uee12 habiter mars epfl

PLANET MARS

Environmental conditions and human exploration

Wednesday, February 19, 2014 Dr Harold Clenet, EPSL, EPFL

DR. HAROLD CLENETEarth and Planetary Science Laboratory

[email protected]

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OUTLINE

Dr Harold Clenet, EPSL, EPFLWednesday, February 19, 2014

• Mars exploration• Why Mars?• History of exploration• Few geophysical parameters

• Resources and constraints for human exploration• Water• Climate / radiation• Building blocks• Constraints for the base site

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WHY MARS?


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MARS EXPLORATION


Giovanni Domenico Cassini

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MARS EXPLORATION


Percival Lowell(≈1900)

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MARS EXPLORATION


France Soir, 8/7/1947

H.G. Wells, 1898

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MARS EXPLORATION


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MARS EXPLORATION


Mariner(1965-1971)

Viking(1975)

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MARS EXPLORATION


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MARS EXPLORATION


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MARS EXPLORATION


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FEW GEOPHYSICAL PARAMETERS


Propriété Valeur martienne Valeur terrestre (Mars % Terre)

Distance au soleil AU 1.524 1

Rayon moyen 3 389,5 km 6 371,0 km (53,2 %)

Masse 6,4185×1023 kg 5,9736×1024 kg (10,7 %)

Gravité de surface à l'équateur 3,711 m/s2 9,780327 m/s2 (37,9 %)

Vitesse de libération 5 027 m/s 11 186 m/s (44,9 %)

Durée du jour solaire 1 sol ≈ 1,027 day ≈ 24.6 h 1 d = 24 h (102,75 %)

Inclinaison de l'axe 25,19° 23,439281°

Période orbitale 6681 sols ≈ 686,971 d 365d 6h 14m (188,1 %)

Rayonnement solaire 492 à 715 W/m2 1 321 à 1 413 W/m2

Température moyenne au sol -63 °C ≈ 210 K 14 °C ≈ 287 K

Température la plus élevée -3 °C ≈ 270 K 58 °C ≈ 331 K

Température la plus basse -133 °C ≈ 140 K -89 °C ≈ 184 K

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FEW GEOPHYSICAL PARAMETERS


Atmospheric pressure560 Pa (T=105 Pa)

Temperatures-133°C / 27°C

No liquid water at surface conditions

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OUTLINE


• Mars exploration• Why Mars?• History of exploration• Few geophysical parameters

• Resources and constraints for human exploration• Water• Climate / radiation• Building blocks• Constraints for the base site

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RESOURCES AND CONSTRAINTS FOR HUMAN EXPLORATION


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EVIDENCE FOR PAST WATER


Valley networks

THEMIS IR Mosaic in the Warrego Valles area

HIRISE image Small Valley Networks in the AncientSouthern Highlands (ESP_012519_1320)

17 Dr Harold Clenet, EPSL, EPFLWednesday, February 19, 2014

High rate of erosion for the craters in the southern

hemisphere

Lake deltas and fans



Outflow channels

MOLA in the Kasei Valles area



Resurfacing of North planes and rampart craters



ACTUAL WATER RESERVOIRS



Layered deposits on the North polar cap



South Polar Ice Cap: 1.6 x 106 km3, which is equivalent to a global water layer of approximately 11 meters thick



Large scale detections: Clays in Mawrth Vallis

Local detections: Clays in Nili Fossae region

Minerals that need water to be produced



Terra Meridiani (Opportunity)Interior Layered Deposits (ILD) in Valles Marineris (HRSC)



Sulfates in ILD Sulfate over clays in Colombus crater



COMMON HYDRATED MG-SULPHATE MINERALS

• Epsomite (MgSO4.7H2O) = 51% H2O

• Kieserite (MgSO4.H2O) = 14% H2O

• Hexahydrite (Mg(SO4) · 6H2O) = 47% H2O

• Bloedite (Na2Mg(SO4)2 · 4H2O) = 37% H2O

OTHER COMMON HYDRATED MINERALS

• Gypsum (CaSO4.2H2O) = 14% H2O

• Montmorillonite clay(Al,Mg,Fe)8(Si4O10)3(OH)10.12H2O) = 26% H2O

Sulfates in ILD


CLIMATE / RADIATIONS



A=Glacial (permanent ice cap); B=Polar (covered by frost during the winter which sublimates during the summer); C=North (mild) Transitional (Ca) and C South (extreme) Transitional (Cb); D= Tropical; E= Low albedo tropical; F= Subpolar Lowland (Basins); G=Tropical Lowland (Chasmata); H=Subtropical Highland (Mountain)



Wind speed:60-90 km/h

But not the same effect as on Earth!


Phoenix

HOW LOOKS MARS’ SURFACE?


Phoenix @northern plains



Sojourner



OpportunitySpirit



Opportunity @Endurance crater



Curiosity



Curiosity @Gale crater



“BUILDINGS” BLOCKS



RegolithBasaltic rocks

SandClays



Gravel



Iron/Nickel meteorites(Opportunity)

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CONSTRAINTS FOR THE BASE SITE


Landing ellipse

50 km

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DRIVING

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THE END


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