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 Physical Sciences Inc. 20 New England Business Center Andover, MA 01810
Abstract VG04-190-1 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.
SERVIS Space Environment Reliability Verification Integrated System VG04-190-2 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
SERVIS-1 Satellite Launch VG04-190-3 ROKET launcher (SS-19) Plesetsk, Russia 30 Oct 2003, 1343 UT 997 km polar orbit 99.52 deg inclination
LPD Light Particle Detector Designed for and manifested on the SERVIS-1 satellite (Japan) Built for Mitsubishi Precision Corp. Space Environment Reliability Verification Integrated System Launch Fall 2003 SERVIS-2 follow-on launch 2005 Energy Range Protons: 1-150 MeV (6 bins) Electrons: 0.3 10 MeV (4 bins) Alphas: >12 MeV (1 bin) Ions: >3 MeV/nucleon (1bin) Large G-factor/high count rate 0.2 cm 2 sr 200 kcps Physical parameters 4 kg (fully redundant) 7 W (HiRel/RadHard) VG04-190-4
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) VG04-190-5 HV HV Energy deposited in SSD & Scintillator Window p+, e-, a, h Scintillator Collimator SSD Shielding PMT PA Calibration Pulse Discriminator/ Multilevel Comparator Electronics RS422 I/F DAE +5V ±15V DAE Change-Sensitive PA Bin Counters E-3907cz
Redundancy As bus component, LPD is required to be fully redundant LPD cannot be susceptible to single point failure Redundancy approach 2 stacked SSDs 1 scintillator 2 PMTs 2 preamp pairs 2 bias supply pairs 2 processing electronics Side A and B do not have identical performance (low energy protons), but offers full redundancy Scint PMT B EMSS I/F VG04-190-6 SSD PA A Electronics EMSS I/F E-5340
GEANT Sensor Model VG04-190-7 We developed a sensor model using the GEANT code - no free parameters The model is validated with calibration data We use the model to: develop and refine the sensor and algorithm design interpolate/extrapolate sensor response to uncalibrated regimes predict on-orbit performance 2001/01/26 15.27 Servis (0.05/0.05/2.4) e/p/alpha/oxygen 2001/01/26 13.45 Servis (0.05/0.05/2.4) e/p/alpha/oxygen 10 2 Ssd > 0.025 Ssinsig < 0.025 10 2 Ssd2 > 0.025 Ssinsig < 0.025 Ssd1, MeV 10 SSD Ssd2, MeV 10 Scintillator 1 1 10-1 10-1 1 10 10 2 Epart, MeV E-8756 10-1 10-1 1 10 10 2 Epart, MeV E-8757
LPD Sensor Model Examples VG04-190-8
Bin Performance - Protons PSI uses a combination of calibration data and a validated Monte-Carlo sensor model to refine the LPD logic and to predict bin performance VG04-190-9 Low energy Servis (0.05/0.05/2.4) p 2001/01/28 15.27 High energy Servis (0.05/0.05/2.4) p 2001/01/28 15.27 Fractional Response 1 0.5 P1P2 P3 P4 SSD > 0.07 Proton Band SCINSIG > 0.025 P5 Fractional Response 1 0.5 0.7 > SSD > 0.25 Proton Band SCINSIG > 0.025 P5 P6 0 0 50 100 150 Incident Energy, MeV E-8754a 0 0 50 100 150 Incident Energy, MeV E-8755a
Bin Performance - Electrons PSI uses a combination of calibration data and a validated Monte-Carlo sensor model to refine the LPD logic and to predict bin performance Servis (0.05/0.05/2.4)e 2001/01/28 15.27 VG04-190-10 Fractional Response 1 0.5 e4 e3 e2 e1 e5 SSD > 0.025 Electron Band SCINSIG > 0.025 0 0 10 20 Incident Energy, MeV E-8753a
SERVIS-1 LPD Bins VG04-190-11 A B Energy Range (FWHM) Energy Range (FWHM) Bin Low (Mev) High (Mev) G-factor (cm 2 sr) Low (MeV) High (MeV) G-factor (cm 2 sr) E1 0.3 1.5 0.21 0.7 1.5 0.21 E2 1.7 3.4 0.17 1.7 3.4 0.17 E3 3.4 6.6 0.18 3.4 6.6 0.18 E4 6.6 >10 0.23 6.6 >10 0.23 P1 1.2 12.5 0.26 8.5 12.5 0.26 P2 12.5 24.5 0.26 12.5 24.5 0.26 P3 24.5 37 0.26 24.5 37 0.26 P4 38 53 0.26 38 53 0.26 P5 53 96 0.23 53 96 0.23 P6 96 150 0.22 96 150 0.22 A 7 640 0.26 7 640 0.26 H 2 MeV/nucl 160 MeV/nucl 0.26 2 MeV/nucl 160 MeV/nucl 0.26
Proton Calibration energy deposited (MeV) 10 8 6 4 2 0 Proton SSD-A response GEANT data 0 20 40 60 80 100 120 140 160 proton energy (MeV) VG04-190-12 Proton calibrations performed at Harvard Cyclotron Lab and at Indiana University CF HCL 30-160 MeV IUCF 50-200 MeV LPD meets its requirement to detect 150 MeV protons energy deposited (MeV) 160 120 80 40 0 GEANT data Proton Scintillator Response 0 20 40 60 80 100 120 140 160 proton energy (MeV) Linear response of SSD SSD and scintillator responses match sensor model predictions
Electron Calibration signal (volts) 0.2 0.15 0.1 0.05 0 SERVIS LPD SSDA - electron signals SSDA fit 0 0.5 1 1.5 energy deposited (MeV) VG04-190-13 Electron calibrations performed at NIST, Gaithersburg, MD Van de Graaf 0.5-2.0 MeV Cascading Rheostat 0.15-0.4 MeV LPD meets its requirement to detect 300 kev electrons 6.E+05 SERVIS LPD SSDA - 300 kev electron Linear response of SSD number/bin 4.E+05 2.E+05 SSD performance matches model predictions 0.E+00 0 0.02 0.04 0.06 0.08 0.1 signal (volts)
LPD Performance Parameters VG04-190-14 de/e (fwhm) relative response 0.15 0.05 1.2 resolution vs. angle - 55 MeV proton 0.2 0.1 1 0.8 0.6 0.4 0.2 0 0-30 -20-10 0 10 20 30 angle (degrees) SERVIS-1 LPD Acceptance Angle predicted measured -60-40 -20 0 20 40 60 angle (degrees) Large acceptance angle required to meet mission goals ±20 deg FWHM ±30 deg acceptance cone G = 0.2 cm 2 sr High count rate capability required to accommodate large acceptance angle 200 kcps Inherent energy resolution of 0.15 de/e even with large acceptance angle
SERVIS-1 Orbit and Radiation Environment 1000 km altitude into the bottom of the van Allen proton belts (650 to 6500 km) VG04-190-15 99.5 deg inclination polar orbit passes though the auroral region magnetic field lines intersect the Earth South Atlantic Anomaly (SAA) Earth's magnetic field is not aligned with geographic coordinates offset from Earth s center and tilted wrt to true north SAA is a region in the South Atlantic where the Earth s magnetic field is closer to the Earth s surface SERVIS1 travels N-S around the Earth and passes through the auroral ring and the SAA
Electron Distribution Auroral zone VG04-190-16 SAA Auroral zone
Proton Distribution Protons primary contribution in SAA Electrons contributions from SAA and Auroral zone VG04-190-17 Auroral zone SAA Auroral zone
LPD Proton Data vs AP8 Model Proton data maps out the SAA Measured flux rates are higher than model predictions (3-4x) LPD data can be used to update orbital flux models VG04-190-18 flux (cm-2 sec-1) 1.E+07 1.E+06 1.E+05 1.E+04 1.E+03 1.E+02 proton data (1 Dec 03) P1 1.5-12 MeV P2 13-25 MeV P3 25-37 MeV P4 38-53 MeV P5 53-96 MeV P6 96-150 MeV 1.E+01 7:59:20 9:16:48 10:34:12 11:51:36 13:09:00 14:26:24 15:43:47 17:01:11 18:18:35 19:36:03 20:53:27 22:10:51 23:28:15 0:45:39 2:03:02 3:20:26 4:37:50 5:55:14 UT (hh:mm:ss)
LPD Electron Data vs AE8 Model VG04-190-19 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 electron data (1 Dec 03) 1.E+08 1.E+07 E1 0.3-1.5 MeV E2 1.7-3.4 MeV E3 3.4-6.6 MeV E4 >6.6 MeV flux (cm-2 sec-1) 1.E+06 1.E+05 1.E+04 1.E+03 1.E+02 1.E+01 7:59:20 9:15:52 10:32:20 11:48:48 13:05:16 14:21:44 15:38:11 16:54:39 18:11:07 19:27:39 20:44:07 22:00:35 23:17:03 0:33:31 1:49:58 3:06:26 4:22:54 5:39:22 6:55:50 UT (hh:mm:ss)
SERVIS LPD - Proton Data Auroral Ring - N SAA Auroral Ring - S VG04-190-20 SAA dominates proton flux Auroral ring is small and spatially small Primarily low energy protons in Auroral zone High energy protons in SAA 1.0E+07 1.0E+06 Measured Trapped Proton Data 2 Dec 03 p 1 - - 1.5-12 M ev p2 -- 13-25 MeV p3 -- 25-37 MeV p4 -- 38-53 MeV p5 -- 53-96 MeV p6 -- 96-150 MeV Proton Flux (cm-2 s-1) 1.0E+05 1.0E+04 1.0E+03 1.0E+02 1.0E+01 8:00 10:00 12:00 14:00 16:00 UT (hh:mm)
SERVIS LPD Electron Data Auroral Zone - N SAA Auroral Zone - S VG04-190-21 Auroral electrons large contribution Auroral ring large and structured High energy electrons in SAA 1.0E+08 1.0E+07 Measured Trapped Electron Data 2 Dec 03 e1 -- 0.3-1.5 M ev e2 -- 1.7-3.4 M ev e3 -- 3.4-6.6 MeV e4 -- >6.6 M ev Electron Flux (cm-2 s-1) 1.0E+06 1.0E+05 1.0E+04 1.0E+03 1.0E+02 1.0E+01 8:00 10:00 12:00 14:00 16:00 UT (hh:mm)
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 VG04-190-22
Late Oct 03 Aurorae VG04-190-23 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
GOES Satellite Protons (26 Oct 03 13 Nov 03) VG04-190-24
SERVIS LPD 2 Dec 03 On 2 Dec 2003, SERVIS LPD detected a sudden, spatially distinct enhancement of lowenergy protons VG04-190-25 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
Proton Flux Enhancement Persistent for Several Days p1 -- 1.5-12 M ev Measured Trapped Proton Data p2 -- 13-25 M ev 2 Dec 3 Dec 2 Dec 03 p3 -- 25-37 M ev 1.0E+07 1.0E+07 1.0E+06 p4 -- 38-53 MeV p5 -- 53-96 MeV p6 -- 96-150 MeV 1.0E+06 Measured Trapped Proton Data 3 Dec 03 VG04-190-26 p1 -- 1.5-12 M ev p2 -- 13-25 M ev p3 -- 25-37 M ev p4 -- 38-53 M ev p5 -- 53-96 MeV p6 -- 96-150 M ev Proton Flux (cm-2 s-1) 1.0E+05 1.0E+04 1.0E+03 1.0E+02 Proton Flux (cm-2 s-1) 1.0E+05 1.0E+04 1.0E+03 1.0E+02 1.0E+01 7:00 9:00 11:00 13:00 15:00 17:00 19:00 21:00 23:00 UT (hh:mm) 1.0E+01 0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00 UT (hh:mm) 1.0E+07 1.0E+06 4 Dec Measured Trapped Proton Data 4 Dec 03 p1 -- 1.5-12 M ev p2 -- 13-25 M ev p3 -- 25-37 M ev p4 -- 38-53 MeV p5 -- 53-96 MeV p6 -- 96-150 M ev 1.0E+07 1.0E+06 5 Dec Measured Trapped Proton Data 5 Dec 03 p1 -- 1.5-12 M ev p2 -- 13-25 M ev p3 -- 25-37 M ev p4 -- 38-53 MeV p5 -- 53-96 MeV p6 -- 96-150 M ev Proton Flux (cm-2 s-1) 1.0E+05 1.0E+04 1.0E+03 1.0E+02 Proton Flux (cm-2 s-1) 1.0E+05 1.0E+04 1.0E+03 1.0E+02 1.0E+01 0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00 UT (hh:mm) 1.0E+01 0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00 UT (hh:mm)
GOES Proton Data 1-7 Dec 03 VG04-190-27 GOES also detected enhanced proton flux simultaneously Same delay between low and high energy proton enhancement GOES satellite in geosynchronous orbit
Proton Enhancement Time History VG04-190-28 Low-energy proton flux rose suddenly (within hours) and decayed over several days Higher energy protons exhibited quick initial decay, but longer secondary decay 1.E+05 Temporal History of Proton Storm 1.E+04 1-12 MeV 12-25 MeV 25-37 MeV Counts 1.E+03 1.E+02 1.E+01 1.E+00 0 10 20 30 40 50 60 70 80 90 100 110 Time (hrs)
Spatial Distribution of Enhancement Enhancement is occurring within the auroral ring at the north and south poles Structure is present within the polar regions VG04-190-29 1.E+07 SAA Proton Flux (cm-2 s-1) 1.E+06 1.E+05 1.E+04 1.E+03 1.E+02 auroral ring - auroral ring - north pole south pole 1.E+01 8:00 10:00 12:00 14:00 16:00 UT (hh:mm)
Electron Activity VG04-190-30 Electron activity is not as distinct Possible spatial distortions in SAA Possible enhancement and spatial structure at poles 1.0E+08 e1 -- 0.3-1.5 MeV 2 Dec Measured Trapped Electron Data e2 -- 1.7-3.4 MeV 3 Dec 2 Dec 03 e3 -- 3.4-6.6 MeV 1.0E+08 e4 -- >6.6 MeV Measured Trapped Electron Data 2 Dec 03 e1 -- 0.3-1.5 MeV e2 -- 1.7-3.4 MeV e3 -- 3.4-6.6 MeV e4 -- >6.6 MeV Electron Flux (cm-2 s-1) 1.0E+07 1.0E+06 1.0E+05 1.0E+04 1.0E+03 1.0E+02 1.0E+01 8:00 10:00 12:00 14:00 16:00 UT (hh:mm) Electron Flux (cm-2 s-1) 1.0E+07 1.0E+06 1.0E+05 1.0E+04 1.0E+03 1.0E+02 1.0E+01 16:00 18:00 20:00 22:00 0:00 UT (hh:mm)
GOES Electrons VG04-190-31 GOES electron data quiet on 2-5 Dec Electron activity observed on 5-7 Dec
SERVIS Electron Data 1/2 1.0E+08 2 Dec Measured Trapped Electron Data 2 Dec 03 e1 -- 0.3-1.5 MeV e2 -- 1.7-3.4 MeV e3 -- 3.4-6.6 MeV e4 -- >6.6 M ev 1.0E+08 3 Dec Measured Trapped Electron Data 3 Dec 03 VG04-190-32 e1 -- 0.3-1.5 MeV e2 -- 1.7-3.4 MeV e3 -- 3.4-6.6 MeV e4 -- >6.6 M ev 1.0E+07 1.0E+07 Electron Flux (cm-2 s-1) 1.0E+06 1.0E+05 1.0E+04 1.0E+03 1.0E+02 Electron Flux (cm-2 s-1) 1.0E+06 1.0E+05 1.0E+04 1.0E+03 1.0E+02 1.0E+01 7:00 9:00 11:00 13:00 15:00 17:00 19:00 21:00 23:00 UT (hh:mm) 1.0E+01 0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00 UT (hh:mm) e1 -- 0.3-1.5 MeV Measured Trapped Electron Data e2 -- 1.7-3.4 MeV 4 Dec 5 Dec 4 Dec 03 e3 -- 3.4-6.6 MeV 1.0E+08 1.0E+08 e4 -- >6.6 M ev Measured Trapped Electron Data 5 Dec 03 e1 -- 0.3-1.5 MeV e2 -- 1.7-3.4 MeV e3 -- 3.4-6.6 MeV e4 -- >6.6 M ev 1.0E+07 1.0E+07 Electron Flux (cm-2 s-1) 1.0E+06 1.0E+05 1.0E+04 1.0E+03 1.0E+02 Electron Flux (cm-2 s-1) 1.0E+06 1.0E+05 1.0E+04 1.0E+03 1.0E+02 1.0E+01 0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00 UT (hh:mm) 1.0E+01 0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00 UT (hh:mm)
SERVIS Electron Data 2/2 VG04-190-33 e1 -- 0.3-1.5 MeV 6 Dec Measured Trapped Electron Data e2 -- 1.7-3.4 M ev 7 Dec 6 Dec 03 e3 -- 3.4-6.6 MeV 1.0E+08 1.0E+08 e4 -- >6.6 M ev Measured Trapped Electron Data 7 Dec 03 e1 -- 0.3-1.5 MeV e2 -- 1.7-3.4 MeV e3 -- 3.4-6.6 MeV e4 -- >6.6 M ev 1.0E+07 1.0E+07 Electron Flux (cm-2 s-1) 1.0E+06 1.0E+05 1.0E+04 1.0E+03 1.0E+02 Electron Flux (cm-2 s-1) 1.0E+06 1.0E+05 1.0E+04 1.0E+03 1.0E+02 1.0E+01 0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00 UT (hh:mm) 1.0E+01 0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00 UT (hh:mm)
Summary and Conclusions VG04-190-34 SERVIS-1 LPD has several performance goals that have now been demonstrated on orbit: Single sensor to detect protons, electrons, alphas, heavy ions Large throughput (AΩ) results in high count rates, efficient detection of small populations of particles, good counting statistics High count rate does not saturate during solar storms Good particle discrimination misassignment of low energy electrons as low energy protons is a chronic problem with most flight sensor designs electrons outnumber protons by 10x to >100x proton channels often get hosed achieving 10-3 or 10-4 contamination High accuracy calibration and validated sensor model returning fully calibrated data from sensor turn-on PSI (LPD & SDOM) sensors are now returning the high-quality on-orbit radiation data