期刊
ASTROPHYSICAL JOURNAL
卷 639, 期 2, 页码 941-950出版社
IOP PUBLISHING LTD
DOI: 10.1086/499221
关键词
ISM : abundances; ISM : clouds; ISM : individual (HD 185418); ISM : structure
We have developed a complete model of the hydrogen molecule as part of the spectral simulation code Cloudy. Our goal is to apply this to spectra of high-redshift star-forming regions where H-2 absorption is seen, but where few other details are known, to understand its implication for star formation. The microphysics of H-2 is intricate, and it is important to validate these numerical simulations in better understood environments. This paper studies a well-defined line of sight through the Galactic interstellar medium ( ISM) as a test of the microphysics and methods we use. We present a self-consistent calculation of the observed absorption-line spectrum to derive the physical conditions in the ISM toward HD 185418, a line of sight with many observables. We deduce density, temperature, local radiation field, cosmic-ray ionization rate, and chemical composition and compare these conclusions with conditions deduced from analytical calculations. We find a higher density and similar abundances, and we require a cosmic-ray flux enhanced over the Galactic background value, consistent with enhancements predicted by MHD simulations.
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