OH cooling of interstellar shocks and masers

Details OH cooling of interstellar shocks and masers OH cooling of interstellar shocks and masers

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982mnras.200p..55f&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 200, Aug. 1982, p. 55P-59P.

Astronomy and Astrophysics

Astronomy

6

Gas Cooling, Hydrogen Clouds, Hydroxyl Emission, Infrared Radiation, Interstellar Masers, Shock Heating, Interstellar Chemistry, Interstellar Gas, Molecular Clouds, Molecular Rotation, Quantum Mechanics, Radiative Transfer

Scientific paper

The results of quantum mechanical calculations of cross-sections for the rotational excitation of OH by H2 have been incorporated in a radiative transfer programme for the OH rotational lines. Calculations with this program show that infrared emission from excited rotational levels of OH is an important cooling process behind shocks in interstellar molecular regions and in H II/OH maser regions. Allowance for this cooling process may significantly reduce the estimates of the amount of CH(plus) formed in interstellar shocks.

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