Open Topics in Jupiter Imaging Science
Kunio M. Sayanagi(California Institute of Technology)
With contributions by:

Leigh N. Fletcher(Oxford University)

Glenn S. Orton and Robert Pappalardo(Jet Propulsion Laboratory)

Andrew P. Ingersoll,
Shawn P. Ewald,
Ulyana Dyudina(California Institute of Technology)

Amy A. Simon-Miller(NASA Goddard Space Flight Center)Outline
1. Jupiter Imaging Milestones
2. Future Planned Missions
3. Imaging Science Topics for Future Missions

Three Jupiter Science Themes
A: Dynamics andCirculation

B: Compositionand Chemistry•Dynamics of Jupiter'sweather layer•Determine the bulk
elemental abundances•Thermodynamics ofatmospheric phenomena•Measure the threedimensional distribution ofstratospheric hydrocarbons
and their long-term
variability•Quantify the roles of wave
propagation andatmospheric coupling•Investigate auroral
structure and energy
transport•Understand theinterrelationships of theionosphere &thermosphere•Study localized and nonequilibrium composition•Understand the importanceof moist convection inmeteorology, cloudformation, and chemistry

C: AtmosphericStructure•Determine the 3-D
structure of Jupiter’s upper
troposphere andstratosphere•Explore atmosphericstructure deep below theclouds•Determine coupling(waves, eddies, etc.)
between different
atmospheric regimes.

Jupiter themes are cross-disciplinary for ‘big picture’ sciencePioneer: Close-up Images
Pioneer 10 Image of Jupiter in 1973

Voyager: Winds
Voyager 1 Approach Movie (1979)

Galileo: Hi-Res Wind Fields
Galileo Wind Field Measurement of GRS (Choi et al. 2007)

Galileo: Lightning
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)

AuroraGalileo Observation of Northern Aurora (Ingersoll et al. 1998)

Cassini: Stable Zonal Jets

Right:
Red = Voyager in 1979
(Limaye, 1986),
Black = Cassini in 2000
(Porco, et al. 2003)

Vertical Shear, Eddy Momentum Flux

Vertical Shear (Li et al. 2006)

Eddy Momentum Flux (Salyk et al. 2007)

Vortex Life Cycle(Li et al. 2004)

Oval BA  “Red Spot Jr”

New Horizons
New Horizons Wind Field Measurement of Oval BA (Hueso et al. 2009)

Equatorial Oscillation = “QQO”

Equatorial Temp. Oscillation Wind Oscillation Periodigram(Simon-Miller et al. 2006)(Simon-Miller et al. 2007)

Stratospheric Vertical Shear(Flasar et al. 2004)

New Exploration of JupiterInternalStructure, Abyssal
Rotation

Polardynamics,
chemistry

Connection with
Jovianmagnetic/charged environment

Bulkcomposition,
origins

Jupiter as the archetypal gas giant
Jupiter as a window on Solar System origin
Jupiter as a template planetary system for exoplanets
Jupiter as a fundamental geophysical fluid dynamics laboratory
Cloud layers,
hazes,
lightening

Storms, hotspots,
instabilities,
upheavals, waves

Polardynamics,
chemistry

Dynamics, Winds,
temperatures,
potential vorticity

Near Future Missions
1. Juno2. Europa Jupiter System Mission- Jupiter Europa Orbiter (NASA)- Jupiter Ganymede Orbiter (ESA)- Jupiter Magnetospheric Orbiter (JAXA)

Juno-Polar Orbiter
Gravity Measurements to study Interior
IR+Microwave Radiometer to find Water

Limited Imaging Science CapabilityJupiter’s Atmosphereand Interior from EJSM

L.N. Fletcher
and the EJSM SDT
A Joint NASA-ESA Outer Planet Mission Study

Jupiter Science as an Element of EJSM
•Jupiter science is a vital element of the studyof interactions between the components ofthis complex planetary system (Jupiter, icy
satellites, rings, magnetosphere and smallbodies).

•Responsive to the ESA Cosmic Vision:– Jupiter’s atmosphere and evolution serves asthe paradigm for the study of giant planets inour solar system and beyond.

•EJSM Jupiter Science seeks to address twoof the Science Themes of the 2002 USDecadal Survey:– The Origin and Evolution of Habitable Worlds;

NASA/ESA/J Clarke, Boston University– How Planetary Systems Work.

Jupiter Working Group has reassessed Jupiter science capabilities
based on Decadal Survey/Cosmic Vision.

Jupiter Science Opportunities••

Example tours feature dedicatedJupiter monitoring campaigns.
Pre-JOI:– Extensive opportunities for global
mapping as JEO/JGO approachJupiter•Jupiter System Tour phase (withmultiple perijove opportunities):– 30 months before Europa Orbital
Insertion, 26 months before
Ganymede OI•

End of Mission (from circularsatellite orbits):– Potential to re-observe Jupiter 3
years after arrival if sciencedrivers are strong enough•Dynamical studies overhourly/weekly/monthly
timescales• Two spacecraft mission– Radio occultation studies S/C>Earth and S/C->S/C.

JEO Baseline Mission Timeline•

Long Cruise to Jupiter– Challenges: Training, Skill Retention, Obsolescence– Opportunities: Process Improvement (methods, S/W, etc), IT infrastructure, ops
approaches•

Two kinds of science missions– Tour: longer, slower, more diverse– Europa: Faster, more intense, more systematic and structured– Cruise: Specialized science not anticipated, calibrations and training use Tour
capabilities– Need one system to meet all needs (process timelines and decision process can vary)Baseline Science Mission Overview
JOIEOI

Jovian TourF

2026
M A M J JA SF2027
M A M J J

A SO N D J

F

2028
2029
M A M J J A S O N D J F M A
GlobalRegional Targeted Focused
Framework Processes Processes ScienceSystem Campaign

1 2AltIo Campaign

O N D J

Europa Campaigns

374200100

68 20 28Eurosols

Io

5Europa

4Ganymede
Cassini Prime
Mission 2.8 Tb

Callisto

2

Satellite encounters
Galileo0.25 Tb

Required to reach Europa,
but also targets of Jupiter system science

31

Data Volume (Tbits)

D J

End of Prime Mission

Model Payload Capabilities= vital forJupiteratmosphericscience

Visible Camera: Narrowfilters to probe strong
CH4 absorptions, cloud
strucure, wind tracking

Near-IR Spectrometer:
5-10 nm to capture ice
absorption; extend
beyond 5 µm for H2O
mapping

Sub-mm: Stratosphericwinds, temperatures,
H2O and trace species.

Model Payload Capabilities= vital forJupiteratmosphericscience

UV: Stellar occulations,high-altitude hazes,
chemistry,ionosphere/thermospherestudies

Thermal-IR: Narrowfilters to probe
tropospheric andstratospherictemperatures.

Radio science: USO
reference, multiple
opportunities to sound arange of latitudes.

+ Doppler spectroimager, thermal spectrometer, X-ray, etc?

Spatial Resolution••Best VIS/NIR resolution surpasses
Voyager, Galileo, New Horizons
Spatial resolutions for JEO (per pixel at9.5 RJ):
– Thermal Instrument: 1700 km– Wide-angle camera & UV spectrometer: 700km– Near-IR Spectrometer: 170 km– Medium-angle camera: 70 km– Narrow-angle camera: 7 km••

Standard JEO spatial resolution wouldbe ~2 times these values.
Jupiter science investigations call forhigher UV/IR spatial resolutions thansatellite science, a challenge toinstrument providers.

Jupiter feature tracking
Example: NAC from 19 RJ

Higher UV/IR spatial resolutions are desirable to match visible imaging.

Spatial Resolution

Optimumrange forcomparison ofvisible,
thermal andcompositionalresults

Spatial Resolution

Aim for even sampling ofphase angles for cloud
scattering and composition
studies.
Nightside for lightning
studiesDayside for cloud tracking

JEO and JGO Nominal Orbits

JEO
JGO

Radio Occultation – 2 Spacecraft

Unique Opportunities for JMO?

Unique Opportunities for JMO?

JEO Sub S/C Latitude: Polar Visibility

JGO Sub S/C Latitude: Polar Visibility

Science Example I: Climate Database••

Energy, momentum and material transport.
High data capacity, long baseline andsophisticated instrumentation should permit
frequent global maps of:– Material tracers (para-H2, phosphine,hydrocarbons, hazes)– Cloud changes (NH3 ice, H2O ice).
– Thermophysical properties (temperatures,potential vorticity).
– Windspeeds at multiple levels.
– Frequency distribution of lightning.

•Constantly evolving dynamic atmosphere:– Jets, waves, plumes, instabilities, upheavals, vortex
interactions.
– Origin, growth, redding and stability of large
anticyclones.

•Search for relationships between variables.

GRS 1992-1999

II: Waves, Periodicity & Coupling••

Waves permit
exploration offundamental fluidproperties andmeteorology, e.g.

Reuter et al., (2007)– Origin of instabilities
and mesoscale wave
production.
– Physics of the QuasiQuadrennial
Oscillation andinfluence on equatorial
dynamics•

Vertical waves couple
different atmosphericlayers•– Origin of thermosphericenergy crisis?

Friedson et al., 1999

Understand non‐seasonal
periodicities– Causes of upheavals: fadingand revival sequences– Changing turbulencesurrounding GRS

Acoustic Waves sample
density gradients of deepinteriorIII: Polar Processes•

Relationship between middle atmosphere andcharged particles of aurora/magnetosphere– Unique polar chemistry, energy sources?

•••

Nature of the polar hazes, origins of asymmetries,
aerosol production mechanisms.
Understand the UV ‘dark spots’ at high altitudes
Meridional transport of energy and chemicals fromequator to poles.
– Polar vortices and polygonal waves like Saturn?

Jupiter’s Poles: Unexplored Frontier
North PoleSouth Pole

Jupiter’s Poles: Unexplored FrontierNorth Pole

South PoleSun et al. (unpublished ISS Data)

Hot Poles of Giant Planets
NeptuneSaturnFletcher et al. 2007

Orton et al. 2007

Orton and Yanamandra-Fischer 2005

Polar Waves of Jupiter

Polar Hood in UV
Vincent et al (2000)

Polar Wave in UV – Near IR
Barrado-Izagirre (2008)

Polar High-Altitude Spots
Orton (personal communication)

Orton (personal communication)

UV Dark Spot
http://photojournal.jpl.nasa.gov/catalog/PIA03473

Blue Circle = Persistent Auroral Zone
While Circle = 60degN

Jupiter Aurora

Saturn Aurora (Cassini View)

Polar TurbulenceThree Dynamic Regimes• Equatorial Jet• Mid-Latitude Mixed Jets + Vortices• Polar TurbulenceLow-lat Jets  Polar Turbulence
Low-Latitude Condition

High-Latitude Condition

Sayanagi et al (2008)

Conclusions••

Community Input developed
Three Science Themes–Three themes encompass 11
investigations, designed to address
cross-disciplinary, ‘big picture’science.

–Complement and extend Juno/Galileo
results, address Cosmic
Vision/Decadal Survey questions.

ESJM offers considerable
potential for Jupiter science:––––Long baseline for regular temporalmonitoring observations.
Wide spectral range.
Dual spacecraft synergies.
Data volume capability for global 4D
mapping from the upper troposphereto the thermosphere.

Atmospheres Objectives:
A. Dynamics and Circulation
B. Composition and Chemistry
C. Vertical Structure•

Addresses unanswered,cross-disciplinary questions
about gas giant phenomena
and processes in the outersolar system.
––––Gas Giant Archetype
Planetary system template
Paradigm for Exoplanets
Laboratory for fundamental physicalprocesses.

JMO Participation in EJSM
Imaging Science by JMO can nicelycomplement the current JEO + JGO plan•

Current EJSM = JEO + JGO plans do not have extensive polar
imaging science coverage•Day-side observation has further room for improvement•Imaging Science Topics enabled by high-inclination orbit include:- Polar Waves/Atmospheric Dynamics- Vortex Life-Cycles- Polar Hood and North/South Asymmetry- Auroras and Magnetospheric Connection
Atmospheres Objectives:
A. Dynamics and Circulation
B. Composition and Chemistry
C. Vertical Structure

A little bit about my own recent work

Saturn’s Polar HexagonβHexagon: Seeing is Believing
Eastward
Wind Speedin m/s

Relative VorticityβRed = AnticyclonicBlue = Cyclonic
Green = Zero
Morales-Juberias et al.
(under review)Jet Width controls the Dominant Wavenumber

b =10 x10-10 [1/ms]

b =20 x10-10 [1/ms]
Relative Vorticity:
Red = AnticyclonicBlue = Cyclonic
Green = Zerob =50 x10-10 [1/ms]

b =30 x10-10 [1/ms]

βb =100 x10-10 [1/ms]

Comparison to Lab Experiment Study

Barbosa-Aguiar et al. (2010)

Saturn’s “Ribbon” Wave
Wavy Feature at New Latitude (~51ºN, 4000-5000 km wavelength)

47ºN Region – Cassini View
Un-Projected
Narrow Angle Camera Images

Ribbon Simulation
Relative Vorticity at the 100-mbar level
White Line traces the velocity peak of the 47degN jetComparison with Gulfstream MeanderingJupiter Atmospheric Science Goals
1. Chemical Composition
2. Thermal Structure

In-situ Sampling, Spectroscopy

Radio Occultation, In-situ,
Multi-wavelength Imaging

3. Nature of Cloud, Haze, Aerosols, Their Layering
In-situ, Multi-wavelength Imaging

4. Radiative Energy Balance
In-situ, Multi-wavelength Imaging, Bolometer

5. Atmospheric Dynamics
In-situ, (Multi-wavelength) Imaging