Molecular abundances in shocked diffuse clouds - Results from time-dependent modelling and comparison with diffuse cloud abundances

Details Molecular abundances in shocked diffuse clouds - Results from time-dependent modelling and comparison with diffuse cloud abundances Molecular abundances in shocked diffuse clouds - Results from time-dependent modelling and comparison with diffuse cloud abundances

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...151..121m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 151, no. 1, Oct. 1985, p. 121-130.

Astronomy and Astrophysics

Astrophysics

43

Abundance, Chemical Reactions, High Temperature Gases, Interstellar Gas, Molecular Clouds, Shock Waves, Gas Density, Hydrogen Clouds

Scientific paper

Chemical abundances in shocked, low-density gas have been obtained for a range of shock speeds, gas densities, and molecular hydrogen concentrations. Calculated abundances are compared with diffuse cloud observations. It is concluded that the species C, CO, CH, CH2, CH3, C2, C2H, C2H2, C3, O2, OH, H2O, CO2, NH, NH2, N2, NO, CN, HCN, OH(+), H2O(+), H3O(+), CH(+), CH2(+), CH3(+), HCO(+), and CO(+) can reach high abundances behind the shocks. For a majority of Ch(+) sources, the observed CH(+) column density exceeds the predicted postshock column density. For two sources, model CH(+) column densities are low by a factor of ten. Shocks with speeds greater than 20 km/s remain nondissociative, and the velocity difference beween CN(+) and CH may therefore exceed 5 km/s. It is predicted that CO should be more abundant than CH by factors of 100 to 1000.

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