Physical Sciences Inc. 20 New England Business Center Andover, MA 01810 VG04-190 Energetic Charged Particle Spectrometer for the Space Environment Reliability Verification Integrated System (SERVIS-1) Satellite G.E. Galica , 1 B.D. Green, 1 T. Nakamura, 1 H. Hasegawa, 2 T. Itoh, 2 and Y. Sasaki, 2 H. Kanai, 3 M. Akiyama, 3 and K. Hama 3 1 Physical Sciences Inc. 2 Mitsubishi Precision Co., Ltd. 3 Institute for Unmanned Space Experiment Free Flyer IEEE Nuclear and Space Radiation Effects Conference July 2004
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Energetic Charged Particle Spectrometer for the … Sciences Inc. 20 New England Business Center Andover, MA 01810 VG04-190 Energetic Charged Particle Spectrometer for the Space Environment
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Physical Sciences Inc. 20 New England Business Center Andover, MA 01810
VG04-190
Energetic Charged Particle Spectrometer for the Space Environment Reliability Verification
Integrated System (SERVIS-1) Satellite
G.E. Galica,1 B.D. Green,1 T. Nakamura,1 H. Hasegawa,2T. Itoh,2 and Y. Sasaki,2 H. Kanai,3 M. Akiyama,3 and K. Hama3
1Physical Sciences Inc. 2Mitsubishi Precision Co., Ltd.
3Institute for Unmanned Space Experiment Free Flyer
IEEE Nuclear and Space Radiation Effects ConferenceJuly 2004
VG04-190-1
Abstract
• We present the design and results from a new radiation sensor, the Light Particle Detector, designed specifically to quantify the orbital environment responsible for microelectronics damage. It supports Japan’s Space Environment Reliability Verification Integrated System.
VG04-190-2
SERVIS
• Space Environment Reliability Verification Integrated System
• A program with two spacecraft to validate the use of commercial electronics in orbit
– better performance– lower cost– faster delivery
• Environment diagnostic instrument suite
– LPD – PSI charged particle spectrometer
– dosimeters
• SERVIS-1 launched in late 2003
VG04-190-3
SERVIS-1 Satellite Launch
• ROKET launcher (SS-19)• Plesetsk, Russia• 30 Oct 2003, 1343 UT• 997 km polar orbit• 99.52 deg inclination
VG04-190-4
LPD – Light Particle Detector
• Designed for and manifested on the SERVIS-1 satellite (Japan)
– Built for Mitsubishi Precision Corp.– Space Environment Reliability
• Large G-factor/high count rate– 0.2 cm2 sr– 200 kcps
• Physical parameters– 4 kg (fully redundant)– 7 W (HiRel/RadHard)
VG04-190-5
LPD Spectrometer Block Diagram
• Energetic particles deposit energy in SSD and Scintillator as they pass through • By analyzing the detector signals, LPD identifies particle type and energy• LPD increments a one of 12 particle-energy bins that represent the orbital
distribution• Only the spectrum is downloaded to the ground (60,000-fold compression)
HV
Window
Scintillator
PMT
PACollimator
SSD
Change-Sensitive PA
Discriminator/Multilevel
ComparatorElectronics
BinCounters
RS422I/F
+5V±15V
DAE
E-3907cz
Shielding
CalibrationPulse DAE
HVEnergy deposited in SSD & Scintillator
p+, e-, a, h
VG04-190-6
Redundancy
• As bus component, LPD is required to be fully redundant
• LPD cannot be susceptible to single point failure
• Measured flux rates are only slightly higher than model predictions• LPD data can be used to update orbital flux models• Level of detail (spatial structure) in the data far exceeds the model
VG04-190-20
SERVIS LPD - Proton Data
• SAA dominates proton flux• Auroral ring is small and spatially small• Primarily low energy protons in Auroral zone• High energy protons in SAA
Measured Trapped Proton Data2 D ec 0 3
1.0E+01
1.0E+02
1.0E+03
1.0E+04
1.0E+05
1.0E+06
1.0E+07
8:00 10:00 12:00 14:00 16:00UT (hh:mm)
Prot
on F
lux
(cm
-2 s
-1)
p1 -- 1.5-12 M eV p2 -- 13-25 M eV p3 -- 25-37 M eV p4 -- 38-53 M eV p5 -- 53-96 M eV p6 -- 96-150 M eV
SAA AuroralRing - S
AuroralRing - N
VG04-190-21
SERVIS LPD – Electron Data
• Auroral electrons large contribution• Auroral ring large and structured• High energy electrons in SAA
Measured Trapped Electron Data2 De c 0 3
1.0E+01
1.0E+02
1.0E+03
1.0E+04
1.0E+05
1.0E+06
1.0E+07
1.0E+08
8:00 10:00 12:00 14:00 16:00UT (hh:mm)
Elec
tron
Flux
(cm
-2 s
-1)
e1 -- 0.3-1.5 M eV e2 -- 1.7-3.4 M eV e3 -- 3.4-6.6 M eV e4 -- >6.6 M eV
SAA
AuroralZone - N Auroral
Zone - S
VG04-190-22
Solar Storms
• Coronal Mass Ejections (CMEs)– large ejections of energetic material from the sun– solar wind accelerates as it approaches the Earth
• CMEs significantly distort the Earth's magnetic field– inject high energy particles into the lower magnetosphere– enhance the aurora
VG04-190-23
Late Oct 03 Aurorae
• Very strong CMEs in Fall 2003
• Strong aurorae visible very far south
– Boston– New York– Carolinas
• SERVIS-1 launched on 30 Oct– missed the initial CME– however LPD detected the
follow-on activity 1 solar rotation period later
VG04-190-24
GOES Satellite Protons (26 Oct 03 – 13 Nov 03)
VG04-190-25
SERVIS LPD – 2 Dec 03
• On 2 Dec 2003, SERVIS LPD detected a sudden, spatially distinct enhancement of low-energy protons
• Low energy protons (1-12 MeV) enhanced first
• Enhancement in higher energy protons (12-25 MeV; 25-50 MeV) occurred after a delay
• No discernable activity in electrons
• SAA proton flux was also enhanced
Measured Trapped Electron D
ata7 Dec 031.E+011.E+021.E+031.E+041.E+051.E+061.E+071.E+08
8:0012:00
16:0020:00
UT (hh:m
m)Flux (cm
-2 s-1) e1 -- 0.
3-1.5 M
eV e2 -- 1.
7-3.4 M
eV e3 -- 3.
4-6.6 M
eV e4 -- >6.6 M
eV
Measured Trapped Proton Data7 Dec 03
1.E+01
1.E+02
1.E+03
1.E+04
1.E+05
1.E+06
1.E+078:00 12:00 16:00 20:00
UT (hh:mm)
Flux
(cm
-2 s
-1)
p1 -- 1.5-12 MeV
p2 -- 13-25 MeV
p3 -- 25-370MeV
p4 -- 38-530MeV
p5 -- 53-960MeV
p6 -- 96-1500MeV
VG04-190-26
Proton Flux Enhancement Persistentfor Several Days
• GOES also detected enhanced proton flux simultaneously• Same delay between low and high energy proton enhancement• GOES satellite in geosynchronous orbit
VG04-190-28
Proton Enhancement Time History
• Low-energy proton flux rose suddenly (within hours) and decayed over several days
• Higher energy protons exhibited quick initial decay, but longer secondary decay
Temporal History of Proton Storm
1.E+00
1.E+01
1.E+02
1.E+03
1.E+04
1.E+05
0 10 20 30 40 50 60 70 80 90 100 110Time (hrs)
Cou
nts
1-12 MeV12-25 MeV25-37 MeV
VG04-190-29
Spatial Distribution of Enhancement
• Enhancement is occurring within the auroral ring at the north and south poles
• Structure is present within the polar regions
1.E+01
1.E+02
1.E+03
1.E+04
1.E+05
1.E+06
1.E+07
8:00 10:00 12:00 14:00 16:00UT (hh:mm)
Pro
ton
Flux
(cm
-2 s
-1)
auroralring -
auroralring -
SAA
northpole
southpole
VG04-190-30
Electron Activity
• Electron activity is not as distinct• Possible spatial distortions in SAA• Possible enhancement and spatial structure at poles