Signatures of C-shocks in molecular clouds

Details Signatures of C-shocks in molecular clouds Signatures of C-shocks in molecular clouds

Apr 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.243..498s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 243, April 1, 1990, p. 498-503.

Astronomy and Astrophysics

Astronomy

37

Emission Spectra, Molecular Clouds, Shock Waves, H Lines, Line Spectra, Molecular Energy Levels, Molecular Excitation, Spectral Line Width, Water

Scientific paper

An attempt is made to interpret the molecular hydrogen emission lines from dense interstellar clouds by planar C-shocks. The lines are predicted to be narrow if H2O dominates the cooling, the full width being less than 20 km/s even for shock velocities near the breakdown level. In contrast, the lines are broad if H2 cooling is dominant (assuming the shock plane is face-on). The profiles are single peaked, double peaked, triangular or flat topped according to the upper energy level and the shock parameters. For double peaked profiles, the maxima are separated by about 30 km/s for a shock velocity of 40 km/s. Excitation temperatures and column densities are obtained. The line ratio data accumulated for OMC-1 cannot be interpreted by a single planar C-shock.

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