SITE SELECTION for the FIRST SUSTAINABLE MARS BASE Workshop Abstract #2001
SITE SELECTION FOR THE FIRST SUSTAINABLE MARS BASE Workshop Abstract #2001
D. C. Barker, MAXD, Inc. G. James, NASA JSC G. Chamitoff, Texas A&M University S. Clifford, LPI Explora on Zone Map #1002
1st EZ Workshop for Human Missions to Mars 150 E 180 E 210 E 40 N
Utopia Plane a
V2 Dorsa Arcadia Plane a
Phlegra EZ 39N, 172E 30 N
Elysium Mons 1
39N, 172E 2 Explora on Zone Map #1002 All RROIs are SROIs but all SROIs are not necessarily RROIs ! 1st EZ Workshop for Human Missions to Mars Dome Structures Landing Zone SROI 1 & Base (25km x 20km) Tyndall S1 Alt -3960 m Crater S3 SROI 4 S4 S1 Fluidized 2 Craters Plains S1 S3 SROI 3 Units S3 RROI 3 S1 2 EZ S2 2 S1 100 km rad Hydrated Minerals S3 SROI 2 Sheet S1 Silicates Near 1 RROI 2 Surface Ice THEMIS Image RROI 1 EZ wide 39N, 172E 3 Explora on Zone Map #1002
1st EZ Workshop for Human Missions to Mars TES Dust Cover Index (DCI)
TES over THEMIS
1
39N, 172E 4 Explora on Zone Map #1002
1st EZ Workshop for Human Missions to Mars TES Rock Abundance
TES over THEMIS
1
39N, 172E 5 Landing Zone
1st EZ Workshop for Human Missions to Mars 172 E Eleva on Thermal Iner a Slope Albedo Dust Index 25km x 20km (larger than Avg: -3966 Avg: 240.2 Avg: 0.33 Avg: 0.156 Avg: 0.968 expected for precision Max: -3953 Max: 253 Max: 0.99 Max: 0.996 Max: 0.983 human landing) Min: -3985 Min: 233 Min: 0.03 Min: 0.025 Min: 0.949
average annual temperature ~(-73.15 C) 39 N Final Landing Sites and Base infrastructure could be moved widely in this region without altering access to
primary resources (i.e., H2O) or areas of scien fic interest.
39N, 172E CTX Image 6 Landing Zone
1st EZ Workshop for Human Missions to Mars 172 E • Low Al tude and Denser Atmosphere supports EDL design and opera ons, reduced radia on budgets, increases
mining abili es (H2O & CO2) • Moderate thermal iner a and albedo 39 N
CTX Image 39N, 172E 7 Science ROI(s) Rubric
1st EZ Workshop for Human Missions to Mars
Site Factors SROI1 SROI1 SROI2 SROI3 SROI4 RROI1 RROI2 RROI3 EZ SUM EZ
Potential for past habitability ? ? ? ? ● ? ? Threshold
AND/OR Potential for present habitability/refugia ? ? ? ? ○ ? ? Astrobio Qualifying Potential for organic matter, w/ surface exposure ? ? ? ? ? ? ? Threshold Noachian/Hesperian rocks w/ trapped atmospheric gases ● ? ○ ○ ? ○ 1,3 Meteorological diversity in space and time ● ● ● ● ● ● 6,0 High likelihood of surface-atmosphere exchange ● ● ● ○ ● 4,2 Qualifying Key Amazonian subsurface or high-latitude ice or sediment ● ● ● ● ● ● ● 6,0 ● Yes
Atmospheric Science Science Atmospheric High likelihood of active trace gas sources ? ? ? ? ○ ? ? 0,1 Partial Support ○ or Debated Range of martian geologic time; datable surfaces ● ○ ● ○ ○ ○ ● 3,4 No Threshold Evidence of aqueous processes ● ● ● ● ● ○ ● 6,1 ? Indeterminate Potential for interpreting relative ages ● ● ● ● ○ ○ ○ 4,3
Igneous Rocks tied to 1+ provinces or different times ● 1,0 Science Criteria Site Near-surface ice, glacial or permafrost ● ● ● ● ● ○ ● 5,1 Noachian or pre-Noachian bedrock units ● ? ○ 0,1 Geoscience Geoscience Qualifying Outcrops with remnant magnetization ● ? 1,2 Primary, secondary, and basin-forming impact deposits ? ? ● ● 2,0 Structural features with regional or global context ● ○ ● ○ ● ● 4,2 Diversity of aeolian sediments and/or landforms ● ● ● ● ● ● ● 6,0 8 Resource ROI(s) Rubric
1st EZ Workshop for Human Missions to Mars
Site Factors SROI1 SROI1 SROI2 SROI3 SROI4 RROI1 RROI2 RROI3 EZ SUM EZ
Engineering Meets First Order Criteria (Latitude, Elevation, Thermal Inertia) ● ● ● ● ● ● ● 6,0 Potential for ice or ice/regolith mix ● ● ● ● ● ● ● 6,0
OR 6,0
AND/ Potential for hydrated minerals ● ● ● ● ● ● ● Quantity for substantial production ● ● ○ ○ ● ● ● 2
Threshold Potential to be minable by highly automated systems ● ● ● ● ● 5,0
Located less than 3 km from processing equipment site ● ● ● ● ● 5,0 Located no more than 3 meters below the surface ● ● ● ● ● ● ● 7,0 Accessible by automated systems ● ● ● ● ● ● ● 7,0 5,0
Water Resource Resource Water Potential for multiple sources of ice, ice/regolith mix and hydrated minerals ● ● ● ● ● ● Key Qualifying Distance to resource location can be >5 km ● ● ● ● ● ● ● 7,0 Route to resource location must be (plausibly) traversable ● ● ● ● ● ● ● 7,0 ● Yes ~50 sq km region of flat and stable terrain with sparse rock distribution ● ● ● ● ● 5,0 Partial Support Threshold 1–10 km length scale: <10° ● ● ● ● ● ● 6,0 ○ or Debated Located within 5 km of landing site location ● ● ● ● 4,0 No Located in the northern hemisphere ● ● ● ● ● ● ● 7,0 Qualifying Evidence of abundant cobble sized or smaller rocks and bulk, loose regolith ● ● ● ● ● ● ● 7,0 ? Indeterminate Utilitarian terrain features ● ● ● ● ● ● ● 7,0 Civil Engineering Low latitude ● ● ● ● ● ● ● 7,0 No local terrain feature(s) that could shadow light collection facilities ● ● ● ● ● ● ● 7,0 Qualifying 7,0 Food Food Access to water ● ● ● ● ● ● ● 7,0 Production Production Access to dark, minimally altered basaltic sands ● ● ● ● ● ● ●
Potential for metal/silicon ● ● ● ● ● ● ● 7,0
Potential to be minable by highly automated systems ● ● ● ● ● ● ● 7,0 5,0 ISRU and Civil Engineering ISRUand Civil Criteria Threshold Located less than 3 km from processing equipment site ● ● ● ● ●
Located no more than 3 meters below the surface ● ● ● ● ● ● ● 6,0
Accessible by automated systems ● ● ● ● ● ● ● 7,0
Resource Resource Potential for multiple sources of metals/silicon ● ● ● ● ● 5,0 Metal/Silicon Qualifying Distance to resource location can be >5 km ● ● 2,0 9 Route to resource location must be (plausibly) traversable ● ● ● ● ● ● ● 5,0 EZ Geological Context
1st EZ Workshop for Human Missions to Mars
Tyndall
EZ
39N, 172E 10 Science ROI 1 The more you look, the more you ques on, the less you know! 1st EZ Workshop for Human Missions to Mars Tyndall • En re EZ region (39E, 172N) Dome • Geoscience (mineralogy, geochemistry, Field petrology, weathering, atmospheric (TDF) interac ons, age associa ons) – Subaerially extruded domes, cryptodomes, intrusive ice/magma interac ons, mud volcanoes, ice rich regolith, obliquity varia ons, silica-rich volcanic rock. • Cross-cu ng (poten al ice rich CTX over deposits & construc on materials) THEMIS
(Rampey et al., 2007; Farrand et al., 2011; Michaut et al., 2013) 11 Science ROI 1
1st EZ Workshop for Human Missions to Mars
Tyndall Dome Field CRISM Example (TDF)
East fo EZ HiRISE Note: polygonal and “brain terrain” West of EZ 39N, 172E 12 Science ROI 2
1st EZ Workshop for Human Missions to Mars Hydrated Mineralogy • SE Quadrant of EZ • Geosciences (mineralogy,
sedimentology, geochemistry, weathering, water/ice processes & history • Cross-cu ng (poten al water & construc on materials)
OMEGA over THEMIS
39N, 172Ec 13 Science ROI 3
1st EZ Workshop for Human Missions to Mars Fluidized • SW and NW Quadrants of EZ Impact Structures • Geosciences (impact processes, water/ice processes, weathering, age da ng • Cross-cu ng (poten al construc on MOC over THEMIS material, ice rich deposits)
39N, 172Ec 14 Science ROI 3
1st EZ Workshop for Human Missions to Mars
S HiRISE
39N, 172Ec 15 Science ROI 4
1st EZ Workshop for Human Missions to Mars Tyndal 170 E 171 E l ~75 km dia • NW Quadrant of EZ Crater • Geosciences (mineralogy,
sedimentology,
geochemistry, weathering,
water/ice processes &
history, impact processes
CTX & HiRISE 39 N 39N, 172Ec 16 Science ROI 4
1st EZ Workshop for Human Missions to Mars Tyndall 170 E 171 E N Crater
crater rim
crater floor HiRISE 39 N 39N, 172Ec 17 Resource ROI 1
1st EZ Workshop for Human Missions to Mars Near Ice Mining • Surface GRS indicates regional water signature at a > 4 wt% level Ice • MARSIS-derived porosity of GRS over ~35% & volumetric ice content THEMIS of ~60% for the top ~60-80 m • Global Climate Models predicts regional ice accumula on during high obliquity
39N, 172Ec 18 Resource ROI 1
1st EZ Workshop for Human Missions to Mars Near Surface Ice Observa ons SE of EZ
Site 2: HiRISE PSP_010440_2235
6-meter-wide, ~1.33 meter- deep crater Oct. 18, 2008, (le ) and on Jan. 14, 2009. Each 43.2°N 164.2°E image is 35 meters across. 39N, 172Ec 19 A li le on Mining/Extrac on Where’s the Energy? 1st EZ Workshop for Human Missions to Mars On Earth, Aluminum is obtained from the mineral bauxite (an aluminum oxide (Al2O3)) through the process of electrolysis. On Mars we have minerals and non-ore rocks. *We have yet to find an tradi onal “ore” deposit on Mars. • The mel ng point of aluminum oxide, over 2000oC requires lots of energy to melt the source material so that ions (Al3+ and O2–) are free to move to the electrodes for the electrolysis to work. On Earth, this process is ~6x more costly than the produc on Fe (reducing method: ore, coke and limestone). • Other mel ng points: • Iron (sulfide or oxide) ore: 1800 °C • Glass: 1400 °C to 1600 °C • Mafic minerals (e.g., pyroxene) 1000 to 1200 °C 43.2°N 164.2°E • Phyllosilicates: > 1000 °C 39N, 172Ec 20 Resource ROI 2
1st EZ Workshop for Human Missions to Mars Sheet Silicate / • Elevated levels through center of EZ High-Si Glass • Evidence of mineral altera on and precipita on
hydrated silicates TES over THEMIS
39N, 172Ec 21 Resource ROI 3
1st EZ Workshop for Human Missions to Mars Arcadia ferric oxide nanopar cles/dust abundance (blue low, red high) Planta • Elevated levels through center of EZ Planes Materials • TES abundances as high as 0.2 (red) or ~10x low abundance areas (blue)
• Evidence of mineral altera on and precipita on
• Ubiquitous, low slope, medium and fine grained surface deposits –> enhancing mining, manufacturing, OMEGA 3D construc on and traverse opera ons over MOLA Shaded • Poten al for lave tube and tunnels Relief • Mul ple elevated mineral assemblages across region
39N, 172Ec 22 RROI3 Poten al Resource ROIs
TES Abundances 1st EZ Workshop for Human Missions to Mars
2− This EZ contains moderately low to elevated Sulfate SO₄ abundances for a variety of minerals and rock types (detec on limits need to be enhanced). These provide for a wide range of poten al resources as well as scien fic points of interest.
CO 2− Carbonate 3 Hema te Fe2O3
39N, 172Ec 23 RROI3 Poten al Resource ROIs
TES Abundances 1st EZ Workshop for Human Missions to Mars
Orthopyroxene Plagioclase (Na,Ca)Al1-2Si3-2O8
(Mg,Fe)SiO3 Clinopyroxene Andesite
(Ca,Mg,Fe,Al)2(Si,Al)206 39N, 172Ec 24 Highest Priority EZ Data Needs
1st EZ Workshop for Human Missions to Mars • Loca ng easily extracted, near surface ice/water deposits is the single most important ongoing data set needed to select a permanent, growing and sustainable se lement. This should include enhanced/high resolu on neutron spectrometer (e.g., GRS) and subsurface radar (e.g., SAR, sounding) at a minimum. • CRISM and HiRISE imaging should be enhanced throughout the region. • Environmental health measures from MARIE or similar instrument should be con nued and enhanced. 39N, 172Ec 25 Conclusions
1st EZ Workshop for Human Missions to Mars • Our primary driver for landing site selec on was driven by the acquisi on of water. • Our assump on being that the primary focus of where we land and what we do there ini ally is to mine water, and as such, no tradi onal science objec ves should be delineated in advance of that goal. • Once suitable sites are found fulfilling proven and producible water needs, than a combined regional assessment of addi onal resources and science poten als within the EZ can be made as a final form of loca on op miza on. 39N, 172Ec 26 EZ Concept Corrobera on and Possible Evolu on 1st EZ Workshop for Human Missions to Mars 160 E 170 E Main Se lement and staged Field Sta ons 40N (FS), including deployable habitats and supply cashes (camping- excursions) and Robo c Recognizance could be used to vastly expand explora on Robo c Recon 30N and safety (network- redundancy)
27 Back Up Slides
1st EZ Workshop for Human Missions to Mars A philosophical cri que/observa on regarding our current path forward, answers to “why” Mars and the reasons why Mars may con nue to remain “20 years from now.”
Read at your leisure!
Barker, D. C., 2015, The Mars impera ve: Species survival and inspiring a globalized culture. Acta Astronau ca, 107, 50-69, doi.10.1016/j.actaastro.2014.11.006.
39N, 172Ec 28 A window of opportunity drawing to a close?
Backup A needed paradigm shi
1st EZ Workshop for Human Missions to Mars The “why” and “when” of sending humans to Mars should be addressed from the beginning.
A full discussion should include constraints and compe on to future funding and programs as a result of projected popula on and social trends, pollu on, climate change, human conflict, governmental par sanship/waste, reduced public a en on span/support, military and social expenditures, ect. A crucial implica on being that our focus should be directed towards permanent and sustainable human se lement of Mars through the iden fica on and acquisi on of water reserves, as this endeavor will likely not happen by scien fic objec ves alone. For example, the direc ons given in this workshop and NASAs historical “modus operandi” con nue to highlight the priori es and goals of a fixated science, engineering and bureaucra cally burdened community without regard to a permanent and sustainable context by addressing “Why” we should go to Mars.
Vocabulary places science over resources: “ROIs are areas that are relevant for scien fic inves ga on and/or development/matura on of capabili es and resources necessary for a sustainable presence.” 29 A window of opportunity drawing to a close?
Backup A needed paradigm shi
1st EZ Workshop for Human Missions to Mars
100 Years of Popula on Given present popula on 9.55 trends and the associated 10 9 trends in resource deple on, Billions 8 7.32 environmental degrada on, 7 human conflict, migra on 6 and economic impacts, the 5 Launch likelihood of future budgets 4 Date ? devia ng from the trends or 3 levels of the past 50 years is 2 0.321 0.398 increasingly difficult if not 1 improbable. 0 • No one should assume things
will change in favor of World Popula on US Popula on Humans to Mars.
39N, 172Ec 30 A window of opportunity drawing to a close?
Backup What If $$$$
1st EZ Workshop for Human Missions to Mars
39N, 172Ec 31