Saturn's Haze Properties in the Near Infrared

Details Saturn's Haze Properties in the Near Infrared Saturn's Haze Properties in the Near Infrared

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7823t&link_type=abstract

HST Proposal ID #7823

Computer Science

Sound

Hst Proposal Id #7823 Solar System

Scientific paper

Our analysis of WFPC and WFPC2 images of Saturn yielded powerful constraints on Saturn's vertical haze structure due to the availability of measuring center-to-limb variation very close to the limb of Saturn's disk. We propose to image Saturn in 12 NICMOS filters to extend our study to longer wavelengths. These wavelengths are more sensitive to probing variations of aerosol sizes than observations at visible wavelengths. The deeper methane bands in the near infrared will allow us to probe higher atmospheric levels more accurately than at visible wavelengths. The presence of pressure dependent hydrogen dipole absorption near 2 micrometer wavelength provides a valuable tool to vertical atmospheric sounding. Several open questions of Saturn's vertical atmospheric structure can be addressed within only one orbit due to Saturn's brightness.

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