Jet Propulsion Lab, California Institute of Technology

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Presentation transcript:

Jet Propulsion Lab, California Institute of Technology * 07/16/96 Titan Haze Robert West Jet Propulsion Lab, California Institute of Technology 25-Jul-05 *

Pioneer and Voyager Measurements * 07/16/96 Pioneer and Voyager Measurements West and Smith Icarus 90 (1991) *

Fractal Aggregates High-dimension Cluster-cluster Low-dimension * 07/16/96 Fractal Aggregates Cluster-cluster aggregate High-dimension aggregate Low-dimension aggregate M. Lemmon Dissertation *

Summary for Titan Aggregates * 07/16/96 Summary for Titan Aggregates Fractal aggregate models naturally account for Titan’s strong polarization and modest forward scattering Early models called for few (~10) monomers, more recent models by Lemmon and by Rannou et al. have more but always the monomer radius is near 0.06 μm. Early Huygens DISR in situ results favor rmon = 0.05 μm; photometry calls for more sophisticated model. *

* 07/16/96 UVIS Contributions Kris Larsen, Yuk Yung, Dane Tice, Don Shemansky, Ian Stewart and others Image cubes from EUVFUV observations Stellar occultation profiles Riders with other instruments *

* 07/16/96 *

UVIS Contributions, Cont. * 07/16/96 UVIS Contributions, Cont. UVIS Samples Highest haze levels UVIS is sensitive to the small end of the particle size distribution. The phase behavior provides information on particle sizes UVIS constrains refractive index below 190 nm Detached haze layer can be seen in stellar occultation data but is below the resolution of EUVFUV Vertical haze profiling may be available from stellar occultations (possible confusion with gaseous constituents?) Acetylene is present in the reflected sunlight spectrum *

Near-term plan I. Data Reduction * 07/16/96 Near-term plan I. Data Reduction Kris Larsen provides image cubes with geometry II. Modeling (West, Larsen, Yung, Tice) Currently testing spherical-shell intensity code (JPL) against pseudo spherical-shell code (Y. Yung and D. Tice, Caltech) Need a model to relate a physical particle (e.g. aggregates) to optical properties (Mackowski and Mishchenko) Run a suite of models for various size parameters, refractive indices and vertical profiles and compare with data (UVIS and ISS). Multi-components and/or vertical structure may be required *