Abstract
The two mechanisms known for the production of cometary C(1D) atoms, namely the dissociative electron recombination of CO+ ions and the photodissociation of CO molecules, have been examined to ascertain whether these mechanisms can produce the observed brightnesses of the comae of Comet 1P/Halley, Comet C/1975 V1 (Comet West 1976 VI) and Comet C/1979 Y1 (Comet Bradfield 1979 X) in the C i (1D–1Po) line at 1931 Å on specific dates. The brightnesses computed from these mechanisms for the respective comets are compared with those quoted in the literature. It is found that the latter of the above two mechanisms can account for the observed brightnesses of these comets in the C i (1D–1Poh) line. A valid, hitherto undiscussed reaction mechanism not involving COH for the production of cometary C(1D) atoms is suggested.
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