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Exploring Mercury's Magnetic Field and Magnetosphere with BepiColombo

This project aims to understand Mercury's unique magnetic field and magnetosphere through precise measurements. Scientists seek to uncover the internal structure and origins of these fields, comparing them to Earth's for a comprehensive study of planetary magnetospheres. By investigating plasma and radio waves around Mercury, PWI will provide insights into energetic processes and atmospheric dynamics in the inner solar system. The project involves detailed observations to understand the generation, loss, and variability of Mercury's exosphere. The agenda includes discussions on spacecraft tests, data acquisition, and team structure. By analyzing density, electric fields, and wave patterns, the mission targets a range of performance metrics across different modes. Telemetry data production is critical for synchronizing measurements and capturing transient phenomena, enhancing our understanding of Mercury's unique space environment.

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Exploring Mercury's Magnetic Field and Magnetosphere with BepiColombo

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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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