Uranus' Vertical Haze Structure and its Variation with Latitude

Details Uranus' Vertical Haze Structure and its Variation with Latitude Uranus' Vertical Haze Structure and its Variation with Latitude

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7429t&link_type=abstract

HST Proposal ID #7429

Physics

Hst Proposal Id #7429 Solar System

Scientific paper

We propose to image Uranus in 27 filters between 220 and 2100 nm wavelength. The wide wavelength range allows determination of aerosol sizes and spectral characteristics superior to previous work. Some of the filters are in methane absorption bands with methane absorption coefficients spanning a factor of 1000, which probe very different altitude layers in Uranus' atmosphere. HST's spatial resolution gives accurate canter-to -limb information for each latitude band, which strongly constrains models of Uranus' vertical haze structure. Our analyzed images of Uranus of Cycle 5 show high albedo contrasts in latitude, but the wavelength coverage of these images was not sufficient. These observations yielded unexpected results on the photometric properties of Uranian rings and satellites. Open questions about the phase function of these objects near zero degree and about their spectral characteristics over an expanded wavelength region can be answered by the proposed observations.

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