Molecular cooling in the diffuse interstellar medium
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...
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| Main Authors: | , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
2014
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2013, Volume: 437, Issue: 1, Pages: 9-20 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stt1809 |
| Online Access: | Resolving-System, lizenzpflichtig, Volltext: https://doi.org/10.1093/mnras/stt1809 Verlag, lizenzpflichtig, Volltext: https://academic.oup.com/mnras/article/437/1/9/992280 
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| Author Notes: | Simon C.O. Glover and Paul C. Clark |
| Summary: | 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. |
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| Item Description: | In original form 2013 May 31 Gesehen am 05.10.2020 |
| Physical Description: | Online Resource |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stt1809 |