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New Surviving in space-3 · 2018. 11. 17. · CERN Course – Lecture 3 October 28, 2005 – L....
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Surviving in space: the challenges Surviving in space: the challenges of a manned mission to of a manned mission to MarsMars
Lecture 3Lecture 3Modeling the Interaction of the Modeling the Interaction of the
Space Radiation in Spacecraft & Space Radiation in Spacecraft & Humans, and Assessing the Risks Humans, and Assessing the Risks
on a Mission to Marson a Mission to Mars
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 2
Back to the Moon…Then, On to Mars
• President Bush has committed the US Space Program to going to Mars…
• The first step will be a return to the Moon to develop and test the techniques needed eventually to go to Mars…
• Crew radiation exposure has been identified as one of the major problems that must be dealt with to make this possible…
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 3
Radiation Exposure Guidelines
• Recall that astronauts will be held to the same exposure limits in terms of risk to health that ground-based atomic workers are!
• Nominally, for chronic exposure threats the biggest risk is radiation-induced cancer, and the current exposure guideline is to keep the Excess Lifetime Risk (ELR) to under 3%...
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 4
NASA Revised Standard for Radiation LimitsRevised standard applies a 95% confidence level to the career limit of 3% risk of lifetime fatal cancer
Approved by NASA Medical Policy Board
95% confidence is conservative Takes specific risk probabilities of individuals into accountNarrows range of increased riskEpidemiology, DDREF (Dose and Dose Rate Effectiveness Factor), quality (QF) and dosimetry uncertainties part of evaluation
“Lack of knowledge” leads to costs and restrictions
ISS Mission Nominal Fatal Cancer Risk
% Fatal Risk per0 1 2 3 4 5 6
Pro
babi
lity
0.0000
0.0025
0.0050
0.0075
0.0100
0.0125
0.0150
Risk DistributionD = 100 mGy E = 252 mSvQ = 2.52R0 = 1.0 %95% C.I. = [0.41, 3.02%]
Slide Courtesy of F. Cucinotta, NASA/JSC
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 5
Mars “Reference”Mission
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 6
Reference Mars Vehicles
Basic idea is to pre-position the ascent stage and habitats on Mars, along with the orbiting return vehicle before sending the crew with the descent stage… This is just a planning concept, and will likely be modified heavily in practice…
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 7
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 8
4-6 crew to Low Earth OrbitCrew Exploration Vehicle: Launch EnvironmentLEO EnvironmentEarth entry, water (or land) recovery
4-6 crew to lunar surface for extended-duration stayCEV:Earth-moon cruise – 4 daysLow lunar orbit (LLO) operations- 1 dayUntended lunar orbit operations – 4-14 daysLow lunar orbit operations – 1 dayMoon-Earth cruise – 4 days
Lunar Lander: Lunar surface operations 60-90 days
Crew TBD to Mars VicinityTransit vehicle: Earth-Mars cruise – 6-9 monthsMars vicinity operations – 30-90 daysMars-Earth cruise – 9-12 months
4-6 crew to lunar surface for long-duration stayLunar Habitat: Lunar surface operations 60-90 days
Crew TBD to Mars surfaceSurface Habitat
2030+
2020
2025+
2014
2015-2020
NASA ESMDSlide Courtesy of F. Cucinotta, NASA/JSC
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 9
Mars Mission Exposure Regimes• Trans-Mars & Trans-Earth Vehicle
– Normal Crew Compartment– “Storm Shelter” within Vehicle– Spacesuit EVAs
• Martian Surface– Within Surface Habitat– Possible “Storm Shelter” within Habitat– EVA Vehicle– Spacesuit EVAs
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 10
DEEP SPACE GCR DOSESTrans-Mars & Trans-Earth
• Annual bone marrow GCR doses will range up to ~ 15 cGy at solar minimum (~ 40 cSv) behind ~ 2cm Al shielding
• Effective dose at solar minimum is ~ 45-50 cSvper annum
• At solar maximum these are ~ 15-18 cSv• Secondary neutrons and charged particles are the
major sources of radiation exposure in an interplanetary spacecraft
• No dose limits yet for these missions
Courtesy of L. Townsend, US NCRP
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 11
From NASA 1996Strategic Program Plan
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 12
Dose v. Shielding DepthFor Various Materials
From NASA CP3360, J.W.Wilson et al., eds.
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 13
Cosmic Rays and Nuclear Physics•• NASANASA Sponsors Nuclear Modeling to
Obtain Nucleus-Nucleus EVENT GENERATORS for use in Monte Carlo Transport Codes…
• Like FLUKAFLUKA…– We have embedded DPMJETDPMJET 2.5 & 3
(for E > 5 GeV/A)– as well as RQMDRQMD
(for 100 MeV/A < E < 5 GeV/A)
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 14
…And, There is an OngoingNASA-Sponsored Program to Improve the
Accuracy of the Event Generators• There is a Dual Program to Both Model and
Measure Cross Sections…– The Focus is on the E < 5GeV/A Region…– Several Approaches are being taken…– The NASA-FLUKA Team is developing a new
Hamiltonian QMD Formalism (HQMD).• These Improvements will Directly benefit many
Cosmic Ray Applicatons…– Air Shower Calculations…– Galactic Transport Calculations…– Experimental Corrections…
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 15
The FLUKA Monte Carlo code
• hadron-hadron and hadron-nucleus interactions 0-100 TeV• nucleus-nucleus interactions 5 GeV/u-10,000 TeV/u(DPMJET) • electromagnetic and μ interactions 0-100 TeV• neutron multigroup transport and interactions 0-20 MeV
• nucleus-nucleus interactions below 5 GeV/u down to 100 MeV/u (by coupling with the RQMD 2.4 code)
• parallel development of an original non-relativistic QMD code down to ∼ 20 MeV/u
Courtesy of F. Balarini
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 16
New Methods
FLUKAGCR and SPE spectra
Quality factors Yields of “Complex Lesions”Dose
Equivalent dose
“Biological dose”(Complex Lesions/cell)
30 DNA base-pairs
mathematical phantom (68 regions)
“voxel” phantom (287 regions, > 2x106 voxels)
Courtesy of F. Balarini
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 17
FLUKA rQMDFragmentation Yields
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 18
FLUKA Simulations
“GOLEM” Voxel Phantom in FLUKA
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 19
FLUKA MIR TPEC Simulations
Neutron Fluences(Note the albedo fluences outside of the phantom…)
Charged Particle Fluences
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 20
Future developments
Further validation of the FLUKA Monte Carlo code in space radiation protection problems with
simple shielding geometry
Repetition for more realistic geometries of shielding and spacecraft
Ultimately, we will need to assess the risk from this kind of radiation field, and that is a Biology Problem,
not a physics challenge…
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 21
Annual GCR Doses
15.414.65.821.86.510
16.715.65.824.66.45
17.916.75.727.46.21
1970-71 Solar Maximum
Annual Dose
Equiv.(cSv)
Annual Dose(cGy)
Annual Dose
Equiv.(cSv)
Annual Dose(cGy)
Annual Effective
Dose (cSv)
Bone MarrowSkin
Al Shield
(g cm-2)
Courtesy of L. Townsend, US NCRP
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 22
Fatal Cancer Risk near Solar MaximumMaximum*(Males)
5 g/cm2 Al
[0.69, 7.2]2.1 0.600.25Mars (1000 d)
[0.65, 6.8]2.00.540.22Mars (600 d)
[0.11,1.2]0.350.090.042Lunar (90 d)
20 g/cm2 Al
[1.5,13.0]4.4 1.240.66Lunar (1000 d)
[1.5,13.3]4.41.210.63Lunar (600 d)
[0.92,7.4]2.70.690.45Lunar (90 d)
95% CI%REIDE, SvD, GyMission
*Phi=1100 MV (solar modulation) with Aug. 1972 SPE in transit
Slide Courtesy of F. Cucinotta, NASA/JSC
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 23
Solar Min Annual GCR Dose
39.337.016.156.218.01043.740.516.366.918.3548.844.516.479.818.41
1977 Solar Minimum
Annual Dose
Equiv.(cSv)
Annual Dose(cGy)
Annual Dose
Equiv.(cSv)
Annual Dose(cGy)
Annual Effective
Dose (cSv)
Bone MarrowSkin
Al Shield
(g cm-2)
Courtesy of L. Townsend, US NCRP
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 24
Fatal Cancer Risk at Solar MinimumMinimum(20 g/cm2 Aluminum Shielding)
Males
[1.4, 14.4]4.1 (4.5)**0.960.41Mars (1000 d)
[1.2, 12.8]3.90.870.36Mars (600 d)
[0.11,1.2]0.340.0710.03Lunar (90 d)
Females
[1.1,11.0]3.4 (3.2)*0.960.41Mars (1000 d)
[1.0,10.5]3.20.870.36Mars (600 d)
[0.09,0.96]0.280.0710.03Lunar (90 d)
95% CI%REIDE, SvD, GyMission
*Parenthesis exclude Prostate cancer; **Parenthesis LSS-report 12 (others report 13)Slide Courtesy of F. Cucinotta, NASA/JSC
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 25
Material Shielding and GCR Risks• Do materials rich in hydrogen and other light atomic mass atoms
significantly reduce GCR risks?• Possible advantages
– High Z/A ratio increases stopping effectiveness– Higher projectile fragmentation per unit mass in hydrogen– Reduced target fragmentation per unit mass in hydrogen
• Possible physics limitations to GCR shielding approaches– GCR not stopped in practical amounts of shielding– Target fragmentation is largely short-range and correlated with
projectile track– Target fragments in tissue occur for all materials and largely produced
by relativistic ions not absorbed by shielding• Do the biological uncertainties prevent us from knowing?
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 26
Significance of Shielding Materials for GCRSpiral 4 (40-yr Males): 20 g/cm2 Shields
(%) Fatal Cancer Risk0 3 6 9 12 15
Pro
babi
lity
0.000
0.003
0.006
0.009
0.012
0.015
Distribution aluminumDistribution polyethyleneDistribution Liq. Hydrogen (H2) E(alum) = 0.87 Sv E(poly) = 0.77 SvE(H2) = 0.43 SvR(alum) = 3.2 [1.0,10.5] (%)R(poly) = 2.9 [0.94, 9.2] (%)R(H2) = 1.6 [0.52, 5.1] (%)
Slide Courtesy of F. Cucinotta, NASA/JSC
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 27
GCR Risks• Clearly, annual doses < 20cGy present no acute health
hazard to crews on deep space missions• Hence only stochastic effects such as cancer induction
and mortality or late deterministic effects, such as cataracts or damage to the central nervous system are of concern.
• Unfortunately, there are NO DATANO DATA for human exposures from these radiations that can be used to estimate risks to crews
• In fact, as noted yesterday, it is not clear that the usual methods of estimating risk by calculating dose equivalent are even appropriate for these particles
Courtesy of L. Townsend, US NCRP
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 28
CONCLUSIONS - GCR• Cancer risks for exploration missions
– Risks from GCR are 2 to 5 percent mortality with upper 95% C.I. exceeding 10% for both males and females
• Shielding will not significantly reduce GCR risks• Materials have unknown benefits because of biological uncertainties
– Risks from SPE are manageable with shielding approaches• Hydro-carbon shields offer a mass reduction over Aluminum shields of factor of
two or more for acute effects from most SPE spectra• Benefits for cancer risk reduction are similar, however not significant for poly or
similar materials again due to biological uncertainties
• Uncertainty factors of 4-fold for GCR and 2.5 fold for SPE do not include several model assumptions– Uncertainties for Mars mission likely higher than estimated here
• Exploration vehicle shielding should focus on SPE not GCR
Slide Courtesy of F. Cucinotta, NASA/JSC
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 29
1.E-05
1.E-04
1.E-03
1.E-02
1.E-01
1.E+00
1.E+01
1.E+02
0 40 80 120 160 200 240
Time, h
Dos
e R
ate,
cSv
/h
Al thickness,g/cm2:
0135
10152030
1 rem/h
August 1972 Solar Particle Event
1.834.5720
10.720.910
39.161.15
PolyAlumDepth
BFO Dose, rem (cSv)
Slide Courtesy ofF. Cucinotta, NASA/JSC
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 30
GCR and SPE Dose: Materials & Tissue- GCR much higher energy producing secondary radiation
Shielding Depth, g/cm20 5 10 15 20 25 30 35
Dos
e E
quiv
alen
t, re
m/y
r
1
10
100
1000
10000
GCR L. HydrogenGCR PolyethyleneGCR GraphiteGCR AluminumGCR RegolithSPE GraphiteSPE Regolith
No Tissue Shielding With Tissue Shielding
August 1972 SPEShielding Depth, g/cm2
0 5 10 15 20 25 30 35D
ose
Equi
vale
nt, r
em/y
r1
10
100
1000
10000GCR L. HydrogenGCR PolyethyleneGCR GraphiteGCR AluminumGCR RegolithSPE GraphiteSPE RegolithSPE L. Hydrogen
Slide Courtesy of F. Cucinotta, NASA/JSC
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 31
August 1972 SPE -comparison to NCRP limits
1 13.31 11.63 6.89 8.01 1.80 2.76
2 7.25 6.57 4.90 5.81 1.32 1.95
5 2.23 2.11 1.60 1.79 0.62 0.88
10 0.62 0.60 0.56 0.42 0.25 0.33 !!!
Skin Lens BFO
NCRP limits for 30 days LEO missions: 1.5, 1.0 and 0.25 Gy-Eq for skin, lens and BFO, respectively ⇒ a 10 g/cm2 Al storm shelter would provide adequate protection
Erma Golem Erma Golem Erma Golem
Al shield (g/cm2)
Courtesy of F. Balarini
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 32
August 1972 SPE - skin vs. internal organs
0
2
4
6
8
10
12
14
1 2 5 10 20
Al thickness (g/cm2)
Total Primary Protons Secondary Hadrons
• much lower doses to liver than to skin (e.g. 1.0 vs. 13.3 Sv behind 1 g/cm2 Al )
• larger relative contribution of nuclear reaction products for liver than for skin (e.g. 14% vs. 7% behind 1 g/cm2 Al)
0
0.2
0.4
0.6
0.8
1
1.2
1 2 5 10 20
Al thickness (g/cm2)
Total Primary Protons Secondary Hadrons
Equivalent dose to skin (Sv) Equivalent dose to liver (Sv)
Courtesy of F. Balarini
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 33
Aug. 1972 and Oct. 1989 SPEs -Effective Dose (Sv)
Al shield August 1972 (Erma) October 1989 (Erma)
(g/cm2) E E* E*NASA E E* E*NASA
1 2.04 1.35 1.31 1.11 0.78 0.78
2 1.43 0.95 0.94 0.79 0.55 0.58
5 0.63 0.43 0.52 0.42 0.30 0.33
10 0.23 0.17 0.27 0.20 0.15 0.18
• large contribution (33-50%) from gonads, especially with small shielding
• E* values (by neglecting gonads) very similar to those calculated with the BRYNTRN code and the CAM phantom (Hoff et al. 2002, J. Rad. Res. 43)
Courtesy of F. Balarini
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 34
Conclusions - SPEs
• calculation of:
- dose decrease with increasing shielding
- differences between internal organs and skin
- relative contribution of primary protons and secondaries
- contribution to effective dose from gonads
• Concludes that in case of an SPE similar to the August 1972event, a 10 g/cm2 Al storm shelter should allow us to respect the30-days NCRP limit.
Courtesy of F. Balarini
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 35
Modeling Lunar & Martian Surface Radiation Environments
• We need to start with the Free Space Fluences• For the Moon, we can just calculate the albedo
produced by the impact of the primary fluencesand add one half the free space fluence to the albedo.
• For Mars, we have to propagate the free space fluence through the atmosphere to and into the surface materials. Then examine the field near and underneath the surface including all secondaries…
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 36
Free Space GCR Environments at 1 AU1977 Solar Minimum (solid)1990 Solar Maximum (dashed)
E n e r g y ( M e V / a m u )
Par
ticle
Flue
nce
(#pa
rticl
es/c
m2 -M
eV/a
mu-
year
)
1 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 61 0 - 3
1 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
Z = 1
Z = 2
3 ≤ Z ≤ 1 01 1 ≤ Z ≤ 2 0
2 1 ≤ Z ≤ 2 8
Courtesy of M. Clowdsley
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 37
Free Space Solar Particle Event Proton Spectra at 1 AU
E n e r g y ( M e V / a m u )
Par
ticle
Flue
nce
(#pa
rticl
es/c
m2 -M
eV/a
mu)
1 0 - 2 1 0 - 1 1 0 0 1 0 1 1 0 2 1 0 3 1 0 41 0 3
1 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
W o r s t C a s e S P EF e b . 1 9 5 6A u g . 1 9 7 2S e p t . 1 9 8 9
Courtesy of M. Clowdsley
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 38
Lunar Surface GCR Environments
E n e r g y ( M e V / a m u )
Par
ticle
Flue
nce
(#pa
rticl
es/c
m2 -M
eV/a
mu-
year
)
1 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 61 0 - 4
1 0 - 2
1 0 0
1 0 2
1 0 4
1 0 6
1 0 8
1 0 1 0
Z = 1
Z = 0
Z = 2
3 ≤ Z ≤ 1 01 1 ≤ Z ≤ 2 02 1 ≤ Z ≤ 2 8
1977 Solar Minimum (solid)1990 Solar Maximum (dashed)
Courtesy of M. Clowdsley
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 39
Lunar Surface “Worst Case SPE”Environment
E n e r g y ( M e V / a m u )
Par
ticle
Flue
nce
(#pa
rticl
es/c
m2 -M
eV/a
mu)
1 0 - 2 1 0 - 1 1 0 0 1 0 1 1 0 2 1 0 3 1 0 41 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
1 0 1 1
Z = 1
Z = 0
Courtesy of M. Clowdsley
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 40
Dose Equivalent on Lunar Surface Due to GCR
Courtesy of M. Clowdsley
S p h e re T h ic k n e s s ( g /c m 2 )
Ann
ualB
FOD
ose
Equ
ival
ent(
cSv)
0 2 5 5 0 7 5 1 0 00
5
1 0
1 5
2 0
2 5
3 0
3 5
4 0A L 2 2 1 9 - 1 9 7 7 m in .P o ly e th y le n e - 1 9 7 7 m in .H N a n o fib e rs - 1 9 7 7 m in .L iq u id H y d ro g e n - 1 9 7 7 m in .A L 2 2 1 9 - 1 9 9 0 m a x .P o ly e th y le n e - 1 9 9 0 m a x .H N a n o fib e rs - 1 9 9 0 m a x .L iq u id H y d ro g e n - 1 9 9 0 m a x .
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 41
Modeling the Martian Surface Radiation Environment
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 42
Planetary Surface Material and Atmosphere
(From Simonsen et al.)
Mars Induced Fields
GCR ion
Diffuseneutrons
High energyparticles
Courtesy of M. Clowdsley
~15% of the primary GCR flux reaches the Martian Surface…
Neutron albedos must be included in dose estimates…
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 43
Mars Surface Environment
Courtesy of M. Clowdsley
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 44
Mars Surface MappingCharged Ions – 1977 Solar Minimum
from Space Ionizing Radiation Environment and Shielding Tools (SIREST) web sitehttp://sirest.larc.nasa.gov
Courtesy of M. Clowdsley
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 45
Mars Surface MappingNeutrons – 1977 Solar Minimum
from Space Ionizing Radiation Environment and Shielding Tools (SIREST) web sitehttp://sirest.larc.nasa.gov
Courtesy of M. Clowdsley
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 46
Mars Surface MappingLow Energy Neutrons – 1977 Solar Minimum
from Space Ionizing Radiation Environment and Shielding Tools (SIREST) web sitehttp://sirest.larc.nasa.gov
Courtesy of M. Clowdsley
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 47
Mars Surface GCR Environments
E n e r g y ( M e V / a m u )
Par
ticle
Flue
nce
(#pa
rticl
es/c
m2 -M
eV/a
mu-
year
)
1 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 61 0 - 4
1 0 - 2
1 0 0
1 0 2
1 0 4
1 0 6
1 0 8
1 0 1 0
Z = 1
Z = 0Z = 2
3 ≤ Z ≤ 1 0
1 1 ≤ Z ≤ 2 0
2 1 ≤ Z ≤ 2 8
1977 Solar Minimum (solid)1990 Solar Maximum (dashed)
Courtesy of M. Clowdsley
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 48
Mars Surface Neutrons
Courtesy of M. Clowdsley
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 49
Mars Surface “Worst Case SPE”Environment
E n e rg y ( M e V / a m u )
Parti
c le
F lu e
nce
(#p a
rt ic l
e s/c
m2 -M
eV/a
mu )
1 0 - 2 1 0 - 1 1 0 0 1 0 1 1 0 2 1 0 3 1 0 41 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
Z = 1
Z = 0Z = 2
Courtesy of M. Clowdsley
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 50
Dose Equivalent on Mars Surface Due to GCR
S p h e re T h ic k n e s s ( g /c m 2 )
Ann
u alB
FOD
ose
Eq u
ival
ent(
cSv)
0 2 5 5 0 7 5 1 0 00
5
1 0
1 5
2 0
2 5
3 0
3 5
4 0A L 2 2 1 9 - 1 9 7 7 m in .P o ly e th y le n e - 1 9 7 7 m in .H N a n o fib e rs - 1 9 7 7 m in .L iq u id H y d ro g e n - 1 9 7 7 m in .A L 2 2 1 9 - 1 9 9 0 m a x .P o ly e th y le n e - 1 9 9 0 m a x .H N a n o fib e rs - 1 9 9 0 m a x .L iq u id H y d ro g e n - 1 9 9 0 m a x .
Courtesy of M. Clowdsley
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 51
Summary and Conclusions
• SPE’s can probably be shielded against– …But only in “Storm-Shelters” or Protected Habitats
on planetary surfaces.– Problematic during EVAs and in thinly shielded
surroundings.
• GCR is more difficult to protect against in terms of keeping the Chronic Dose acceptable during a long mission, but enough shielding or a shorter mission could work…
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CERN Course – Lecture 3October 28, 2005 – L. Pinsky
Modeling the Interaction of the Space Radiation in Spacecraft & Humans, and
Assessing the Risks on a Mission to Mars 52
AcknowledgementsN. Zapp (University of Houston) A. Ferrari (CERN & INFN-Milan)
J. Wilson (NASA -Langley) L. Townsend (Univ. of Tennessee)
M. Clowdsley (NASA-Langley) J. Barth (NASA-GSFC)
F. Cucinotta (NASA-JSC) S. Antiochos (NRL)
F. Balarini (INFN-Pavia) G.P. Zank (UC Riverside)
C. Cohen (Cal Tech) G. Reeves (LANL)
…And Many Others
European Community (EC contract # FI6R-CT-2003-508842)Italian Space Agency (ASI contract # I/R/320/02)NASA (Grants NAG8-1658 and NAG8-1901)UH Institute for Space Systems Operations