Non-equilibrium radiative processes in the atmospheres of the giant planets

Details Non-equilibrium radiative processes in the atmospheres of the giant planets Non-equilibrium radiative processes in the atmospheres of the giant planets

Apr 1971

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1971pepi....4..243s&link_type=abstract

Physics of the Earth and Planetary Interiors, Volume 4, Issue 3, p. 243-247.

Physics

Scientific paper

In the case of Jupiter at least, there is a strong possibility that some of the visible sunlight absorbed is converted by a fluorescent or cyclic process into infrared quanta distributed differently in frequency from that for equilibrium processes. In this case, the monochromatic temperatures reported by some observers may be significantly higher than the translational temperature of the gas from which the radiation emerges. Some of the perplexing observations which might be explained by such processes are the observation by Murray et al. (1964a, b) of a strong enhancement of 8-14 μm emission in the vicinity of the shadows of Jupiter's satellites II and III and the observation of a strong 7.7 μm methane emission peak in Jupiter's spectrum by Gillett et al. (1969).

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