Spatially-resolved polarimetry of Titan

Details Spatially-resolved polarimetry of Titan Spatially-resolved polarimetry of Titan

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hst..prop.9385l&link_type=abstract

HST Proposal ID #9385

Physics

Hst Proposal Id #9385

Scientific paper

Titan's stratospheric haze not only hides the surface in visible light, it also traces the progress of Titan's seasons and controls the solar flux into the troposphere. Since 1994, we have monitored the seasonal context on Titan. We propose to continue this program and, with ACS and NICMOS, we can add important new measurements. Spacecraft polarimetry has suggested small particles, while high phase angle images suggest larger particles. Two types of models have been used to successfully explain the discrepancy: larger particles held above smaller particles by Titan's atmospheric dynamics; or a more uniform distribution of fluffy aggregate aerosols. The distinction is not just a question of large particles vs. small, it is about the process that governs the evolution of Titan's haze. New constraints have been slow in coming. Titan's disk integrated polarization near zero-phase angle does not distinguish the models. Intensity alone does not distinguish the models. We have the opportunity to make a set of observations that can test the models. We propose to obtain disk-resolved polarization measurements from 0.2 to 2 micron. We will use this information to develop a set of constraints on the type of particles in Titan's stratosphere. We will also continue our program of monitoring seasonal change on Titan, and use the data sets to provide context to the Cassini mission.

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