core technologies for space systems
TRANSCRIPT
J. Barth/CTS 1998
Core Technologies for Space Systems
Space Radiation Environments
Janet Barth & Ken LaBelNASA/NASA/GoddardGoddard Space Flight Center Space Flight Center
Greenbelt, MarylandNovember 12, 1998
J. Barth/CTS 1998
The Radiation Environment
Solar Protons&
Heavier Ions
Galactic Cosmic Rays
Trapped Particles
Nikkei Science, Inc. of Japan, by K. Endo
J. Barth/CTS 1998
Effects on Electronicsu Total Ionizing Dose
» Trapped Protons & Electrons» Solar Protons
u Single Event Effects» Protons
− Trapped− Solar
» Heavier Ions− Galactic Cosmic Rays− Solar
» Neutrons
u DisplacementDamage» Protons» Electrons» Neutrons
J. Barth/CTS 1998
Sun:Dominates the Environment
Trapped Particles
Heavier Ions
ProtonsSource
SunModulator
Galactic Cosmic RaysAtmospheric
NeutronsTrapped Particles
J. Barth/CTS 1998
Gradual Eventsu Coronal Mass
Ejectionsu Particles Accelerated
by Shock Waveu Largest Proton Eventsu Decay of X-Ray
Emission Occurs OverSeveral Hours
u Large Distribution inSolar LongitudeHolloman AFB/SOON
J. Barth/CTS 1998
Impulsive Events
u Solar Flaresu Particles Accelerated
Directlyu Heavy Ion Richu Sharp Peak in X-Ray
Emissionu Concentrated Solar
LongitudeDistribution
J. Barth/CTS 1998
1947 1997
Sunspot Cycle
Length Varies from 9 - 13 Years7 Years Solar Maximum, 4 Years Solar Minimum
Years0
50
150
200
250
100
300
Suns
pot N
umbe
rs Cycle 18
Cycle 22Cycle 21Cycle 20Cycle 19
after Lund Observatory
J. Barth/CTS 1998
Galactic Cosmic Ray Ionsu All Elements in Periodic Tableu Energies in GeVu Found Everywhere in Interplanetary Spaceu Omnidirectionalu Mostly Fully Ionizedu Cyclic Variation in Fluence Levels
» Lowest Levels = Solar Maximum Peak» Highest Levels = Lowest Point in Solar Minimum
u Single Event Effects Hazardu Model: CREME96
J. Barth/CTS 1998
1 0 2 0 3 0 4 0 5 0 6 0 7 0 8 0 9 0 1 0 01 0 -2
1 0 -1
1 0 0
1 0 1
1 0 2
1 0 3
1 0 4
1 0 5
1 0 6
1 0 7
1 0 8
1 0 9
1 0 1 0
GCRs: Nuclear CompositionRe
lativ
e Flu
x (S
i = 1
06 )
C
Nuclear Charge (Z)
HHe
OSi Fe
ZrBa Pt
PbIndividual Elements Even-Z Elements Elemental Groups
Energy = 2 GeV/n, Normalized to Silicon = 106
J. Barth/CTS 1998
1 9 7 5 1 9 7 7 1 9 7 9 1 9 8 1 1 9 8 3 1 9 8 5 1 9 8 7 1 9 8 9 1 9 9 1 1 9 9 3 1 9 9 51 0 -5
1 0 -4
1 0 -3
1 0 -2
1 0 -1
1 0 0
1 0 1
1 0 2
GCRs: Solar Modulation
Date
CNO
(#/c
m2 /
ster
/s/M
eV/n
) CNO - 24 Hour Averaged Mean Exposure Flux
Energy = 25-250 MeV/n IMP-8
J. Barth/CTS 1998
1 0 -1 1 0 0 1 0 1 1 0 2 1 0 3 1 0 4 1 0 51 0 -6
1 0 -5
1 0 -4
1 0 -3
1 0 -2
1 0 -1
1 0 0
1 0 1
S u rfa c e I n c i d e n t1 0 0 m ils ( 2 . 5 4 m m ) A l5 0 0 m ils ( 1 2 . 7 m m ) A l
GCRs: Shielded Fluences - FePa
rticle
s (#/
cm2 /
day/
MeV
/n) Interplanetary, CREME 96, Solar Minimum
Energy (MeV/n)
J. Barth/CTS 1998
1 0 -1 1 0 0 1 0 1 1 0 2 1 0 3 1 0 4 1 0 51 0 -6
1 0 -5
1 0 -4
1 0 -3
1 0 -2
1 0 -1
G E OG T OM E OE O SL E O
GCRs: Shielded Fluences - FeCREME 96, Solar Minimum, 100 mils (2.54 mm) Al
Energy (MeV/nuc)
Parti
cles (
#/cm
2 /da
y/M
eV/n
uc)
J. Barth/CTS 1998
GCRs: Integral LET SpectraCREME 96, Solar Minimum, 100 mils (2.54 mm)Al
LET (MeV-cm2/mg)
LET
Flue
nce (
#/cm
2 /da
y)
1 0 -1 1 0 0 1 0 1 1 0 21 0 - 81 0 - 71 0 - 61 0 - 51 0 - 41 0 - 31 0 - 21 0 - 11 0 01 0 11 0 21 0 31 0 4
G E OG T OM E OE O SL E O
Z = 2 - 92
J. Barth/CTS 1998
Solar Particle Eventsu Results in Increased Levels of Protons & Heavier Ionsu Energies
» Protons - 100s of MeV» Heavier Ions - 100s of GeV
u Abundances Dependent on Radial Distance from Sunu Partially Ionized - Greater Ability to Penetrate
Magnetosphere Than Galactic Cosmic Raysu Number & Intensity of Events Increases Dramatically
During Solar Maximumu Models
» Dose & Displacement Damage - SOLPRO, JPL, Xapsos/NRL» Single Event Effects - CREME96 (Protons & Heavier Ions)
J. Barth/CTS 1998
Sunspot Cycle with Solar Proton Events
1 9 6 5 1 9 7 0 1 9 7 5 1 9 8 0 1 9 8 5 1 9 9 0 1 9 9 51 0 7
1 0 8
1 0 9
1 0 1 0
1 0 1 1> 1 0 M e V ; Φ ≥ 1 0 8 p /c m 2
> 3 0 M e V ; Φ ≥ 1 0 7 p /c m 2
Z u r i c h S m o o t h e d S u n s p o t N u m b e r
C y c l e 2 0 C y c l e 2 1 C y c le 22
*
**
0
2 0
4 0
6 0
8 0
1 0 0
1 2 0
1 4 0
1 6 0
1 8 0
2 0 0
Prot
ons (
#/cm
2 )
Year
Proton Event Fluences
Smoo
thed
Sun
spot
Num
bers
J. Barth/CTS 1998
Solar Proton Event - October 1989
10 -4
10 -3
10 -2
10 -1
1 0 0
1 0 1
1 0 2
1 0 3
1 0 4
1 0 5
1 5
1 6
1 7
1 8
19
20
2 1
2 2
2 3
2 4
2 5
2 6
2 7
2 8
2 9
3 0
3 1
1
2
3
4
5
6
7
8
9
1 0
1 1
1 2
1 3
1 4
1 5
-2000
2 0 0
O c t o b e r N o v e m b e r
Coun
ts/c
m2 /
s/st
er/M
eVnT
Protons & Electrons - Magnetic Field99% Worst Case Event
GOES Space Environment Monitor
J. Barth/CTS 1998
Proton Event Spectra - Cycle 22
1 0 0 1 0 1 1 0 21 0 4
1 0 5
1 0 6
1 0 7
1 0 8
1 0 9
1 0 1 0
1 0 1 1
1 0 1 2
1 0 1 3
2 0 M a r 1 9 9 14 J u n e 1 9 9 12 7 S e p t 1 9 9 12 0 F e b 1 9 9 4A u g 1 9 7 21 9 O c t 1 9 8 9
Energy (> MeV)
Prot
on F
luen
ce (#
/cm
2 /ev
ent)
Total Integral Proton Fluence
J. Barth/CTS 1998
Solar Protons: Orbits
1 0 -1 1 0 0 1 0 1 1 0 2 1 0 3 1 0 4 1 0 5
e 2
1 0 -1 41 0 -1 31 0 -1 21 0 -1 11 0 -1 0
1 0 -91 0 -81 0 -71 0 -61 0 -51 0 -41 0 -31 0 -21 0 -11 0 01 0 11 0 21 0 31 0 4
GE
O
G E OE O SI = 6 0 d e g / H = 8 0 0 k mL E O
Energy (MeV)
Prot
ons (
#/cm
2 /se
c/M
eV)
Proton Levels Predicted by CREME 96
Averaged Over Worst Day
J. Barth/CTS 1998
Effect of Shielding on Heavy Ions
1 0 - 1 1 0 0 1 0 1 1 0 2
s e 1 0 0
1 0 - 1 51 0 - 1 41 0 - 1 31 0 - 1 21 0 - 1 11 0 - 1 0
1 0 -91 0 -81 0 -71 0 -61 0 -51 0 -41 0 -31 0 -21 0 -11 0 01 0 11 0 21 0 31 0 4
slet
100
S o la r P e a k s - 1 0 0 m ilsS o la r P e a k s - 2 0 0 m ilsS o la r P e a k s - 4 0 0 m ilsP e a k G C R - 1 0 0 m ilsP e a k G C R - 4 0 0 m ilsFl
uenc
e (#/
cm2 /
s)
LET (MeV-cm2/mg)
Transient Particles Unattenuated by the Magnetosphere
CREME96
J. Barth/CTS 1998
Trapped Radiation
Trapped ParticlesProtons, Electrons, Heavy Ions
Nikkei Science, Inc. of Japan, by K. Endo
J. Barth/CTS 1998
Trapped - Van Allen Beltsu Omnidirectionalu Components
» Protons: E ~ .04 - 500 MeV» Electrons: E ~ .04 - 7(?) MeV» Heavier Ions: Low E - Non-problem for Electronics
u Location of Peak Levels Depends on Energyu Average Counts Vary Slowly with the Solar Cycleu Location of Populations Shifts with Timeu Counts Can Increase by Orders of Magnitude During
Magnetic Storms» March 1991 Storm - Increases Were Long Term
J. Barth/CTS 1998
Trapped Particle Modelsu NASA AP-8 & AE-8u Air Force CRRES & APEX Models
» CRRESPRO, CRRESELE, CRRESRAD & APEXRADu New Models - NASA Space Environment and Effects
Program» Low Altitude Model for Protons- < 1000 km
− Boeing− Based on TIROS Data
» Model Being Extended to Higher Altitudes− Will Combine CRRES and TIROS Data
» Will Begin Electron Modeling if Funding is Available
J. Barth/CTS 1998
Proton & Electron Intensities
1 2 3 4 5 6 7 8 9 101234
L-Shell
AP-8 Model AE-8 ModelEp > 10 MeV Ee > 1 MeV
NASA/GSFC
#/cm2/sec #/cm2/sec
J. Barth/CTS 1998
TIROS/NOAA Trapped Protons
1976 1980 1984 1988 1992 1996
104
103
102
101 50
100
150
200
250
Prot
on F
lux
(#/c
m2 /s
)
Date
Solar Cycle Variation: 80-215 MeV Protons
L=1.20
L=1.18
L=1.16
L=1.14
B/Bmin=1.0
Rad
io F
lux
F 10
.7
Huston et al.
J. Barth/CTS 1998
Trapped Protons - 1000 km
-180 -150 -120 -90 -60 -30 0 30 60 90 120 150 180
Geographic Longitude (deg)
-80
-60
-40
-20
0
20
40
60
80
Geo
cent
ric L
atitu
de (d
eg)
1 10
100 1000
5000
Integral Proton Flux Contours for E > 30 MeV (#/cm 2/s)Altitude = 1000 km, Solar Maximum
J. Barth/CTS 1998
Trapped Electrons - 1000 km
-180 -150 -120 -90 -60 -30 0 30 60 90 120 150 180
Geographic Longitude (deg)
-80
-60
-40
-20
0
20
40
60
80
Geo
cent
ric L
atitu
de (d
eg)
1
1
1
1
1
1
1000
1000
1000
1000
10000
10000
10000 10000 10000
100000 100000
100000
100000 500000
Integral Electron Flux Contours for E > 0.5 MeV (#/cm 2/s)Altitude = 1000 km, Solar Maximum
J. Barth/CTS 1998
SRAM Upset Rates on CRUX/APEX
- 1 8 0 - 1 5 0 - 1 2 0 - 9 0 - 6 0 - 3 0 0 3 0 60 9 0 1 2 0 1 5 0 1 8 0
L o n g i t u d e
- 9 0
- 7 5
- 6 0
- 4 5
- 3 0
- 1 5
0
1 5
3 0
4 5
6 0
7 5
9 0
Latit
ude
H i t a c h i 1 M : A l t i t u d e : 1 2 5 0 k m - 1 3 5 0 k m
1 . 0 E - 7 t o 5 . 0 E - 75 . 0 E - 7 t o 1 . 0 E - 61 . 0 E - 6 t o 5 . 0 E - 65 . 0 E - 6 t o 1 . 0 E - 51 . 0 E - 5 t o 5 . 0 E - 55 . 0 E - 5 t o 1 . 0 E - 41 . 0 E - 4 t o 5 . 0 E - 45 . 0 E - 4 t o 1 . 0 E - 31 . 0 E - 3 t o 5 . 0 E - 3
U p s e t s / B i t / D a y
-180 -150 -120 -90 -60 -30 0 30 60 90 120 150 180
L o n g i t u d e
-90
-75
-60
-45
-30
-15
0
15
30
45
60
75
90
Latit
ude
Hi tach i 1M:A l t i t ude :650km - 750km
1.0E-7 to 5 .0E-75 .0E-7 to 1 .0E-61 .0E-6 to 5 .0E-65 .0E-6 to 1 .0E-51 .0E-5 to 5 .0E-55 .0E-5 to 1 .0E-41 .0E-4 to 5 .0E-45 .0E-4 to 1 .0E-31 .0E-3 to 5 .0E-3
Upsets /B i t /Day
- 1 8 0 - 1 5 0 - 1 2 0 - 9 0 - 6 0 - 3 0 0 3 0 6 0 9 0 1 2 0 1 5 0 1 8 0
L o n g i t u d e
- 9 0
- 7 5
- 6 0
- 4 5
- 3 0
- 1 5
0
1 5
3 0
4 5
6 0
7 5
9 0
Latit
ude
H i t a c h i 1 M :A l t i t u d e : 1 7 5 0 k m - 1 8 5 0 k m
1 . 0 E - 7 t o 5 . 0 E - 75 . 0 E - 7 t o 1 . 0 E - 61 . 0 E - 6 t o 5 . 0 E - 65 . 0 E - 6 t o 1 . 0 E - 51 . 0 E - 5 t o 5 . 0 E - 55 . 0 E - 5 t o 1 . 0 E - 41 . 0 E - 4 t o 5 . 0 E - 45 . 0 E - 4 t o 1 . 0 E - 31 . 0 E - 3 t o 5 . 0 E - 3
U p s e t s / B i t / D a y
- 1 8 0 - 1 5 0 - 1 2 0 - 9 0 - 6 0 - 3 0 0 3 0 6 0 9 0 1 2 0 1 5 0 1 8 0
L o n g i t u d e
- 9 0
- 7 5
- 6 0
- 4 5
- 3 0
- 1 5
0
1 5
3 0
4 5
6 0
7 5
9 0
Latit
ude
H i t a c h i 1 M : A l t i t u d e : 2 4 5 0 k m - 2 5 5 0 k m
1 . 0 E - 7 t o 5 . 0 E - 75 . 0 E - 7 t o 1 . 0 E - 61 . 0 E - 6 t o 5 . 0 E - 65 . 0 E - 6 t o 1 . 0 E - 51 . 0 E - 5 t o 5 . 0 E - 55 . 0 E - 5 t o 1 . 0 E - 41 . 0 E - 4 t o 5 . 0 E - 45 . 0 E - 4 t o 1 . 0 E - 31 . 0 E - 3 t o 5 . 0 E - 3
U p s e t s / B i t / D a y
J. Barth/CTS 1998
Magnetic Storms - HipparcosL-
Shel
l
4-Day, 9-Orbit Averages
Star Mapper - Radiation Background
Daly, et al.
March1990 1991 1992
2
4
6
J. Barth/CTS 1998
CRRES - Measured Proton Belt
AF Phillips Laboratory, SPD/GD
J. Barth/CTS 1998
Solar Cycle Effectsu Solar Maximum
» Trapped Proton Levels Lower, Electrons Higher» GCR Levels Lower» Neutron Levels in the Atmosphere Are Lower» Solar Events More Frequent & Greater Intensity» Magnetic Storms More Frequent --> Can Increase Particle
Levels in Beltsu Solar Minimum
» Trapped Protons Higher, Electrons Lower» GCR Levels Higher» Neutron Levels in the Atmosphere Are Higher» Solar Events Are Rare
J. Barth/CTS 1998
Models of the Environmentu Trapped Particles
» NASA AP-8 & AE-8 - Data from 1960s & 1970s» AFRL CRRESPRO & CRRESELE - Solar Max Only» MDAC* - Low Altitude Improvements for Protons Based on
NOAA/TIROS Data» “AP-9”* in Development» Will Begin “AE-9” Development if Funding Levels Permit
u Galactic Cosmic Ray Heavy Ions» CREME96* - Update to Outdated CREME86
u Solar Protons - Dose & Degradation» New Solar Proton Model* - Total Fluence
u Solar Heavy Ions - Single Event Effects» CREME96* - Update to Inadequate CREME86
* Supported by NASA/Space Environment & Effects Program
J. Barth/CTS 1998
Environment Definitionu Total Ionizing Dose
» Dose-Depth Curves or Spacecraft Specific Dose Levels− Trapped Protons & Electrons− Solar Protons− Secondary Bremsstrahlung (High Electron Environments)
u Single Event Effects - Average & Peak Conditions» Galactic Cosmic Ray Heavy Ions (LET Spectra)» Solar Heavy Ions (LET Spectra)» Solar Protons (Energy Spectra)» Trapped Protons (Energy Spectra)