Magnetic Properties Experiments on the Mars Pathfinder Lander: Preliminary Results

Hviid, S. F.; Madsen, M. B.; Gunnlaugsson, H. P.; Goetz, W.; Knudsen, J. M.; Hargraves, R. B.; Smith, Peter H.; Britt, D. T.; Dinesen, A. R.; Mogensen, C.; Olsen, M. W.; Pedersen, C. Th.; Vistisen, L.

doi:10.1126/science.278.5344.1768

Cited by 104 publications

(63 citation statements)

References 21 publications

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“…A ferric component was also inferred from the Viking magnetic properties experiments which indicated the presence of 1% to 7% of a highly magnetic mineral phase, likely maghemite (¾-Fe203), in the Martian soil [Hargraves et al, 1977]. These Viking results are supported by the Pathfinder data which suggest that most dust particles contain about 6% maghemite [Hviid et al, 1997]. On a more global scale, Morris et al [1993] suggest that the primary Copyright 2000 by the American Geophysical Union.…”

Section: Ferric Minerals On Marssupporting

confidence: 72%

Stability of hydroxylated minerals on Mars: A study on the effects of exposure to ultraviolet radiation

Yen¹,

Murray²,

Rossman³

et al. 1999

J. Geophys. Res.

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Abstract. The density and composition of the Martian atmosphere allow solar ultraviolet photons with wavelengths as short as 190 nm to reach the surface. We investigate the hypothesis that this UV radiation is capable of inducing the release of water from iron oxyhydroxide minerals resulting in the formation of oxide phases. These experiments, which utilize a quadrupole mass spectrometer to monitor the water vapor pressure above mineral samples during cyclic exposure to ultraviolet radiation, offer 5 to 6 orders of magnitude greater sensitivity than previous attempts to establish and quantify this process. We find no evidence that UV photons are capable of liberating OH from the crystal lattice of minerals, and we set a minimum ultraviolet radiationinduced dehydroxylation time of 108 years for removal of this structural OH from mineral particles at the Martian surface. The overturning timescales for surface fines are likely to be shorter than this lower limit for exposure time. Thus we conclude that UV-stimulated dehydroxylation is not a significant process at the Martian surface and that iron oxyhydroxides, if formed during an earlier water-rich environment, should still be found on Mars today. The lack of clear evidence for iron oxyhydroxides at the Martian surface further suggests that Mars' surface was never warm and wet for a long enough period of time for Earth-like weathering to have occurred.

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Section: Ferric Minerals On Marssupporting

confidence: 72%

Stability of hydroxylated minerals on Mars: A study on the effects of exposure to ultraviolet radiation

Yen¹,

Murray²,

Rossman³

et al. 1999

J. Geophys. Res.

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“…Magnetite is thought to be the main magnetic phase in Martian regolith, and hematite is thought to be responsible for the red surface of Mars (Hargraves et al 1977(Hargraves et al , 1979Moore and Jakosky 1989;Hviid et al 1997;Madsen et al 1999Madsen et al , 2003. This is consistent with JMSS-1, which has an average magnetic component (magnetite) of~5 and~2 wt% hematite.…”

Section: Comparison With Martian Soilsupporting

confidence: 73%

JMSS-1: a new Martian soil simulant

Zeng

Wang

et al. 2015

Earth Planet Sp

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It is important to develop Martian soil simulants that can be used in Mars exploration programs and Mars research. A new Martian soil simulant, called Jining Martian Soil Simulant (JMSS-1), was developed at the Lunar and Planetary Science Research Center at the Institute of Geochemistry, Chinese Academy of Sciences. The raw materials of JMSS-1 are Jining basalt and Fe oxides (magnetite and hematite). JMSS-1 was produced by mechanically crushing Jining basalt with the addition of small amounts of magnetite and hematite. The properties of this simulant, including chemical composition, mineralogy, particle size, mechanical properties, reflectance spectra, dielectric properties, volatile content, and hygroscopicity, have been analyzed. On the basis of these test results, it was demonstrated that JMSS-1 is an ideal Martian soil simulant in terms of chemical composition, mineralogy, and physical properties. JMSS-1 would be an appropriate choice as a Martian soil simulant in scientific and engineering experiments in China's Mars exploration in the future.

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“…The existence of Fe-saponites on Mars is also suggested by petrographic observations and microprobe data for iddingsite in SNC meteorites (Burns 1993;Gooding 1992). Finally, the Pathfinder lander's dust magnetic properties experiments found evidence of clay-like aggregates stained or cemented with ferric oxides (Hviid et al 1997), consistent with a hydrothermal origin for the clays (Newsom, Hagerty, and Goff 1999).…”

Section: Implications For Marssupporting

confidence: 48%

Hydrothermal alteration at the Lonar Lake impact structure, India: Implications for impact cratering on Mars

Hagerty

Newsom

2003

Meteorit & Planetary Scien

101

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Abstract-The 50,000 year old, 1.8 km diameter Lonar crater is one of only two known terrestrial craters to be emplaced in basaltic target rock (the 65 million year old Deccan Traps). The composition of the Lonar basalts is similar to martian basaltic meteorites, which establishes Lonar as an excellent analogue for similarly sized craters on the surface of Mars. Samples from cores drilled into the Lonar crater floor show that there are basaltic impact breccias that have been altered by post-impact hydrothermal processes to produce an assemblage of secondary alteration minerals. Microprobe data and X-ray diffraction analyses show that the alteration mineral assemblage consists primarily of saponite, with minor celadonite, and carbonate. Thermodynamic modeling and terrestrial volcanic analogues were used to demonstrate that these clay minerals formed at temperatures between 130°C and 200°C. By comparing the Lonar alteration assemblage with alteration at other terrestrial craters, we conclude that the Lonar crater represents a lower size limit for impact-induced hydrothermal activity. Based on these results, we suggest that similarly sized craters on Mars have the potential to form hydrothermal systems, as long as liquid water was present on or near the martian surface. Furthermore, the Fe-rich alteration minerals produced by post-impact hydrothermal processes could contribute to the minor iron enrichment associated with the formation of the martian soil.

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Magnetic Properties Experiments on the Mars Pathfinder Lander: Preliminary Results

Cited by 104 publications

References 21 publications

Stability of hydroxylated minerals on Mars: A study on the effects of exposure to ultraviolet radiation

Stability of hydroxylated minerals on Mars: A study on the effects of exposure to ultraviolet radiation

JMSS-1: a new Martian soil simulant

Hydrothermal alteration at the Lonar Lake impact structure, India: Implications for impact cratering on Mars

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