Mathematics – Logic
Scientific paper
Jan 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998uisr.work...14n&link_type=abstract
Workshop on Using In Situ resources for Construction of Planetary Outposts, p. 14
Mathematics
Logic
Chondrites, Glass, Granite, Hydrogen Peroxide, Ice, Mars Surface, Metals, Planetary Geology, Regolith, Soils, Polar Caps, Mars (Planet), Breccia, Cratering, Extraterrestrial Life, Impact Melts, Life Support Systems, Manufacturing, Radiation Shielding, Viking Lander Spacecraft, Volcanoes
Scientific paper
The long-term exploration of Mars will require the utilization of surface and near-surface materials for construction, radiation shielding, and life support. Eventually, such materials could be used as raw materials in manufacturing. While there is a resemblance between the surface of Mars, as revealed in Viking and Pathfinder images, and terrestrial desert environments, there are distinct differences that will affect the utilization of in situ resources. In general, the surface geological features are extremely old compared to Earth, dating back to the early evolution of the solar system. Therefore, materials created by processes such as impact cratering are important on Mars. Impact cratering probably created extensive sheets of impact melt bearing breccias on the surface and resulted in the formation of a thick regolith of broken rock fragments in the ancient terrains of Mars. Another key feature is the lack of rainfall over most of Mars' history. This resulted in the lack of extensive erosion. On Earth, extensive erosion of volcanic centers, for example, has exposed deep hydrothermal deposits that are mined for Cu, Mo, and W, but such deposits are not likely to be exposed at the surface on Mars. Similarly, deposits of quartz sand, used for glass making, are created by the erosion of granitic terrains on Earth, and are not likely to be found on Mars. The soil on Mars is also very different from wind-blown material on Earth. Virtually no organic material is present, and the material is enriched in volatile elements, such as S and Cl, and possibly also toxic heavy metals, derived from volcanic gases and hydrothermal waters that poured onto the surface. The volatile elements have remained in the soil due to the absence of processes that recycle volatile elements back into the planet's crust. Hydrogen peroxide originally formed in the atmosphere is also mixed into the soil and regolith, and was probably responsible for the "oxidant" found in the soil by the Viking biology experiments. The surface may also contain material delivered to the surface, including solar-wind He-3, and chondritic material from meteorites and cosmic dust. One of the biggest problems is the probable lack of water any where near the surface, except in the the form of ice near the poles. A list summarizing some of the familiar and unfamiliar materials that may be encountered on the martian surface is presented.
Hagerty Justin J.
Newsom Horton E.
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