Spatially resolved methane band photometry of Jupiter. I - Absolute reflectivity and center-to-limb variations in the 6190-, 7250-, and 8900-A bands. II - Analysis of the south equatorial belt and south tropical zone reflectivity

Details Spatially resolved methane band photometry of Jupiter. I - Absolute reflectivity and center-to-limb variations in the 6190-, 7250-, and 8900-A bands. II - Analysis of the south equatorial belt and south tropical zone reflectivity Spatially resolved methane band photometry of Jupiter. I - Absolute reflectivity and center-to-limb variations in the 6190-, 7250-, and 8900-A bands. II - Analysis of the south equatorial belt and south tropical zone reflectivity

Apr 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979icar...38...12w&link_type=abstract

Icarus, vol. 38, Apr. 1979, p. 12-53.

Astronomy and Astrophysics

Astronomy

10

Jupiter Atmosphere, Line Spectra, Methane, Planetary Radiation, Spectrophotometry, Absorption Spectra, Aerosols, Astronomical Models, Atmospheric Models, Cloud Cover, Infrared Reflection, Jupiter (Planet), Spectral Line Width, Spectral Reflectance, Vertical Distribution, Data Reduction, Wavelengths, Spatial Resolution, Methane, Jupiter, Absorption Spectra, Photometry, Spectral Reflectivity, Observatins, Position (Location), Scattering, Clouds, Great Red Spot, Aerosols, Limbs, Darkening

Scientific paper

Spatially resolved measurements of the absolute reflectivity and center to limb variations of Jupiter in the 6190, 7250 and 8900 A methane bands and nearby continuum regions are presented and analyzed for the south equatorial belts (SEBs) and south tropical zone (STrZ). It is found that the polar hoods, equatorial zone, Red Spot and north tropical zone have highest methane reflectivities, with the temperate zones and polar regions having low reflectivity and the STrZ and SEBs having intermediate values. The data on the SEB and STrZ are analyzed in terms of diffuse reflecting-scattering and two-cloud models of the vertical distribution of aerosols in the Jovian atmosphere. To fit observations, the STrZ cloud top must have between 0.55 and 0.43 bar total pressure and optical depth between 1.5 and 2.5. The reflecting-scattering models are not suitable for the SEBs. The SEB upper cloud is deeper, cloud thickness is less and the lower cloud is deeper than in the STrZ. A forward scattering haze layer accounts for limb darkening in the continuum.

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