La magnétosphère de Jupiter avant JUNO
P. Zarka LESIA & USN
NASA’s 2nd New Frontiers mission https://www.missionjuno.swri.edu/
PI: Scott Bolton (SwRI) • ~60 Co-Is, ~10% Fr. • Solar-powered, spinning spacecraft • 8 Science instruments • Launched 5 August 2011 • 5-year cruise to Jupiter • Arrives at Jupiter 4 July 2016 Juno Science Objec ves
Origin Determine O/H ra o (water abundance) and constrain core mass to decide among alterna ve theories of origin.
Interior Understand Jupiter's interior structure and dynamical proper es by mapping its gravita onal and magne c fields
Atmosphere Map varia ons in atmospheric composi on, temperature, cloud opacity and dynamics to depths greater than 100 bars at all la tudes.
Magnetosphere Characterize and explore the three-dimensional structure of Jupiter's polar magnetosphere and auroras. Juno - Spacecra & Payload SPACECRAFT DIMENSIONS Diameter: 20 meters JunoCam Height: 4.5 meters camera UVS UV spectrometer Waves Radio & plasma JIRAM JEDI IR spectrometer High-energy particles JADE Gravity Science Low-energy particles Magnetometer
MWR Microwaves Juno Payload
Gravity Science (X and Ka Band) — GRAV (JPL/ASI, Folkner)
Microwave Radiometers (6) — MWR (JPL, Janssen)
Magnetometer — MAG (GSFC/DTU, Connerney)
Energe c Par cle Detectors (3) — JEDI (APL, Mauk)
Jovian Auroral Distribu ons Exp. (4 → 3) — JADE (SwRI, McComas)
Waves — (U of Iowa, Kurth)
UV Spectrometer — UVS (SwRI, Gladstone)
IR Camera/Spectro — JIRAM (ASI, Adriani)
+ Camera — JunoCam (Malin, Hansen) Juno Mission Plan
Baseline mission: 32 polar orbits
Perijove ~5000 km
14 day period Polar Magnetosphere Explora on
Loca on is Key: Juno passes directly through auroral field lines.
A suite of instruments is used to understand the physics: JADE, JEDI, MAG, Waves, JIRAM, UVS Juno Orbit In Magnetic Coordinates
15 15 Perijove 3 Perijove 3Perijove 17 Perijove 17Perijove 31 Perijove 31 Perijove 2016 DOY 315 16:46 Perijove 2016PerijovDOY 31e520116:746DOY 103 07:28 Perijove 2017PerijovDOY 10e320107:728DOY 256 21:49 Perijove 2017 DOY 256 21:49 10 10
5 5 315 315
103 103 ) ) J J (R (R 0 0 z z
-5 -5 256 256
-10 -10
5 10 15 20 25 305 105 1510 2015 2520 3025 305 105 1510 1520 2520 3025 305 10 15 20 25 30 ρ(R ) ρ(R ) ρ(R ) ρ(R ) ρ(R ) ρ(R ) J J J J J J Early orbit Late orbit Auroral field lines crossings
PJ5 Science Ac vity Period PJ 50 North starts DOY 334 = 11/29/2016 15:52 As Seen From Above North Pole
Juno Orbit #5 50 10 Pj 5 2016 335 15:51:60 70
5 270 90 334 335
0 ]
J VIT4 VIP4 VIPAL Khurana −5 180 336
Z magnetic [R PJ 50 South As Seen From Above North Pole −10 −50
337 −70 −15
270 90
−20 0 5 10 15 20 25 30 Rho [R ]
VIT4 VIP4 VIPAL Khurana 180 Key measurement « Perfect » magnetic field model post JUNO → reliable context for magnetospheric studies Key measurement « Perfect » magnetic field model post JUNO → reliable context for magnetospheric studies Open questions (After Bagenal et al., Space Sci. Rev., 2014 + update STM 2016/03) http://lasp.colorado.edu/home/mop/resources/hosted-meetings/junostm16/workshop-on-jupiters-aurora/
STRUCTURE • Is the kink of the oval a longitude or Local Time effect ? Why is the north auroral ≠ from the south ? • Is there a polar cap with open field lines ? Of what size ? Variability ? • Where do the dark regions and various auroras map ? • How do the polar regions relate to the long magnetotail observed by Voyager 2 and New Horizons ? Open questions DYNAMICS • What is the role of the solar wind ? How is the magnetosphere coupled to it ? How deep does its influence penetrate the magnetosphere ? How does it (+shocks) modulate the main oval + radio emissions ? Relatively to internal dynamics ? • Over what timescales does Io volcanic activity affect magnetosphere? Io’s Sodium Nebula Open questions
DYNAMICS • How much mass and momentum are transferred through the magnetopause ? Is there reconnection (at high-latitude?) vs small-scale Kelvin-Helmholtz Instability ? • What is the origin of quasi-periodic flares ? Ionosphere modulated ? in phase ? How can distant regions communicate ? • Are there Planetary Period Oscillations at Jupiter ? Observable ? Are Saturn’s PPO comparable to system IV ? UV brightness
Where KH instabilities are probable
Where magnetic reconnection is probable β=10 >16MeV electrons β=1 Open questions AURORA • How are the x-ray/UV/Vis/IR/radio emissions related ? • What is the source of the various auroras ? Why is there (transient) UV emission everywhere at high latitudes ? How can there be emission on field lines that should connect to the sw (don’t quite see this at other planets) ? • Do auroras reveal the energy and mass transfer in Jupiter’s magnetosphere ? • What is the relationship with local injections (importance, scale size) ?
Auroral Patch Open questions AURORA • What is the source of the various auroras ? Why is there (transient) UV emission everywhere at high latitudes ? How can there be emission on field lines that should connect to the sw (don’t quite see this at other planets) ? • Where does the downward current region(s) lie(s) ? • How does f-a current density relate to auroral intensity ?
Downward Current?
Upward Current Alfven Aurora Alfven Aurora
Upward Current Downward Current Alfven Aurora Jupiter’s Main Oval: Upward Current Region
(1)Parallel electric fields (double layers). (2)Perpendicular electrostatic shocks. (3)Accelerated electrons. (4)Anti-Earthward ion beam. (5)Strong wave activity. (6)Deep density cavity. Upward Current Region: Electric Fields & electron energies
FAST ORBIT 1858 FAST ORBIT 1858 500 500 250 250 0
(mV/m) -250 0 -500 (mV/m) 1000 -250 500 -500 0 -500 1000 (mV/m) -1000 -1500 500
) -3 10 0 -500 5 (mV/m) -1000 5 to 50 V/m
Density (cm 0 -1500 4 9
10 ) 103 -3 10 500 km, 10 s
2 -s-sr-eV 10 2 Log eV/
1 cm Electrons (eV) 10 6 5 7 104 103 Density (cm Electric 0 field amplitudes should be considerably
2 -s-sr-eV 10 2 Log eV/ Ions (eV)
1 cm larger4 and, depending on boundary layer 9 10 4 10 101 -4 thickness, much faster time scale.
/Hz 3 2 10 100
2 -s-sr-eV 10 2 Log eV/ Freq. (kHz) -1
10 -12 Log (V/m)
Electrons1 should have higher energies. cm
UT :06:35 :06:40 :06:45 :06:50 :06:55 :07:00 Electrons (eV) 10 6 ALT 3953.1 3950.3 3947.4 3944.5 3941.6 3938.6 ILAT 70.8 71.0 71.1 71.2 71.3 71.4 MLT 21.2 21.2 21.2 21.2 21.2 21.2 4 7 Minutes from 1997-02-09/06:06:35 10 103
2 -s-sr-eV 10 2 Log eV/ Ions (eV)
1 cm 10 4 101 -4 /Hz 2 100
Freq. (kHz) -1
10 -12 Log (V/m) UT :06:35 :06:40 :06:45 :06:50 :06:55 :07:00 ALT 3953.1 3950.3 3947.4 3944.5 3941.6 3938.6 ILAT 70.8 71.0 71.1 71.2 71.3 71.4 MLT 21.2 21.2 21.2 21.2 21.2 21.2 Minutes from 1997-02-09/06:06:35 Alfven Aurora
Ionospheric resonator at Jupiter ~20 Hz (Earth is <1 Hz) ⇒ Jovian S-bursts ? Downward Current Region: Where is it ? What to look for ?
(1) Anti-Jovian accelerated electrons: field-aligned and broader energy. (2) Strong wave activity (3) Parallel electric fields (double layers). (4) Perpendicular electrostatic shocks (diverging). (5) Ion conics. Open questions ACCELERATION • X-ray aurora is unique on Jupiter, how/why ? Are there MeV potential drops ? • Is there energetic particle precipitation of 100s of keV (Are atmospheric models reliable) ? Why are the precipitating electrons so energetic ? How does the auroral acceleration process work at Jupiter ? Are they completely different from Earth ? • Heating vs acceleration for producing energetic plasma ? • What is the altitude/vertical structure of the acceleration region above aurora ? Satellite footprints ? • What mechanisms accelerate particles to radiation belt energies (injections, w-p, etc.)?
X-ray emissions Open questions
RADIO / WAVES • Where and how are auroral radio components generated ? • Is the Cyclotron Maser oblique mode dominant (why) ?
Resonance condition : Growth rate : Oblique/ Loss-cone Open questions RADIO / WAVES • Will in-situ JUNO measurements permit us to address Cyclotron Maser microphysics in unexplored regimes (100s keV) ?
10
8
6
4 (%)
ce fcutoff
)/f 2 ce
(f-f 0
-2 fCMI -4 A B C 08:12 08:24 08:36 08:48 09:00 09:12 Day 2008-291 (h:m) Open questions
RADIO / WAVES • Are there Double-Layers, Electron/Ion holes in auroral regions? • How are they related to Up/Down/Alfvén regions ? How interleaved ? • Role of plasma waves in the auroral acceleration region ?
T ~ 1.5 eV
~ 200 s ? T ~ 0.14 eV
0 0 Open questions SATELLITES • How different are acceleration processes in the Io spots and in the wake ? • Does Ganymede interact with Jupiter’s B field via reconnection of Alfvén waves ? • Is there heavy mass loading from Europa (e.g. via atmospheric escape)? UV wake? Radio emission?
Ganymede footprint
Europa footprint Comparisons with Cassini
(16 sept. 2017) JUNO’s Earth-based Suppor ng Observa ons
+ • HST UV, IRTF H3 , Giant Telescopes: COMICS, VISIR, CanariCam (Mid-IR) • Professionals, Amateurs → Glenn Orton coordinator
• HISAKI / EXCEED, small JAXA EUV spectrometer in Earth orbit (Kimura et al.)
• Radio Decameter : Nançay Decameter Array (France), LOFAR (various European loca ons), UTR-2, URAN 1-4 (Ukraine), LWA (USA), Tohoku U., Fukui Inst. Tech., U. Elect. & Comm., Kochi U. (Japan), Radio Jove = “Juno Ground Radio” → Bap ste Cecconi, coordinator → VO / VESPA, MASER web site @ Meudon
• JUNO dedicated receiver at Nançay Decameter Array
• Synchrotron observa ons (LOFAR) : Daniel Santos-Costa, Julien Girard et al. (coll. ONERA)
Data
• JUNO data will be put into the PDS within 6 months → public !
Related Posters
• Ionosphere-magnetosphere coupling studies with Juno and Cassini proximal orbits M. Blanc, N. André, P.-L. Blelly, V. Génot, P. Louarn, A. Marchaudon, C. Peymirat, C. Tao, B. Cecconi, L. Lamy, C. Louis, Ph. Zarka, S. Hess, A. Sicard, F. Mo ez
• Modéliser les émissions radio aurorales joviennes avec SERPE C. Louis, L. Lamy, P. Zarka
• Europlanet/VESPA et les plasmas du système solaire B. Cecconi, S. Erard, P. Le Sidaner, N. André, V. Génot, M. Gangloff
IRAP / Meudon / ... workshop(s)
JADE
JADE-E JADE-I 2 (3 Sensors)
Energy Range 100 eV – 100 keV 10 eV/q – 50 keV/q
ΔE/E 10-14% (depends on E) 18-28% (depends on E) FOV (Inst) 360°x 3-6° 270°x 8.5°
FOV Tracking Uses 1s Mag data - Pixels/Res 2 3 Sensors x 16 / 7.5° 12 / 22.5° Mass Range - 1 - 64 amu M/ΔM - 2.5 – 11 (depends on M & E) G factor/pixel ~2-5 x10-5 cm2 sr eV/eV ~4 x10-5 cm2 sr eV/eV
Time Res Full PAD each 1s 4π each 30s spin JEDI Juno Waves Overview
Electric Antenna
Preamps & Electronics
Instrument Characteris cs Spectral Coverage 50 Hz – 20 kHz Magne c Spectral Coverage 50 Hz – 40 MHz Electric Spectral Resolu on ~20 Channels/decade
Search Coil Periapsis Mode Cadence 1 spectrum/s LF and MF Burst Modes Waveform Captures in all bands to 150 kHz triggered onboard HF Burst Modes Ability to select a 1-MHz band including fce Juno
34 Juno
35 Juno
36 Juno
37