The structure and dynamics of H2 regions

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Emission Spectra, H Lines, Interstellar Radiation, Spectrum Analysis, Cosmic Dust, Ionization, Shock Fronts, Shock Layers

Scientific paper

The early evolution of H2 regions, through the first few 100,000 years, is investigated under conditions of enhanced central density and increasing cluster luminosity. It is found that a D type ionization front can overtake the precursor shock under conditions of a fairly steep density-gradient such as may exist just beyond a stellar dust cocoon, or as new stars turn on within the H2 region. The shock is converted into a strong, outward moving pressure pulse as it is ionized. Rayleigh-Taylor instability in the shocked layer occurs as the ionization front approaches the shock, but the neutral globules so produced have a comparatively small and short term effect on nebular dynamics. The evolutionary effects of different recombination rates within the ionization front and different cooling rates within the shocked layer are investigated and found to be small. Possible modifications which the presence of dust or stellar winds could produce are briefly considered.

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