THE SYSTEM THEORY OF NETWORK CALCULUS J.-Y. Le Boudec EPFL WoNeCa, 2012 Mars 21 1.
Lecture EPFL Water on Mars
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Transcript of Lecture EPFL Water on Mars
Water on Mars. Past and presentLecture 7
Tuesday, November 12 2013 Dr Harold Clenet, EPSL, EPFL
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Outline
Tuesday, November 12 2013 Dr Harold Clenet, EPSL, EPFL
• History of Mars exploration and relationship with water• Why Mars and why water?• Insight from space probes• Water on Mars through time
• Actual water reservoirs• Today’s atmospheric conditions• Polar ice caps• Near subsurface ice• Subsurface ice
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Why Mars and why water?
Tuesday, November 12 2013 Dr Harold Clenet, EPSL, EPFL
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Why Mars and why water?
Tuesday, November 12 2013 Dr Harold Clenet, EPSL, EPFL
©NASA
What are the current outstanding questions to drive future exploration?• When and where did liquid water persist with a
sufficiently high activity to support life? Did life or pre-biotic chemistry develop?
• What drove a fundamental change, from the Noachian to Hesperian periods, in the surface environment recorded in aqueous deposits?
• How did Mars' internal evolution influence the surface environment?
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Insight from space probes
Percival Lowell(≈1900)
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Insight from space probes
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Mariner(1965-1971)
Viking(1975)
Insight from space probes
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Insight from space probes
Viking(1975)
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Insight from space probes
Mars Global Surveyor1996
Mars Express2003
Mars Reconnaissance Orbiter2005Mars Odyssey
2001
Global mapping with many observation techniques
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Insight from space probes
MGSMOC - 1996
MExHRSC - 2003
MROCTX & HiRISE - 2005
MOGRS - 2001
MOTHEMIS - 2001
MGSTES - 1996
MExOMEGA - 2003
MROCRISM - 2005
MROSHARAD - 2005
MExMARSIS - 2003
Radar
Thermal infrared
Visible – Near Infrared spectroscopyVisible optical imagery
Gamma spectroscopy
11Tuesday, November 12 2013 Dr Harold Clenet, EPSL, EPFL
Insight from space probes
Radar
Thermal infrared
Visible – Near Infrared spectroscopyVisible optical imagery
Gamma spectroscopy
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Insight from space probes
MGSMOLA - 1996
MGSMOC - 1996
MExHRSC - 2003
MROCTX & HiRISE - 2005
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Water on Mars through time
Evidence of water from:• Morphology• Mineralogy
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Water on Mars through time
Evidence of water from:• Morphology• Mineralogy
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Water on Mars through time
Valley networks
THEMIS IR Mosaic in the Warrego Valles area
HIRISE image Small Valley Networks in the AncientSouthern Highlands (ESP_012519_1320)
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Water on Mars through time
High rate of erosion for the craters in the southern
hemisphere
Lake deltas and fans
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Water on Mars through time
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Water on Mars through time
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Water on Mars through time
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Water on Mars through time
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Water on Mars through time
Large scale detections: Clays in Mawrth Vallis
Local detections: Clays in Nili Fossae region
Minerals that need water to be produced
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Water on Mars through time
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Water on Mars through time
•
•
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Water on Mars through time
Outflow channels
MOLA in the Kasei Valles area
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Water on Mars through time
Resurfacing of North planes and rampart craters
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Water on Mars through time
Terra Meridiani (Opportunity)Interior Layered Deposits (ILD) in Valles Marineris (HRSC)
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Water on Mars through time
Sulfates in ILD Sulfate over clays in Colombus crater
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Water on Mars through time
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•
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Water on Mars through time
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Water on Mars through time
Layered deposits on the North polar cap
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Water on Mars through time
Gullies
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Water on Mars through time
gullies
viscous flow
Low-latitude gullies
Brine with ferric sulfate
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Outline
Tuesday, November 12 2013
• History of Mars exploration and relationship with water• Why Mars and why water?• Insight from space probes• Water on Mars through time
• Actual water reservoirs• Today’s atmospheric conditions• Polar ice caps• Near subsurface ice• Subsurface ice
Dr Harold Clenet, EPSL, EPFL
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Today’s atmospheric conditions
Atmospheric pressure560 Pa
Temperatures-133°C / 27°C
Atmosphere95.3% CO2
No liquid water at surface conditions
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Polar ice caps
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Polar ice caps
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Polar ice caps
South Polar Ice Cap: 1.6 x 106 km3, which is equivalent to a global water layer of approximately 11 meters thick
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Near subsurface ice
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Near subsurface ice
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Near subsurface ice
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Subsurface ice
Found in few place under the surface (depths 1 to 3 km)Represent 1% of the total water volume contained in the polar
caps, equivalent to a global water layer 20 cm thick.
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Summary
Tuesday, November 12 2013
• Evidence for liquid water during Mars history• Noachian warm and wet
• Valley networks• Craters erosion• Deltas and fans• Hydrated minerals
• Hesperian colder and dryer but water still present• Outflow channels• Rampart craters• Sulfates and layered deposits
• Amazonian to present• Almost no water activity except at high latitudes and in polar caps
• Actual water reservoirs• Polar ice caps• Near subsurface ice• Subsurface ice
Dr Harold Clenet, EPSL, EPFL