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Science, 1966 With the scarcity of factual data and the difficulty of applying crucial tests, many of the properties of the Martian surface remain a mystery; the planet may become a source of great surprises in the future. In the following, the conclusions are enumerated more or less in the order of their reliability, the more certain ones first, conjectures or ...
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Coupled Ferric Oxides and Sulfates on the Martian Surface
Science, 2007The Mars Exploration Rover (MER), Opportunity, showed that layered sulfate deposits in Meridiani Planum formed during a period of rising acidic ground water. Crystalline hematite spherules formed in the deposits as a consequence of aqueous alteration and were concentrated on the surface as a lag deposit as wind eroded the softer sulfate rocks.
Bibring, J.-P. +11 more
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Scratching the surface of martian habitability
Science, 2014Are the right chemical ingredients enough to make a habitable planet?
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A model of interaction of Phobos’ surface with the martian environment
Icarus, 2011Abstract We simulate space weathering of Phobos’ surface due to both sputtering by solar wind ions (H+ and He2+) and planetary protons, and surface material vaporization by micrometeoroids impact. Assuming an Iron-rich composition of Phobos’ regolith, we find that densities of neutral species (Fe, O, Al, Ca, Mg, Na) in the martian environment are in ...
Cipriani, Fabrice +4 more
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Weathering of Martian Surface Rocks
1986The early 1960s marked the beginning of an extremely important trend in Martian investigation, i.e., exploration by space missions. From 1962 to 1976 more than a dozen spacecraft in the framework Mars, Mariner, and Viking space missions were launched, providing new and important data on the composition and structure of the Martian atmosphere and soil ...
M. Yu. Zolotov, Yu. I. Sidorov
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The age of SNC meteorites and the antiquity of the Martian surface
Earth and Planetary Science Letters, 2005We report new Sm–Nd, Lu–Hf, and Pb–Pb mineral and whole-rock isotope data for the basaltic shergottite Zagami, as well as Pb–Pb whole-rock isotope data for the basaltic shergottite Los Angeles, the lherzolitic shergottite Dar-al-Gani 476 (DaG 476), and the clinopyroxenite Nakhla. In agreement with previous findings, our new Sm–Nd and Lu–Hf mineral ages
Bouvier, Audrey +3 more
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On the composition of martian surface materials
Icarus, 1967Abstract Observations were made of Mars with the birefringent interferometer. These observations when combined with spectra of the Sun show that Mars has an extremely strong band at 3.1 μ. This band is presumably produced by hydrated minerals on the surface of Mars.
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Orbital monitoring of martian surface changes
Icarus, 2016Abstract A history of martian surface changes is documented by a sequence of global mosaics made up of Mars Global Surveyor Mars Orbiter Camera daily color images from 1999 to 2006, together with a single mosaic from the Mars Reconnaissance Orbiter Mars Color Imager in 2009.
Priyanjoli Mukherjee +3 more
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Mineral stability at the Martian surface
Journal of Geophysical Research, 1968Thermodynamic calculations of mineral stability fields under a range of predicted surface conditions for Mars indicate that goethite will be unstable except under the wettest and coldest parts (pH2O ∼ 10−6 atm, T < 200°K) of this range. If the planetary atmosphere is strongly reducing, as implied by some estimates of CO abundance, the measured water ...
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Distribution of small channels on the Martian surface
Icarus, 1976The distribution of small channels on Mars has been mapped from Mariner 9 images at the 1:5,000,000 scale. The small channels referred to here are small valleys ranging in width from the resolution limit of the Mariner 9 wide-angle images (about 1 km) to about 10 km. The greatest density of small channels occurs in dark cratered terrain.
David C. Pieri, David C. Pieri
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