Vibrational and rotational excitation of CO in comets Nonequilibrium calculations

Details Vibrational and rotational excitation of CO in comets Nonequilibrium calculations Vibrational and rotational excitation of CO in comets Nonequilibrium calculations

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...285..858c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 285, Oct. 15, 1984, p. 858-869.

Statistics

Computation

30

Carbon Monoxide, Cometary Atmospheres, Computational Astrophysics, Molecular Excitation, Vibrational Spectra, Astronomical Models, Molecular Rotation, Nonequilibrium Conditions, Plasma Pumping, Radiative Transfer, Solar Flux

Scientific paper

Ultraviolet observations of atomic carbon in cometary comae show that carbon-bearing compounds must comprise a significant fraction (approximately equal to or greater than 10 percent) of the volatiles. One likely source is CO. This compound is an important constituent of at least some cometary nuclei, even though it may not be the ultimate source of atomic carbon in all comets. Feldman (1983) has suggested that the relative abundance of CO may be one of the few fundamental characteristics which distinguish one comet from another. The present investigation is, therefore, concerned with the vibrational and rotational excitation of the CO molecule in cometary comae. Two previously neglected factors are taken into account in the study. The fractional populations of CO as solutions to time-dependent differential equations are derived, and a nonisothermal and cold kinetic temperature profile for the inner coma is considered.

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