Spectroscopy of the C2N2 C(sup 1)Bu <-- X(sup 1)Sigma g(sup +) Transition

Details Spectroscopy of the C2N2 C(sup 1)Bu <-- X(sup 1)Sigma g(sup +) Transition Spectroscopy of the C2N2 C(sup 1)Bu <-- X(sup 1)Sigma g(sup +) Transition

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997taea....1..301h&link_type=abstract

NASA University Research Centers Technical Advances in Education, Aeronautics, Space, Autonomy, Earth and Environment, vol. 1, p

Computer Science

Satellite Atmospheres, Titan, Ultraviolet Spectroscopy, Absorption Spectra, Molecular Absorption, Ultraviolet Absorption

Scientific paper

Ethanedinitrile (C2N2) is an important photochemically active species in Titan's atmosphere. It may be found in comets, where it would be a source of CN radicals whose emission is prominent in the cometary tail. Moreover, this relatively simple, molecule has become an exemplary system for photochemical studies. The first ethanedinitrile (C2N2) vacuum ultraviolet (VUV) absorption spectra were measured by Price and Walsh. The most striking feature was a strong absorption system between 145 and 170 nm which, at least at the red end, had fairly sharp vibrational structure. Twenty years later, Bell, et al assigned this system as C(sup 1) Pi u <- X(sup 1)Sigma g(sup +). The origin was given as 60,420 cm-'. The strength of the transition showed that it was electronically allowed, which for a linear-linear transition with an X(sup 1)Sigma g(sup +) ground state limits the upper electronic state to either (sup 1)Sigma u(sup +) <- (sup 1)Sigma g(sup +) or (sup 1)Pi u. The complicated vibrational band pattern at the red end of the spectrum spoke against (sup 1)Sigma u(sup +) <- (sup 1)Sigma g(sup +). Several three and four member progressions can be seen with about 2050 cm-1 between the bands. Molecular absorption coefficients in the VUV were measured by Connors, et al., and Nuth and Glicker.

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