The radiative association of CH2/+/

Details The radiative association of CH2/+/ The radiative association of CH2/+/

May 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...213..696h&link_type=abstract

Astrophysical Journal, Part 1, vol. 213, May 1, 1977, p. 696-704.

Astronomy and Astrophysics

Astrophysics

39

Interstellar Chemistry, Interstellar Matter, Molecular Ions, Quantum Mechanics, Radiative Recombination, Astrophysics, Reaction Kinetics, Steady State

Scientific paper

Previous computations regarding the formation of interstellar CH, interstellar CH(+), and CH2(+) collision complexes are reviewed. A three-step mechanism for radiative association between C(+) and H2 is proposed and evaluated in a steady-state semiclassical treatment. It is found that the overall rate coefficient for radiative association depends solely on the rate coefficient for the third step and the ratio of the rate coefficients for the two directions of the reversible first step. Various approximations are used to obtain a value for the overall rate coefficient at 90 K with an estimated uncertainty of 1.5 orders of magnitude. It is concluded that the radiative association of C(+) with H2 to form CH2(+) proceeds at an astrophysically significant rate, that gas-phase synthesis of CH in diffuse interstellar clouds appears to rest on a firm foundation, and that the problem of CH(+) is still unresolved.

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