Computer Science
Scientific paper
Jan 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999nvm..conf...72w&link_type=abstract
Workshop on New Views of the Moon 2: Understanding the Moon Through the Integration of Diverse Datasets, p. 72
Computer Science
Lunar Resources, Lunar Roving Vehicles, Lunar Laboratories, Lunar Environment, Mission Planning, Life Support Systems, Lunar Surface, Marsokhod Mars Roving Vehicles, Mass Spectrometers, Lunar Soil
Scientific paper
The success of a manned lunar outpost may require that indigenous resources be utilized in order to reduce the requirements for the periodic resupply from Earth for the human inhabitants. Some indigenous lunar resources do exist. For instance, studies of the lunar regoliths, acquired by the Apollo and Luna missions from several maria, indicate that upon heating in a vacuum, these soils evolve the volatile gases: helium (He), hydrogen (H2), carbon dioxide (CO2), carbon monoxide (CO), nitrogen (N2), and sulfur dioxide (SO2). The He, H, C, and N were originally implanted by solar wind These gases would be valuable to supply life-support systems. For instance, the H2 could be used as a rocket fuel, or alternatively, reacted with the mineral ilmenite (FeTiO3), indigenous to the lunar soil, to yield water (H2O). In an enclosed structure irradiated by solar energy, the H2O, N2, and CO2 could be utilized to grow edible plants for lunar inhabitants. Alternatively, the H2O could be electrolyzed, using photovoltaic cells, yielding breathable O. The inert gas He, would be useful for filling inflatable structures. In addition, the lunar He contains a high abundance of the rare isotopic He-3, which has been identified as a potentially valuable fuel for nuclear-fusion space power systems. In order to determine the economic potential of these lunar volatiles, we need information to assess the in situ quantities of these gases and identify the most abundant sites. In order to acquire such information, a large number of soil samples must be acquired and analyzed because it is not known if these volatile gases in the soil vary widely over the distance of a few meters or several kilometers. In addition, all of the lunar soil samples were analyzed on Earth, after being contaminated by terrestrial air and water. For these reasons, therefore, a mobile, robotic vehicle has been proposed that would be landed-on a lunar maria and assay the volatiles evolved by heating the indigenous lunar regolith. A lunar rover platform with the sample equipment attached has been designed. This science platform was conceptionally designed to fit on a small Marsokhod Rover (75 kg) with a 100-km range. The proposed sampling protocol would be to collect two samples, nearly adjacent. If the results agreed within the experimental deviation, the rover would proceed 0.5 km along the planned route and select two new samples. The progress of the rover and the results of the analyses would be continuously monitored from Earth so that the sampling protocol could be revised as needed. The scientific equipment would accomplish the assay of the regolith samples in the following sequence: (1) retrieve a sample of regolith from the lunar surface by use of a scoop mounted on the platform; (2) reduce the sample to about 1 g of particles <200 pm; (3) weigh the sample; (4) characterize the mineral content (TiO2); (5) heat the sample to 1200C in a vacuum furnace; (6) collect the volatiles; (7) characterize the volatile products; and (8) transmit the data. The components of the scientific package were conceptually designed and are briefly described: (1) The heater unit. A 1 g sample of the surface regolith would be placed in a ferritic steel crucible 0.8 cm OD x 1.57 cm high. This container would be placed in a coiled electrical heater inside an evacuated 1-L container. Heat transfer calculations indicate that the sample would attain 1200C in 14 min with a 25-W heater. For a high-Ti maria regolith sufficient gases are released to create a pressure of 70 Pa at 30C, which is a sufficient sample for the mass spectrometer. (2) Determination of metallic elements. Before the sample is heated, a laser beam delivers 0.45-2.0 Joules per pulse at a wave length of 1 micron to the surface of the sample. The absorption of the laser energy vaporizes some of the minerals in the soils. The vaporized ions are quantitatively determined by the mass spectrometer. (3) Mass spectrometer. This instrument must be utilized to characterize the mineral content of the soil and the volatile gases, essentially from 1 to 72 AMU range. A Fourier Transform Mass Spectrometer (FTMS) may be particularly useful for this analysis, but requires testing. (4) Powersupply. The initial power subsystem assumed the availability of a general purpose heat source, or a Radioisotope Thermoelectric Generator. If the launch of an RTG is forbidden for safety reasons, alternative power supplies would be considered such as solar-electric or beamed microwave sources.
Kulcinski Gerald L.
Mogahed E. A.
Sviatoslavsky I. N.
Wittenberg L. J.
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