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1974•Monthly Notices of the Royal Astronomical SocietyOpen access

CH and CH+ in interstellar clouds

T. P. Stecher, David A. Williams

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Abstract

Mechanisms for forming and destroying interstellar CH and CH + are discussed. The most rapid production of CH + usually occurs in reaction of C + with vibrationally excited H 2 . However, if dissociative recombination of CH + with electrons is fast (rate coefficient ∼ 10 −7 cm 3 s −1 ) then known processes in an equilibrium situation cannot account for the observed column density of CH + . A non-equilibrium model is then necessary.

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Mechanisms for forming and destroying interstellar CH and CH + are discussed. The most rapid production of CH + usually occurs in reaction of C + with vibrationally excited H 2 . However, if dissociative recombination of CH + with electrons is fast (rate coefficient ∼ 10 −7 cm 3 s −1 ) then known processes in an equilibrium situation cannot account for the observed column density of CH + . A non-equilibrium model is then necessary.

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Available abstract

Mechanisms for forming and destroying interstellar CH and CH + are discussed. The most rapid production of CH + usually occurs in reaction of C + with vibrationally excited H 2 . However, if dissociative recombination of CH + with electrons is fast (rate coefficient ∼ 10 −7 cm 3 s −1 ) then known processes in an equilibrium situation cannot account for the observed column density of CH + . A non-equilibrium model is then necessary.

Key concepts: Physics, Dissociative recombination, Interstellar cloud, Excited state, Interstellar medium, Atomic physics, Cosmochemistry, Thermodynamic equilibrium

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