High-Phase-Angle Observations of Uranus at 2650 A: Haze Structure and Particle Properties

Details High-Phase-Angle Observations of Uranus at 2650 A: Haze Structure and Particle Properties High-Phase-Angle Observations of Uranus at 2650 A: Haze Structure and Particle Properties

Jun 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997icar..127..508p&link_type=abstract

Icarus, Volume 127, Issue 2, pp. 508-522.

Physics

5

Scientific paper

Spatially resolved photometric observations of Uranus at 2650 A obtained with the Voyager 2 Photopolarimeter Subsystem (PPS) are presented and analyzed with model atmospheres. A vertically homogenous atmospheric model with Rayleigh scattering and absorption fits Uranus well at 2650 A at phase angles from 16 deg to 157 deg no strong forward scattering typical of abundant large particles is observed. A microphysical model developed for Uranus to fit Voyager imaging system data (K. Rages, J. B. Pollack, M. G. Tomasko, and L. R. Doose, 1991, Icarus 89, 359-376) predicts the vertical distribution and properties of stratospheric haze aerosols at 22.5 deg and 65 degS. This microphysical model also fits the 2650-A PPS data at low latitudes. Increasing the aerosol sizes in the Rages et al. size distribution by a factor of 1.2 creates an unobserved forward scattering peak and can be excluded. The low-latitude upper stratospheric aerosols on Uranus are smaller (<0.1 μm radius) and/or much less abundant than the 0.2 to 0.25-μm stratospheric aerosol population found by PPS on Neptune; however, to fit the Uranus 2650-A data at all latitudes requires darker and/or more abundant (1.5-3 times more) aerosols near the sunlit pole.

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