1. Notification: fce: electron cyclotron frequencyfci: proton cyclotron frequency fpe: electron plasma frequencyfpi:proton plasma frequency fLH: Lower Hybrid Resonance frequency *The present tables propose the target physics and the necessary data qualities for us to study them. The time resolutions, frequency resolutions etc. in the tables have not been listed under the consideration of the telemetry capacity and the onboard data processing capabilities of the MDP. The listed values are presented only in the scientific point of view. *To the speakers of the morning session Please close your talk with some addition / correction of items in this tables and/or the proposal of ‘new’ pages. Baseline of the PWI target physics and necessary data qualities

2. RegionsAll regions Energy sourceSolar activity TargetType II, Type III DataSpectrumDirection findingPhase difference (E-B) ComponentEx or Ey/ Bx or Bzk-vector at several spectral peaks E-B phase difference at several spectral peaks Frequency range10kHz < f < 10MHz Frequency resolution 5kHz (10kHz< f < 100kHz) 50kHz (100kHz < f < 1MHz) 100kHz (1MHz < f < 10MHz) NA Time resolution1.5sec16sec1.5sec Collecting time period NA NoteDetection of the plasma cloud direction

3. RegionsAll regions Energy sourceMacroscopic motion TargetConvection electric field DataWave form ComponentInstantaneous |E| Frequency rangeNA Frequency resolutionNA Time resolution1sec Collecting time periodNA Note

4. RegionsAll regions Energy sourceNA TargetStudy of the macroscopic structure of the Mercury magnetosphre DataElectron densityElectron temperature ComponentEx or Ey Frequency range*target: around fpe 1kHz < f < 20kHz(Magnetosphere) 20kHz < f < 200kHz (Solar wind) Frequency resolution100Hz NA Time resolutiona few sec Collecting time periodNA Note

5. RegionsMagnetosphere (Tail) Plasma sheet, Lobe Energy sourceBursty electrons associated with the substorm TargetLangmuir waves, ECH waves, Electron hole generated by electron beam instabilities. That can be observed in the plasma sheet boundary layer or the separatrix region just close to the plasma sheet boundary. DataSpectrumWaveforms ComponentEpara or EperpEx and Ey Frequency range*target: fpe 1kHz < f < 20kHz *target: fpe f < 20kHz Frequency resolution100HzNA Time resolution1secNA Collecting time periodNA200msec NoteInterferometry mode is also useful for the detection of the potential polarity of the electron hole.

6. RegionsMagnetosphere (Tail) Periapsis in the night side region Energy sourceTrapped electrons TargetThe temperature anisotropy of trapped electrons around the magnetic equator destabilize the Whistler mode waves. Similar situation can be appeared in the generation of Chorus emissions in the terrestrial magnetosphere. DataSpectrumWavenormalWaveforms Component|E| (integrated in time), |B|(integrated in time) Wave normal vector relative to the ambient magnetic field Ex, Ey, Bx, By, Bz Frequency range*target: fce/10~fce/2 100Hz < f < 3kHz at several frequency points corresponding to spectral peaks of waves *target: fce/10~fce/2 f < 3kHz Frequency resolution 30Hz (100< f < 1kHz) 100Hz (1kHz < f < 3kHz) NA Time resolution1sec NA Collecting time period NA 200msec Note Observations of the spectrum do not aim at identifying the dispersion of the Chorus spectrum. wave norimal vector can be calculated by the polarization plane of the magnetic field components with an ambiguity of 180degree

7. RegionsMagnetosphere (Tail) Magnetopause boundary (if exists) Energy sourceCurrent is formed by velocity difference of the sputtered ions and invaded solar wind plasmas around the magnetopause boundary? In such a situation, the current driven type instabilities take place. TargetIon acoustic mode, ion hole, electron hole DataSpectrumWaveforms ComponentEx or EyEx and Ey Frequency range*target: fpi/5 < f < fpe 100Hz < f < 20kHz *target: f < fpe f < 20kHz Frequency resolution30Hz (100Hz < f < 1kHz) 300Hz (1kHz < f < 20kHz) NA Time resolution1secNA Collecting time period NA1sec NoteInterferometry mode is also useful for the detection of the potential polarity of the electron /ion hole.

8. RegionsMagnetosphere (Tail) Boundaries: Magnetopause, Plasma sheet (if exists) Energy sourceDensity gradient with magnetic field TargetLower Hybrid waves, Electron cyclotron harmonic: Mode conversion/Drift instability such a Lower Hybrid Drift Instability DataSpectrum ComponentEx or Ey Frequency range*target: fce/2 < f < 3fce 200Hz < f < 3kHz *target: f < 3fLH 0< f < 30Hz Frequency resolution50Hz0.02Hz: (f < 3Hz) 1Hz: (3Hz < f < 30Hz) Time resolution< 1sec Collecting time period NA NoteElectron cyclotron wavesLower Hybrid Waves

9. RegionsMagnetosphere (Polar) Energy sourceHigh energy precipitated electrons TargetElectron cyclotron waves DataSpectrum Component|E| or |B| Frequency range*target: f < fce 1kHz < f < 20kHz Frequency resolution50Hz Time resolution10 sec Collecting time periodNA Note

10. RegionsMagnetosphere (Polar) Energy sourceUpward ions escaping from the polar atmosphere TargetIon acoustic waves, Ion hole DataSpectrumWaveforms Component|E|Ex, Ey Frequency range*target: fpi/4 < f < fpe 100Hz < f < 20kHz *target: fpi/4 < f < fpe 100Hz < f < 20kHz Frequency resolution30Hz (f < 1kHz) 200Hz (1kHz < f < 20kHz) NA Time resolution10 secNA Collecting time period NA200msec Note

11. RegionsMagnetosphere (Dayside) Energy sourceDirect interaction of the solar wind with photo electrons emitted from the planetary surface Current driven type instability ? TargetIon acoustic waves, Ion hole DataSpectrumWaveforms Component|E|Ex, Ey Frequency range*target: fpi/4 < f < fpe 1kHz < f < 200kHz *target: f < fpe f < 200kHz Frequency resolution100Hz (1kHz < f < 10kHz) 1kHz (10kHz < f < 200kHz) NA Time resolution1 secNA Collecting time periodNA50msec NoteTrigger sequence is necessary.

12. RegionsMagnetosphere/Magnetosheath (Tail) Energy sourcePick up process of the sputtered ions by solar wind TargetAlfven waves, Ion cyclotron waves, Ion turbulence excited by the non-gyrotropic heavy ions. The situation is similar to the wave instabilities driven by cometary ions. This process may take place in the whole regions of the Mercury magnetosphere. DataSpectrumWaveforms Component|E| and |B|Ex, Ey Bx, By, Bz Frequency range*target: f < fLHR f < 100Hz *target: f < fci f < 2Hz Frequency resolution0.1Hz (f < 1Hz) 5Hz (1Hz < f < 100Hz) NA Time resolutiona few secNA Collecting time periodNA30sec Note

13. RegionsBow Shock: Upstream region Energy sourceReflected ions TargetAlfven waves, Ion cyclotron waves DataSpectrumWaveforms Component|E| and |B|Ex, Ey Bx, By, Bz Frequency range*target: f < fci f < 2Hz *target: f < fci f < 2Hz Frequency resolution0.1Hz (f < 1Hz)NA Time resolutiona few secNA Collecting time periodNA30sec Note

14. RegionsBow shock: Upstream region Energy sourceUpstream electron beams TargetLangmuir waves, 2fp emission, electron hole DataSpectrum ComponentEx or Ey and Bx or Bz Frequency range*target: fpe < f < 3fpe 50kHz < f < 400kHz Frequency resolution5kHz: 50kHz < f < 100kHz 50kHz: 100kHz < f < 400kHz Time resolution2sec Collecting time periodNA Note

15. RegionsBow shock: Transition, downstream region Energy sourceCurrent, electron accelerated at the shock potential TargetIon acoustic wave, Electron acoustic wave, Electron hole DataSpectrum ComponentEx or Ey Frequency range*target: fpi/4 < f < fpe 1kHz < f < 200kHz Frequency resolution1kHz: 1kHz < f < 10kHz 50kHz: 100kHz < f < 400kHz Time resolution2sec Collecting time periodNA Note

16. RegionsSolar wind: CME/CIR Energy sourceElectron beam, Temperature anisotropy of electrons TargetLangmuir waves, Whistler mode wave DataSpectrum ComponentEx or Ey/Bx or Bz Frequency range*target: f ~fpe for E, f < fce/2 for B 50kHz < f < 200kHz for E f < 300Hz for B Frequency resolution10kHz: for E 10Hz for B Time resolutionless than 1 sec Collecting time periodNA NoteTrigger sequence is necessary.