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BepiColombo MMO Plasma Wave Investigation (PWI)

BepiColombo MMO Plasma Wave Investigation (PWI). Jan 7 2009 PWI Meeting Jan 8 2009 MMO-SWG meeting. Discovery of magnetic field by Mariner10 Internal magnetic field describes the internal structure & its evolution. ○ Magnetic field: Why does Mercury have?

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BepiColombo MMO Plasma Wave Investigation (PWI)

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  1. BepiColombo MMO Plasma Wave Investigation (PWI) Jan 7 2009 PWI Meeting Jan 8 2009 MMO-SWG meeting

  2. Discovery of magnetic field by Mariner10 Internal magnetic field describes the internal structure & its evolution ○ 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 / Exophere Magnetosphere different from the Earth pgenerates the comparative study of the planetary Magnetosphere. Bepi will make first complete study of Herman Magnetic field & Magnetosphere Mercury is the unique terrestrial planet which still keeps its magnetic field, except Earth. -Why does this planet have magnetic field? -How is the magnetosphere similar or different ? PWI

  3. *Agenda (7 Jan 2009) 1300 EWO 1340 SORBET 1420 AM2P 1500 MEFISTO 1540 WPT 1600 Software 1640 EMC 1720 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!]

  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.)

  5. 2. Science *Close-relationship shall be expected with : - All in-situ measurements --- Synchronous Measurements for Electric Field : Plasma Motion / Acceleration Waves : All energetic processes etc. Onboard Triggering for Short & Transient phenomena Electron density & temperature - MMO/MDM --- Plasma ejection by dust impact - MPO/MAG & Serena --- Remote sensing of possible radio waves --- Simultaneous propagating wave measurement

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

  7. 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 : Survey with high time resolution … 8 Hz with precise measurement … 1/16 Hz - DC Electric Field & ULF Wave Measurement (Ion Cyclotron / Alfven) with synchronicity to MGF … 8 Hz - Spectrum : Minimum-resolution with medium frequency resolution … 1/16 Hz df/f = 230% with medium time resolution … 1 Hz df/f = 12%

  8. 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. 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%

  10. 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

  11. 3. Telemetry *Close-relationship shall be expected with : - All in-situ measurements --- Synchronous Measurements for Electric Field : Plasma Motion / Acceleration Waves : All energetic processes etc. Onboard Triggering for Short & Transient phenomena Electron density & temperature - MMO/MDM --- Plasma ejection by dust impact - MPO/MAG & Serena --- Remote sensing of possible radio waves --- Simultaneous propagating wave measurement

  12. PWI RAW data production [Jan 2009] (non-compression)

  13. PWI TLM Production from MDP [Jan 2009] (non-compression) [50% compression] *1) Data rate in the magnetosphere/solar wind. *2) Data rate is same as Bit-M mode

  14. 30～40(depends on data compression efficiency) PWI TLM Production from MDP [Jan 2008] (non-compression) Reference • Data compression concept (Lossy or Lossless ?) • Data triggering concept Bit H: 56kbps (After data compression) should be compressed 0.2 and 3kbps in Bit-L and M, respectively *1) Data rate in the magnetosphere/solar wind. *2) Data rate is same as Bit-M mode

  15. EWO-EFD (data rate: without compression) "Low rate mode"0.397kbps Spectrum(*1) 8bits x [8-32Hz df=2Hz] x 2(E||/E⊥) x 1/16Hz 0.013kbps E-vector(*2) 16bits x 2 (X/Y) x 8Hz 0.256kbps Potential 16bits x 1 x 8Hz 0.128kbps HK negligible "Medium rate mode"0.436kbps Spectrum(*1) 8bits x [8-32Hz df=2Hz] x 2(E||/E⊥) x 1/4Hz 0.052kbps E-vector(*2) 16bits x 2 (X/Y) x 8Hz 0.256kpbs Potential 16bits x 1 x 8Hz 0.128kbps HK negligible “High rate mode" (RAW)6.1kbps E-vector(*) 16bits x 2 (X/Y) x 128Hz 4.1kbps Potential 16bits x 4 (X1/X2/Y1/Y2) x 32Hz 2.0kbps HK negligible Others CAL & Sweep data 4kB (6.1kbps x 4sec)

  16. EWO-E&B (data rate: without compression) "Low rate mode"0.18 / 0.22kbps Spectrum-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] 0.088kbps Spectrum-B(VL) [1Hz-10Hz] TBD "Medium rate mode"4.8 / 5.6kbps Spectrum-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] 3.17kbps Spectrum-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 kbits Interferometry mode (Ey1, Ey2) 1,049/810 kbits Electromagnetic wave observation mode(Bx, By, Bz) 1,570/393 kbits Vector observation mode(Ex, Ey, Bx, By, Bz) 2,619/1,203 kbits Others Impedance measurement mode(Ex) 671 kbit ISDM (Intelligent Signal Detector Module) [short duration event (< 4s) data]

  17. SORBET SORBET data production Auto1 E on TNR Auto 2 E or B on TNR + HFR Cross1/2 Total bps Medium Res. Mode (nominal) Apo Mode1) (~7.5h) 585 Peri Mode2) (~ 2h) 975 Low Res. Mode Solar Wind Mode (or any triggered low mode ) 0 390 to 49 The SORBET data stream rates per operating modes Note: the fractions shown here read as: #frequencies+cag×wordof12bits 1) periapsis part of the MMO orbit 2) apoapsis part of the MMO orbit There is no H-mode on SORBET. M-modes are nominally used to keep a rough spatial resolution of about 30-40km.

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