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...
Gespeichert in:
| Hauptverfasser: | , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
2014
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2013, Jahrgang: 437, Heft: 1, Pages: 9-20 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stt1809 |
| Online-Zugang: | 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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| Verfasserangaben: | Simon C.O. Glover and Paul C. Clark |
MARC
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| 520 | |a 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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