Radiative association rate coefficients under shocked conditions in interstellar clouds - The case of CH3(+) + H2

Details Radiative association rate coefficients under shocked conditions in interstellar clouds - The case of CH3(+) + H2 Radiative association rate coefficients under shocked conditions in interstellar clouds - The case of CH3(+) + H2

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...153..151h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 153, no. 1, Dec. 1985, p. 151-156.

Astronomy and Astrophysics

Astrophysics

17

Association Reactions, Interstellar Chemistry, Interstellar Matter, Molecular Clouds, Reaction Kinetics, Shock Waves, Hydrogen, Methane, Molecular Excitation, Molecular Rotation

Scientific paper

The rate coefficients of radiative association reactions under the nonequilibrium conditions present in interstellar clouds subjected to shock waves are discussed. A theory is presented which permits the calculation of radiative association rate coefficients for reactants under non-thermal conditions. The theory is utilized to calculate the rate of the important interstellar radiative association reaction CH3++H2 → CH5++hν under shocked conditions at kinetic temperatures up to 4000K. It is seen that non-thermal effects are present in this reaction but are stronger for polar reactants because these species have their internal energy modes more significantly relaxed below the kinetic temperatures present in the shock.

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