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Jupiter and Saturn; What We Know, How We Study Them, and What We JupiterJupiter andand Saturn;Saturn; WhatWhat wewe know,know, HowHow wewe studystudy them,them, andand WhatWhat wewe stillstill dondon’’tt knowknow Kunio M. Sayanagi (UCLA) OutlineOutline 1. Giant Planets of our Solar System 2. Jupiter Mission Milestones 3. Cassini at Saturn Solar System Overview VitalVital StatsStats Planet Distance from Orbital Period Radius Mass Rotation Period Sun (Earth-yr) (Earth = 1) (Earth = 1) (AU) Earth 1.0 1.00 1.00 1.00 24h Jupiter 5.20 11.89 11.21 317.94 9h 50min Saturn 9.54 29.46 9.45 95.18 10h 14min Uranus 20.08 84.23 4.0 14.54 17h 14min Neptune 30.44 164.79 3.88 17.14 16h 6min SaturnSaturn’’ss LoveLove HandlesHandles VerticalVertical AtmosphericAtmospheric StructureStructure Jupiter Saturn GiantGiant PlanetPlanet JetstreamsJetstreams Beebe. (2005) Fig. 1 InteriorInterior StructureStructure • Bulk Composition • Presence of Rocky Core -- mostly Hydrogen and Helium - Unknown! -- Noble Gas Isotope abundance - Hydrogen Eq. State will reveal formation history ? Ice Giants Gas Giants MagneticMagnetic FieldsFields ofof GiantGiant PlanetsPlanets • Jupiter and Saturn • Uranus and Neptune -- Generated in Metal-H Layer -- Generated in Water+Ice Layer -- Strongly Dipolar -- Messy Field ? HowHow dodo wewe studystudy GiantGiant Planets?Planets? -- ObservationsObservations (Earth(Earth andand SpaceSpace--BasedBased Telescopes)Telescopes) -- SpaceSpace ProbesProbes -- ComputerComputer ModelingModeling HistoryHistory ofof JupiterJupiter ExplorationExploration Hooke (1665) Pioneer:Pioneer: CloseClose--upup ImagesImages Pioneer 10 Image of Jupiter in 1973 Voyager:Voyager: WindsWinds Voyager 1 Approach Movie (1979) Ulysses:Ulysses: MagnetosphereMagnetosphere Galileo:Galileo: HiHi--ResRes WindWind FieldsFields Galileo Wind Field Measurement of GRS (Choi et al. 2007) Galileo:Galileo: LightningLightning Galileo Observation of Lightning Flashes (Little et al. 1999) Cloud Composition & Vertical Structures Galileo NIMS Observation of Fresh Ammonia Ice Clouds (Baines et al. 2002) AuroraAurora Galileo Observation of Northern Aurora (Ingersoll et al. 1998) Cassini:Cassini: StableStable ZonalZonal JetsJets Right: Red = Voyager in 1979 (Limaye, 1986), Black = Cassini in 2000 (Porco, et al. 2003) VerticalVertical Shear,Shear, EddyEddy MomentumMomentum FluxFlux Vertical Shear (Li et al. 2006) Eddy Momentum Flux (Salyk et al. 2007) VortexVortex LifeLife CycleCycle (Li et al. 2004) OvalOval BABA ““RedRed SpotSpot JrJr”” NewNew HorizonsHorizons New Horizons Wind Field Measurement of Oval BA (Hueso et al. 2009) JupiterJupiter && Saturn:Saturn: WhatWhat && HowHow - Jupiter and Saturn have: - 3 kinds of clouds (H2O, NH3, NH4SH) - Banded Clouds Jetstreams - Jetstreams are very stable (and we don’t know why) - Long Lived Vortices - Aurora and Magnetospheric Dynamics - How We Study: - Space Missions - Jets are measured by observing cloud motions - Cloud Composition = Spectroscopy NearNear FutureFuture MissionsMissions 1. Juno 2. Europa Jupiter System Mission - Jupiter Europa Orbiter (NASA) - Jupiter Ganymede Orbiter (ESA) - Jupiter Magnetospheric Orbiter (JAXA)? JunoJuno - Polar Orbiter - Gravity Measurements to study Interior - IR+Microwave Radiometer to find Water Limited Imaging Science Capability View from Europa Jupiter Orbiter Science Example I: Climate Database • Observing Jupiter from an Orbiter enables measurements of: – Cloud changes (NH3 ice, H2O ice). – Thermal Structure/Changes. – Jetstreams. – Lightning. • Constantly evolving dynamic atmosphere: • Search for relationships between changes. GRS 1992-1999 II: Waves, Periodicity & Coupling Reuter et al., (2007) Friedson et al., 1999 III: Polar Processes • Aurora • High-Latitude Jets and Vortices JupiterJupiter’’ss Poles:Poles: UnexploredUnexplored FrontierFrontier North Pole South Pole JupiterJupiter’’ss Poles:Poles: UnexploredUnexplored FrontierFrontier North Pole South Pole Sun et al. (unpublished ISS Data) PolarPolar WavesWaves ofof JupiterJupiter Polar Hood in UV Polar Wave in UV – Near IR Vincent et al (2000) Barrado-Izagirre (2008) PolarPolar HighHigh--AltitudeAltitude SpotsSpots Orton (personal communication) Orton (personal communication) UV Dark Spot http://photojournal.jpl.nasa.gov/catalog/PIA03473 Blue Circle = Persistent Auroral Zone While Circle = 60degN PolarPolar TurbulenceTurbulence ThreeThree DynamicDynamic RegimesRegimes • Equatorial Jet • Mid-Latitude Mixed Jets + Vortices • Polar Turbulence LowLow--latlat JetsJets PolarPolar TurbulenceTurbulence Low-Latitude Condition High-Latitude Condition Sayanagi et al (2008) UnknownsUnknowns - Jetstreams - Why are they stable? - What drives them? - How deep do they reach? - Polar Turbulence - What process separates the Jets region and Polar Turbulence? - Waves - What excites the waves? - Auroras - Effects on Atmosphere TakeTake HomeHome MessageMessage - Jupiter and Saturn have: - 3 kinds of clouds (H2O, NH3, NH4SH) - Banded Clouds Jets - Jets are measured thru moving Clouds - Long Lived Vortices - Aurora and Magnetospheric Dynamics - Unknowns - Jets; Why Stable, How Deep, What drives them - Jets vs. Turbulence - Internal Structure (rocky core?) - Auroras’ effects - History of Space Missions - Changes in Clouds and Winds Detected - Vertical Thermal and Dynamic Structure - Support Future Planetary Missions (please ).
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