Triplet transitions of neutral CO in the spectra of comets and the abundance of CO2 or molecules containing the CO group in comets

The high-dispersion spectra of comet Mrkos (1957 V) taken at Mt. Palomar by J. L. Greenstein and remeasured by A. Woszczyk contain many unidentified weak lines. The possibility that some of these lines belong to transitions between triplet levels of neutral CO molecules is investigated. Their presence would suggest excitation related to the dissociative recombination of a parent containing the CO group, which is first ionized by solar uv. Of 31 CO lines (of the Asundi and Triplet systems), 14 are masked by known or by questionably identified lines as statistically expected. Of the remaining 17, 13 coincide within a few tenths of an Angstrom with an unidentified line and 4 do not. These results are contrary to statistical expectations. (Some members of the third positive system of CO, which might be present, have not been included in the figures.) Although these figures strongly favor the identification proposed, the numbers are not large enough to support entirely the argument of a small statistical probability (0.2 percent) of the observed state. Also, the rotational structure of the CO bands for the triplet systems needs further investigation. C. F. Lillie's observations of comet Bennett (1970 II) between 1200 and 1800 A, especially of the fourth positive system of CO, seem to favor a cometary atmosphere characterized by a large relative abundance of CO2 and/or molecules containing the CO group. A model outlined for comet Bennett at 0.8 a.u. seems to be approximately consistent with observations. The chemical aspects, however, especially need further consideration. New observations, particularly of the Cameron bands of CO, are needed to settle the questions raised