UNDERSTANDING THE FORMATION AND EVOLUTION OF SATURN S RINGS NOT ONLY INFORMS MODELS FOR THE HISTORY OF OUR OWN SOLAR SYSTEM BUT ALSO HAS APPLICATIONS FOR THE DEVELOPMENT AND DYNAMICS IN MORE DISTANT STRUCTURES SUCH AS PROTO-PLANETARY DISKS. TWO CRITICAL PARAMETERS FOR DETERMINING THE AGE MAKEUP AND ACTIVITY IN THE RINGS ARE THE SIZE AND COMPOSITION OF THE RING PARTICLES. DATA FROM ACROSS THE INSTRUMENT SUITE ON CASSINI HAVE BEGUN CONSTRAINING THESE PARAMETERS; HOWEVER MANY DETAILS INCLUDING THE VARIATION OF THE FRACTIONAL ABUNDANCE OF CONTAMINANTS AND OF THE SIZE OF THE SMALLEST PARTICLES ACROSS THE RING REMAIN ELUSIVE. INDIVIDUAL SMALL PARTICLES RAPIDLY SPIRAL INWARD TO SATURN OR ARE SWEPT UP BY LARGER PARTICLES IN THE RING. THEIR PRESENCE INDICATES THAT THEY HAVE BEEN RECENTLY RELEASED LIKELY THROUGH COLLISIONS OF LARGER RING PARTICLES AND THUS CAN SERVE AS A TRACER FOR DYNAMIC ACTIVITY. THE COMPOSITION OF THE NON-ICY MATERIAL COULD BE INDICATIVE OF THE RINGS PROGENITOR AND VARIATIONS OF THAT MATERIAL WITHIN THE RINGS COULD HAVE IMPLICATIONS FOR DIFFERENT FORMATION OR EVOLUTION SCENARIOS ACROSS SATURN S RING SYSTEM. WE PROPOSE TO MEASURE THE PARTICLE SIZE AND COMPOSITION WITH UNPRECEDENTED ACCURACY BY UTILIZING THREE TYPES OF UNIQUE OBSERVATIONAL EXPERIMENTS CONDUCTED BY CASSINI THROUGHOUT THE MISSION AND FOR WHICH THE DATA HAS YET TO BE ANALYZED. MEASUREMENTS OF THE I/F REFLECTANCE ARE CRITICAL FOR DECIPHERING THE COMPOSITION OF THE RINGS. THIS MEASUREMENT HAS BEEN COMPLICATED BY THE VARIABILITY OF THE OPTICAL DEPTH IN THE RINGS DUE TO STRUCTURES SUCH AS SELF-GRAVITY WAKES. WE PROPOSE TO USE A UNIQUE EXPERIMENT THAT ENABLED UVIS S HIGH SPEED PHOTOMETER AND FUV CHANNEL TO SIMULTANEOUSLY OBSERVE A STELLAR OCCULTATION BY THE RINGS RESULTING IN BOTH THE FAR-UV SOLAR-REFLECTED SIGNAL AND HIGH SPATIAL-RESOLUTION OPTICAL DEPTH MEASUREMENTS. THESE DUAL OBSERVATIONS ELIMINATE THE UNCERTAINTY IN THE OPTICAL DEPTH NEEDED TO DETERMINE THE I/F AND WILL ENABLE THE ASSESSMENT OF COMPOSITIONAL VARIATIONS ACROSS THE RINGS WITH HIGH SPATIAL RESOLUTION AND ACCURACY. ONE OF THE MOST SUCCESSFUL TECHNIQUES FOR ASSESSING THE PARTICLE SIZE DISTRIBUTION OF RING PARTICLES IS FROM OCCULTATIONS. UVIS SOLAR OCCULTATIONS HAVE THE ADVANTAGE OF PROVIDING AN EXTREMELY BRIGHT SOURCE AT THE SHORT WAVELENGTHS UNOBSERVABLE DURING STELLAR OCCULTATIONS. THE SOLAR SIGNAL IS DIFFRACTED BY THE RING PARTICLES IN A MANNER DEPENDENT ON THEIR SIZE. AT EUV WAVELENGTHS THIS EXPERIMENT IS SENSITIVE TO THE SMALLEST EXPECTED PARTICLES. PREVIOUS ANALYSES HAVE SHOWN THAT VARIATIONS IN THE POPULATION OF MICRONSIZED PARTICLES CORRESPOND WITH COLLISIONAL EVENTS IN THE F RING BUT THE DATA HAVE NOT BEEN STUDIED FOR THE MAIN RINGS. WE EXPECT TO CONSTRAIN BOTH THE VARIABILITY OF THE COMPOSITION AND PARTICLE SIZES IN THE RINGS BY CAPITALIZING ON THE MULTI-WAVELENGTH OBSERVATIONS OBTAINED FROM SIMULTANEOUS CIRS STELLAR OCCULTATIONS AND UVIS REFLECTANCE MEASUREMENTS. INITIAL ANALYSES OF THE CIRS DATA HAVE IDENTIFIED REGIONS WITH EITHER A LARGER POPULATION OF MICRON-SIZED PARTICLES OR A REGION OF INCREASED NON-ICY CONTAMINATION IN THE C RING. IN THE UV THE WAVELENGTH AND SHAPE OF THE SHARP WATER ICE ABSORPTION FEATURE CAN DISTINGUISH BETWEEN PARTICLE SIZES AND INDICATE NON-WATER-ICE CONTAMINANTS RESPECTIVELY. THE COMBINED CIRS-UVIS DATASET CAN IDENTIFY REGIONS OF MICRON-SIZED DUST INDICATIVE OF ENERGETIC COLLISIONS OR IDENTIFY REGIONS OF CONTAMINATION POTENTIALLY FROM THE SOURCE MATERIAL OF THE C RING. THESE OBSERVATIONAL EXPERIMENTS PROMISE UNIQUE AND INDEPENDENT MEASUREMENTS OF TWO CRITICAL PARAMETERS - THE COMPOSITION AND PARTICLE SIZE OF SATURN S RINGS. WE PROPOSE TO REDUCE THE DATA AND APPLY COMPUTATIONAL MODELS TO SYSTEMATICALLY ASSESS THESE PARAMETERS. CAPTURING THE VARIATION OF THE COMPOSITION AND PARTICLE SIZE DISTRIBUTION OF THE RINGS WILL PLACE CONSTRAINTS ON DIFFERENT FORMATION AND EVOLUTION SCENARIOS ACROSS THE SATURNIAN RING SYSTEM.