51
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Ruff SW, Christensen PR, Clark RN, Kieffer HH, Malin MC, Bandfield JL, Jakosky BM, Lane MD, Mellon MT, Presley MA. Mars' “White Rock” feature lacks evidence of an aqueous origin: Results from Mars Global Surveyor. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001329] [Citation(s) in RCA: 40] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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52
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Banin A, Carle GC, Chang S, Coyne LM, Orenberg JB, Scattergood TW. Laboratory investigations of Mars: chemical and spectroscopic characteristics of a suite of clays as Mars soil analogs. ORIGINS LIFE EVOL B 2001; 18:239-65. [PMID: 11538359 DOI: 10.1007/bf01804672] [Citation(s) in RCA: 16] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/25/2022]
Abstract
Two major questions have been raised by prior explorations of Mars. Has there ever been abundant water on Mars? Why is the iron found in the Martian soil not readily seen in the reflectance spectra of the surface? The work reported here describes a model soil system of Mars Soil Analog Materials, MarSAM, with attributes which could help resolve both of these dilemmas. The first set of MarSAM consisted of a suite of variably iron/calcium-exchanged montmorillonite clays. Several properties, including chemical composition, surface-ion composition, water adsorption isotherms, and reflectance spectra, of these clays have been examined. Also, simulations of the Viking Labeled Release Experiment using the MarSAM were performed. The results of these studies show that surface iron and adsorbed water are important determinants of clay behavior as evidenced by changes in reflectance, water absorption, and clay surface reactions. Thus, these materials provide a model soil system which reasonably satisfies the constraints imposed by the Viking analyses and remote spectral observations of the Martian surface, and which offers a sink for significant amounts of water. Finally, our initial results may provide insights into the mechanisms of reactions that occur on clay surfaces as well as a more specific approach to determining the mineralogy of Martian soils.
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Affiliation(s)
- A Banin
- Hebrew University, Rehovot, Israel
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53
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Lawless JG, Banin A, Church FM, Mazzurco J, Huff R, Kao J, Cook A, Lowe T, Orenberg JB, Edelson E. pH profile of the adsorption of nucleotides onto montmorillonite. I. Selected homoionic clays. ORIGINS LIFE EVOL B 2001; 15:77-88. [PMID: 11539613 DOI: 10.1007/bf01809490] [Citation(s) in RCA: 30] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/25/2022]
Abstract
The effect of adsorbed ions and pH on the adsorption of several purine and pyrimidine nucleotides on montmorillonite was studied. The cations used to prepare homoionic montmorillonite was Na+, Mn2+, Fe3+, Co2+, Ni+, Cu2+, and Zn2+. The nucleotides studied were 5'-,3'-, and 2'-AMP, and 5'-CMP in the pH range 2 through 12. The results show that preferential adsorption amongst nucleotides and similar molecules is dependent upon pH and the nature of the substituted metal cation in the clay. At neutral pH, it was observed that 5'-AMP was more strongly adsorbed than 2'AMP, 3'-AMP, and 5'-CMP. Cu2+ and Zn2+ clays showed enhanced adsorption of 5'-AMP compared to the other cation clays studied in the pH range 4-8. Below pH 4, the adsorption is attributed to cation and anion exchange adsorption mechanisms: above pH 4, anion exchange may also occur, but the adsorption (when it occurs) likely depends on a complexation mechanism occurring between metal cation in the clay exchange site the biomolecule. It is thus proposed that homoionic clays may have played a significant role in the concentration mechanism of biomonomers in the prebiotic environment, a prerequisite step necessary for the formation of biopolymers in the remaining steps leading to the origin of life.
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Affiliation(s)
- J G Lawless
- Extraterrestrial Research Division, NASA Ames Research Center, Moffett Field, CA 94035, USA
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54
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Esposito F, Colangeli L, Palomba E. Infrared reflectance spectroscopy of Martian analogues. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001223] [Citation(s) in RCA: 12] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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55
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Kraft MD, Greeley R. Rock coatings and aeolian abrasion on Mars: Application to the Pathfinder landing site. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001229] [Citation(s) in RCA: 19] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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56
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Christensen PR, Bandfield JL, Clark RN, Edgett KS, Hamilton VE, Hoefen T, Kieffer HH, Kuzmin RO, Lane MD, Malin MC, Morris RV, Pearl JC, Pearson R, Roush TL, Ruff SW, Smith MD. Detection of crystalline hematite mineralization on Mars by the Thermal Emission Spectrometer: Evidence for near-surface water. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001093] [Citation(s) in RCA: 379] [Impact Index Per Article: 15.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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57
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58
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Farquhar J, Savarino J, Jackson TL, Thiemens MH. Evidence of atmospheric sulphur in the martian regolith from sulphur isotopes in meteorites. Nature 2000; 404:50-2. [PMID: 10716436 DOI: 10.1038/35003517] [Citation(s) in RCA: 227] [Impact Index Per Article: 9.5] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
Abstract
Sulphur is abundant at the martian surface, yet its origin and evolution over time remain poorly constrained. This sulphur is likely to have originated in atmospheric chemical reactions, and so should provide records of the evolution of the martian atmosphere, the cycling of sulphur between the atmosphere and crust, and the mobility of sulphur in the martian regolith. Moreover, the atmospheric deposition of oxidized sulphur species could establish chemical potential gradients in the martian near-surface environment, and so provide a potential energy source for chemolithoautotrophic organisms. Here we present measurements of sulphur isotopes in oxidized and reduced phases from the SNC meteorites--the group of related achondrite meteorites believed to have originated on Mars--together with the results of laboratory photolysis studies of two important martian atmospheric sulphur species (SO2 and H2S). The photolysis experiments can account for the observed sulphur-isotope compositions in the SNC meteorites, and so identify a mechanism for producing large abiogenic 34S fractionations in the surface sulphur reservoirs. We conclude that the sulphur data from the SNC meteorites reflects deposition of oxidized sulphur species produced by atmospheric chemical reactions, followed by incorporation, reaction and mobilization of the sulphur within the regolith.
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Affiliation(s)
- J Farquhar
- Department of Chemistry, University of California, San Diego, La Jolla 92093, USA.
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59
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Bell JF, McSween HY, Crisp JA, Morris RV, Murchie SL, Bridges NT, Johnson JR, Britt DT, Golombek MP, Moore HJ, Ghosh A, Bishop JL, Anderson RC, Brückner J, Economou T, Greenwood JP, Gunnlaugsson HP, Hargraves RM, Hviid S, Knudsen JM, Madsen MB, Reid R, Rieder R, Soderblom L. Mineralogic and compositional properties of Martian soil and dust: Results from Mars Pathfinder. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001060] [Citation(s) in RCA: 230] [Impact Index Per Article: 9.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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60
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Morris RV, Golden DC, Bell JF, Shelfer TD, Scheinost AC, Hinman NW, Furniss G, Mertzman SA, Bishop JL, Ming DW, Allen CC, Britt DT. Mineralogy, composition, and alteration of Mars Pathfinder rocks and soils: Evidence from multispectral, elemental, and magnetic data on terrestrial analogue, SNC meteorite, and Pathfinder samples. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001059] [Citation(s) in RCA: 257] [Impact Index Per Article: 10.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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61
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Hargraves RB, Knudsen JM, Bertelsen P, Goetz W, Gunnlaugsson HP, Hviid SF, Madsen MB, Olsen M. Magnetic enhancement on the surface of Mars? ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001032] [Citation(s) in RCA: 25] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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62
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Farmer JD, Des Marais DJ. Exploring for a record of ancient Martian life. JOURNAL OF GEOPHYSICAL RESEARCH 1999; 104:26977-95. [PMID: 11543200 DOI: 10.1029/1998je000540] [Citation(s) in RCA: 245] [Impact Index Per Article: 9.8] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Abstract
The immediate task facing exopaleontology is to define a strategy to explore Mars for a fossil record during the decade-long exploration program that lies ahead. Consideration of the quality of paleontological information preserved under different geological conditions is important if we are to develop a strategy with broad applicability. The preservation of microbial fossils is strongly influenced by the physical, chemical, and biological factors of the environment which, acting together, determine the types of information that will be captured and retained in the rock record. In detrital sedimentary systems, preservation is favored by rapid burial in fine-grained, clay-rich sediments. In chemical sedimentary systems, preservation is enhanced by rapid entombment in fine-grained chemical precipitates. For long-term preservation, host rocks must be composed of stable minerals that are resistant to chemical weathering and that form an impermeable matrix and closed chemical system to protect biosignatures from alteration during subsequent diagenesis or metamorphism. In this context, host rocks composed of highly ordered, chemically stable mineral phases, like silica (e.g., cherts) or phosphate (e.g., phosphorites), are especially favored. Such lithologies tend to have very long crustal residence times and, along with carbonates and shales, are the most common host rocks for the Precambrian microfossil record on Earth. Although we make the defensible assumption that Mars was more like the Earth early in its history, clearly, the geological and historical differences between the two planets are many. Such differences must be carefully considered when adapting an Earth-based strategy to Mars.
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Affiliation(s)
- J D Farmer
- Department of Geology, Arizona State University, Tempe, USA.
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63
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Herkenhoff KE, Vasavada AR. Dark material in the polar layered deposits and dunes on Mars. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/1998je000589] [Citation(s) in RCA: 33] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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64
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Catling DC. A chemical model for evaporites on early Mars: Possible sedimentary tracers of the early climate and implications for exploration. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/1998je001020] [Citation(s) in RCA: 105] [Impact Index Per Article: 4.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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65
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Madsen MB, Hviid SF, Gunnlaugsson HP, Knudsen JM, Goetz W, Pedersen CT, Dinesen AR, Mogensen CT, Olsen M, Hargraves RB. The magnetic properties experiments on Mars Pathfinder. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/1998je900006] [Citation(s) in RCA: 79] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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66
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Thomas PC, Malin MC, Carr MH, Danielson GE, Davies ME, Hartmann WK, Ingersoll AP, James PB, McEwen AS, Soderblom LA, Veverka J. Bright dunes on Mars. Nature 1999. [DOI: 10.1038/17557] [Citation(s) in RCA: 61] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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67
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Bishop JL, Froschl H, Mancinelli RL. Alteration processes in volcanic soils and identification of exobiologically important weathering products on Mars using remote sensing. JOURNAL OF GEOPHYSICAL RESEARCH 1998; 103:31457-76. [PMID: 11542259 DOI: 10.1029/1998je900008] [Citation(s) in RCA: 38] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Abstract
Determining the mineralogy of the Martian surface material provides information about the past and present environments on Mars which are an integral aspect of whether or not Mars was suitable for the origin of life. Mineral identification on Mars will most likely be achieved through visible-infrared remote sensing in combination with other analyses on landed missions. Therefore, understanding the visible and infrared spectral properties of terrestrial samples formed via processes similar to those thought to have occurred on Mars is essential to this effort and will facilitate site selection for future exobiology missions to Mars. Visible to infrared reflectance spectra are presented here for the fine-grained fractions of altered tephra/lava from the Haleakala summit basin on Maui, the Tarawera volcanic complex on the northern island of New Zealand, and the Greek Santorini island group. These samples exhibit a range of chemical and mineralogical compositions, where the primary minerals typically include plagioclase, pyroxene, hematite, and magnetite. The kind and abundance of weathering products varied substantially for these three sites due, in part, to the climate and weathering environment. The moist environments at Santorini and Tarawera are more consistent with postulated past environments on Mars, while the dry climate at the top of Haleakala is more consistent with the current Martian environment. Weathering of these tephra is evaluated by assessing changes in the leachable and immobile elements, and through detection of phyllosilicates and iron oxide/oxyhydroxide minerals. Identifying regions on Mars where phyllosilicates and many kinds of iron oxides/oxyhydroxides are present would imply the presence of water during alteration of the surface material. Tephra samples altered in the vicinity of cinder cones and steam vents contain higher abundances of phyllosilicates, iron oxides, and sulfates and may be interesting sites for exobiology.
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Affiliation(s)
- J L Bishop
- NRC/NASA Ames Research Center, Moffett Field, California, USA
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68
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Zent AP. On the thickness of the oxidized layer of the Martian regolith. JOURNAL OF GEOPHYSICAL RESEARCH 1998; 103:31491-8. [PMID: 11542261 DOI: 10.1029/98je01895] [Citation(s) in RCA: 44] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Abstract
A revised model of the diffusion of H2O2 through the Martian regolith is presented, which argues that oxidant diffusion may be more efficient than previously thought. Recent models of the adsorption of H2O at Mars-like conditions indicate that it adsorbs more poorly than previously believed. H2O adsorption is a necessary proxy for peroxide adsorption; hence the adsorptive slowing of peroxide diffusion is modeled as less efficient. Because the peroxide has a finite lifetime, it has a finite extinction depth as well. The effects of regolith gardening by impacts are quantitatively estimated and combined with the effects of oxidation by atmospheric gases to produce estimates of the degree of oxidation of the Martian surface with depth. We explore the effects of different crater production populations along with variations in H2O2 extinction depths, and hydrothermal oxidation of ejecta. In very select circumstances involving very early onset of oxidizing conditions during heavy bombardment, 150-200 m of regolith could be fully oxidized. More likely scenarios for the crater production population, onset of oxidizing conditions, and oxidant extinction depth yield estimates of no more than a few meters to putative reducing material. In addition, uncertainties remain regarding the degree to which hydrothermal or other high-temperature chemistry might oxidize materials in ejecta blankets. The trade-off between accessing unlithified sediments or rock interiors must be considered.
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Affiliation(s)
- A P Zent
- Space Sciences Division, NASA Ames Research Center, Moffett Field, California, USA
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69
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Yen AS, Murray BC, Rossman GR. Water content of the Martian soil: Laboratory simulations of reflectance spectra. ACTA ACUST UNITED AC 1998. [DOI: 10.1029/98je00739] [Citation(s) in RCA: 39] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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70
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Christensen PR. Variations in Martian surface composition and cloud occurrence determined from thermal infrared spectroscopy: Analysis of Viking and Mariner 9 data. ACTA ACUST UNITED AC 1998. [DOI: 10.1029/97je02114] [Citation(s) in RCA: 36] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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71
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72
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Stoker CR, Bullock MA. Organic degradation under simulated Martian conditions. JOURNAL OF GEOPHYSICAL RESEARCH 1997; 102:10881-8. [PMID: 11541744 DOI: 10.1029/97je00667] [Citation(s) in RCA: 94] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Abstract
We report on laboratory experiments which simulate the breakdown of organic compounds under Martian surface conditions. Chambers containing Mars-analog soil mixed with the amino acid glycine were evacuated and filled to 100 mbar pressure with a Martian atmosphere gas mixture and then irradiated with a broad spectrum Xe lamp. Headspace gases were periodically withdrawn and analyzed via gas chromatography for the presence of organic gases expected to be decomposition products of the glycine. The quantum efficiency for the decomposition of glycine by light at wavelengths from 2000 to 2400 angstroms was measured to be 1.46 +/- 1.0 x 10(-6) molecules/photon. Scaled to Mars, this represents an organic destruction rate of 2.24 +/- 1.2 x 10(-4) g of C m-2 yr-1. We compare this degradation rate with the rate that organic compounds are brought to Mars as a result of meteoritic infall to show that organic compounds are destroyed on Mars at rates far exceeding the rate that they are deposited by meteorites. Thus the fact that no organic compounds were found on Mars by the Viking Lander Gas Chromatograph Mass Spectrometer experiment can be explained without invoking the presence of strong oxidants in the surface soils. The organic destruction rate may be considered as an upper bound for the globally averaged biomass production rate of extant organisms at the surface of Mars. This upper bound is comparable to the slow growing cryptoendolithic microbial communities found in dry Antarctica deserts. Finally, comparing these organic destruction rates to recently reported experiments on the stability of carbonate on the surface of Mars, we find that organic compounds may currently be more stable than calcite.
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Affiliation(s)
- C R Stoker
- Space Science Division, NASA Ames Research Center, Moffett Field, California, USA
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73
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Bell JF, Wolff MJ, James PB, Clancy RT, Lee SW, Martin LJ. Mars surface mineralogy from Hubble Space Telescope imaging during 1994-1995: Observations, calibration, and initial results. ACTA ACUST UNITED AC 1997. [DOI: 10.1029/96je03990] [Citation(s) in RCA: 50] [Impact Index Per Article: 1.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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74
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Smith PH, Tomasko MG, Britt D, Crowe DG, Reid R, Keller HU, Thomas N, Gliem F, Rueffer P, Sullivan R, Greeley R, Knudsen JM, Madsen MB, Gunnlaugsson HP, Hviid SF, Goetz W, Soderblom LA, Gaddis L, Kirk R. The imager for Mars Pathfinder experiment. ACTA ACUST UNITED AC 1997. [DOI: 10.1029/96je03568] [Citation(s) in RCA: 116] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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75
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Golombek MP, Cook RA, Moore HJ, Parker TJ. Selection of the Mars Pathfinder landing site. ACTA ACUST UNITED AC 1997. [DOI: 10.1029/96je03318] [Citation(s) in RCA: 78] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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76
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Roush TL, Orenberg JB. Estimated detectability limits of iron-substituted montmorillonite clay on Mars from thermal emission spectra of clay-palagonite physical mixtures. ACTA ACUST UNITED AC 1996. [DOI: 10.1029/96je02863] [Citation(s) in RCA: 9] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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77
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Madsen MB, Agerkvist DP, Gunnlaugsson HP, Hviid SF, Knudsen JM, Vistisen L. Titanium and the magnetic phase on Mars. ACTA ACUST UNITED AC 1995. [DOI: 10.1007/bf02146321] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/25/2022]
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78
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Banin A, Mancinelli RL. Life on Mars? I. The chemical environment. ADVANCES IN SPACE RESEARCH : THE OFFICIAL JOURNAL OF THE COMMITTEE ON SPACE RESEARCH (COSPAR) 1995; 15:163-170. [PMID: 11539220 DOI: 10.1016/s0273-1177(99)80079-9] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
The origin of life at its abiotic evolutionary stage, requires a combination of constituents and environmental conditions that enable the synthesis of complex replicating macromolecules from simpler monomeric molecules. It is very likely that the early stages of this evolutionary process have been spontaneous, rapid and widespread on the surface of the primitive Earth, resulting in the formation of quite sophisticated living organisms within less than a billion years. To what extent did such conditions prevail on Mars? Two companion-papers (Life on Mars? I and II) will review and discuss the available information related to the chemical, physical and environmental conditions on Mars and assess it from the perspective of potential exobiological evolution.
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Affiliation(s)
- A Banin
- The Hebrew University, Rehovot, Israel
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79
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Bishop JL, Pieters CM. Low-temperature and low atmospheric pressure infrared reflectance spectroscopy of Mars soil analog materials. ACTA ACUST UNITED AC 1995. [DOI: 10.1029/94je03331] [Citation(s) in RCA: 61] [Impact Index Per Article: 2.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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80
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Lee P, Thomas PC. Longitudinal dunes on Mars: Relation to current wind regimes. ACTA ACUST UNITED AC 1995. [DOI: 10.1029/95je00225] [Citation(s) in RCA: 45] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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81
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Blaney DL, McCord TB. Indications of sulfate minerals in the Martian soil from Earth-based spectroscopy. ACTA ACUST UNITED AC 1995. [DOI: 10.1029/95je00224] [Citation(s) in RCA: 44] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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82
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Roush TL, Bell JF. Thermal emission measurements 2000–400 cm−1(5–25 μm) of Hawaiian palagonitic soils and their implications for Mars. ACTA ACUST UNITED AC 1995. [DOI: 10.1029/94je02448] [Citation(s) in RCA: 19] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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83
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Bell JF, Roush TL, Morris RV. Mid-infrared transmission spectra of crystalline and nanophase iron oxides/oxyhydroxides and implications for remote sensing of Mars. ACTA ACUST UNITED AC 1995. [DOI: 10.1029/94je01389] [Citation(s) in RCA: 17] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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84
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Morris RV, Golden DC, Bell JF, Lauer HV. Hematite, pyroxene, and phyllosilicates on Mars: Implications from oxidized impact melt rocks from Manicouagan Crater, Quebec, Canada. ACTA ACUST UNITED AC 1995. [DOI: 10.1029/94je01500] [Citation(s) in RCA: 56] [Impact Index Per Article: 1.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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85
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Heated nontronite: Possible relations to the magnetic phase in the Martian soil. ACTA ACUST UNITED AC 1994. [DOI: 10.1007/bf02064565] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/25/2022]
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86
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Quinn R, Orenberg J. Simulations of the Viking Gas Exchange Experiment using palagonite and Fe-rich montmorillonite as terrestrial analogs: implications for the surface composition of Mars. GEOCHIMICA ET COSMOCHIMICA ACTA 1993; 57:4611-4618. [PMID: 11539578 DOI: 10.1016/0016-7037(93)90186-z] [Citation(s) in RCA: 9] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
Simulations of the Gas Exchange Experiment (GEX), one of the Viking Lander Biology Experiments, were run using palagonite and Fe-rich montmorillonite as terrestrial analogs of the Martian soil. These terrestrial analogs were exposed to a nutrient solution of the same composition as that of the Viking Landers under humid (no contact with nutrient) and wet (intimate contact) conditions. The headspace gases in the GEX sample cell were sampled and then analyzed by gas chromatography under both humid and wet conditions. Five gases were monitored: CO2, N2, O2, Ar, and Kr. It was determined that in order to simulate the CO2 gas changes of the Viking GEX experiment, the mixture of soil analog mineral plus nutrient medium must be slightly (pH = 7.4) to moderately basic (pH = 8.7). This conclusion suggests constraints upon the composition of terrestrial analogs to the Mars soil; acidic components may be present, but the overall mixture must be basic in order to simulate the Viking GEX results.
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Affiliation(s)
- R Quinn
- Department of Chemistry and Biochemistry, San Francisco State University, CA 94132, USA
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87
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Feldman WC, Boynton WV, Jakosky BM, Mellon MT. Redistribution of subsurface neutrons caused by ground ice on Mars. ACTA ACUST UNITED AC 1993. [DOI: 10.1029/93je02325] [Citation(s) in RCA: 38] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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88
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Banin A, Ben-Shlomo T, Margulies L, Blake DF, Mancinelli RL, Gehring AU. The nanophase iron mineral(s) in Mars soil. ACTA ACUST UNITED AC 1993. [DOI: 10.1029/93je02500] [Citation(s) in RCA: 49] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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89
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Bishop JL, Pieters CM, Burns RG. Reflectance and Mossbauer spectroscopy of ferrihydrite-montmorillonite assemblages as Mars soil analog materials. GEOCHIMICA ET COSMOCHIMICA ACTA 1993; 57:4583-4595. [PMID: 11539454 DOI: 10.1016/0016-7037(93)90184-x] [Citation(s) in RCA: 18] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
Spectroscopic analyses show that Fe(3+)-doped smectites prepared in the laboratory exhibit important similarities to the soils on Mars. Ferrihydrite has been identified as the interlayer ferric component in Fe(3+)-doped smectites by a low quadrupole splitting and magnetic field strength of approximately 48 tesla in Mossbauer spectra measured at 4.2 K, as well as a crystal field transition at 0.92 micrometer. Ferrihydrite in these smectites explains features in the visible-near infrared region that resemble the energies and band strengths of features in reflectance spectra observed for several bright regions on Mars. Clay silicates have met resistance in the past as Mars soil analogs because terrestrial clay silicates exhibit prominent hydrous spectral features at 1.4, 1.9, and 2.2 micrometers; and these are observed weakly, if at all, in reflectance spectra of Mars. However, several mechanisms can weaken or compress these features, including desiccation under low-humidity conditions. The hydration properties of the interlayer cations also effect band strengths, such that a ferrihydrite-bearing smectite in the Martian environment would exhibit a 1.9 micrometers H2O absorption that is even weaker than the 2.2 micrometers structural OH absorption. Mixing experiments demonstrate that infrared spectral features of clays can be significantly suppressed and that the reflectance can be significantly darkened by mixing with only a few percent of a strongly absorbing opaque material. Therefore, the absolute reflectance of a soil on Mars may be disproportionately sensitive to a minor component. For this reason, the shape and position of spectral features and the chemical composition of potential analogs are of utmost importance in assessing the composition of the soil on Mars. Given the remarkable similarity between visible-infrared reflectance spectra of soils in bright regions on Mars and Fe(3+)-doped montmorillonites, coupled with recent observations of smectites in SNC meteorites and a weak 2.2 micrometers absorption in some Mars soils, ferrihydrite-bearing smectites warrant serious consideration as a Mars soil analog.
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Affiliation(s)
- J L Bishop
- Department of Chemistry, Brown University, Providence, RI 02912, USA
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90
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Clifford SM. A model for the hydrologic and climatic behavior of water on Mars. ACTA ACUST UNITED AC 1993. [DOI: 10.1029/93je00225] [Citation(s) in RCA: 555] [Impact Index Per Article: 17.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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91
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Moll DM, Vestal JR. Survival of microorganisms in smectite clays: implications for Martian exobiology. ICARUS 1992; 98:233-239. [PMID: 11539360 DOI: 10.1016/0019-1035(92)90092-l] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
Manned exploration of Mars may result in the contamination of that planet with terrestrial microbes, a situation requiring assessment of the survival potential of possible contaminating organisms. In this study, the survival of Bacillius subtilis, Azotobacter chroococcum, and the enteric bacteriophage MS2 was examined in clays representing terrestrial (Wyoming type montmorillonite) or Martian (Fe(3+)-montmorillonite) soils exposed to terrestrial and Martian environmental conditions of temperature and atmospheric pressure and composition, but not to UV flux or oxidizing conditions. Survival of bacteria was determined by standard plate counts and biochemical and physiological measurements over 112 days. Extractable lipid phosphate was used to measure microbial biomass, and the rate of 14C-acetate incorporation into microbial lipids was used to determine physiological activity. MS2 survival was assayed by plaque counts. Both bacterial types survived terrestrial or Martian conditions in Wyoming montmorillonite better than Martian conditions in Fe(3+)-montmorillonite. Decreased survival may have been caused by the lower pH of the Fe(3+)-montmorillonite compared to Wyoming montmorillonite. MS2 survived simulated Mars conditions better than the terrestrial environment, likely due to stabilization of the virus caused by the cold and dry conditions of the simulated Martian environment. The survival of MS2 in the simulated Martian environment is the first published indication that viruses may be able to survive in Martian type soils. This work may have implications for planetary protection for future Mars missions.
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Affiliation(s)
- D M Moll
- Department of Biological Sciences, University of Cincinnati, Ohio 45221-0006, USA
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92
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Knudsen JM, Madsen MB, Olsen M, Vistisen L, Koch CB, Mørup S, Kankeleit E, Klingelhöfer G, Evlanov EN, Khromov VN, Mukhin LM, Prilutski OF, Zubkov B, Smirnov GV, Juchniewicz J. Mössbauer spectroscopy on the surface of Mars. Why? ACTA ACUST UNITED AC 1992. [DOI: 10.1007/bf02396454] [Citation(s) in RCA: 26] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/30/2022]
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93
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Haynes RH, McKay CP. The implantation of life on Mars: feasibility and motivation. ADVANCES IN SPACE RESEARCH : THE OFFICIAL JOURNAL OF THE COMMITTEE ON SPACE RESEARCH (COSPAR) 1992; 12:133-140. [PMID: 11538133 DOI: 10.1016/0273-1177(92)90167-v] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
Environmental conditions on Mars are extremely hostile, and would be destructive to any organisms which might arrive there unprotected to-day. However, it is a biocompatible planet. Its unalterable astrophysical parameters would allow the maintenance of a much thicker, warmer carbon dioxide atmosphere than that which currently exists. Though very cold (averaging about -60 degrees C), highly oxidizing and desiccated, Mars may possess substantial quantities of the materials needed to support life--in particular, water and carbon dioxide. A general scenario for implanting life on Mars would include three main phases: (1) robotic and human exploration to determine whether sufficiently large and accessible volatile inventories are available; (2) planetary engineering designed to warm the planet, release liquid water and produce a thick carbon dioxide atmosphere; and (3) if no indigenous Martian organisms emerge as liquid water becomes available, a program of biological engineering designed to construct and implant pioneering microbial communities able to proliferate in the newly clement, though still anaerobic, Martian environment. The process of establishing an ecosystem, or biosphere, on a lifeless planet is best termed 'ecopoiesis.' This new word, derived from Greek, means 'the making of an abode for life.' It is by no means clear whether ecopoiesis on Mars is scientifically possible or technologically achievable. Thus we urge that it be one of the objectives of space research during the next century to assess the feasibility of ecopoiesis on Mars.
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Affiliation(s)
- R H Haynes
- Department of Biology, York University, Toronto, Canada
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94
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Crisp J, Bartholomew MJ. Mid-infrared spectroscopy of Pahala ash palagonite and implications for remote sensing studies of Mars. ACTA ACUST UNITED AC 1992. [DOI: 10.1029/92je01248] [Citation(s) in RCA: 24] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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95
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Abstract
Mars is believed to be lifeless, but it may be possible to transform it into a planet suitable for habitation by plants, and conceivably humans. The success of such an enterprise would depend on the abundance, distribution and form of materials on the planet that could provide carbon dioxide, water and nitrogen.
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Affiliation(s)
- C P McKay
- Space Science Division, NASA Ames Research Center, Moffett Field, California 94035, USA
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96
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Clark RN, Swayze GA, Singer RB, Pollack JB. High-resolution reflectance spectra of Mars in the 2.3-μm region: Evidence for the mineral scapolite. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/jb095ib09p14463] [Citation(s) in RCA: 68] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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97
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Zent AP, Fanale FP, Roth LE. Possible Martian brines: Radar observations and models. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/jb095ib09p14531] [Citation(s) in RCA: 16] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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98
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Coey JMD, Mørup S, Madsen MB, Knudsen JM. Titanomaghemite in magnetic soils on Earth and Mars. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/jb095ib09p14423] [Citation(s) in RCA: 38] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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99
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Burns RG, Fisher DS. Iron-sulfur mineralogy of Mars: Magmatic evolution and chemical weathering products. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/jb095ib09p14415] [Citation(s) in RCA: 87] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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100
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Bell JF, McCord TB, Owensby PD. Observational evidence of crystalline iron oxides on Mars. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/jb095ib09p14447] [Citation(s) in RCA: 136] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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