bepicolombo/mmo pwi : mmo-swg #11 (8 jan 2009) -1- bepicolombo mmo plasma wave investigation (pwi)...

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


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


*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!]


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.)


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


PWI will observe plasma/radio waves in Mercury, which no man has seen before.


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 )


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%


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%


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?)


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%


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)


H-Mode *Requested Target

*Expected Performance-RAW waveform data triggered by specific conditions


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


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)


*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]


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


"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)


"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)


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.

bepicolombo/mmo pwi : mmo-swg #11 (8 jan 2009) -1- bepicolombo mmo plasma wave investigation (pwi)...

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