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dc.contributor.authorCecchi-Pestellini, C.
dc.contributor.authorCasu, S.
dc.contributor.authorDalgarno, Alexander
dc.date.accessioned2017-02-21T21:48:00Z
dc.date.issued2005
dc.identifier.citationCecchi-Pestellini, C., S. Casu, and A. Dalgarno. 2005. “H2 Excitation in Turbulent Interstellar Clouds.” Monthly Notices of the Royal Astronomical Society 364 (4) (December 21): 1309–1314. doi:10.1111/j.1365-2966.2005.09652.x.en_US
dc.identifier.issn0035-8711en_US
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:30403730
dc.description.abstractWe discuss the observational differences between lines of sight that intercept a group of turbulent dissipative structures and lines of sight that cross less-active regions. Using time-dependent calculations we show that the energy level distribution of the hydrogen molecule evolves in time in response to the local thermal phase. We find that relatively simple models can explain the observed properties of molecular hydrogen in diffuse interstellar clouds in terms of time evolution induced by collisional excitation in a low-density, high-temperature gas.en_US
dc.description.sponsorshipPhysicsen_US
dc.language.isoen_USen_US
dc.publisherOxford University Press (OUP)en_US
dc.relation.isversionofdoi:10.1111/j.1365-2966.2005.09652.xen_US
dash.licenseLAA
dc.subjectmolecular processesen_US
dc.subjectturbulenceen_US
dc.subjectISM: cloudsen_US
dc.subjectISM: moleculesen_US
dc.titleH2 excitation in turbulent interstellar cloudsen_US
dc.typeJournal Articleen_US
dc.description.versionVersion of Recorden_US
dc.relation.journalMonthly Notices of the Royal Astronomical Societyen_US
dash.depositing.authorDalgarno, Alexander
dc.date.available2017-02-21T21:48:00Z
dc.identifier.doi10.1111/j.1365-2966.2005.09652.x*
dash.contributor.affiliatedDalgarno, Alexander


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