Post on 18-Dec-2015
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -1-
BepiColombo MMO Plasma Wave Investigation (PWI)
Jan 7 2009 PWI MeetingJan 8 2009 MMO-SWG meeting
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -2-
PWI○ Magnetic field: Why does Mercury have? → Precise measurement of magnetic field structure enables the structure & origin of the internal fields.
○ Magnetosphere: No ionosphere & Different scales → Detailed structure/dynamics/energetic process show what is general / special in Magnetosphere physics.
○ Exosphere: Highly variability → Observations of structure & variations of Na Exosphere enable its generation/loss & origins.
○ Inter planetary space in the most inner solar system → Highest Mach number shocks (~40) which are only directly observed around the Mercury. Statistics & origins of Dusts in the inner solar system.
Model of Magnetosphere / ExophereMagnetosphere different from the Earth pgenerates the comparative study of the planetary Magnetosphere.
?
Discovery of magnetic field by Mariner10
Internal magnetic field describes the internal structure & its evolution
Mercury is the unique terrestrial planetwhich still keeps its magnetic field, except Earth. -Why does this planet have magnetic field? -How is the magnetosphere similar or different ?
Mercury is the unique terrestrial planetwhich still keeps its magnetic field, except Earth. -Why does this planet have magnetic field? -How is the magnetosphere similar or different ?
Bepi will make first complete study ofHerman Magnetic field & Magnetosphere
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -3-
*Agenda (7 Jan 2009)1300 EWO1340 SORBET1420 AM2P1500 MEFISTO1540 WPT1600 Software1640 EMC1720 Overall test plan & Schedule in 2009
<REQUEST for each> 1. Summary of Previous Action Items[from the past!]
2. Summary Report of EM/STM test-Internal development / test status
ALL CRITICAL ITEMS must be trased.-I/F development / test status
ALL CRITICAL ITEMS must be trased.3. Summary Plan of EM/STM test
[especially from Jan to June]4. Summary of Current&New Action Items
[to the next!]
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -4-
1. Team Structure [Jan 2009]PI Yasumasa Kasaba (Tohoku Univ.)
Co-PI Jean-Louis Bougeret (Obs. de Paris)
Co-PI / MEFISTO Lars Blomberg (KTH)
Co-PI / EWO / Eng. Manager Hirotsugu Kojima (Kyoto Univ.)with [EWO/EFD] Keigo Ishisaka (Toyama Pref. Univ.)
Co-PI / LF-SC Satoshi Yagitani (Kanazawa Univ.)
SORBET Michel Moncuquet (Obs. de Paris)
AM2P Jean-Gabriel Trotignon (LPCE/CNRS)
DB-SC Gerard Chanteur (CETP/IPSL)
WPT Atsushi Kumamoto (Tohoku Univ.)
Software Y. Kasahara (Kanazawa Univ.)with Janos Lichtenberger (Eotvos Univ.)
Theoretical/Data Yoshiharu Omura (Kyoto Univ.)with [Data] Takeshi Murata (Ehime Univ.)with [Theoretical] One European member
PI Emeritus Hiroshi Matsumoto (Kyoto Univ.)
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -5-
2. Science
*Close-relationship shall be expected with : - All in-situ measurements --- Synchronous Measurements for
Electric Field : Plasma Motion / AccelerationWaves : All energetic processes etc.
Onboard Triggering for Short & Transient phenomenaElectron density & temperature
- MMO/MDM --- Plasma ejection by dust impact
- MPO/MAG & Serena --- Remote sensing of possible radio waves--- Simultaneous propagating wave measurement
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -6-
PWI will observe plasma/radio waves in Mercury, which no man has seen before.
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -7-
0 .1 1 1 0 1 0 0 1 k 1 0 k 1 0 0 k 1 M 1 0 M
E le c t ro n P la s m a F re q .
E le c t ro n C y c lo t ro n F re q .
S o la r B u rs tMe rc u ry My ria m e t ric ?
E le c t ro n p la s m a w a v e s (LW, EC H, 2 fp )Io n A c o u s t ic w a v e s
Wh is t le r m o d e w a v e
Io n C y c lo t ro n F re q .
A lf v e n / Io n C y c lo t ro n w a v e s
Io n P la s m a F re q .
EF D ( MEF IS T O / WP T )O F A - E/ WF C - E(MEF IS T O / WP T )
F re q u e n c y D ia g ra m
[ Hz ]
O F A - B / WF C - B / S O R B ET (LF - S C / D B - S C )
S O R B ET ( MEF IS T O o r WP T )
S O R B ET ( D B - S C )
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -8-
2. Magnetosphere/ Closed field lines ULF waves and pulsations5. All regions Study of the macroscopic structure of the Mercury
magnetosphre7. All regions Macroscopic electric field17. Everywhere / close to Mercury Synchrotron radiation (escaping)
L(s
urv
ey)
PWI baseline of the concept [based on the discussion in the Paris PWI science meeting]
L-Mode
*Requested Target
*Expected Performance[Data Acquisition Interval]
- Density : Surveywith high time resolution … 8 Hzwith precise measurement … 1/16 Hz
- DC Electric Field & ULF Wave Measurement (Ion Cyclotron / Alfven)with synchronicity to MGF … 8 Hz
- Spectrum : Minimum-resolutionwith medium frequency resolution … 1/16 Hz df/f = 230%with medium time resolution … 1 Hz df/f = 12%
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -9-
3. All regionsStudy of the electron kinematics in and around the Mercurymagnetosphere
4. All regionsStudy of Non- MHD plasma characteristics in and around theMercury magnetosphere
6. All regions Type II, Type III8. All regions Electron cyclotron waves10. Magnetosphere(Boundaries,Interior)
Non thermal continuum radiation
13. Magnetosphere/ Magnetosheath(Tail)
Alfven waves, Ion cyclotron waves, Ion turbulence excitedby the non- gyrotropic heavy ions. The situation is similar tothe wave instabilities driven by cometary ions. This processmay take place in the whole regions of the Mercurymagnetosphere.
18. Magnetosphere (Polar) Ion acoustic waves, Ion hole19. Polar cusp Kinetic alfven waves, Whistler mode waves22. Bow shock: Transition,downstream region
Ion acoustic wave, Electron acoustic wave, Electron hole
23. Bow Shock: Ion foreshock Alfven waves, Ion cyclotron waves24. Bow shock: Electron foreshock Langmuir waves, 2fp emission, electron hole
M (
nom
inal
)PWI baseline of the concept [based on the discussion in the Paris PWI science meeting]
M-Mode *Requested Target
*Expected Performance- Density, DC Electric field, and ULF waves … same as L- Spectrum : Fine frequency resolution … 1/2 Hz df/f = 2%
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -10-
9. Magnetosphere (Tail) :Boundaries: Magnetopause, Plasmasheet (if exists)
Lower Hybrid waves, Electron cyclotron harmonic: Modeconversion/ Drift instability such a Lower Hybrid DriftInstability
11. Magnetosphere (Tail) : Plasmasheet, Lobe
Langmuir waves, ECH waves, Electron hole generated byelectron beam instabilities. That can be observed in theplasma sheet boundary layer or the separatrix region justclose to the plasma sheet boundary.
12. Magnetosphere (Tail)Magnetopause boundary (if exists)
Ion acoustic mode, ion hole, electron hole
14. Magnetosphere (Tail) : Periapsisin the night side region
The temperature anisotropy of trapped electrons around themagnetic equator destabilize the Whistler mode waves.Similar situation can be appeared in the generation ofChorus emissions in the terrestrial magnetosphere.
20. Magnetosphere (Dayside) Ion acoustic waves, Ion hole21. Magnetosheath Lion's roar
M(f
ast)
[M
-H?)
PWI baseline of the concept [based on the discussion in the Paris PWI science meeting]
M-H Mode *Requested Target
*Expected Performance
- Density, DC Electric field, and ULF waves … same as L- Spectrum : Fine frequency resolution … 2 Hz df/f = 8%
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -11-
1. Regions including dust Dusty plasma diagnostic (dust typical grain size, dust plasmacooling)
15. Magnetosphere(Tail): Preiapsis inthe night side region
Whistler mode transients generated by seismic processes
16. Magnetosphereperiapsis in the night side region
Triggered emissions by wave- particle interaction
25. Solar wind Short impulse whistler mode wave26. Solar wind: CME/ CIR Langmuir waves, Whistler mode wave
H(t
rigg
er)
PWI baseline of the concept [based on the discussion in the Paris PWI science meeting]
H-Mode *Requested Target
*Expected Performance-RAW waveform data triggered by specific conditions
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -12-
3. Telemetry
*Close-relationship shall be expected with : - All in-situ measurements --- Synchronous Measurements for
Electric Field : Plasma Motion / AccelerationWaves : All energetic processes etc.
Onboard Triggering for Short & Transient phenomenaElectron density & temperature
- MMO/MDM --- Plasma ejection by dust impact
- MPO/MAG & Serena --- Remote sensing of possible radio waves--- Simultaneous propagating wave measurement
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -13-
Receiver Data total (kbps)
Packet to MDP
EWO-EFD DPB[Sweep]
128Hz x 16bit x 2ch (sync)(1024Hz x 16bit x 2ch x 0.5/4sec (sync)
4.1Unit: 6.1kB
Interval: 4secSPB 32Hz x 16bit x 4ch (non-sync) 2.0
Total 6.1
EWO-OFA/WFC(E)SW-mode
MS-mode
SW-AM2P-mode
349.525kHz x 14(16)bit x 2ch x
(0.117/0.8125)sec 65.536kHz x 14(16)bit x 2ch
349.525kHz x 14(16bit) x 2ch x 0.468sec
1611or
2097
1938(2.7sec
)
Unit: 2kB
Interval:8ms
EWO-OFA/WFC(B)MS-mode
SW-mode
65.536kHz x 14(16)bit x 3ch
16.384kHz x 14(16)bit x 3ch
3146or
786
Unit: 3kBInterval:8ms
SORBET Apoapsis mode
132ch x 12bit x 1/8sec x 3 0.6Unit: 0.8kB
Interval: 1 spin
(~4sec)
Periapsismode
132ch x 12bit x 1/4sec x 2 1.0
PWI RAW data production [Jan 2009] (non-compression)
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -14-
*1) Data rate in the magnetosphere/solar wind.*2) Data rate is same as Bit-M mode
Receiver Data bit ch Raw (kbps) Bit- L (kbps) Bit M (kbps) Bit- H (kbps)
Total 6.1 0.397 0.436 6.1 kbps
Spectrum 8 2 L: 13ch x 2(X/ Y) x 8bit x 1/ 16HzM: 13ch x 2(X/ Y) x 8bit x 1/ 4Hz 0.013 0.052
E- Vector 16 3L/ M: 2(X/ Y) x 16bit x
8Hz0.256 0.256
Potential 16 4 L/ M: 1 x 16bit x 8Hz 0.128 0.128
Total 2097/ 1611 (*1) 0.09 / 0.13 1.6/ 2.40.8- 2.6 Mbps
(E&B)
Spectrum 8 2 0.09 / 0.13 1.6/ 2.4
Total 3146/ 786(*1) 0.09 3.2 ^
Spectrum 8 3 0.09 3.2
Total0.049(Min)0.195(Max)
0.585 (Apo)0.975 (Peri)
***
TNR 12 20.025(Min)0.099(Max)
0.297(Apo)0.495(Peri)
Phase 12 2 0 0.192
HFR 12 20.024(Min)0.096(Max)
0.096(Apo)0.288(Peri)
AM2PL: 1/ 32 spin (1.8kB each)M: 1/ 16 spin (1.8kB
0.113 0.225 ***
Total 5.2Mbps / 4.8Mbps0.74 Min)(0.93(Max)
6.0 (Min)7.2 (Max)
0.8- 2.6 Mbps
SORBETL: 16- 64secM: 8sec(Apo) / 4sec(Peri)
EWO- EFD
EWO- E
EWO- B
PWI TLM Production from MDP [Jan 2009] (non-compression)
[50% compression]
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -15-
PWI TLM Production from MDP [Jan 2008] (non-compression)
*1) Data rate in the magnetosphere/solar wind.*2) Data rate is same as Bit-M mode
Bit H: 56kbps(After data compression)
Receiver Data bit ch Raw (kbps) Bit- L (kbps) Bit M (kbps)Bit- H(kbps)
Total 4.608 0.027 0.576 4.608
Spectrum 8 2 0.013 0.128 (*2)
E- Vector 16 3 0.006 0.384 4.096
Potential 16 4 0.008 0.064 (*2)
Total 1920/ 1152 (*1) 0.08/ 0.12 1.5/ 2.3 TBD
Spectrum 8 2 0.08/ 0.12 1.5/ 2.3 (*2)
Waveform 16 N/ A N/ A TBD
Total 2880 0.11 2.3 TBD
Spectrum 8 3 0.11 2.3 (*2)
Waveform 16 N/ A N/ A TBD
Total0.049(Min)0.195(Max)
0.585 (Apo)0.975 (Peri)
(*2)
TNR 12 20.025(Min)0.099(Max)
0.297(Apo)0.495(Peri)
(*2)
Phase 12 2 0 0.192 (*2)
HFR 12 20.024(Min)0.096(Max)
0.096(Apo)0.288(Peri)
(*2)
AM2P Included in WFC/ OFA- E 0.01 0.01 (*2)
Total 4806 / 40380.28 Min)(0.46(Max)
4.97(Min)6.16(Max)
80~
SORBETData will be processed inSOBET and directly sentto MDP
EWO- EFD
EWO- OFA/ WFC- E
EWO- OFA/ WFC- B
should be compressed 0.2 and 3kbps in Bit-L and M, respectively
30 ~ 40(depends on data
compression efficiency)
• Data compression concept (Lossy or Lossless ?)• Data triggering concept
ReferenceReference
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -16-
"Low rate mode" 0.397kbpsSpectrum(*1) 8bits x [8-32Hz df=2Hz] x 2(E||/E⊥) x 1/16Hz 0.013kbpsE-vector(*2) 16bits x 2 (X/Y) x 8Hz 0.256kbpsPotential 16bits x 1 x 8Hz 0.128kbps
HK negligible
"Medium rate mode" 0.436kbpsSpectrum(*1) 8bits x [8-32Hz df=2Hz] x 2(E||/E⊥) x 1/4Hz 0.052kbpsE-vector(*2) 16bits x 2 (X/Y) x 8Hz 0.256kpbsPotential 16bits x 1 x 8Hz 0.128kbps
HK negligible
“High rate mode" (RAW) 6.1kbpsE-vector(*) 16bits x 2 (X/Y) x 128Hz 4.1kbpsPotential 16bits x 4 (X1/X2/Y1/Y2) x 32Hz 2.0kbps
HK negligible
OthersCAL & Sweep data 4kB (6.1kbps x 4sec)
EWO-EFD (data rate: without compression)
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -17-
"Low rate mode" 0.18 / 0.22kbpsSpectrum-E 8bit x [10Hz- 20kHz, 9- 72ch] x (1ch/peak) x [1/8-1Hz] 0.088kbps
or 8bit x [10Hz-120kHz, 14-112ch] x (1ch/peak) x [1/8-1Hz] 0.128kbps------------------------------------------------------------------------------------------------------------------Spectrum-B(L/H) 8bit x [10Hz- 6/20kHz, 9-72ch] x (1ch/peak) x [1/8-1Hz] 0.088kbpsSpectrum-B(VL) [1Hz-10Hz] TBD
"Medium rate mode" 4.8 / 5.6kbpsSpectrum-E 8bit x [10Hz- 20kHz, 90-360ch] x (1ch/phase/peak) x [1/2-2Hz] 1.64kbps
or 8bit x [10Hz-120kHz, 140-560ch] x (1ch/phase/peak) x [1/2-2Hz] 2.44kbps------------------------------------------------------------------------------------------------------------------Spectrum-B (L/H) 8bit x [10Hz- 6/20kHz, 90-360ch] x (2ch/peak) x [1/2-2Hz] 3.17kbpsSpectrum-B(VL) [1Hz-10Hz] TBD
“ High rate mode” [Short term RAW data] x N sets *Several patterns: (ex. MS mode/SW mode for 1sec observation) [50%
compression]Electrostatic wave observation mode(Ex, Ey) 1,049 / 810 kbitsInterferometry mode (Ey1, Ey2) 1,049 / 810 kbitsElectromagnetic wave observation mode(Bx, By, Bz) 1,570 / 393 kbitsVector observation mode(Ex, Ey, Bx, By, Bz) 2,619 / 1,203
kbits
OthersImpedance measurement mode(Ex) 671 kbitISDM (Intelligent Signal Detector Module) [short duration event (< 4s) data]
EWO-E&B (data rate: without compression)
BepiColombo/MMO PWI : MMO-SWG #11 (8 Jan 2009) -18-
SORBET
The SORBET data stream rates per operating modes Note: the fractions shown here read as: #frequencies+cag×word of 12bits
1) periapsis part of the MMO orbit 2) apoapsis part of the MMO orbit
132128
1321216 12812
16
128 12162
132124
1321216 312812
16
128 12162
132 128 64from to 128 12
8 64from to
390 to 49 0Solar Wind Mode (or any triggered low mode )
Low Res. Mode
975Peri Mode2)
( ~ 2h)
585Apo Mode1) (~ 7.5h) Medium Res.
Mode(nominal)
Total bps
Cross1/2 Auto 2 E or B on TNR + HFR
Auto1 E on TNR
SORBET data production
There is no H-mode on SORBET. M-modes are nominally used to keep a rough spatial resolution of about 30-40km.