Estimating the Porosity of the Interstellar Medium from Three‐dimensional Photoionization Modeling of Hii Regions
| Autor: | L. M. Haffner, G. J. Madsen, John S. Mathis, Ronald J. Reynolds, Kenneth Wood |
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| Rok vydání: | 2005 |
| Předmět: |
Physics
H II region 010308 nuclear & particles physics Astronomy and Astrophysics Context (language use) Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics Photoionization 01 natural sciences Interstellar medium 13. Climate action Space and Planetary Science 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Emission spectrum Surface brightness 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics Line (formation) O-type star |
| Zdroj: | The Astrophysical Journal. 633:295-308 |
| ISSN: | 1538-4357 0004-637X |
| DOI: | 10.1086/432831 |
| Popis: | 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. Comment: Accepted for publication in ApJ |
| Databáze: | OpenAIRE |
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