UVIS Team Meeting Report June 2010 Josh Colwell UVIS Team Meeting June 28-30, 2010, Boulder 1 RWG Solstice Mission Update • 399.1 of 400 PIE hours allocated. • UVIS has 17 ring occs as PIEs (2 in EQ1), plus additional handful of Apo-PIEs. • Rings Science Traceability Matrix completed and submitted. –No open items. –Some convolution of the language to link observations to goals. UVIS Team Meeting June 28-30, 2010, Boulder 2 Solstice Mission Inclination Profile UVIS Team Meeting June 28-30, 2010, Boulder 3 Ring Science EM and SM Status Update • Three more ring stellar occs in 2010: Alp Vir (next Monday), Beta Ori (Aug. 16 and Sep. 23). • Next ring stellar occ after that are two PIEs in EQ1 (Jan. 2012). Iot Ori. • IN1 occs begin in June 2012. • 99 ring occ requests in CIMS from bridge through EOM. Aiming to capture 40-50 of 4 these. UVIS Team Meeting June 28-30, 2010, Boulder Dedicated UV Imaging Observation • Took advantage of a 4-hour hole in the timeline for dedicated UVIS ring imaging observation. • July 5 2010 (Monday) • 9 fixed pointings, 3 each on C, B, and A rings. • Offsets between the pointings to allow for sub-pixel resolution. UVIS Team Meeting June 28-30, 2010, Boulder 5 Cassini orbit Projected field of view SM PIE Occs • Tracking occs: –Eps Sgr (1.1 km/s) in 2016 –Kap CMa in 2012 –Zet CMa (0.1 km/s) in 2012 –Zet Pup (1 km/s) in 2012 • Azimuthal structure: –Bet Cru (496 km from Bleriot) in 2017 –Zet Cen (147 km from Daphnis) in 2016 • Occs with VIMS (Alpha Lyrae) • Orionis occs (low elevation angle to rings) • Kap Ori 10 hour occ 8 UVIS Team Meeting June 28-30, 2010, Boulder PDS Deliveries • Calibration process defined in paper submitted to Astron. J. (currently out for review) • High-level ring occultation files are being delivered to PDS containing: –radius, time, longitude, optical depth, binned counts, number of bins, I0, background, taumax –1 km and 10 km resolution UVIS Team Meeting June 28-30, 2010, Boulder 9 Sample Product: Cassini Division UVIS Team Meeting June 28-30, 2010, Boulder 10 Sample Product: B Ring UVIS Team Meeting June 28-30, 2010, Boulder 11 UVIS Team Meeting June 28-30, 2010, Boulder 12 Sharp Edge Modeling Update Josh Colwell and Richard Jerousek UCF UVIS Team Meeting June 28-30, 2010, Boulder Modeling Sharp Edges: Viewing Geometry The line-of-sight path from the star to the spacecraft pierces the ring plane at various angles, , with respect to the ring plane normal and various angles, , with respect to the radial direction. We use these angles to compute , the projection of in the radial direction. UVIS Team Meeting June 28-30, 2010, Boulder Step-function Model with Constant Optical Depth Normal Optical Depth For a step-function edge geometry with constant normal optical depth, , inside the ring, the vertical thickness, h, of the ring plane is easily determined from the radial distance, dr, over which the optical depth transitions from its maximum value to its minimum value. dr Ring Plane Radius (km) dr h tan( ) UVIS Team Meeting June 28-30, 2010, Boulder Sigmoid Optical Depth Model Using the same step-function geometry, we introduce a new parameter, ∆, representing a radial length scale over which the transition from ring to gap is softened. The functional form of the optical depth becomes (r) 1 rred g e 1 e representing a sigmoid particle density distribution. z (vertical thickness of ring plane) Outer edge of ring or ringlet optical depth = (r) UVIS Team Meeting June 28-30, 2010, Boulder r (radial distance from Saturn) A More Physical Model Using the same step-function geometry, we vary the particle number density (and thus optical depth) vertically as well as radially. We chose a functional form of (x h / 2)2 (r, z) 1 2 2 e 2 2 r red g e 1 e representing a gaussian particle density distribution, centered on the half-width of the ring plane, vertically and a sigmoid density softened over a transition region, ∆, radially. distribution, z (vertical thickness of ring plane) Outer edge of ring or ringlet optical depth = (r,z) UVIS Team Meeting June 28-30, 2010, Boulder r (radial distance from Saturn) A More Physical Model By integrating the optical depth along the line-of-sight, we produce a new edge profile depending on the parameters, h, ∆, , and . l (t) h cot( ) 0 (tan( )rh / 2)2 / 2 1 tan ( ) e (rr0 redge )/ dr 2 2 1 e 2 2 z (vertical thickness of ring plane) (r,z) UVIS Team Meeting June 28-30, 2010, Boulder line-of-sight path, l r (radial distance from Saturn) Knife-edge model fits. Fixing ∆ = 0, we reproduce the original knife-edge geometry. There is no vertical or radial variation of particle density near the edge, and the only unconstrained parameter is h. Best-fit lightcurve corresponding to the data/lightcurve pair UVIS Team Meeting June 28-30, 2010, Boulder with the minimum 2-value. Best-fit lightcurve corresponding to the data/lightcurve pair with the maximum 2-value. Knife-edge model fits. UVIS Team Meeting June 28-30, 2010, Boulder Huygens Ringlet Inner Edge: Complex Edges UVIS Team Meeting June 28-30, 2010, Boulder Huygens Ringlet Inner Edge: Simple Edges UVIS Team Meeting June 28-30, 2010, Boulder Huygens Ringlet Inner Edge: =100h vs. =h/8 UVIS Team Meeting June 28-30, 2010, Boulder UVIS Team Meeting June 28-30, 2010, Boulder 24 Huygens Ringlet Outer Edge: Complex Edges UVIS Team Meeting June 28-30, 2010, Boulder Huygens Ringlet Outer Edge: Simple Edges UVIS Team Meeting June 28-30, 2010, Boulder Huygens Ringlet Outer Edge: =100h vs. =h/8 UVIS Team Meeting June 28-30, 2010, Boulder Dependence on UVIS Team Meeting June 28-30, 2010, Boulder Dependence on ‘B’ UVIS Team Meeting June 28-30, 2010, Boulder C Ring Wave Analysis. Kevin Baillié • Performed WWZ analysis on individual occultations. • Co-added power to look for weak periodic signals. • Identified 38 total waves or wavelike features in the C ring, 16 of which previously unreported. • Calculated resonance locations for all known moons to eighth order. • A handful of waves have promising associations with resonances. Most do30 not. UVIS Team Meeting June 28-30, 2010, Boulder Biggest Wave in the C Ring UVIS Team Meeting June 28-30, 2010, Boulder 31 UVIS Team Meeting June 28-30, 2010, Boulder 32 UVIS Team Meeting June 28-30, 2010, Boulder 33 34 UVIS Team Meeting June 28-30, 2010, Boulder 35 UVIS Team Meeting June 28-30, 2010, Boulder 36 UVIS Team Meeting June 28-30, 2010, Boulder 37