Space Radiation EnvironmentMagnetic Storms •Solar Wind Disturbs the Current Systems in the...

Space Radiation Environment

Behcet ALPATINFN -Perugia, Italy

IV Corso di Formazione INFN su “Qualità e Progettazione di Sistema per Esperimenti di Fisica nello Spazio e agli

Acceleratori” 20-22 Ottobre , 2010, Assisi

B.Alpat, Corso di Formazione INFN, 20-22- Ottobre, 2010, Assisi2

SQ Constraints

• The following constraints shall be taken into account according to the mission:– resistance to corrosion,

– resistance to mechanical load (dynamic or static),

– resistance and performance in vacuum,

– performance in microgravity,

– resistance to radiation,

– resistance to thermal cycling,

– resistance to fluids according to mission requirements,

– resistance to other conditions specific to the mission (atomic oxygen, offgassing, flammability, odour, etc...).

– resistance to combined actions of the environment and loads (stress corrosion cracking, thermoelastic behavior, cold welding,...).


Radiation Hardness Assurance

(RHA)

• The organization, documentation and procedures developed and applied to assure that a system can operate in a specified radiation environment

• These activities may occur at the system, sub-system, module/board and piece part levels


Critical Parameters for

Mission Definition for

Radiation Predictions

• When and how long the mission will fly • Where the mission will fly • When the systems are deployed • What systems must operate during worst

case environment conditions • What systems are critical to mission

success • Amount of shielding surrounding devices


Components of the Natural

Environment

• Solar Particle Events– Protons & Heavier Ions

• Transient– Galactic Cosmic Rays

• Protons & Heavier Ions

• Trapped– Electrons, Protons, & Heavier Ions

• Atmospheric & Terrestrial Secondaries– Neutrons


Radiation & Effects

• Total Ionising Dose– Cumulative long term

ionising damage due to protons & electrons

• Displacement Damage– Cumulative long term

non-ionising damage due to protons, electrons, & neutrons

• Single Event Effects– Event caused by a

single charged particle -heavy ions & protons for some devices


Sun

• Dominates theRadiationEnvironment– Source

– Modulator

• Structure– Photosphere

– Chromosphere

– Corona


Solar Flares

• Sudden BrighteningNear Sunspots

• Solar System’ sLargest ExplosiveEvents

• Particles AcceleratedDirectly by Event

• Heavy Ion Rich SolarEvents


Coronal Mass Ejection

• Observed byLASCO C2 on 2000.

• Bubble of Gas & Magnetic Field

• Ejects ~10 17 grams of Matter (mostly protons and electrons)

• Shock Wave AcceleratesParticles to Millions of km/hr

• Associated with Magnetic Storms

• Proton Rich Solar Events


TIROS Measurements of

Protons

Day Before Coronal Mass Ejection


TIROS Measurements of

Protons (cont’d)

November 6, 1997 Coronal Mass Ejection


Eruptive Prominance

• Erupting prominances when Earthward directed can affect communications, navigation systems even power grids, while also producing auroras visible in the night skies

Prominance 24 Juy 1999 (extends over 35 Earths out from Sun)


Coronal Holes

• Darker/cooler zone of corona

• Observed by X-ray telescope on Skylab

• Fast moving solar wind pass through (magnetic fields lines)

• Contribute to flux modulation in outer belts

From G.Berger SERESSA09


Solar Wind

• Stream of Charged Particles from Sun’ sCorona– Electrons– Protons Density ~ 1 - 30 / cm 3– Heavy Ions

• Magnetized Plasma• Detected Out to 10 billion km from Earth by

Pioneer 10• Velocity ~ 300 - 900 km/s• Energy ~ .5 - 2.0 keV/nuc


Aurora

• Particles stream down onmagnetic field lines from the geomagnetic tail forming an auroral belt

• Electrons collide withatmospheric gases

• Electrons give energy to atoms and molecules which emit energy as light

• Oxygen ---> GreenNitrogen ---> Red


Solar Wind Density & VelocityD

ensi

ty (

#/c

m3)

Velo

city

(km

/s)


Solar Activity: Cyclic

Variation

• Sunspot Cycle Discovered in mid 1800s

• Used as Indicator of Solar Activity

• Increased Solar Activity Results in:– Increased Rate of CME

– Increased Rate of Solar Flares

– Increased Rate of Magnetic Storms

– Increased Levels of Electrons in Van Allen Belts

– Decreased Levels of Protons in Van Allen Belts

– Increased Incidence of New Belt Formation

– Decreased Levels of Galactic Cosmic Rays

– Increased Rate of Solar Particle Events

• Effects on Climate?


Sunspot Cycle

Length Varies from 9 – 13 Years, 7 years Solar Maximum, 4 Years Solar

Minimum

Su

nsp

ot N

um

ber

s


Sunspot CycleS

un

spo

t N

um

ber

s


Solar Particle Events

• Increased Levels of Protons & Heavier Ions• Energies

– Protons - 100s of MeV– Heavier Ions - 100s of GeV

• Abundances Dependent on Radial Distance from Sun• Partially Ionized - Greater Ability to Penetrate

Magnetosphere• Number & Intensity of Events Increases Dramatically

During Solar Maximum• Models

– Dose - SOLPRO, JPL, Xapsos/NRL– Single Event Effects - CREME96 (Protons & Heavier Ions)



• Poor Correlation with Solar Flares• Strong Correlation with Coronal Mass

Ejections– No Fundamental Association with Flares– Transient Shock Wave Disturbances in the

Solar Wind– Large Geomagnetic Storms– Large Particle Events


Rapid onset times (minutes), with durations up to hours or days

Essentially unpredictable, however generally coincide with solar maximum periods

Proton energies up to ~100s ofMeV, sometimes GeV range

Integral fluence up to ~109 –1010 p/cm2 (>1 MeV)

Some contribution from heavierions and e-

In the main phase of an event,particle fluxes isotropic

In space mission design andoperational context, treated withstatistical models (JPL-91, ESP,Rosenqvist) and “SpaceWeather” updates

From P.Nieminen, CERN, Februray 2010



14 July 2000, Protons and X-

Rays

From G.Berger SERESSA09


Sunspot Cycle with Solar

Proton Events

Proton Event Fluences

Years

Pro

ton

s (#

/cm

2)


Solar Protons:Orbits

Proton Levels Predicted by CREME96

Pro

ton

s (#

/cm

2/s

ec/M

eV)

Energy (MeV)


Magnetosphere


Magnetic Storms

• Solar Wind Disturbs the CurrentSystems in the Magnetosphere

• Major Storms Probably the Result of CMEs– Must Be Pointed Toward Earth– Strongest Arrive with Interplanetary

Magnetic Field Oriented South

• Cause Increase in Rate & Intensity ofMagnetic Sub-storms in the Geotail


Effects of Solar Storms

• Power Black-outs on Earth• Block Some Radio Communication

– Disturbs electrically charged gases in the ionosphere

• Interfere with Cellular Phone Systems– Ionospheric disturbances & satellite system

failures


Effects of Solar Storms

(cont’d)

• Interfere with GPS Navigation (Ships & Airplanes)

• Trigger Phantom Commands on Spacecraft

• Increased Atmospheric Drag on Low Earth Orbit (LEO) Satellites

• Increased Protons & Heavy Ion Particle Counts

• “Pump Up” the Van Allen Belts


Discovery of Galactic

Cosmic Rays - 1913

• Electroscope Experiments– Dissipation of Charge on Leaves?– Emissions from Materials on Earth– “Clean” Instruments Did Not Eliminate Dissipation

• Hess– Balloon Experiments with Electroscopes– Hypothesis: Background Radiation Will Disappear

with Increasing Altitude– > 10,000 feet - Background Increased with Altitude– Named “Cosmic Rays” by Hess

B.Alpat, Corso di Formazione INFN, 20-22- Ottobre, 2010, Assisi

32

All Particle Spectrum and

Composition of Cosmic Rays

•All stable elements ofperiodic table are presentin CR

•Abundances equal tothose of solar system


Particle Composition at Low

Energies


GCRs: Solar Modulation

• CNO-24 hour mean exposure

CN

O (

#/c

m2/s

ter/

s/M

eV/n

)

Date


GCRs:Shielded Fluences-Fe

• Interplanetary,CREME96, Solar Minimum

Part

icle

s (#

/cm

2/d

ay/M

eV/n

)

Energy (MeV/n)


GCRs:Shielded Fluences-Fe

• CREME96, Solar Minimum, 100 mils (2.54mm) Al

Part

icle

s (#

/cm

2/d

ay/M

eV/n

)

Energy (MeV/n)


Trapped Radiation


Discovery of Radiation Belts

(Trapped Radiation-Van

Allen Belts)

• Omnidirectional

• Components– Protons: E ~ .04 - 500 MeV

– Electrons: E ~ .04 - 7(?) MeV

– Heavier Ions: Low E - Non-problem for Electronics

• Location of Peak Levels Depends on Energy

• Average Counts Vary Slowly with the Solar Cycle

• Location of Populations Shifts with Time

• Counts Can Increase by Orders of Magnitude DuringMagnetic Storms– March 1991 Storm - Increases Were Long Term


Trapped Particle Motions

Spiral, Bounce, Drift


Van Allen Belts

High Latitude Horns

Outer Belt


Proton & Electron

Intensities

AP-8 Model AE-8 Model


TIROS/NOAA Trapped Protons

Radio

Flu

x F

10

.7

Solar Cycle Variation: 80-215 MeV Protons

Pro

ton F

lux (

#/c

m2/s

ec)

Date


Activity in the Slot Region-

SAMPEX

SAMPEX/P1ADC: Electrons E > 0.4 MeV

L-S

hell

Day(1992)


SRAM Upset Rates on

CRUX/APEX


Terrestrial Radiation Sources

• Man-made• Natural Emissions from Earth Materials

– Package Contamination

• Cosmic Rays - Particle Showers


Terrestrial Cosmic Rays

• Particles That Hit the Earth from Outer Space• Need > 1 GeV to Penetrate to Sea Level• Fewer Than 1% Are Primary• Mostly 3rd to 7th Generation Cascade Particles• Search for Cause of Interference on Laboratory• Instruments in Early 1900s

– Led to Discovery of Cosmic Rays by Hess

• Induce SEUs: Neutrons + Protons + Pions


47

The process begins in space with primary galactic cosmic rays

entering the atmosphere after passing through the heliosphere

(solar modulation) and geomagnetic field (rigidity cutoff).

Most of these primaries are energetic enough to produce

a nuclear or high energy interaction initiating a cascade

of particles through the atmosphere.

As the ensemble of cascades

develop the particle density and

the particle type distribution varies

with atmospheric depth as shown

in the Figure.

The passage of each particle type

through atmosphere is

determined by different interaction

channels. The dominate

interaction depends on particle

type, energy and material.

Above energies of 100MeV muons are the dominate species at

sea-level, however when considering all energies neutrons

dominate in numbers.


Neutrons

• Source - Secondary Products of Particle• Cascades

– Spacecraft Materials– Galactic Comic Ray Collisions with Atmospheric O

& N

• Single Event Upset Hazard– Ground Level in Large Memory Banks– Avionics– Low Earth Orbits – Shuttle

• First Recognized as Problem in 1980s


Neutron Environment(Normand et al.)


Neutron Flux MeasurementsN

orm

aliz

ed t

o P

eak

Altitude (feet)


AM9114 4K NMOS Error Rates

Protons Neutrons Muons Pions Pions

>100 MeV >10 MeV (Stopping) >100 MeV (Stopping)

Pre

dic

ted

Err

ors

/Dev

ice/

s

Predicted Error Rates at Two Altitudes

52

Involves 3 different quantities;

1. The cross section of the device,often determined empirically;

2. The distribution of particlesexpected in the spaceenvironment, which depends onassumptions about solar flareactivity, radiation belt activity,and shielding;

3. The critical charge, sensitive areaand sensitive volume associatedwith the SEE phenomenon ofinterest.

Expected SEE Rate Calculation


52

B.Alpat, "Space Radiation and its Effects" Course, ASELSAN, July 14-16th, 201053

Simulations of the

Space Radiation

Environment

• From G.Santin

Protons, some ions, electrons, neutrons,

gamma rays, X-rays…

Softer spectrum

Event driven – occasional high fluxes over short

periods.

Solar radiation Electrons ~< 10 MeV

Protons ~< 102 MeV

Trapped radiation

Sourc

es

Protons and Ions

<E> ~ 1 GeV, Emax > 1021 eV

Continuous low intensity

(Extra) Galactic and

anomalous Cosmic Rays

Effects

Single Event Effects

(SE Upset, SE Latchup, …)

Degradation

(Ionisation, displacement,…)

Effects in components

Signal, Background

(Spurious signals, Detector overload,…)

Charging

(internal, interferences, …)

Effects to science detectors

Dose (dose equivalent) and dose rate in

manned space flights

Radiobiological effects

Threats to life

Ground tests

Extrapolation to real life in space

Cheaper than accelerator tests

Mission design

Goals

Particle signal extraction

Background

Degradation

Science analyses

Simulation of the emission and the

propagation of radiation in space

Environment models

From G.Santin

54

Radiation Environment Simulation

Current tools include:

SPENVIS – models of space environment & basic effects analysis (ESA/BIRA)

CREME96 – Cosmic Ray/SEU analysis (NRL)

SIREST – space environment analysis for Shuttle missions (NASA/LaRC)

SEDAT (Space Environment Data Analysis Tool) – databases of space environment data & tools for analysis. (ESA/RAL)

ESABASE/Radiation Space Systems Analyser

…

GEANT4Physics models

– Scientific Exploration,

Manned space flight:

– Low En EM, Ion hadronics

Engineering tools

– PlanetoCosmics (mg cut-off)

– SSAT (Ray-Tracing)

– MULASSIS (1D shielding)

– GEMAT (micro-dosimetry)

– NIEL (Displacement Damage)

– Reverse MC

– GRAS ( 3D, multi-purpose analysis framework)Interfaces

– Materials

– GDML

– CAD geometries

– SPENVISB.Alpat, Corso di Formazione INFN, 20-22- Ottobre, 2010, Assisi

54

Radiation Environment Simulation

Particle fluxes simulated using SPENVIS, CREME96, AF-GEOSPACE

Effects on devices simulated using GEANT4, GRAS, FLUKA

By simulating both diffuse and location dependent contributions (like Particles Trapped by Geomagnetic field) we are able to estimate the effects on average and in the Worst Case Scenario.

The SPENVIS, ESA's Space Environment Information System, is basedon a WWW interface to models of the space environment and its effects,including the natural radiation belts, solar energetic particles, cosmicrays, plasmas, gases, and "micro-particles”.Th:user should provide to SPENVIS as input several information such as,-The mission parameters,- the space weather conditions,- the type of particles for which the SEE effects can be estimated,- DUT parameteres (i.e. dimensions, bulk material, layout etc.)shielding configurations,cross section versus LET values including saturated cross section and -LET threshold values deriving from Weibull fit


55

B.Alpat, "Space Radiation and its Effects" Course, ASELSAN, July 14-16th, 201056

FRAM TEST REPORT AND

MITIGATION SUGGESTED

• FRAM -> SEE_Rates_and_Mitigation3-2.pdf

SERMS_SEE_Rates_and_Mitigation3-2.pdf







Useful Links

• SPENVIS http://www.spenvis.oma.be/spenvis/

• CREME96 https://creme96.nrl.navy.mil/

• GEANT4-Space http://geant4.esa.int/

• ESA-ESCC https://spacecomponents.org/

• ESA- Space Weather http://esaspaceweather.net/spweather/BACKGROUND/index.html

• NASA-RadHome http://radhome.gsfc.nasa.gov/radhome/Nat_Space_Rad_Tech.htm

• NASA Standards http://standards.nasa.gov/

• MIL Standards http://assist.daps.dla.mil/quicksearch/

• JEDEC Standars: www.jedec.org

ESA Space Environments and Effects http://space-env.esa.int/

http://www.spenvis.oma.be/spenvis/

https://creme96.nrl.navy.mil/

http://geant4.esa.int/

https://spacecomponents.org/

http://esaspaceweather.net/spweather/BACKGROUND/index.html

http://radhome.gsfc.nasa.gov/radhome/Nat_Space_Rad_Tech.htm

http://radhome.gsfc.nasa.gov/radhome/Nat_Space_Rad_Tech.htm

http://standards.nasa.gov/

http://assist.daps.dla.mil/quicksearch/

http://www.jedec.org/


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