Theoretical studies of interstellar molecular shocks. III - The formation of CH(+) in diffuse clouds

Details Theoretical studies of interstellar molecular shocks. III - The formation of CH(+) in diffuse clouds Theoretical studies of interstellar molecular shocks. III - The formation of CH(+) in diffuse clouds

Jun 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.220..801p&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 220, June 15, 1986, p. 801-824. NSF-supported research.

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117

Computational Astrophysics, Gaseous Diffusion, Hydrocarbons, Interstellar Chemistry, Interstellar Matter, Molecular Clouds, Hydrodynamic Equations, Magnetohydrodynamic Flow, Reaction Kinetics, Shock Wave Interaction, Tables (Data)

Scientific paper

The results of computations of both one-fluid hydrodynamic and three-fluid MHD models of interstellar molecular shocks are presented. A network of over 150 chemical reactions was incorporated in the models, with a view to correctly predicting the variation of the fractional ionization in the precursors of MHD shocks and the column densities of a number of chemical species, particularly CH(+), which may be selectively formed in shocks. It is found that one-fluid hydrodynamic models predict column densities of CH(+) which are too small to be considered compatible with observations. The MHD models are more successful in this respect, CH(+) being formed by the endothermic C(+)(H2,H)CH(+) reaction, driven by ambipolar diffusion. However, difficulties remain in simultaneously reproducing the observed column densities of other species which are formed in shocks, specifically the excited rotational states of H2.

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