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    A shock model for infrared line emission from H2 molecules

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    Chu_Shock_Model_For_Infrared_Line_Emission_From_H2_Molecules.pdf (163.4Kb)
    Issue Date
    1977-10-01
    Author
    London, Richard
    McCray, Richard
    Chu, Shih-I
    Publisher
    American Astronomical Society
    Type
    Article
    Article Version
    Scholarly/refereed, publisher version
    Metadata
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    Abstract
    A 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.
    Description
    This is the published version, also available here: http://dx.doi.org/10.1086/155593.
    URI
    http://hdl.handle.net/1808/15827
    DOI
    https://doi.org/10.1086/155593
    Collections
    • Chemistry Scholarly Works [610]
    • Distinguished Professors Scholarly Works [918]
    Citation
    London, 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.

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    Contact KU ScholarWorks
    785-864-8983
    KU Libraries
    1425 Jayhawk Blvd
    Lawrence, KS 66045
    785-864-8983

    KU Libraries
    1425 Jayhawk Blvd
    Lawrence, KS 66045
    Image Credits
     

     

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