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Human Landing Site HangoutPaving the Road to Mars: Civil Engineering at the Human Landing Site
Michelle M. Munk
Entry, Descent and Landing Systems Capability Lead
27 February 2020
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Process of delivering a vehicle from the
top of the atmosphere to the surface and
landing safely
Three phases of flight
Entry – Hypersonic flight: Guide to the target
Descent – Supersonic flight: Turn on engines
Landing – Subsonic flight: Extend landing
gear and throttle engines for touchdown
EDL is riskiest part and largest unknown
of Human Exploration of Mars
Entry, Descent and Landing (EDL)
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Human Landers: A Leap in Scale3
Steady progression of “in family” EDLNew Approach
Needed for Human Class Landers
Viking 1/2 Pathfinder MER A/B Phoenix MSL Human
Scale
Lander
(Projected)
Diameter, m 3.505 2.65 2.65 2.65 4.5 16-19Entry Mass, kg 930 585 840 602 3151 47-62 tLanded Mass (kg) 603 360 539 364 1541 36-47 tLanding Altitude (km)
-3.5 -1.5 -1.3 -3.5 -4.4 + 2
Peak Heat Rate (W/cm2)
24 106 48 56 ~120 ~120-350
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To establish a sustained Human mission will require multiple landers
NASA’s Evolvable Mars Campaign has identified a 4-lander manifest
Must land within 50 m of a target
Must remain 1 km from other landed assets to prevent sand blasting
Landing Four 2-Story Houses
Lander 2 Lander 3 Lander 4Lander 1
Requires orders of magnitude improvement on pinpoint landing capability
MAV-1
CL-1
2
3CL-3
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6
4
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TD-1
1
1 km
CL-2
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Mission Sequence: 4-8 landers to the same site
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Mars Landing Footprint Improvement
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1997 Pathfinder:200km x 70km 2012 MSL:
20km x 6.5km Needed for Humans:.05km x .05km
Gale Crater
Site A
Landing Site Within Jezero Crater
Jezero contains Fe-Mg smectite clay indicative of multiple episodes of fluvial/aqueous activity on ancient Mars, elevating the potential for preservation of organic material.(Green = phyllosilicates, orange = olivine, purple = neutral/weak bands.) 7
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Mars 2020 Range Trigger
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Future Safe, Precise Landings
Divert
Approach
Star
Tracker
Pitch Up
Maneuver
Powered Descent
Final
Targeting
Burn
Acti
ve
Sen
sors
Desc
ent
Ph
ase
s
TDsafe site
identification
HD
Velocimetry
TRN
Precise
Ellipse
Entry
Ellipse
Inertial Measurement Unit touchdown
Initial Entrymission-dependent
deceleration method
Altimetry
HRNSafe
Site
AcronymsTRN Terrain Relative NavigationHD Hazard DetectionHRN Hazard Relative NavigationTD Terminal DescentConOps Concept of Operations
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Plume Impingement – Temperature
Supersonic fountain flow develops below 18 m elevation
Hot plume gases impinge on heatshield below 20 m elevation
Unsteady plume motion below 15 m elevation
Credit: Peter Liever et al, CFDRC/NASA MSFC
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Plume Impingement – Pressure
Plume envelope depicted by M=1 iso-surfaces
Ground surface impingement pressures shown
Near-surface outward supersonic flow pockets below 18 m elevation
Credit: Peter Liever et al, CFDRC/NASA MSFC
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Plume Impingement – Cratering
Credit: Peter Liever et al, CFDRC/NASA MSFC
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What is Next?
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Representative Site
1 km
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Human Landing Site HangoutPaving the Road to Mars: Civil Engineering at the Human Landing Site
Mars In-Situ Construction
February 26, 2020
Robert P. Mueller
Senior Technologist
Swamp Works
NASA Kennedy Space Center (KSC)
Environmental Considerations
Gravity
Atmosphere or Vacuum
Dust
Rotation Period (day/night cycles)
Seasons
Temperature Extremes
Particle Radiation
Electrostatics and charging
Solar Flux
Magnetic Field
Soil Characteristics
Ice Characteristics
Subsurface Geology
Planetary Protection
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Mars Resources
Atm. CO2
Water
Soil
Mars ResourcesRegolith*
Silicon Dioxide (43.5%)
Iron Oxide (18.2%)
Sulfur Trioxide (7.3%)
Aluminum Oxide (7.3%)
Magnesium Oxide (6.0%)
Calcium Oxide (5.8%)
Other (11.9%)
Water (2 to >50%)XX
*Based on Viking DataXXMars Odyssey Data
Atmosphere
Carbon Dioxide (95..5%)
Nitrogen (2.7%)
Argon (1.6%)
Oxygen (0.1%)
Water (210 ppm)
Mars Resources Atmospheric gases, and in particular carbon dioxide, are available everywhere at 6 to 10 torr
(0.1 psi)
Viking and Mars Odyssey data shows that water is wide spread but spatial distribution and form of water/ice is not well understood (hydrated clays and salts, permafrost, liquid aquifers, and/or dirty ice)
Regolith is plentiful and dust fines have been blown around the planet by the winds
Basaltic rock mineral regolith is common
Gypsum sand dunes 18
Resources ofInterest:
• Oxygen• Water• Hydrogen• Metals• Silicon• Gases• Aggregates• Binders• Energy
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Regolith is an Abundant Resource on Mars
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Surface Construction
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Planetary Surface Construction Tasks
Launch/Landing Pads
Beacon/Navigation Aids
Lighting Systems
Communications Antenna Towers
Blast Protection Berms
Perimeter Pad Access & Utility Roads
Spacecraft Refueling Infrastructure
Power Systems
Radiation, Thermal & Micro Meteorite Shielding
Electrical Cable/ Utilities Trenches
Foundations / Leveling
Trenches for Habitat & Element Burial
Regolith Shielding on Roof over Trenches
Equipment Shelters
Maintenance Hangars
Dust free zones
Thermal Wadi’s for night time
Regolith Mining for O2 Production
H2O Ice/Regolith Mining from Shadowed Craters
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Construct a Launch/Landing Pad using In Situ Regolith for rocket plume impingement mitigation
Hawaii PISCES Rover on Mauna Kea with PayloadsNASA Chariot Bull Dozer
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Launch / Landing Pad Construction
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Mars Space Civil Engineering Capability Concepts
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What is Next?
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Mars Gravity ~3/8 of Earth (0.376 G) Atmospheric pressure ~1% of Earth’s, but varies seasonally by 30% as it
freezes and unfreezes from the polar caps Wind only has ~10 % dynamic force of equivalent Earth’s wind Mars has CO2 frost & snow Sand carried by the wind still abrades like on Earth Atmosphere mostly carbon dioxide (95.5 %) Very dusty atmosphere; dust storms, dust devils Four seasons – seasons are twice as long as on Earth Mars gets about 40 percent more energy from the sun during perihelion —
when the planet is closest to the sun — than during aphelion In the winter, much like on Earth, heavy storms of thick cloud cover and dust
move over Mars’ continents toward the equator. When Mars sweeps closest to the sun during its southern hemisphere
summer, temperatures increase greatly; the extra energy is enough to launch dust storms that envelop large regions of Mars — sometimes the entire planet — for weeks or months.
Global dust storms tend to occur only during perihelion season and once every three or so Martian years
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Mars, continued
Radiation environment on the surface is bad Soil is weathered, behaves like terrestrial soil Soil is diverse Geology is complex & diverse Little is known about subsurface geology Mars is in glacial retreat – radar observations The glaciers are located in belts around Mars between the latitudes 30.0-
50.0, equivalent to just south of Denmark's location on Earth. The glaciers are found on both the northern and southern hemispheres.
• Mixture of CO2 and water ice and clathrates(A clathrate is a snow like substance that can exist below 283K (10°C) at a range of pressures of carbon dioxide)
Varying mechanical strength Ice is on the surface at high latitudes Ice is near the surface at moderate latitudes Ice is deep beneath the surface at low latitudes
Credit: Mars Digital Image Model, NASA/Nanna Karlsson
CONSTRUCTION AXIOMS
WHEN ALL YOU HAVEIS A HAMMER, EVERYPROBLEM LOOKS LIKEA NAIL!
3D CONCRETE PRINTING
PENN STATE, MARS HABITAT CHALLENGE
BRICK LAYING ROBOT
GILBRETH 1911
USE OF LANDER AS PART OF STUCTUREKHAN-YATES
USE OF LANDER AS CONSTRUCTION EQUIPMENTTEAM ZOPHERUS
NO STRUCTURE HAS BEEN BUILT ON THE SURFACE OF ANOTHER HEAVENLY BODY?
ISS CONSTRUCTION
IN SPACE
1804.3.1 Increases in allowable lateral sliding resistance.
The resistance values derived from the table are permitted to
be increased by the tabular value for each additional foot
(305 mm) of depth to a maximum of 15 times the tabular
value.
Isolated poles for uses such as flagpoles or signsand
poles used to support buildings that are not adversely
affected by a 0.5 inch (12.7 mm) motion at the ground surface
due to short-term lateral loads are permitted to be
designed using lateral-bearing values equal to two times the
tabular values.
OFF-WORLD SURFACE STRUCTURE COVERED BY EARTHLY BUILDING CODE
Surface penetrability decreases quickly withinthe first few inches of the surface. … Whenspecifically probed more than 4 or 5 in., thesurface was found to be quite firm. This firmnesswas clearly evident during deployment of thestaffs of the U.S. flag and the Solar WindComposition Experiment. Probing of the initial 4or 5 in. of the surface was relatively easy;however, 6 to 8 in. was as far as the flagstaffwould penetrate the surface. The surfacepenetration by the core tubes was no greaterthan 8 or 9 in., even when the sampler extensionwas hammered hard enough to be significantlydented. In contrast, the soil offered very littlelateral support to the staffs and core tubes whenthey were left to stand by themselves.
CURIOSITY CROSSING DINGO GAP – FEB 9, 2014
DIFFERENTIAL SETTLEMENT ISSUE, TOWER OF PISA
FLAT ROCKS TO STACK – CURIOSITY ROVER AT GALE CRATER
The scene combines multiple frames taken with Mastcam's right-eye camera on Aug. 7, 2014, during the 712th Martian day, or sol, of Curiosity's work on Mars. It shows an outcrop at the edge of "Hidden Valley," seen from the valley floor. This view spans about 5 feet (1.5 meters) across in the foreground.
DRY STACKED STONE WALL ARAN ISLAND IRELANDDun Aonghasa 1000 BC
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THANK YOU!
REACH OUT:
FIND MORE INFORMATION AT:
http://www.nasa.gov/journeytomars/mars-exploration-zones