Query : 2004A&A...424..877G

2004A&A...424..877G - Astronomy and Astrophysics, volume 424, 877-885 (2004/9-4)

Propagation of ionizing radiation in HII regions: The effects of optically thick density fluctuations.


Abstract (from CDS):

The accepted explanation of the observed dichotomy of two orders of magnitude between in situ measurements of electron density in HII regions, derived from emission line ratios, and average measurements based on integrated emission measure, is the inhomogeneity of the ionized medium. This is expressed as a ``filling factor", the volume ratio of dense to tenuous gas, measured with values of order 10–3. Implicit in the filling factor model as normally used, is the assumption that the clumps of dense gas are optically thin to ionizing radiation. Here we explore implications of assuming the contrary: that the clumps are optically thick. A first consequence is the presence within HII regions of a major fraction of neutral hydrogen. We estimate the mean H°/H+ ratio for a population of HII regions in the spiral galaxy NGC 1530 to be the order of 10, and support this inference using dynamical arguments. The optically thick clumpy models allow a significant fraction of the photons generated by the ionizing stars to escape from their HII region. We show, by comparing model predictions with observations, that these models give an account at least as good as, and probably better than that of conventional models, of the radial surface brightness distribution and of selected spectral line diagnostics for physical conditions within HII regions. These models explain how an HII region can appear, from its line ratios, to be ionization bounded, yet permit a major fraction of its ionizing photons to escape.

Abstract Copyright:

Journal keyword(s): ISM: general - ISM: HII regions - ISM: clouds - methods: numerical

Simbad objects: 3

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Number of rows : 3
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
1 M 33 GiG 01 33 50.8965749232 +30 39 36.630403128 6.17 6.27 5.72     ~ 5638 1
2 NGC 604 HII 01 34 32.1 +30 47 01           ~ 579 0
3 NGC 1530 G 04 23 27.102 +75 17 44.05   13.40       ~ 268 1

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