Determining the H+ Region/PDR Equation of State in Star Forming Regions
arXiv:astro-ph/0604210 · doi:10.1086/505175
Abstract
The emission line regions of starburst galaxies and active nuclei reveal a wealth of spectroscopic information. A unified picture of the relationship between ionized, atomic, and molecular gas makes it possible to better understand these observations. We performed a series of calculations designed to determine the equation of state, the relationship between density, temperature, and pressure, through emission-line diagnostic ratios that form in the H+ region and PDR. We consider a wide range of physical conditions in the H+ region. We connect the H+ region to the PDR by considering two constant pressure cases, one with no magnetic field and one where the magnetic field overwhelms the thermal pressure. We show that diagnostic ratios can yield the equation of state for single H+ regions adjacent to single PDRs, with the results being more ambiguous when considering observations of entire galaxies. As a test, we apply our calculations to the Orion H+/PDR region behind the Trapezium. We find the ratio of thermal to magnetic pressure in the PDR to be \~1.2. If magnetic and turbulent energy are in equipartition, our results mean the magnetic field is not the cause of the unexplained broadening in M 42, but may significantly affect line broadening in the PDR. Since Orion is often used to understand physical processes in extragalactic environments, our calculations suggest magnetic pressure should be considered in modeling such regions.
arXiv comment21 pages, 7 figures, accepted for publication in ApJ
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