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S. P. Kounaves et al., J. Geophys. Res. 113, 10.1029/ 2008JE003084 (2009).
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16
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67650041982
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The onset temperature for this endothermic peak is similar to the calcite decomposition onset temperature of 738°C measured in the TEGA engineering qualification model 17, Other carbonates have decomposition temperatures that are lower than that of calcite
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The onset temperature for this endothermic peak is similar to the calcite decomposition onset temperature of 738°C measured in the TEGA engineering qualification model (17). Other carbonates have decomposition temperatures that are lower than that of calcite.
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17
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67650051280
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In a calibration run on the TEGA engineering qualification model with a known amount of calcite, we found the heat of transition to be 2550 J/g, which implies 2.4 mg of CaCO° in the Wicked Witch sample
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In a calibration run on the TEGA engineering qualification model with a known amount of calcite, we found the heat of transition to be 2550 J/g, which implies 2.4 mg of CaCO° in the Wicked Witch sample.
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18
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67650041984
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Estimation of the concentration of calcium carbonate in the sample is uncertain because the mass of sample in the oven is not tightly constrained. We estimate that this error is on the order of ± 25
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Estimation of the concentration of calcium carbonate in the sample is uncertain because the mass of sample in the oven is not tightly constrained. We estimate that this error is on the order of ± 25%.
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19
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67650030309
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2 to condense out on any plumbing surfaces. The sol 70 run shows that this effect is not due to a background signal.
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2 to condense out on any plumbing surfaces. The sol 70 run shows that this effect is not due to a background signal.
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20
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67650008597
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A martian solar day has a mean period of 24 hours 39 min 35.244 s and is referred to as a sol to distinguish this from a ∼3% shorter solar day on Earth.
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A martian solar day has a mean period of 24 hours 39 min 35.244 s and is referred to as a sol to distinguish this from a ∼3% shorter solar day on Earth.
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22
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17644378913
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J. B. Dixon, D.G. Schulze, SSSA, Madison, WI
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Grossl, P.2
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Zent, A.1
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67650006270
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T. L. Heet, R. E. Arvidson, M. Mellon, Abstr. 1114, 40th Lunar and Planetary Science Conference, The Woodlands, TX, 23 to 27 March 2009.
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T. L. Heet, R. E. Arvidson, M. Mellon, Abstr. 1114, 40th Lunar and Planetary Science Conference, The Woodlands, TX, 23 to 27 March 2009.
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28
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67650044385
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A previous experiment suggested that carbonate could form in relatively dry Mars-like conditions as submi-crometer coatings on soil particles (5, However, the results from this study cannot be extrapolated over time because the experiments did not proceed beyond a monolayer of carbonate. A more comprehensive experimental study under Mars-like conditions showed that, in a given time span, carbonate forms on the surface of basaltic particles in an amount that increases with the thickness of films of water around the particles (30, 31, Growth of more than a monolayer of carbonate occurs with logarithmic reaction kinetics. For damp or wet conditions (meaning 0.1 to 0.5 g H2O per g soil, equivalent to 102 to 103 monolayers of water, the number of CO2-reacted monolayers of substrate, L, per particle is found empirically to follow the relationship (30, 32) L(t, Dlog101, t/t0, Eq. 1, Here, the constant of proporti
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2 pressures, up to 995 mbar (32).
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29
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67650039609
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H. U. Keller et al., Abstr. 1671, 40th Lunar and Planetary Science Conference, The Woodlands, TX, 23 to 27 March
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H. U. Keller et al., Abstr. 1671, 40th Lunar and Planetary Science Conference, The Woodlands, TX, 23 to 27 March
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31
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67650036515
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S. K. Stephens, thesis, California Institute of Technology, Pasadena (1995).
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S. K. Stephens, thesis, California Institute of Technology, Pasadena (1995).
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Ballou, E.V.1
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35
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67650051275
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We acknowledge the work of the Robotic Arm team in delivering the samples to TEGA and WCL and the contributions of the engineers, scientists, and managers who made these instruments and the analysis of their data possible, including H. Enos, C. Fellows, K. Harshman, M. Finch, M. Williams, M. Fitzgibbon, G. Droege, J. M. Morookian, V. Lauer, D. C. Golden, R. Chaney, H. Hammack, L Brooks, M. Mankey, K. Gospodinova, J. Kapit, C. Cable, P. Chang, E. Coombs, and S. Stroble. The Phoenix Mission was led by the University of Arizona, Tucson, on behalf of NASA and was managed by NASA's Jet Propulsion Laboratory, California Institute of Technology, of Pasadena, CA. The spacecraft was developed by Lockheed Martin Space Systems, Denver
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We acknowledge the work of the Robotic Arm team in delivering the samples to TEGA and WCL and the contributions of the engineers, scientists, and managers who made these instruments and the analysis of their data possible, including H. Enos, C. Fellows, K. Harshman, M. Finch, M. Williams, M. Fitzgibbon, G. Droege, J. M. Morookian, V. Lauer, D. C. Golden, R. Chaney, H. Hammack, L Brooks, M. Mankey, K. Gospodinova, J. Kapit, C. Cable, P. Chang, E. Coombs, and S. Stroble. The Phoenix Mission was led by the University of Arizona, Tucson, on behalf of NASA and was managed by NASA's Jet Propulsion Laboratory, California Institute of Technology, of Pasadena, CA. The spacecraft was developed by Lockheed Martin Space Systems, Denver.
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