A shock model for infrared line emission from H2 molecules

Details A shock model for infrared line emission from H2 molecules A shock model for infrared line emission from H2 molecules

Oct 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...217..442l&link_type=abstract

Astrophysical Journal, Part 1, vol. 217, Oct. 15, 1977, p. 442-447.

Astronomy and Astrophysics

Astronomy

83

Astronomical Spectroscopy, Infrared Astronomy, Nebulae, Shock Wave Propagation, Astronomical Models, Hydrogen, Line Spectra, Molecular Spectra, Plane Waves, Steady Flow, Thermodynamic Equilibrium

Scientific paper

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.

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