The states of carbon and nitrogen atoms after photodissociation of CN, CH, CH(+), C2, C3, and CO in comets

Details The states of carbon and nitrogen atoms after photodissociation of CN, CH, CH(+), C2, C3, and CO in comets The states of carbon and nitrogen atoms after photodissociation of CN, CH, CH(+), C2, C3, and CO in comets

Mar 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991icar...90...74s&link_type=abstract

Icarus (ISSN 0019-1035), vol. 90, March 1991, p. 74-78. Research supported by Southwest Research Institute, NASA, and NSF.

Other

7

Carbon Compounds, Cometary Atmospheres, Nitrogen Compounds, Photodissociation, Resonance Fluorescence, Solar Radiation, Emission Spectra, Solar Orbits, Spectral Line Width, Ultraviolet Radiation, Comets, Carbon, Nitrogen, Photochemistry, Carbon Monoxide, Cyanide, Ultraviolet, Wavelengths, Radiation, Solar Radiation, Emissions, Resonance, Fluorescence, Distance

Scientific paper

The photodissociation of carbon compounds by solar UV radiation at a heliocentric distance of 1 AU is examined, comparing published observational data with the predictions of theoretical models and results from laboratory experiments. It is shown that species other than CO, including CN, CH, CH(+), C2, and C3, can contribute to the observed brightness of the VUV lines of C I (156.1, 165.7, and 193.1 nm) and C II (133.5 nm) in comet comae. CN photodissociation is also found to produce metastable 2D0 and 2P0 N I atoms, possibly leading (at heliocentric distances less than 0.25 AU) to 143.9-nm emission via resonance fluorescence.

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