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Jupiter and Saturn; Jupiter and Saturn; What we know, How we study them,What we know, How we study them,
and What we and What we stillstill dondon’’t knowt know
Kunio M. Sayanagi (UCLA)
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OutlineOutline
1. Giant Planets of our Solar System
2. Jupiter Mission Milestones
3. Cassini at Saturn
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Solar System Overview
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Vital StatsVital Stats
16h6min
17.143.88164.7930.44Neptune
17h14min
14.544.084.2320.08Uranus
95.18
317.94
1.00
Mass (Earth = 1)
10h14min
9h50min
24h
Rotation Period
1.001.001.0Earth
9.4529.469.54Saturn
11.2111.895.20Jupiter
Radius (Earth = 1)
Orbital Period (Earth-yr)
Distance from Sun
(AU)
Planet
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SaturnSaturn’’s Love Handless Love Handles
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Vertical Atmospheric StructureVertical Atmospheric Structure
Jupiter Saturn
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Giant Planet Giant Planet JetstreamsJetstreams
Beebe. (2005) Fig. 1
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Interior StructureInterior Structure
?
• Presence of Rocky Core- Unknown!- Hydrogen Eq. State
• Bulk Composition-- mostly Hydrogen and Helium-- Noble Gas Isotope abundance
will reveal formation history
Gas GiantsIce Giants
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Magnetic Fields of Giant PlanetsMagnetic Fields of Giant Planets
?
• Jupiter and Saturn-- Generated in Metal-H Layer-- Strongly Dipolar
• Uranus and Neptune-- Generated in Water+Ice Layer-- Messy Field
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How do we study Giant Planets?How do we study Giant Planets?
-- Observations (Earth and SpaceObservations (Earth and Space--Based Telescopes)Based Telescopes)
-- Space ProbesSpace Probes
-- Computer ModelingComputer Modeling
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History of Jupiter ExplorationHistory of Jupiter Exploration
Hooke (1665)
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Pioneer: ClosePioneer: Close--up Imagesup ImagesPioneer 10 Image of Jupiter in 1973
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Voyager: WindsVoyager: WindsVoyager 1 Approach Movie (1979)
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Ulysses: MagnetosphereUlysses: Magnetosphere
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Galileo: HiGalileo: Hi--Res Wind FieldsRes Wind FieldsGalileo Wind Field Measurement of GRS (Choi et al. 2007)
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Galileo: LightningGalileo: LightningGalileo Observation of Lightning Flashes (Little et al. 1999)
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Cloud Composition & Vertical StructuresCloud Composition & Vertical StructuresGalileo NIMS Observation of Fresh Ammonia Ice Clouds (Baines et al. 2002)
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AuroraAuroraGalileo Observation of Northern Aurora (Ingersoll et al. 1998)
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Cassini: Stable Zonal JetsCassini: Stable Zonal Jets
Right:Red = Voyager in 1979 (Limaye, 1986), Black = Cassini in 2000 (Porco, et al. 2003)
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Vertical Shear, Eddy Momentum FluxVertical Shear, Eddy Momentum Flux
Vertical Shear (Li et al. 2006)Eddy Momentum Flux (Salyk et al. 2007)
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Vortex Life CycleVortex Life Cycle
(Li et al. 2004)
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Oval BA Oval BA ““Red Spot Red Spot JrJr””
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New HorizonsNew HorizonsNew Horizons Wind Field Measurement of Oval BA (Hueso et al. 2009)
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Jupiter & Saturn: What & HowJupiter & Saturn: What & How
- 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
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Near Future MissionsNear Future Missions
1. Juno
2. Europa Jupiter System Mission- Jupiter Europa Orbiter (NASA)- Jupiter Ganymede Orbiter (ESA)- Jupiter Magnetospheric Orbiter (JAXA)?
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JunoJuno
- Polar Orbiter- Gravity Measurements to study Interior- IR+Microwave Radiometer to find Water
Limited Imaging Science Capability
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View from Europa Jupiter Orbiter
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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
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II: Waves, Periodicity & Coupling
Reuter et al., (2007)
Friedson et al., 1999Friedson et al., 1999
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III: Polar Processes
• Aurora• High-Latitude Jets and Vortices
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JupiterJupiter’’s Poles: Unexplored Frontiers Poles: Unexplored Frontier
North Pole South Pole
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JupiterJupiter’’s Poles: Unexplored Frontiers Poles: Unexplored Frontier
North Pole South Pole
Sun et al. (unpublished ISS Data)
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Polar Waves of JupiterPolar Waves of Jupiter
Polar Hood in UVVincent et al (2000)
Polar Wave in UV – Near IRBarrado-Izagirre (2008)
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Polar HighPolar High--Altitude SpotsAltitude Spots
UV Dark Spothttp://photojournal.jpl.nasa.gov/catalog/PIA03473
Orton (personal communication)
Orton (personal communication)
Blue Circle = Persistent Auroral Zone
While Circle = 60degN
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Polar TurbulencePolar Turbulence
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Three Dynamic RegimesThree Dynamic Regimes
• Equatorial Jet
• Mid-Latitude Mixed Jets + Vortices
• Polar Turbulence
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LowLow--lat Jets lat Jets Polar TurbulencePolar Turbulence
Low-Latitude Condition High-Latitude Condition
Sayanagi et al (2008)
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- 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
UnknownsUnknowns
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Take Home MessageTake Home Message- 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 )