Kenneth Wood

Publications (2)0 Total impact

• Article: Three dimensional geometries and the analysis of H II regions

  Kenneth Wood, J. E. Barnes, Barbara Ercolano, L. M. Haffner, R. J. Reynolds, J. Dale
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  ABSTRACT: We compare emission line intensities from photoionization models of smooth and fractal shell geometries for low density H II regions, with particular focus on the low-ionization diagnostic diagram [N II]/H-alpha vs H-alpha. Building on previously published models and observations of Barnard's Loop, we show that the observed range of intensities and variations in the line intensity ratios may be reproduced with a three dimensional shell geometry. Our models adopt solar abundances throughout the model nebula, in contrast with previous one dimensional modeling which suggested the variations in line intensity ratios could only be reproduced if the heavy element abundances were increased by a factor of 1.4. For spatially resolved H II regions, the multiple sightlines that pierce and sample different ionization and temperature conditions within smooth and fractal shells produce a range of line intensities that are easily overlooked if only the total integrated intensities from the entire nebula model are computed. Our conclusion is that inference of H II region properties, such as elemental abundances, via photoionization models of one dimensional geometries must be treated with caution and further tested through three dimensional modeling.
  04/2013;
• Source

  Available from: L. Matthew Haffner

  Article: Estimating the Porosity of the Interstellar Medium from Three-Dimensional Photoionization Modeling of H II Regions

  Kenneth Wood, L. M. Haffner, R. J. Reynolds, John Mathis, Greg Madsen
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  ABSTRACT: We apply our three dimensional photoionization code to model Wisconsin H-alpha Mapper observations of the H II region surrounding the O9.5V star Zeta Oph. Our models investigate the porosity of the interstellar medium around zeta Oph and the effects of 3D densities on the H-alpha surface brightness and variation in the [N II]/H-alpha line ratio. The Zeta Oph H II region has a well characterized ionizing source, so it is an excellent starting point for 3D models of diffuse ionized gas. We investigate various hierarchically clumped density structures, varying the overall smoothness within the clumping algorithm. By simulating the observations, we can estimate the porosity of the medium in the vicinity of Zeta Oph and find that within the context of our hierarchically clumped models, around 50% to 80% of the volume is occupied by clumps surrounded by a low density smooth medium. We also conclude that in order for O stars to ionize the diffuse Warm Ionized Medium, the O star environment must be more porous than that surrounding Zeta Oph, with clumps occupying less than one half of the interstellar volume. Our clumpy models have irregular boundaries, similar to observed H II regions. However, in observed H II regions it is difficult to identify the precise location of the boundary because of the foreground and/or background emission from the widespread Warm Ionized Medium. This complicates the interpretation of the predicted rapid rise of some emission line ratios near the edge of uniform density H II regions and combined with the three dimensional clumpy nature of the interstellar medium may explain the apparent lack of distinctive emission line ratios near H I -- H II interfaces.
  06/2005;