energetic charged particle spectrometer for the … sciences inc. 20 new england business center...

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

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 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

• 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

PMT

Scint

SSD

PA

Electronics

EMSS I/FEMSS I/F

B A

E-5340

VG04-190-7

GEANT Sensor Model

• 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

Epart, MeV10-1 1 102

10

1

Ssd > 0.025Ssinsig < 0.025

Ssd

1,M

eV

Servis (0.05/0.05/2.4) e/p/alpha/oxygen

2001/01/26 15.27

E-8756

1010-1

102

Epart, MeV10-1 1 102

10

1

Ssd2 > 0.025Ssinsig < 0.025

Ssd

2,M

eV

Servis (0.05/0.05/2.4) e/p/alpha/oxygen

2001/01/26 13.45

E-8757

1010-1

102

SSD Scintillator

VG04-190-8

LPD Sensor Model Examples

VG04-190-9

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

Low energy High energy

Incident Energy, MeV0 50 150

0

0.5

1

SSD > 0.07Proton BandSCINSIG > 0.025

Frac

tiona

lRes

pons

e

Servis (0.05/0.05/2.4) p

2001/01/28 15.27

E-8754a

100

P1P2 P3 P4

P5


0

0.5

1

0.7 > SSD > 0.25Proton BandSCINSIG > 0.025

Frac

tiona

lRes

pons

e

Servis (0.05/0.05/2.4) p

2001/01/28 15.27

E-8755a

100

P5

P6

VG04-190-10

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


0

0.5

1

SSD > 0.025Electron BandSCINSIG > 0.025

Frac

tiona

lRes

pons

eServis (0.05/0.05/2.4)e

2001/01/28 15.27

E-8753a

e1e2

e3e4 e5

VG04-190-11

SERVIS-1 LPD Bins

0.26160 MeV/nucl2 MeV/nucl0.26160 MeV/nucl2 MeV/nuclH0.2664070.266407A0.22150960.2215096P60.2396530.239653P50.2653380.265338P40.263724.50.263724.5P30.2624.512.50.2624.512.5P20.2612.58.50.2612.51.2P10.23>106.60.23>106.6E40.186.63.40.186.63.4E30.173.41.70.173.41.7E20.211.50.70.211.50.3E1

High(MeV)

Low(MeV)

High(Mev)

Low(Mev)

G-factor(cm2 sr)

Energy Range (FWHM)G-factor(cm2 sr)

Energy Range (FWHM)BA

Bin

VG04-190-12

Proton Calibration

• 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

• Linear response of SSD

• SSD and scintillator responses match sensor model predictions

Proton SSD-A response

0

2

4

6

8

10

0 20 40 60 80 100 120 140 160proton energy (MeV)

ener

gy d

epos

ited

(MeV

)

GEANTdata

Proton Scintillator Response

0

40

80

120

160

0 20 40 60 80 100 120 140 160proton energy (MeV)

ener

gy d

epos

ited

(MeV

)

GEANTdata

VG04-190-13

Electron Calibration

SERVIS LPD SSDA - electron signals

0

0.05

0.1

0.15

0.2

0 0.5 1 1.5energy deposited (MeV)

sign

al (v

olts

) SSDAfit

SERVIS LPD SSDA - 300 keV electron

0.E+00

2.E+05

4.E+05

6.E+05

0 0.02 0.04 0.06 0.08 0.1signal (volts)

num

ber/b

in

• 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

• Linear response of SSD

• SSD performance matches model predictions

VG04-190-14

LPD Performance Parameters

resolution vs. angle - 55 MeV proton

0

0.05

0.1

0.15

0.2

-30 -20 -10 0 10 20 30angle (degrees)

dE/E

(fw

hm)

• Large acceptance angle required to meet mission goals

– ±20 deg FWHM– ±30 deg acceptance cone– G = 0.2 cm2 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 LPD Acceptance Angle

0

0.2

0.4

0.6

0.8

1

1.2

-60 -40 -20 0 20 40 60angle (degrees)

rela

tive

resp

onse

predictedmeasured

VG04-190-15

SERVIS-1 Orbit and Radiation Environment

• 1000 km altitude– into the bottom of the van Allen proton belts

(650 to 6500 km)

• 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

VG04-190-16

Electron Distribution

SAA

Auroral zone

Auroral zone

VG04-190-17

Proton Distribution

• Protons – primary contribution in SAA• Electrons – contributions from SAA and Auroral zone

Auroral zone

Auroral zone

SAA

VG04-190-18

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

proton data (1 Dec 03)

1.E+01

1.E+02

1.E+03

1.E+04

1.E+05

1.E+06

1.E+07

7:59

:20

9:16

:48

10:3

4:12

11:5

1:36

13:0

9:00

14:2

6:24

15:4

3:47

17:0

1:11

18:1

8:35

19:3

6:03

20:5

3:27

22:1

0:51

23:2

8:15

0:45

:39

2:03

:02

3:20

:26

4:37

:50

5:55

:14

UT (hh:mm:ss)

flux

(cm

-2 s

ec-1

)

P1 1.5-12 MeVP2 13-25 MeVP3 25-37 MeVP4 38-53 MeVP5 53-96 MeVP6 96-150 MeV

VG04-190-19

LPD Electron Data vs AE8 Model

electron data (1 Dec 03)

1.E+01

1.E+02

1.E+03

1.E+04

1.E+05

1.E+06

1.E+07

1.E+08

7:59

:20

9:15

:52

10:3

2:20

11:4

8:48

13:0

5:16

14:2

1:44

15:3

8:11

16:5

4:39

18:1

1:07

19:2

7:39

20:4

4:07

22:0

0:35

23:1

7:03

0:33

:31

1:49

:58

3:06

:26

4:22

:54

5:39

:22

6:55

:50

UT (hh:mm:ss)

flux

(cm

-2 s

ec-1

)

E1 0.3-1.5 MeVE2 1.7-3.4 MeVE3 3.4-6.6 MeVE4 >6.6 MeV

• 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

Measured Trapped Proton Data3 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

0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00UT (hh:mm)

Prot

on F

lux

(cm

-2 s

-1)



1.0E+01

1.0E+02

1.0E+03

1.0E+04

1.0E+05

1.0E+06

1.0E+07

0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00UT (hh:mm)

Pro

ton

Flux

(cm

-2 s

-1)



1.0E+01

1.0E+02

1.0E+03

1.0E+04

1.0E+05

1.0E+06

1.0E+07

0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00UT (hh:mm)

Pro

ton

Flux

(cm

-2 s

-1)


Measured Trapped Proton Data2 Dec 03

1.0E+01

1.0E+02

1.0E+03

1.0E+04

1.0E+05

1.0E+06

1.0E+07

7:00 9:00 11:00 13:00 15:00 17:00 19:00 21:00 23:00UT (hh:mm)

Pro

ton

Flux

(cm

-2 s

-1)

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

2 Dec 3 Dec

5 Dec4 Dec

VG04-190-27

GOES Proton Data – 1-7 Dec 03

• 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

Measured Trapped Electron Data2 Dec 03

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

Flu

x (c

m-2

s-1

)

e1 -- 0.3-1.5 MeV e2 -- 1.7-3.4 MeV e3 -- 3.4-6.6 MeV e4 -- >6.6 MeV

Measured Trapped Electron Data2 Dec 03

1.0E+01

1.0E+02

1.0E+03

1.0E+04

1.0E+05

1.0E+06

1.0E+07

1.0E+08

16:00 18:00 20:00 22:00 0:00UT (hh:mm)

Elec

tron

Flux

(cm

-2 s

-1)

e1 -- 0.3-1.5 MeV e2 -- 1.7-3.4 MeV e3 -- 3.4-6.6 MeV e4 -- >6.6 MeV

2 Dec 3 Dec

VG04-190-31

GOES Electrons

• GOES electron data quiet on 2-5 Dec• Electron activity observed on 5-7 Dec

VG04-190-32

SERVIS Electron Data – 1/2


1.0E+01

1.0E+02

1.0E+03

1.0E+04

1.0E+05

1.0E+06

1.0E+07

1.0E+08

7:00 9:00 11:00 13:00 15:00 17:00 19:00 21:00 23:00UT (hh:mm)

Ele

ctro

n Fl

ux (c

m-2

s-1

)



1.0E+01

1.0E+02

1.0E+03

1.0E+04

1.0E+05

1.0E+06

1.0E+07

1.0E+08

0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00UT (hh:mm)

Ele

ctro

n Fl

ux (c

m-2

s-1

)



1.0E+01

1.0E+02

1.0E+03

1.0E+04

1.0E+05

1.0E+06

1.0E+07

1.0E+08

0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00UT (hh:mm)

Ele

ctro

n Fl

ux (c

m-2

s-1

)



1.0E+01

1.0E+02

1.0E+03

1.0E+04

1.0E+05

1.0E+06

1.0E+07

1.0E+08

0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00UT (hh:mm)

Ele

ctro

n Fl

ux (c

m-2

s-1

)


3 Dec2 Dec

4 Dec 5 Dec

VG04-190-33

SERVIS Electron Data – 2/2


1.0E+01

1.0E+02

1.0E+03

1.0E+04

1.0E+05

1.0E+06

1.0E+07

1.0E+08

0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00UT (hh:mm)

Ele

ctro

n Fl

ux (c

m-2

s-1

)



1.0E+01

1.0E+02

1.0E+03

1.0E+04

1.0E+05

1.0E+06

1.0E+07

1.0E+08

0:00 2:00 4:00 6:00 8:00 10:00 12:00 14:00 16:00 18:00 20:00 22:00 0:00UT (hh:mm)

Elec

tron

Flu

x (c

m-2

s-1

)


6 Dec 7 Dec

VG04-190-34

Summary and Conclusions

• 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

energetic charged particle spectrometer for the … sciences inc. 20 new england business center...

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