasdynamics of H II regions. IV - The champagne phase and the propagation of ionization fronts into dense clouds
1981A&A....98...85B
This seems to be the one that is most relevant to our work.
They have 1-d plane-parallel models with a high density on one side and a low density on the other. They are mainly studying the non-steady evolution of things. When the champagne flow breaks out on the RHS, then a rarefaction wave travels toward the IF on the RHS and causes the material to flow away from the IF.
Still it is nothing like our models in that it never gets to a steady flow pattern. Never shows anything like our density and velocity profil either.
The Gasdynamics of HII Regions: V. The interaction of Weak R ionization Fronts with Dense Clouds
1981A&A....99..305T
Plane-parallel calculation that tries to explain bright rims as due to dense obstacles on the side of the star away from the molecular cloud in a champagne flow. Only seems to be able to reproduce the bright rim properties if the ionizing flux is increasing with time (as it is in the case of a champagne flow that is breaking out of the cloud).
The gas dynamics of H II regions. VI - H II regions in collapsing massive molecular clouds
1982A&A...108...25Y
The effects of the coronal gas on the champagne phase
1982A&A...115..207T
The formation and evolution of bright rims
1984A&A...135...81B
This is a follow up to 1981A&A....99..305T that uses much-improved numerical resolution and also considers spherical geometry. They contradict much of the findings of the previous paper - they now can produce bright rims with a constant ionizing flux. They say that the flow in the ionized gas is not steady - this may be because their shock is propagating into the undisturbed neutral gas at nearly the ionized sound speed.
The evolution of HII regions in disk-like clouds. The appearance of neutral high velocity outflows
1989RMxAA..18...65F
On the formation and expansion of H II regions
1990ApJ...349..126F
The Disruption of Molecular Cloud Cores by Photoionization
1995ApJ...451..210R
This calculates the line profiles of Hα and [O III] for spherical 1-d champagne flows. They get fast shocks going into the low density medium and the formation of interesting line profiles, especially for OIII.
From Ultracompact to Extended H II Regions
1996ApJ...469..171G
Talks about formation of elephant-trunk like structures by means of thin-shell instabilities.
On the Large Escape of Ionizing Radiation from Giant Extragalactic H II Regions
2002ApJ...565L..79C
Find that 10%-73% of the Lyman continuum radiation escapes from nebulae. Sort of consistent with my models.
Dynamical evolution of wind-driven HII regions in strong density gradients
1997A&A...326.1195C
Self-similar Champagne Flows in H II Regions
2002ApJ...580..969S
A bit of an odd paper. They do 1-d spherical models of completely ionized cloud cores with various density distributions and derive semi-analytic models for their champagne evolution. Not surprisingly, they find that they don't last very long.