Other
Scientific paper
Feb 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...236..172e&link_type=abstract
Astrophysical Journal, Part 1, vol. 236, Feb. 15, 1980, p. 172-181.
Other
115
Hydrocarbons, Interstellar Gas, Molecular Ions, Shock Wave Propagation, Abundance, Chemical Reactions, Cooling, Gas Density, Molecular Rotation, Propagation Velocity
Scientific paper
The influence of shocks on molecular abundances in diffuse interstellar clouds is investigated numerically, with emphasis on interstellar CH(+) abundances. The time development of the material behind a one-dimensional shock front under interstellar conditions is calculated, taking into account the effects of ram pressure and helium content, beginning at the end of the brief adiabatic compression phase of the shock by computing the radiative cooling of the gas at each point. Calculated abundances of the rotational states of postshock H2, as well as CH(+), CH, OH and H2O are presented, and the column density of CH(+) is approximated, together with line profiles for CH(+) and OH. Observations of the Zeta Ophiuchi clouds, including the velocity shift between CH(+) and the other species, are then accounted for in terms of the interstellar shock model, however it is noted that rather powerful shocks are required to produce the CH(+) column densities observed.
Elitzur Moshe
Watson William D.
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