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Molecular cooling in the diffuse interstellar medium

Glover, S. C. O. and Clark, Paul 2013. Molecular cooling in the diffuse interstellar medium. Monthly Notices of the Royal Astronomical Society 437 (1) , pp. 9-20. 10.1093/mnras/stt1809

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Abstract

We use a simple one-zone model of the thermal and chemical evolution of interstellar gas to study whether molecular hydrogen (H2) is ever an important coolant of the warm, diffuse interstellar medium (ISM). We demonstrate that at solar metallicity, H2 cooling is unimportant and the thermal evolution of the ISM is dominated by metal-line cooling. At metallicities below 0.1 Z⊙, however, metal-line cooling of low-density gas quickly becomes unimportant and H2 can become the dominant coolant, even though its abundance in the gas remains small. We investigate the conditions required in order for H2 to dominate, and show that it provides significant cooling only when the ratio of the interstellar radiation field strength to the gas density is small. Finally, we demonstrate that our results are insensitive to changes in the initial fractional ionization of the gas or to uncertainties in the nature of the dust present in the low-metallicity ISM.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Subjects: Q Science > QB Astronomy
Uncontrolled Keywords: stars: formation; ISM: clouds; ISM: molecules; galaxies: ISM
Publisher: Oxford University Press
ISSN: 0035-8711
Last Modified: 04 Jun 2017 06:25
URI: http://orca.cf.ac.uk/id/eprint/59744

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Cited 6 times in Web of Science. View in Web of Science.

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