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Exploration of Martian Lava Tubes
Christoph Brendel and Janko Trisic
1
Introduction
Study about the Lava Tubes on Mars
Can they provide shelter for humans in the future?
Source: Wikipedia2
Objectives
Define the main criteria for the lava tubes:
● Over 100 m wide
● Close to ancient ocean
● Possibility to contain water: find out if they contain H2
O ice, separate those who have it
from the rest
Find the tubes that meet the requirements
Find out if they can provide shelter for humans
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The Lava Tubes
Skylights and rilles
Way bigger than the ones on Earth Source: Wikipedia
Source: http://blogs.esa.int/caves/2015/05/06/caves-the-hidden-side-of-planets/ Red line represents 50mSource: Google Images.
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Ancient ocean
“Oceanus Borealis”
Still a hypothesis, but with many features that
back it up:
● Shorelines
● Flow lines
● Clay sediments
● Cross bedding
4.1-3.8 Billion years ago
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Location
Many volcanoes on Mars
Areas with the highest rates of lava tubes: Tharsis and Elysium
Tharsis has plenty volcanoes but is far away from theoretical shore
Elysium is in the middle of hypothetical ocean
Source: Google Earth 6
Elysium Mons
Good location
Rootless cones
Lava tubes
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Lava tubes locations
Elysium Mons
Olympus Mons
Arsia Mons
Pavonis Mons
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Rootless cones
http://www.dronestagr.am/pseudocraters-in-myvatn-lake-iceland/9
B. C. Bruno / Spatial Analysis of Rootless Cone Groups on Iceland and Mars 10
Criteria
Skylights:
Optical imaging
● Diameter of 80-200 m● Hole in the surface● Shadows within the circle
Lava tubes:
GPR
● Hyperbolas in cross section and continuous lines on longitudinal section
Gravimetry
● Gravimetric anomalies
Rootless cones:
Optical imaging
● Diameter between 0.5 km and 1.5 km
● No central mountain in the crater
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Optical imaging
Minimum resolution Available resolution
Skylights 30 m/pixel 0.3 m/pixel
Collapsed Tubes
30 m/pixel 0.3 m/pixel
Rootless Cones 15 m/pixel 0.3 m/pixel
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Optical imaging
Lava tube southeast of Elysium Mons, approx 130m in diameter
150 m
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Nasa/JPL/University of Arizona / https://www.uahirise.org/ESP_035098_2065
Elysium Mons
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500 m
d = 1 km
d = 0.7 km
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If we analyzed a scan that was cutting
the tube, we would see the hyperbola
from figure A.
If we were to scan along the tube, we
would see a constant, horizontal line
A: hyperbola marking a cavity
B: Ice layer C: water layer
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Gravity anomaly
C. Rowell / Geophysical analysis of structures and flow geometry of the Blue Dragon lava flow
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MethodsFrom Earth:
● Analysis of previous imaging and GPR data
From orbiter:
- SHARAD - 20 MHz
- MARSIS - between 1,8 and 5 MHz
- HiRISE images - resolution of 0.3 m/pixel
- Spectrometer (CRISM)
From Orbit:
● Radar sounding (GPR)
● Gravity anomaly
On site:
● Lander: GPR and gravimetric tools
● Helicopter 3D modeling 18
Methods
Currently available methodsMethods that could be provided
in the next few yearsMethods that need more
research and better technology
High resolution imaging from Mars orbit 3D modeling with a helicopter Robotic exploration the cavesShallow and ground penetrating radar on orbiter Human exploration of caves
Spectrometer on orbiter
Tracing of gases
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25 MHz 5 MHz 0.5 MHz
Material v in m/ns λ depending on frequencyvacuum 0.3 12 60 600fresh water 0.034 1.36 6.8 68basalt 0.11 4.4 22 220clay 0.15 6 30 300granite 0.13 5.2 26 260ice 0.16 6.4 32 320limestone 0.13 5.2 26 260permafrost 0.15 6 30 300sand 0.15 6 30 300volcanic ash 0.09 3.6 18 180
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3D modeling of lava tubes
● JPL Mars Helicopter Scout will be on board of the Mars 2020 mission
● If the helicopter is a success, 3D modeling of the entrances will be available
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Exploration with robots
● Getting the robot into the cave is very challenging
● Data transfer from within the cave is limited
○ Ceiling very thick
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Exploration with robots
R. Whittaker / Technologies for Exploring Skylights, Lava Tubes and Caves - NASA 23
Conclusion
Detection of lava tubes is already possible
Modeling of the entrances is possible in the near future
Entering the caves is still a huge obstacle
High importance for humanity if we intend to colonize Mars
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