Observations of the limb darkening of Jupiter at ultraviolet wavelengths and constraints on the properties and distribution of stratospheric aerosols

Details Observations of the limb darkening of Jupiter at ultraviolet wavelengths and constraints on the properties and distribution of stratospheric aerosols Observations of the limb darkening of Jupiter at ultraviolet wavelengths and constraints on the properties and distribution of stratospheric aerosols

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986icar...65..218t&link_type=abstract

Icarus (ISSN 0019-1035), vol. 65, Feb.-Mar. 1986, p. 218-243.

Physics

35

Aerosols, Jupiter Atmosphere, Limb Darkening, Stratosphere, Ultraviolet Spectra, Clouds, Haze, Iue, Spatial Distribution, Spectral Reflectance, Troposphere, Jupiter, Atmosphere, Limbs, Ultraviolet, Wavelengths, Physical Properties, Distribution, Stratosphere, Aerosols, Spectra, Iue Satellite, Procedure, Reflectivity, Satellite Observations, Latitude, Comparisons, Absorption, Optical Properties, Models, Depth, Pressure, Particles, Distribution, Size, Mass Loading, Haze, Concentration, Composition, Tropospher

Scientific paper

The absolute reflectivity of Jupiter has been obtained in 50 A-wide regions centering on 0.221, 0.233, 0.252, and 0.330 microns from three series of IUE satellite spectra taken in November 1979. The data indicate a strong decrease in reflectivity for latitudes greater than about 30 deg, in keeping with Voyager measurements. An additional 24 spectra were also obtained in a west-east series along the equator, as well as near 40 deg N latitude. These data favor models in which the haze particles have effective radii within a factor of 2 of 0.2 microns. Near the equator, the haze aerosols produce much less absorption than near 40 deg N; the aerosol distributions and optical properties derived are noted to be more dependent on the assumed location and reflectivity of the top of the tropospheric cloud.

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