2 jun 2022 jan 2030 sep 2032 jun 2033 11 months 1 month 9 months 11 months 9 months launch ariane-5...
DESCRIPTION
Europa Ganymede Callisto 3TRANSCRIPT
Towards a Radiation Monitor for the Jovian System
Patrícia Gonçalves
New Worlds in Particle, Astroparticle & CosmologyBraga, January 2014
JUICEThe Jupiter Icy Moons Explorer
2
Jun2022
Jan2030
Sep2032
Jun2033
11 months
1 month
9 months
11months
9 months
Launch
Ariane-5
Jupiter
orbit insertion
Transfer to Callisto
Europa phase: 2 Europa +2 Callisto flybys
Jupiter High Latitude Phase
Transfer to Callisto
Ganymede Orbit
insertion
Ganymede tour:Orbits at several altitudes: High altitude500 km200km
End of nomin
al missio
n
Next Class-L (Large) ESA Mission
Current JUICE mission plan
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Study the emergence of habitable worlds around gas giants
• Characterise the Jupiter Icy Moons: Ganymede, Europa and Callisto as planetary objects and potential habitats •Explore the Jovian system as an archetype for gas giants
EuropaGanymedeCallisto
Juice Mission Objectives
Juice mission
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Implications for Astrophysics & Planetary Physics
Extra Solar Planetary Systems
The Plasma UniversePlanetaryAtmospheres
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Juice Scientific Payload11 instruments with total mass of ~100 kg
Narrow Angle CameraWide Angle CameraVisible and Infrared Hyperspectral Imaging SpectrometerUltraviolet Imaging SpectrometerSubmillimetre Wave InstrumentLaser AltimeterIce penetrating radarMagnetometerParticle PackageRadio and Plasma Wave instrumentRadio Science Instrument and Ultrastable Oscillator
Possible configuration
for Scientific Payload
accomodation
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Jovian System Energetic Particle Environment
Severe environment in terms of ionizing particles
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Courtesy of H.B.Garret, Jet Prop.Lab
Data and models Limited data from
Missions- Pioneer 10-11 (1973, 1974) - Voyager 1-2 (1979)- Galileo (1989)- Ulysses and Cassini (2000)
Synchrotron emission observations
Synchrotron emission predictions from Divine model
Models-Divine e- and proton models- GIRE (Galileo Interim Radiation Environment Model)- Salammbô(e-belt model from Jupiter surface to Europa)- JOSE (based on Divine+GIRE+Salammbô+data)
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Very Hard Electron Spectrum
40 MeV300 keV
What is a radiation monitor?
1Radiation
Housekeeping
2Alert and
safeguarding
3Support to
platform and payload
4Future mission preparation & provision of science data
Particle detector Mass ~ 1 kg
Power ~ 1 WattVolume - 1 lt
RADEM Radiation Hard Electron Monitor
RADEM requirements:
Electron detectorSpectral range 300 keV – 40 MeVPeak flux 109 e/cm2/s
Proton and heavy ion detectorSpectral range 5 MeV – 250 MeVpeak flux 108 p/cm2/s
Radiation harddose determination and alarm function
Particle separation from Helium to Oxygen; LET spectra
Phase A RADEM Model (PSI)
A radiation monitor is a key piece in keeping the mission safe but it can also provide valuable scientific data!
ESA RADEM PROTO-FLIGHT model
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LIP is in a consortium with european institutes and industry
for phases B2, C and D, to develop, qualify and build
RADEM PROTO-FLIGHT MODEL
2.5 year project - February 2014 to July 2016
RADEM Phase A and B1 Preliminary Analysis and Definition ( PSI & RUAG) Complete
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Proton Telescope 8 Si layers, 8mm Copper shielding) Electron Spectrometer
permanent magnet
Credits to Wojtek Hadjas & Laurent Desorgher (PSI) @ ESA Space Radiation Workshop, May 2012
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Electron directionality
Ganymede Flyby
304–527 keV electrons
DATA: EPD measurementsGalileo G29 encounter with GanymedeDecember 2000
Electron Directionality Detector
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An additional detector module for RADEM
31 Si sensors (300 μm) = 22.5o , φ = 36o & FOV= 7.2o
Shielding:8 mm Copper to stop electrons with E < 10 MeV
300 μm Al absorber stops e- with E < 300 keV & protons with E< 6 MeV
Collimators
y
z
x
y
Electrons 300 keV < E < 10 MeV
Preliminary Assessment with GEANT4
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Electron Directionality DetectorPreliminary assessment
Geant4 models of the detectors interfaced with electron, proton and ion source spectra predicted by the JOSE model at different locations in the Jovian System.
WORK IN PROGRESS
θ
e-
Primary Electron Incident angle θ (deg)
300keV- 10 MeVElectrons> 10 MeV
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Electron Directionality DetectorPreliminary assessment
300keV- 10 MeV electrons
WORK IN PROGRESS
Primary Electron Incident angle θ vs ϕ (deg)
300keV- 10 MeVElectrons
Primary Electron Incident angle θ (deg) vs Kinetic Energy (MeV))
Electron Directionality Detector
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Ongoing DD Concept Optimization Studies
- trade-off in the number of sensors : 31 vs 24 vs 16 … ( 32 channel ASIC ) - include extra sensors below shielding to veto background- …
Detector configurations and readout to be optimized during design, development and calibration of RADEM .
Improved design
WORK IN PROGRESS !
RADEM
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DD integration in RADEM
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It is not every year “we” travel to Jupiter!
The exploration of the Jovian System is an engineering & scientific challenge
RADEM will be ESA “small” tool to study the Energetic Particle Environment of a giant and complex magnetosphere
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Outlook
LIP participates in a consortium with scientific institutes (PSI & LIP) and with the industry (RUAG,
IDEAS, EFACEC) for the development of a proto-flight model of
RADEM
due to the complex and radiation hard environment, there are strong limitations for thr JUICE mission
a radiation monitor is a key piece in keeping the mission safe but it will also provide valuable scientific data.
The exploration of the Jovian System is an engineering & scientific challenge!
WORK IN PROGRESS
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It is not every year “we” travel to Jupiter!
Electron Directionality DetectorAn additional detector module
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Cumulative dose for the Juice mission
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Electron Directionality DetectorPreliminary assessment
Deposited Energy vs. Primary Electron Kinetic Energy (MeV)
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Europa
Ganymede
Callisto
Io
Jupiter
The Jovian Icy Moons
Ice layer. Thickness?
Liquid water?
Surface and Subsurface
composition Geology
Loc environmentInteraction with
JM
Ice layer. Thickness?
Liquid water?
a cold rigid ice crust, an outer warm ice mantle, an inner silicate mantle, and a metallic core
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Model of Callisto's internal structure showing a surface ice layer, a possible liquid water layer, and an ice-rock interior
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Model of Europa's interior showing a solid ice crust over a layer of liquid water or soft ice, a silicate mantle and a metallic core.
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Very Hard Electron Spectrum
Worst case integral electron flux spectra for worst averaged over 24 h and 20 min.
Earth - GEO
Jupiter - JUICE
Electron Flux #/(cm2.sr.s)
0.2 MeV 5 MeV
Jupiter -JUICE ~5 x E+7 ~5 x E+5
Earth - GEO 1 x E+7 /4π 1 x E+1 /4π
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Particles in the magnetosphere
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