1. *
07/16/96
Constraints on Titan’s Hign Haze from Cassini UVIS/ISS and Huygens DISR Observations *

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

3. 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 *

4. Cassini/Huygens Observations*
07/16/96
Cassini/Huygens Observations
UVIS Stellar Occultations: Aerosol extinction vertical profiles nm
UVIS Spectral Image Cubes: Scattering properties (phase function, albedo) nm)
ISS Limb Images: Scattering Profiles above 300 Km, 270 nm to 934 nm
ISS Disk images: Aerosol Albedo, Surface Albedo (near 940 nm), Spatially-Resolved Polarization, Methane-Band Imagery
DISR internal radiation measurements.
Particle phase function, optical depth, wavelength dependence from ~400 nm to 1600 nm, but only at one location and altitudes less than 150 Km *

5. *
07/16/96
Titan EUVFUV *

6. *
07/16/96
938 nm
Phase Angle 10 24 60
137
147
Data
Model
Ratio *

7. *
07/16/96
Phase 10
137 60
147 *

8. Derived Haze Properties*
07/16/96
Derived Haze Properties
H = 65 Km
Surface average albedo = 0.35; Haze single-scatter albedo = 0.99 *

9. Near-term plan Modeling*
07/16/96
Near-term plan
Modeling
Currently testing a spherical-shell intensity code (JPL) against pseudo spherical-shell code (Y. Yung and D. Tice, Caltech). Outcome will determine if a polarization pseudo-spherical code can be used.
Need a model to relate a physical particle (e.g. aggregates) to optical properties (Mackowski and Mishchenko multi-sphere code combined with aggregate model)
Run a suite of models for various size parameters, refractive indices and vertical profiles and compare with data (ISS, UVIS and DISR).
Multi-components and/or vertical structure will be required – investigate direct inversion techniques
Add NIMS data (1-5 micron wavelength) *