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Introducing the science teams at JAXA for the ESA CosmicVision Jupiter mission

Introducing the science teams at JAXA for the ESA CosmicVision Jupiter mission. Masaki Fujimoto Space Plasma Phys Div ISAS/JAXA. JAXA Missions to Planets. Mars: Nozomi (1998~2004: orbit insertion failed).

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Introducing the science teams at JAXA for the ESA CosmicVision Jupiter mission

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  1. Introducing the science teams at JAXA for the ESA CosmicVision Jupiter mission Masaki Fujimoto Space Plasma Phys Div ISAS/JAXA

  2. JAXA Missions to Planets • Mars: Nozomi (1998~2004: • orbit insertion failed) Study of plasmasphere & atmosphere ~ escape of the water ~ • Asteroid Itokawa: Hayabusa(2003~) Remote sensing and sample return ~ Origin of the Solar system ~ • Venus: Planet-C(2010~) Study of atmosphere ~ Mechanism of the super-rotation ~ • Mercury：BepiColombo (2013~) Mission for full-scale study of Mercury [ESA & ＪＡＸＡ] • Jupiter：Solar Sail (2012?) Engineering mission for “Solar Sail concept” with small orbiter for magnetospheric and atmospheric sciences

  3. We have been working together with ESA on BepiColombo. We have been thinking about a mission to Jupiter.

  4. Jovian Small Orbiter for Magnetospheric and Auroral Studies: “Solar Sail Project” “The pathfinder” for a possible future full-scale Jovian mission. We were not quite sure what that future missionwould be. Now we wish the ESA mission to be the full-scale mission.

  5. Jovian Small Orbiter for Magnetospheric and Auroral Studies [Engineering Target] * Establishment for feasibility of outer planet missions [Scientific Target] * In-situ observation of Jovian Magnetosphere & Auroral regions >10MeV electron model ? Quick-look observation in the vicinity of “most active objects in the Solar System” Target-1: Jovian-type “Magnetosphere-Ionosphere” coupling Target-2: Strongest “particle accelerator” in the solar system Polar region Radiation belt Payloads: <4kg (mainly based on the heritage of BepiColombo / MMO) [In-situ] - Magnetic field, Low-E / High-E particles, … [Remote sensing] - Auroral Image, Radio, Camera, … [Common] - Integrated Digital Processing & Power Supply Units Io torus Observation of Polar region & whole magnetosphere by in-situ & remote - Crossing auroral field lines of both hemisphere - Covering whole latitudes - Avoiding the Radiation belt entry

  6. Jupiter Z [RJ] X[RJ] Bow shock Y[RJ] Jupiter X[RJ] ○: 10days interval Small Jovian Orbiter Base Plan Orbit : “near Jupiter” x 300 Rj (230day) [Life: >1 year] - Crossing auroral field lines of both hemisphere - Covering from the solar wind to the region within the radiation belt

  7. Remote sensing~Polar region of Jupiter~ Candidates Mass Objectives Remote Auroral imager (Priority-1) 1.5kg Auroral / Lightening observations Radio/Waves with antenna in sail (Priority-2) 0.5kg Radio / wave activities which can not be observed from Earth (few 10k ～ few tens MHz) Wide-field camera (Priority-3) (0.5kg) Jovian atmosphere (with Probe entry) UV image of HST X-ray image of Chandra

  8. In-situ observation: ~Solar wind – Magnetosphere – Jupiter Coupling ~ Candidates Mass Objectives Local: -Flyby -Magnetosphere -Solar wind Magnetic field (without boom) (Priority-2) 0.5kg [0.1kg] Magnetic field structure & current system High-E particles (Priority-2) 0.7kg [0.3kg] Auroral accerelation region Low-E particles (Priority-2) 0.7kg [0.3kg] Solar wind monitor Detection of mass outflow from Jupiter Common Digital / Power TBD Integrated for the mass reduction Multi-scale Magnetospheres in universe Acceleration Convection

  9. Atmospheric Entry Probe ~ option: if possible~ Payload: < several 100g in total ? <higher altitude> * Magnetic field Multi-point studies of Jovian magnetic field * Radiation beltHigh energy particle monitoring * Lightening detection Narrow-band radio detection * H2O detectionSimple IR-spectrometry <lower altitude>

  10. Jovian Entry Probe Jovian Orbiter Mother Spacecraft Solar Sail Project:The Mother S/C System: Complex of Mother, Daughter, and Probe * Mother : ~300-500kg Flyby of asteroids and Jupiter * Daughter : ~100kg Jovian orbiter * Probe : ~30kg [option] Jovian entry probe [Mother] * Cosmic IR background * Gamma-ray burst detection in deep space * Dust measurement with a largest detector * Flyby of asteroids in main belt & Trojan group

  11. For the ESA mission: The team leaders • Theme 1 ・Characterize Europa as a planetary object and a potential habitat • Theme 2 ・Study the origin, formation and evolution of the Jovian satellites system S. Sasaki (NAOJ Mizsawa) sho@miz.nao.ac.jp • Theme 3 ・Jupiter system science: magnetosphere and nebula T. Takashima (ISAS/JAXA) ttakeshi@stp.isas.jaxa.jp • Theme 4 ・Jupiter system science: atmosphere Y. Takahashi (Tohoku U) yukihiro@pat.geophys.tohoku.ac.jp

  12. Team 1&2: theory-oriented • Interested to get Information on The sub-disc properties and structure The final stage of the Jovian accretion from the amount of the heavy elements in the envelope via search for water-bearing minerals on the satellites (c.f., Amalthea, Thebe) Europa vs Titan: why are they so different? Methane captured in fractured ice Europa vs Ganymede: rocky vs icy sea floor? The sea salt on the surface ・The ice crust thickness Radio Sounding

  13. Finding Jupiter’s moon sea below the ice surface by HF sounder Observation of plasma structure around Jupiter’s moon by MF/LF sounder Europa Ganymede Io Callisto Ganymede’s ionosphere? fUH=100kHzNe=100/cc Space e=1 Echo from Ice surface Skin depth Ice e=3 s=6mS/m Echo from Water surface Water e=80 Reflectivity [Gurnett et al., 1996]

  14. Team 3: The Plasma Universe • BepiColombo(Mercury), XScale(Earth) and the Jupiter mission as a set High quality data and SW/IMF monitor Global via imaging and in-situ at the same time Orbit determines the science Orbit that enables us to pursue fundamental plasma physical processes

  15. Instruments we are especially interested in • Heavy ion acceleration 20-200 keV (MEP) and beyond up to 10MeV(HEP) • Plasma wave sounder multi-purpose • UV/soft-X-ray Imager for Aurora • EUV imaging of the plasma • Continue to update the ground observatory at Tohoku U

  16. Team 4: The Cloud Dynamics • Experience in Planet-C (Venus Climate Orbiter) • Experience in ground based observations Lightning as a sensing tool for violent vertical convection

  17. CH4 798 nm NH3 791nm NH3 930 nm Reflectivityobsλ CH4 725 nm CH4 890 nm Wavelength [nm] 750 nm 800 nm 890 nm Instrument-wise • Multiple probes down to 20bar depth At least, one in a belt and another in a zone • Usage of LC variable wavelength filter CH4,NH3 absorption line, H2O at 940nm • Lightning detection High-speed optical, X/Gamma ray

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