The far infrared spectrum of Jupiter - Its dependence on the vertical thermal structure

Details The far infrared spectrum of Jupiter - Its dependence on the vertical thermal structure The far infrared spectrum of Jupiter - Its dependence on the vertical thermal structure

Jun 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....58..113v&link_type=abstract

Astronomy and Astrophysics, vol. 58, no. 1-2, June 1977, p. 113-119.

Astronomy and Astrophysics

Astrophysics

5

Ammonia, Far Infrared Radiation, Infrared Spectra, Jupiter Atmosphere, Spectrum Analysis, Atmospheric Models, Molecular Spectra, Temperature Distribution, Vertical Distribution

Scientific paper

Theoretical spectra of Jupiter have been calculated between 70 and 190 kaysers, using different atmospheric models. Comparison with a previous spectrum shows that the observations can be explained with the 'classical' assumptions of an adiabatic gradient in the convective zone, a NH3 density distribution limited by its saturation law, and a minimum temperature around 108 K. As a result, it appears that a constraint of T(P) may be obtained in the convective zone from observation of the brightness temperature in the continuum level at wavenumbers greater than 130 kaysers. Spectra between 70 and 130 kaysers at 0.5-kayser resolution, may provide some constraints on the temperature lapse rate and/or the photodissociation of ammonia in the lower stratosphere.

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