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dc.contributor.authorLondon, Richard
dc.contributor.authorMcCray, Richard
dc.contributor.authorChu, Shih-I
dc.date.accessioned2014-11-21T17:30:08Z
dc.date.available2014-11-21T17:30:08Z
dc.date.issued1977-10-01
dc.identifier.citationLondon, R., McCray, R., Chu, Shih-I. "A shock model for infrared line emission from H2 molecules." Astrophysical Journal, Part 1, vol. 217, Oct. 15, 1977, p. 442-447. http://dx.doi.org/10.1086/155593.
dc.identifier.urihttp://hdl.handle.net/1808/15827
dc.descriptionThis is the published version, also available here: http://dx.doi.org/10.1086/155593.
dc.description.abstractA shock model is considered for the H2 infrared line emission detected in the Orion Nebula by Gautier et al. (1976). The equations are solved which describe stationary gas flow and excitation of H2 in the radiative cooling region behind a shock. It is found that for the high densities needed to explain the observed line strengths, the populations of the vibration-rotation levels are nearly in LTE. By matching the calculated line strengths to the observations, it is found that the acceptable values of shock velocity and upstream molecular density must be between 8 and 21 km/s and between 100,000 and 1 million per cu cm, respectively.
dc.publisherAmerican Astronomical Society
dc.subjectAstronomical Spectroscopy
dc.subjectInfrared Astronomy
dc.subjectNebulae
dc.subjectShock Wave Propagation
dc.subjectAstronomical Models
dc.subjectHydrogen
dc.subjectLine Spectra
dc.subjectMolecular Spectra
dc.subjectPlane Waves
dc.subjectSteady Flow
dc.subjectThermodynamic Equilibrium
dc.titleA shock model for infrared line emission from H2 molecules
dc.typeArticle
kusw.kuauthorChu, Shih-I
kusw.kudepartmentChemistry
kusw.oastatusna
dc.identifier.doi10.1086/155593
kusw.oaversionScholarly/refereed, publisher version
kusw.oapolicyThis item does not meet KU Open Access policy criteria.
dc.rights.accessrightsopenAccess


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