Future missions 2020’s’s andd Key technologies
h lin Space PlasmalGroupPlPlanetaryt
Exploration
E l ti

Jupiter/LAPLACEp /((‐ 20202020’s)s))

The giant particle accelerator : JUPITER
A further,f hllargely
l unresolved
l d problem
bloff a fundamental
f dl
nature regards
gthe Jovian magnetospheregp
as a tremendouslyy
efficient particle accelerator.
accelerator There is no question that Io isth primarytheisource off particles
ti l ini theth Jovian
J i environment.
itThe new pplasma p
populations
phave, however, typicalypenergies
gof a few 10
10’ss eV at best.
best At what time and spatial scales,scales andby what mechanisms,
mechanisms does a significant part of them reach
MeV energies and populateltheh harshesth hradiatingenvironment of the solar system? The fact that suchenvironments can exist has direct relevance to the notion of‘h bit bilit ’ A large‘habitability’.
land
d highly
hi hl variable
i bl levell l off radiation
di ti
mayy actuallyy modifyy or control the emergence
gof life.

Environment Observation
Near Earth

PLASMA UNIVERSU

ERG (‐2013)( 2013))SCOPE/Cross
SCOPE/Cross‐/‐Scale
Scale ((‐2017)2017))SCOPE(cross‐Scale
SCOPE(S l CouplingCli ini PlasmPl ma universE)iE) consists
i t off fivefi satellites,t llitone 450kgg mother satellite and four 90kgg daughters,
g, which are assumed tobe launched by JAXAJAXA’ss H
H‐IIA
IIA rocket ata once.
once Five satellites fly in basically atetrahedron formation,formation minimum 5km5apart from each other,other at theirperigee of 30 Earth‐radii distance. To obtain the highly accurate spatial
distribution of the magnetospheric phenomena, the quality of the clock
synchronization and the relative orbit determination between satellites areessential.
i l SCOPE aims
i at observingb
i theh Earth’s
E h’ magnetotailil where
htheh ions
iand electrons interact with each other,, with 5 satellites flyingy g in formation.
To fully resolve the time‐domain behaviour and spatial distribution of themagnetospherict h i phenomena,
ha simimultaneous
ltobservationbti
b spatiallybyti ll
distributed electro‐magnetic
ginstrumments is essential.

For the purpose of studying the unresolved major problems
underlying in Geospace,Geospace a small satellite mission named ERG(E(Energizationi i andd Radiation
R di i ini Geospace)G) isi proposed,d beingb ifocused on the formation of the radiation belts associatedwith magnetic storms.
storms The scientific instruments on‐board
are arranged
d tot makek definitived fi iti
evaluationl ti
off possible
ibl
mechanisms for the formation of the radiation belts. The ERG
mission will achieve comprehensive plasma observations
with magnetic/electric field,
field wave,
wave and plasma detectors witha wided energy range (10( eV ‐ 10 MeV)) to capture acceleration,
ltransport, and loss of charged particles in Geospace. TheERG mission also establish less expensive plasma observatory
underd strong
tradiationdi ti environment.
it

Th
Three
MainMai streams
We will know mechanism of spaace plasma phenomena perfectly!

K y tech
Keyt hnology
h l gyObObservationi fromfeVV to MeV
M V Time resollution to 10 msec
withoutihenergy
gy gapg p:
MediumdiEnergy
gy P article(MEP)i l ()

Spin axis antenna

New Development target:
MEP‐ion10 keV/q – 180 keV/q
MEP‐elel
10 keV‐100keVkk

Cusp typeESA
ToF unit

Development
Dlt off Spin
S i axisi antenna
ttot beb able
bl totobserve 3D electric field and p
plasma wave.
It is key measurement to understand space plasma

Carbon foil
SSD
MCP

Cross section of medium energy ion mass spectrometer and particle
trajectories.
jiLi h blueLight
bl curves are ion
i trajectories.
ji Violet
Vi l andd white
hi curves arestart and stopp electron trajectories,j, respectively.
py A black belt indicates theposition of carbon foils,
foils and a green belt represents the position of SSDs.
SSDs Abl plateblue
l t isi MCP;
MCP it detects
d t t startt t andd stopt electrons.
l t APD is a SSD‐like photon
pdetector havingg internal ggain ((Strongg for noise)) Medium energy e‐ was highly resolved!!!
 Newe MEP foro eelectron
ect o ususingg ESA
S + APD canca measureeasu e electrone ect o fluxes
u eswith the energy band at least 5 keV to 50 keV

We have newlyy deveeloped
p an electron energy
gy analyzer
y FESA(Fast Electron energgy Spectrum Analyzer) for a futuremagnetospheric satellite mission SCOPE.
SCOPE The SCOPE mission
is designed in orderr that observational studies from thecross‐scalecrossscale coupling viewpointv
are enabled. One of the key
observations necessaary for the SCOPE mission is high‐timehigh time
resolutionl i electron
lmmeasurement.
Ei h FESAs
EightFESA on a spinningi ispacecraft
pare capa
pable of measuringg three dimensional
electron distribution function
fwith time resolution of 8 msec.
msec
FESA consists
i t off twot
electrostaticl t t ti analyzers
lth t arethat
composed
pof three nested
nhemisphericalpdeflectors. SinglegFESA functions as fo
our top
top‐hat
hat type electrostatic analyzers
that can measure electrons
ewith four different energies
simultaneously.
ll By measuringmtheh characteristics
hoff theh test
model FESA, we provved the validity of the design concept ofFESA Based on the measured characteristics,FESA.
characteristics we designed
FESA optimized
ti i d forfth SCOPE mission.
thei iThi optimized
Thisti i danalyzer
yhas ggood enougheg pperformance to measure three
dimensional electron distribution functions around themagnetic reconnectio
on region in the Earth’s magnetotail.
magnetotail

Low power
p&Highg p
performance
Developmentl
Magnetic Field(MGF)
ld() sensor core
and the new electric circuit wide dynamic range(20bits)

Measurement technique of a few 10 keV ionsDevelopment
pof Singleg Sided Si Detector andvery low noise read‐out
read out ASIC (noise < 150e‐)