1. The High Energy Particle Detector for CSES Mission The Scientific Case
Piergiorgio Picozza
INFN and University of Rome Tor Vergata
35th International Cosmic Ray Conference
Busan, Korea
July 12-20, 2017

2. CSES - China Seismo-Electromagnetic Satellite-Mission The Main Objective
Study of the Litosphere-Ionosphere-Magnetosphere coupling by :
monitoring the electromagnetic field, plasma and particle perturbations of the atmosphere, ionosphere and magnetosphere induced by natural sources and anthropocentric emitters
studying their correlations with the occurrence of seismic events

3. Physics Program Cosmic Rays Physics of Radiation Belts Solar Physics
Physics of Ionosphere
Phenomena Sismo-Associated

4. CSES Mission

5. Satellite Launch August 16th, 2017, 3.51 p.m. (Delayed)
 3-axis attitude stabilized, based on the Chinese CAST2000 platform
Total mass: 730 kg
Total power budget: 900 W
Scientific data transmitted in X-band at 120 Mbps.
98° Sun-synchronous circular orbit; altitude 500 km
Expected lifetime: 5 years.

6. CHINESE Collaboration Italian-Limadou collaboration
CSES Collaboration
CHINESE Collaboration
Italian-Limadou collaboration
China National Space Administration (CNSA)
 China Earthquake Administration (CEA)
Lanzhou Institute of Physics (LIP)
DFH Satellite Co.    
Italian Space Agency ASI
National Institute for Particle and Nuclear Physics INFN
National Institute of Astrophysics INAF
National Institute of Geophysics and Volcanology INGV
Universities of Trento, Bologna, Rome Tor Vergata, Rome UTIU

7. High-Energy Particle Package (HEPP)

8. HEPD
GENERAL DESIGN
Two planes of double-side silicon microstrip detectors which provide the direction of the incident particle
Two layers of plastic scintillators for trigger (one thin segmented counter S1 and one deep counter S2)
A range calorimeter made of:
15 layers of plastic scintillator planes (15 × 15 × 1 cm3) read out by PMTs;
a 3 × 3 matrix of inorganic scintillator LYSO (15 × 15 × 4 cm3) read out by PMTs
An anticoincidence system made of 5 mm thick plastic scintillator veto planes surrounding the calorimeter
Silicon tracker
Triggerplane
Plastic scintillator
planes
LYSO cubes
Veto counters
PhotoMultipliers 8 8

9. HEPD Parameters Energy range elettrons 3 - 100 MeV
protons MeV
Nuclei up to Oxygen
Geometry factor elettrons cm2.sr
protons cm2.sr
Energy resolution < 10%
Angular resolution < 8°
Field of view °

10. Calorimeter Muon Calibration

11. Calorimeter Electron Calibration BTF at INFN LNF
30 MeV

12. Calorimeter Proton Calibration Trento proton-cyclotron
37 MeV
Sigma/peak
0.11
51 MeV
Sigma/peak
0.09
70 MeV
Sigma/peak
0.08
100 MeV
Sigma/peak
0.08

13. Calorimeter Resolution

14. HEPD and HEPP
Scientific Program

15. Low Energy Cosmic Rays (a) solar wind (b) large sep events
CSES ENERGY RANGE
(a) solar wind
(b) large sep events
(c) galactic cosmic rays
(d) intermediate solar/heliospheric
quiet-time particles
(e) anomalous Cosmic Rays
CSES can investigate a very complex region of the spectrum with different particle populations 15

16. Anomalous Component of CR
Some cosmic rays (anomalous cosmic rays or ACR) are accelerated in the Solar System, at the shock where the solar wind meets interstellar space and NOT in the Galaxy (GCR) → reach the inner heliosphere
GCRs have higher energies than ACRs. Therefore, CSES should be able (theoretically) to identify the two components by looking at their spectra
For ACR He/H > 1
The nuclei ID of HEPD and HEPP can measure the energy interval where ACR may be found
ACRs
GCRs 16

17. Study of the Solar Cycles 24-25
The solar cycle 24 is in its ending phase → Only CSES and AMS02 can give new flux measurements of cycle 25
The 5-years CSES mission will investigate the new minimum phase → comparison with previous anomalous minimum ( )
Possible strong SEP during quiet phase (like December 13/14, 2006)?
CSES 17

18. Electron Solar Modulation
PAMELA 18

19. Proton Solar Modulation
Proton modulated spectra 
studied by PAMELA down to
80 MeV​
CSES can reach lower energies       
CSES can explore a range lower than PAMELA and also validate PAMELA models for low energy spectra
CSES
PAMELA 19

20. Solar Energetic Proton Spectrum
SEP spectra are wide in energy and intensity (poorly known)
GOES measures low energy SEP spectra with low precision, with poor energy reslution and with high contamination at highest channles
CSES 20

21. Jovian Protons
PAMELA

22. Pamela World Maps: 350 – 650 km alt
Study terrestrial magnetosphere
Pamela World Maps: 350 – 650 km alt
36 MeV p, 3.5 MeV e-

23. Trapped Protons CSES REGION PAMELA REGION
PAMELA observation of trapped radiation performed down to L shell 1.1RE and up to 4 GeV
Comparison with empirical model
Improvement in low altitude radiation -environment description
CSES can explore lower energies inside the radiation belts (< PAMELA) 23

24. Early Space Missions Electron and Proton flux variations
Electron Intercosmos Bulgaria-1300 and Meteor 3
Mariya Salyut 7
Mariya MIR
Gamma GAMMA Astrophysical Station
Meteor 3A
Oreol 3
NINA
SAMPEX

25. Electron Bursts
SAMPEX
MARYA-2
GAMMA-1

26. Correlations between EQ & ps: TEQ-PB distributions
MIR mission
METEOR-3 mission
Altitude: 400 km
ORR
(Orbit Rate Rotation;
July May 1994)
GAMMA-1 mission
Altitude: 1250 km
Inclination: 51°
SAMPEX/PET
Mission
Altitude: 350km
Ee: 20  200 MeV
Ep: 20  200 MeV
Inclination: 82°
Inclination: 51°
Altitude: 520740km
Ee:  30 MeV
Inclination: 82°
Ee: > 50 MeV
4  Ee  15 MeV

27. 2008

30. 2008

31. Ionosphere-lithosphere coupling
The lithosphere may produce electric and wave perturbations
that can propagate in the ionosphere and inner magnetosphere
An earthquake is a sudden perturbation that can induce e.m.
and particle signals in the ionosphere/lower magnetosphere

32. Wave – particles interaction mechanism
Schematic representation in a meridian plane of the trapped particle trajectories
PBs
EARTHQUAKE PREPARATION AREA
EM WAVES PROPAGATION
INTO THE IONO-MAGNETOSPHERE
PARTICLE PITCH ANGLE CHANGES 
MIRROR POINTS LOWERING
PARTICLE PRECIPITATION
PBs PROPAGATE AROUND THE EARTH ALONG THE L-SHELL
(LONGITUDINAL DRIFT)
PBs DETECTABILITY AT ANY LONGITUDE
EM WAVES GENERATE
PERTURBATIONS IN THE LOWER IONOSPHERE 5 6
geomagnetic field lines
stationary trajectory of
trapped particles
mirror points
lowering 1 3 2
EM WAVES INTERACT WITH CHARGED TRAPPED PARTICLES IN THE INNER RADIATION BELT 4
stationary lower boundary
of the radiation belt

33. Wave-particle interaction
Cyclotron resonance - Whistler mode
Cumulative deflection from many interaction with VLF (3-30 kHz period s) circularly polarized waves would force electrons into the loss cone i.e. pitch angle diffusion
Bounce resonance - Alfven mode
Magnetosonic micropulsation or electrostatic ULF waves (< 3Hz period 300 s) can interact resonantly with particles during their bouncing motion

34. Conclusion ? Seismic Precursors Geomagnetic Field Fluctuations
External Sources
(Sun & Cosmic Rays)
Atmo-Ionosferic
EM secondary
emissions
Seismo-EM Emissions
Mirror
point
Ionospheric
region
Lower boundary of the
inner radiation belt
Trajectory of
trapped particles
PBs
Seismic gas
exalation ?
Man-made e.m. effects
Thunderstorm
Activity
Seismic Precursors
Geomagnetic Field Fluctuations
Magnetospheric Dynamics
Ionospheric Perturbations

35. Thanks!