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Introduction of Graduate School of Science, the University of Tokyo and Associated
Institute (ISAS/JAXA)and
Suggestions on SpaceMaster Thesis ThemesMasafumi HIRAHARA
Space and Planetary Science Group,Department of Earth and Planetary Science,
Graduate School of Science, The University of Tokyo(email: [email protected]) (skype: masa.hirahara)
http://www.s.u-tokyo.ac.jp/en/ http://www.eps.s.u-tokyo.ac.jp/index_en.html
Departments in Graduate School of SciencePhysicsAstronomyEarth and Planetary Science (EPS)ChemistryBiophysics and BiochemistryBiological Sciences
Research Groups in Our DepartmentAtmospheric and Oceanic Science GroupSpace and Planetary Science GroupEarth and Planetary System Science GroupSolid Earth Science GroupGeosphere and Biosphere Science Group
Introduction of myself• Solar-terrestrial physics (STP), Space (plasma) physics• Auroral and geospace/planetary explorations through
satellites and spacecraft operations from ground-based sites
• Developments of plasma/particle instruments and associated calibration facility for in-situ observation in space
• Experimental/data analysis works for space plasma/particle observationsToday I am a representative of three research groups; two in Univ. Tokyo and one in ISAS/JAXA.
1. Space instrumentation/data analysis in Hongo of Univ. Tokyo2. Planetary research in Kashiwa of Univ. Tokyo3. Satellite component development in Sagamihara of ISAS/JAXA
Solar wind plasma stream and interplanetary magnetic field(Expansion of solar corona)
Terrestrial upper atmosphereand intrinsic magnetic field
Mercury’s magnetospheric formation andacceleration of space plasma particles due tointeraction between solar wind and Mercury’sIntrinsic magnetic field
Mercury magnetosphericexploration mission
Atmospheric escape/evolution and climatechange due to direct interaction between solar wind and Martian ionosphere
Solar-TerrestrialEnvironment
Mercury Mars
Sun
Earth
Geospace-magnetosphere
Solar wind
Radiation belt(Van Allen belt)
Gespace-ionosphereRing current
Graduate School of Science (GSS),the University of Tokyo (UT)
Main Island of Japan
Central Area of TokyoCentral Tokyo
Akihabara
Univ. TokyoIn Hongo Area
Campuses of Univ. TokyoHongo, Komaba, Kashiwa,Shirokane, Nakano
Graduate School of Science (GSS),the University of Tokyo (UT)
Main Island of Japan
Central Area of TokyoCentral Tokyo
Akihabara
Univ. TokyoIn Hongo Area
Hongo Campus of Univ. Tokyo
GSS of UT forSpaceMaster
Campuses of Univ. TokyoHongo, Komaba, Kashiwa,Shirokane, Nakano
In Hongo campus of Univ. Tokyo
Master Themes in Hongo of Univ. Tokyo• Construction and automation of ion/electron beam facility for
calibrating space plasma/particle instruments for BepiColomboMercury magnetosphere and future terrestrial/planetary explorations– 1 – 200 keV ion/electron beam line – Beam line profiling and calibration system control– Final calibration for BepiColombo high-energy ion sensor– A few eV – a few tens of keV ion beam line
• Design of suprathermal ion energy/mass spectrometers for future terrestrial/planetary explorations– Polar-ionosphere and Geospace explorations– Martian upper atmosphere and ionosphere exploration
• Data display/analysis system for auroral images and plasma particle data– Auroral imaging camera data from Reimei and ALIS– Google Earth or other visualization platform
SunSolar Wind
Auroral Camera
Geospace-Ionosphere
Aurora
Magnetometer
ORBITALS
Radiation BeltsRing Current
RBSP
ERG
RadarLidarHeater
International Geospace Observation Network
RESONANCE
KuaFu
LANLGOES
POES
Geospace-Magnetosphere
THEMIS
GeotailCluster II
AkebonoFAST
Reimei
FORMOSAT-5
CASSIOPE
Earth
Radiation Belts(Van Allen Belts)
Ring Current
Magnetosphere
Sun
Ionosphere
Solar Wind
PlasmaSheet
Geospace
plasmasphere
ring current
plasma sheet
inner belt outer belt
1 eV
100 keV
1 MeV
Space Plasma/Particle Energy Distributionin Geospace
LEP-i
MEP-i
HEP-i
1 keVLEP-e
MEP-e
HEP-e
XEP
10 MeV
ion(H+, He+, O+)
electron
Plasma/particle instrument package has to cover a wide energy range over more than 7 orders.
L=5 ReL=2 Re
TSP-i TSP-e
Altitude from Earth
Ene
rgy
Calibration Facility for Space Plasma/Particle Instruments~200-keV ion/electron beam line
IsolationTransformer
(200kV)High-voltage power supply (+50kV)
High-voltage power supply (+150kV)
Vacuum chamber
Vacuum pumps
Turntableand X-stage
Isolation tube with linear accelerator
Ionization source withmass separator and beam expander
Inside of clear room(GSS, UT)
outside of clear room(GSS, UT)
Air shower
Air shower
EU-Japan Joint Mercury Exploration Mission
0
2
4
6
8
10
0 500 1000 1500
55-keV_H^+_He^2+_He^+_N^+H^+He^2+He^+N^+
H^+
TOF-ch
0
2
4
6
8
10
12
14
0 500 1000 1500
110-keV_H^+_He^2+_He^+_N^+H^+He^2+He^+N^+
H^+
TOF-ch
Master Themes in Hongo of Univ. Tokyo• Construction and automation of ion/electron beam facility for
calibrating space plasma/particle instruments for BepiColomboMercury magnetosphere and future terrestrial/planetary explorations– 1 – 200 keV ion/electron beam line – Beam line profiling and calibration system control– Final calibration for BepiColombo high-energy ion sensor– A few eV – a few tens of keV ion beam line
• Design of suprathermal ion energy/mass spectrometers for future terrestrial/planetary explorations– Polar-ionosphere and Geospace explorations– Martian upper atmosphere and ionosphere exploration
• Data display/analysis system for auroral images and plasma particle data– Auroral imaging camera data from Reimei and ALIS– Google Earth or other visualization platform
Auroral emission and particle observations by ReimeiEmission-particle simultaneous measurements with high time/spatial resolutions
Launch August 23 in 2005 as piggy-back by a Dnepr rocketfrom the Baikonur Cosmodrome in Kazakhstan
Orbit Sun-synchronous
Inclination: 98.6 deg.
Meridian: 12:50 - 0:50 LT
Altitude: 610-670 km
Orbital period: 98.8 min.
Attitude Three-axis stabilized, sun-oriented (basically)
Telemetry S-band for up- and down-link from 1 to 133 kbps
Size/Weight 724×626×609 mm3 / 71.623 kg
Operation Extended to 2010 or later
Introduction of Reimei
Multi-Spectral AuroralImaging Camera (MAC)
Electron/Ion Energy Spectrum Analyzer (ESA/ISA)
Calibration of ESA/ISA
Development of MAC
Plasma Current Monitor(CRM)
Multi-spectral Auroral Camera(MAC)
Electron Spectrum Analyzer(ESA)
Ion Spectrum Analyzer(ISA)
Appearance of Reimei Movie of Aurora ImagesDecember 26, 2005
Ch.1 (427.8 nm) Ch.2 (557.7 nm) Ch.3 (670.0 nm)
70 km (64 bins)at 110-km altitude
70 k
m (6
4 bi
ns)
Exposure time: 60 msec.Exposure cycle: 120 msec.
Northward (Poleward)
Footprint of S/C mappedonto 110-km altitude along field line
10
1
0.1
0.01
Elec
tron
(0 –
60 d
eg.)
Ener
gy (k
eV)
Elec
tron
(60
–12
0 de
g.)
Ener
gy (k
eV)
Elec
tron
(120
-18
0 de
g.)
Ener
gy (k
eV)
10
1
0.1
0.0110
1
0.1
0.01UT(09:MM:SS) 10:40 10:45 10:50 10:55 11:00 11:05
ILAT 74.2 73.9 73.7 73.4 73.1 72.8MLT 0.9 0.8 0.8 0.8 0.8 0.8
Electron Energy-Time SpectrogramsDecember 28, 2005
Electron Energy-Time Spectrograms and Aurora ImagesDecember 26, 2005
UT(09:MM:SS) 10:40 10:45 10:50 10:55 11:00 11:05ILAT 74.2 73.9 73.7 73.4 73.1 72.8MLT 0.9 0.8 0.8 0.8 0.8 0.8
ALIS (Auroral Large Imaging System)
• Spectroscopic imaging system
• Absolute measurements
• 6 imager units• 6+4 fixed stations• 1 mobile station (bus)• Remote control• Campaigns• Free data on Internet
Detector units
• CCD detectors:1024x1024 pixels
• FOV: 60 or 90 degrees• Maximum resolution:
100 m at 100 km• Typical exposure time:
1-2 s• Typical temporal
resolution: 5 s• High sensitivity,
manages few Rayleigh
Shops and cafeterias in Hongo campus Near Hongo Campus of Univ. Tokyo
LIFE @ KOMABA LODGE
by Ting
Rent around 100 euro!!!!
Before move in
Desk & Bookshelf
Bed
Bathroom
Kitchenette
wardrobe
Balcony
After … Cafeteria @ Komaba Campus
Transportation • 10mins
• Walking from HongoCampus of Univ. of Tokyo to Nezu Station
• 25mins• Subway from Nezu
Station to Yoyogi-Uehara Station without Line Change
• 15mins• Walk from Yoyogi-
Uehara Station to Komaba Lodge
Central business districtFashion forefront of
JapanKomaba Lodge Shibuya
20 mins walk
Sakura in Aprilcheerful cherry blossom season
All photos taken by Ting
And …..?
Shinjuku?Akihabara?
Ginza?
Check out by yourselves!
Let me know if you have any [email protected]
Planetary Research (Astrobiology Laboratory)in Kashiwa Campus of Univ. Tokyo
Prof. Seiji SugitaE-mail: [email protected]
URL: http://www.astrobio.k.u-tokyo.ac.jp/ Not much in English info yet…
We do laboratory experiments.
~25
km
Hongo CampusUniv. Tokyo
Kashiwa CampusUniv. Tokyo
Locations of Hongo Campus
andKashiwa Campus
of Univ. Tokyo
Kashiwa Campus
• Kashiwa Campus is north east of Tokyo. Let me honest with you. It’s in the middle of nowhere; not so close to nearest train station…
• But we have great research facility, an international lodge, and less air pollution. • It’s also cheap to live around here as well.
Train station
Kashiwa Campus
Kashiwa Campus
Cafeter
ia 2
Mon-Fri: 11
:00-20
:00
Sat: Lunch
only
Clinic
LibraryCafeteria 1
Food shop
Mon-Fri, 11:00-21:00
Our building
Mon-Fri, 11:00-20:00
◆ Instrumental developmentLaser-Induced Breakdown Spectroscopy (LIBS)
Nd:YAG laser Spectrometer
Vacuum ChamberEmission spectrum
◆High-speed impact processesExperimental facilities to study planetary evolution
Facilities to conduct high-speed impact experiments
Laser gun BBM LIBS system
• We study the early evolution of planets and satellites, and the origin of their atmospheres.
• We compare our Earth and other planets in order to understand why our Earth could harbor life.
Titan
Comets
Mars
Moon
Venus
Asteroids
Light-gas gun
Earth
Comparative Planetology
Research Interests Potential Research Topics•Impact Research
–Giant meteo impact causing Cretaceous-Tertiary dinosaur extinction
–The origin of life, particularly supply of organics to pre-biotic Earth
•Comparative Planetology–The origin of the Titan atmosphere–The subsurface structure of comet 9P/Tempel 1 using Deep Impact data
• Instrumental Development–Elemental analysis instrument (LIBS)
Potential Research Topics
Ejecta from Deep Impact
Titan atmosphere Polycarbonate impacting Cu at 6km/s
Projectile
Research Approaches
•Hypervelocity Impact experiments–Degassing experiments and chemical analysis–High-speed spectroscopy
• Instrument development–LIBS (laser-induced breakdown spectroscopy)–TOF MS (Time-of-flight mass spectrometer)
•Data analysis–Development of spectral data analysis algorithms.–Image and spectral analysis of mid-IR data from AKARI satellite and the Subaru telescope.
Research Approaches
2-stage light gas gun@ISAS Laser gun@Osaka Univ.
AKARI Satellite Subaru telescope
LIBS system@Kashiwa
Research Themesfor SpaceMaster Program
in Sagamihara of ISAS/JAXA
Hirobumi SaitoInstitute of Space and Astronautical Science (ISAS)
Japan Aerospace Exploration Agency (JAXA)([email protected])
Institute of Space and Astronautical Science (ISAS),Japan Aerospace Exploration Agency (JAXA)
Main Island of Japan
Sagamihara
~30 km
Hongo CampusUniv. Tokyo
ISAS/JAXA
Institute of Space and Astronautical Science (ISAS),Japan Aerospace Exploration Agency (JAXA)
~30 km
ISAS/JAXA
ISAS/JAXA
ISAS/JAXA Institute of Space and Astronautical Science (ISAS),Japan Aerospace Exploration Agency (JAXA)
(http://www.isas.jaxa.jp/e/index.shtml)National Space Institutes in the world• US: NASA (National Aeronautics and Space Administration) • EU: ESA (European Space Agency)• Japan: JAXA (Japan Aerospace Exploration Agency)• Russia: RFSA (Russian Feredal Space Agency) / Roskosmos• China: CNSA (China National Space Administration)• Korea: KARI (Korean Aerospace Research Institute)• Taiwan: NSPO (National Space Organization)• India: ISRO (Indian Space Research Organization)• Canada: CSA (Canadian Space Agency)• Sweden: SNSB (Swedish National Space Board)• UK: BNSC, France: CNES, Germany: DLR, Italy: ASIBrazil: INPE
Research Themes for SpaceMaster ProgramHirobumi Saito Lab. at ISAS/JAXA
1. Automated Ground Operation System
for Micro Satellite REIMEI
2. Compensation Method of Satellite Fiber
Optical Gyroscope with “Shupe” Effect
3. GPS Receiver for Spinning Rocket
4. High Speed Data Communications for
Small Satellite
1.Automated Ground Operation System for Micro Satellite REIMEI
- We have operated micro satellite REIMEI from small tracking station at our laboratory.
- Scientists at remote area send their observation plans.
- At tracking station, plans are integrated and verified nearly automatically.
- At present we are constructing automatedsystem for satellite tracking.
Outline of INDEX (REIMEI)
160W (MAX)PowerTechnologyValidation
Engineering Mission
Aurora ObservationScienceMission
72 kgMass
72 x 62 x 62cm3Size
Outline of INDEX (REIMEI) Contd.
One Year PassedMission Life
Near Sun Synchronous(608 x 655 km)
Orbit24/8/2005, from BaikonurLaunch Date
$ 4 million + our salaryCost
Dnepr RocketLaunch Vehicle
- Three-Axis Controlledw/ Bias-Momentum
- Magnetic Control- Accuracy : 0.05deg
Attitude Control
ISAS/JAXA Sagamihara Campus Station• The station has an antenna of 3 meter
in diameter on the roof of the main building.
• Downlink: 131kbps* / Uplink: 1kbps• Orbit determination is based on:
– one-way doppler– TLE information– onboard GPS receiver (mission)
• The REIMEI operation team consists of young researchers, engineers, and students. Most operation software and tools are developed by themselves and a venture software house.>> Flexible operation!!!
*The onboard S-band transmitter (STX) is in the high-power mode. The mode is limitedly used when the satellite faces a critical situation.
Operation / Ground StationPhotos during the REIMEI operation
The REIMEI project has received a technical award from the Japan
society for aeronautical and space sciences in Jan., 2010.
2. Compensation Method of Satellite Fiber Optical Gyroscope with Shupe Effect
- Fiber optical gyroscopes (FOG) are suitablefor small satellite attitude control sensors.
- Bias angular rate of FOG due to temperaturevariation (“Shupe” effect) degrades FOG performances.
- We study on the compensation method of FOG “Shupe” effect by means of temporal measurement of temeperature.
FIBER OPTICAL GYRO with TEMPERATURE CONTROL
Commercial FOG(JAE JG-34)
Mass 1axis 140g Radiation 15 kradVibration 20GrmsShock 50G, 11msBias Stability is Critical
0.1[deg/h] with temp. cntl.
Measurement System of FOG Bias Rate due to “Shupe” Effects
3. GPS Receiver for Spinning Rocket
- GPS receivers for spinning rocket are
developed with antenna diversity techniques.
- Software receiver algorithm is proposed and
investigated by means of simulations.
- The algorithm will be implemented in the GPS
hardware.
Background• Cost effective GPS receivers for the
next-generation solid motor launchers and sounding rockets of ISAS/JAXA– Precise payload insertion– Redundant flight safety
©JAXA
Open Source GPS Receiver
Total Price<$200
• Originally designed by Clifford Kelly and released under GNU Public License (GPL)
• Ported to ARM7-based GPS baseband processor (Zarlink GP4020) and running on NovAtel SuperStar II
High-Dynamic Flights • Frequency lock loop (FLL) provides
robust signal tracking • Successful flights on several high power
model rocket missions
Dual Antenna Software-Defined GPS Receiver
Digitized GPS signal data will be transferred to the host PC via USB 2.0 and post-processed by a software-defined GPS receiver
Multi-Antenna Receiver Development
Namuru II L1/L2C receiver with reconfigurable FPGA core
©General Dynamics
©SpaceLink
Quad-antenna receiver using GP4020-compatible GPS correlator chipsets
4. High Speed Data Communicationsfor Micro Satellite
- The graduate school of technology in the University of Tokyo plans to develop micro satellite with 50kg for earth image monitoring.
- Besides imaging sensors, high data transmissions are a key technology.
- We plan to develop high data transmissiontechnology.
- On-board instruments should be compact and low-power consuming for matching micro satellite.
- Ground demodulation should be sophisticated, using error correcting code and equalization techniques.
High Speed Data Communications for Small Satellite
Conventional System for Large Satellite
Advanced System for Small Satellite
Satellite has to transmit clear waves receivable at any ground stations.
Satellite can transmit somewhatwarped/peculiar waves becauseground station can correct them.Electrical Control
of Beam Directionby Phased Array System
Mechanical Control
of Antenna Direction
低電力高速
RF Measurement Instruments for Space Communications
Software Simulation System for RF Communications
Accommodation at ISAS/JAXA
• http://www.isas.jaxa.jp/e/index.shtml• http://www.isas.jaxa.jp/e/researchers/accommodation/index.shtml
Air conditioner, TV, small refrigerator, desk/chair, bed with linens, toilet and shower with small bathtub in 15 m2
• Common kitchen, clothes mashers/ driers available anytime
• Cafeteria open for lunch at weekday
• Shop open for 9:30-16:30 at weekday
Interview through skype or TV conference system using internet
Before mutual decision/agreement to study together in Japan for master thesis subject, a remote interview between SpaceMaster students and Japanese groups is preferable.
Please contact to Masa Hirahara and the professor by whom you wish to be supervised via email.
1. Masa Hirahara (Space Physics in Hongo of Univ. Tokyo)email: [email protected]: masa.hirahara
2. Seiji Sugita (Planetary Research in Kashiwa of Univ. Tokyo)email: [email protected]
3. Hirobumi Saito (Satellite Subsystem in Sagamihara of ISAS/JAXA)email: [email protected]