Abstract. Large portions of Mars' surface are covered with deposits of fine, homogeneous, weathered dusty-soil material. Nanophase iron oxides, silicate mineralolds, and salts prevail in the soil. The mode of formation of this somewhat peculiar type of soil is still far from being clear. One scenario suggests that weathering took place during early epochs when Mars may have been "warm and wet." The properties of the soil are not easily reconciled wi.'th this scenario. We propose another possible scenario that attributes, in part, the peculiar nature of the Martian dust and soft to a relatively "young" weathering product formed during the last few hundreds of millions of years in a process that involves acidic volatiles. We tested this hypothesis in an experimental study of the first step of acidolytic weathering of a partly palagonitized VOlcanic tephra of hawaiitic lava origin, using sulfi•c, hydrochloric and nitric acids and their mixtures. The tephra effectively "neutralize" the added acidity. The protonic acidity added to the tephra attacks the primary-minerals, releasing Fe, A1, and Mg, which control the pH, acting as Lewis-acid species of varying acid strengths. The full mount of acidity added to the tephra is stored in it, but only a very small fraction is preserved as the original protonic acidity. The majority of the added sulfate and chloride were present as salts and easily solubilized minerals. Well-crystallized sulfate salt minerals of aluminum and calcium were detected by powder X ray diffractomen, whereas secondary magnesium and iron minerals were not detected, due probably to lack of crystallinity. The presence of gyps m (CaSO4'2H20) and alunogen (A12(SO4)3'17H20) is probably responsible for the observed increased hygroscopicity of the acidified tephra and their tendency. to form hardened crusts. We suggest that if this mechanism is of importance on Mars, then the chemically weathered component of the Martian soil consists of a salt-rich mineral mixture containing the salts of the anionicligands SO4 and C1 resulting from volafiles emitted from volcanoes during more recent eruptions (up to 109 years B.P.). The lack of liquid water on Mars surface during that time slowed or halted mineralogical evolution into highly crystallized minerals having large mineral grains. The chemically weathered components are mixed wi.th _the products of physical weathering. The recently formed soil may cover and coat more evolved, hydrothermally modified, mineral deposits formed in earlier epochs Of Mars.

Abstract. Rock and soil samples from the planet Mars are due to be returned to Earth within a decade. Martian samples initially will be tested for evidence of life and biological hazard under strict biological containment. Wider distribution of samples for organic and inorganic analysis may occur only if neither evidence of life nor hazard is detected, or if the samples are first sterilized. We subjected a range of Mars analog rocks and minerals to high doses of gamma radiation in order to determine the effects of gamma sterilization on the samples' isotopic, chemical, and physical properties. Gamma photons from 6øCo (1.17 and 1.33 MeV) in doses as high as 3 x 107 rads did not induce radioactivity in the samples and produced no measurable changes in their isotopic and chemical compositions. This level of irradiation also produced no measurable changes in the crystallographic structure of any sample, the surface areas of soil analogs, or the fluid inclusion homogenization temperature of quartz. The only detectable effects of irradiation were dose-dependent changes in the visible and near-infrared spectral region (e.g., discoloration and darkening of quartz and halite and an increase in albedo of carbonates) and increases in the thermoluminescence of quartz and plagioclase. If samples returned from Mars require biological sterilization, gamma irradiation provides a feasible option. BackgroundMartian rock and soil, collected by robotic spacecraft, will be returned to terrestrial laboratories early in the next century. The return of documented samples, carefully collected and preserved, will be a major step in the search for evidence of Martian life. Martian conditions, including the lack of organic matehal, subfreezing temperatures, high flux of solar ultraviolet radiation, and strongly oxidizing chemical species in the soil, severely limit the survival of organisms at or near the surface [Klein, 1998] inCenters for Disease Control and Prevention, Atlanta, Georgia.•University of Portsmouth, Portsmouth, England.Copyright 1999 by the American Geophysical Union. Paper number 1999JE001064.0148-0227/99/1999JE001064509.00 specialized organisms at low concentrations in the returned samples is conceivable [Clark, 1998].Current planetary protection strategies call for the samples to be immediately placed into biological containment and tested for signs of present or past life and biological hazard [DeVincenzi et al., 1998]. It is recommended that "Controlled distribution of unsterilized materials from Mars should occur only if rigorous analyses determine that the materials do not constitute a biological hazard. If any portion of the sample is removed from containment prior to completion of these analyses it should first be sterilized" [Space Studies Board, 1997]. While sterilization of Mars samples may not be required, an acceptable method must be available before the samples are returned to Earth.A variety of sterilization techniques have been used or proposed for spacecraft missions to Mars. These include dry heating to t...