The Mars Science Laboratory Organic Check Material

Conrad, Pamela G.; Eigenbrode, J. L.; Heydt, Max O. Von der; Mogensen, C.; Canham, John S.; Harpold, D. N.; Johnson, Joel A.; Errigo, Therese; Glavin, Daniel P.; Mahaffy, P. R.

doi:10.1007/s11214-012-9893-1

Cited by 15 publications

(11 citation statements)

References 12 publications

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“…FeSO 4 •4H 2 O (Sigma‐Aldrich, product # F8048, batch # 048K0680) and CaCO 3 (calcite — Sigma‐Aldrich, standard A.C.S. reagent, product #398101, batch # 16826BH) were mixed with fused silica (FS‐120 from HP technical ceramics [see Conrad et al ., ]) that had been crushed and sieved to collect the 20–150 µm size fraction and baked at 550°C for 2 h in air to remove organic contamination. During pyrolysis, these samples thermally decomposed and released H 2 O and SO 2 from the FeSO 4 •4H 2 O and CO 2 from calcite, shown in the reactions:

{FeSO}_{4} • 4 {normalH}_{2} O \to {FeSO}_{4} + 4 {normalH}_{2} O

followed by

{FeSO}_{4} \to FeO + {SO}_{2} + ½ {normalO}_{2}

and

{CaCO}_{3} \to CaO + {CO}_{2}

…”

Section: Experimental Methodsmentioning

confidence: 99%

Abundances and implications of volatile‐bearing species from evolved gas analysis of the Rocknest aeolian deposit, Gale Crater, Mars

et al. 2014

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The Sample Analysis at Mars (SAM) instrument on the Mars Science Laboratory (MSL) roverCuriosity detected evolved gases during thermal analysis of soil samples from the Rocknest aeolian deposit in Gale Crater. Major species detected (in order of decreasing molar abundance) were H 2 O, SO 2 , CO 2 , and O 2 , all at the μmol level, with HCl, H 2 S, NH 3 , NO, and HCN present at the tens to hundreds of nmol level. We compute weight % numbers for the major gases evolved by assuming a likely source and calculate abundances between 0.5 and 3 wt.%. The evolution of these gases implies the presence of both oxidized (perchlorates) and reduced (sulfides or H-bearing) species as well as minerals formed under alkaline (carbonates) and possibly acidic (sulfates) conditions. Possible source phases in the Rocknest material are hydrated amorphous material, minor clay minerals, and hydrated perchlorate salts (all potential H 2 O sources), carbonates (CO 2 ), perchlorates (O 2 and HCl), and potential N-bearing materials (e.g., Martian nitrates, terrestrial or Martian nitrogenated organics, ammonium salts) that evolve NH 3 , NO, and/or HCN. We conclude that Rocknest materials are a physical mixture in chemical disequilibrium, consistent with aeolian mixing, and that although weathering is not extensive, it may be ongoing even under current Martian surface conditions.

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{FeSO}_{4} • 4 {normalH}_{2} O \to {FeSO}_{4} + 4 {normalH}_{2} O

followed by

{FeSO}_{4} \to FeO + {SO}_{2} + ½ {normalO}_{2}

and

{CaCO}_{3} \to CaO + {CO}_{2}

…”

Section: Experimental Methodsmentioning

confidence: 99%

Abundances and implications of volatile‐bearing species from evolved gas analysis of the Rocknest aeolian deposit, Gale Crater, Mars

et al. 2014

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“…Any contamination of the sample should be at or below the sensitivity suggested for the instrumentation: 1 ppb both for complex organic contaminants and for inorganic contaminants. This desired cleanliness level-for the samples and the sample handling system-is about an order of magnitude more stringent than that required of the sample handling equipment on the Mars Phoenix ( < 10 ppb) and Curiosity ( < 40 ppb) missions (Ming et al, 2008;Conrad et al, 2012).…”

Section: Investigating Compositionmentioning

confidence: 99%

Science Potential from a Europa Lander

et al. 2013

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The prospect of a future soft landing on the surface of Europa is enticing, as it would create science opportunities that could not be achieved through flyby or orbital remote sensing, with direct relevance to Europa's potential habitability. Here, we summarize the science of a Europa lander concept, as developed by our NASA-commissioned Science Definition Team. The science concept concentrates on observations that can best be achieved by in situ examination of Europa from its surface. We discuss the suggested science objectives and investigations for a Europa lander mission, along with a model planning payload of instruments that could address these objectives. The highest priority is active sampling of Europa's non-ice material from at least two different depths (0.5-2 cm and 5-10 cm) to understand its detailed composition and chemistry and the specific nature of salts, any organic materials, and other contaminants. A secondary focus is geophysical prospecting of Europa, through seismology and magnetometry, to probe the satellite's ice shell and ocean. Finally, the surface geology can be characterized in situ at a human scale. A Europa lander could take advantage of the complex radiation environment of the satellite, landing where modeling suggests that radiation is about an order of magnitude less intense than in other regions. However, to choose a landing site that is safe and would yield the maximum science return, thorough reconnaissance of Europa would be required prior to selecting a scientifically optimized landing site.

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“…The ionization rate caused by the cosmic rays, galactic or solar, is also of interest for studying ground‐level chemistry. Chemical measurements performed at the surface of Mars have yet to detect organic materials [ Kolb , ], which is an objective of Curiosity [ Conrad et al , ]. It is assumed that chemical reactions at the Martian surface caused the depletion of organic materials, and that drilling, an operation performed by Curiosity, will permit discovering these species.…”

Section: Introductionmentioning

confidence: 99%

Influence of dust loading on atmospheric ionizing radiation on Mars

2014

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Measuring the radiation environment at the surface of Mars is the primary goal of the Radiation Assessment Detector on the NASA Mars Science Laboratory's Curiosity rover. One of the conditions that Curiosity will likely encounter is a dust storm. The objective of this paper is to compute the cosmic ray ionization in different conditions, including dust storms, as these various conditions are likely to be encountered by Curiosity at some point. In the present work, the Nowcast of Atmospheric Ionizing Radiation for Aviation Safety model, recently modified for Mars, was used along with the Badhwar & O'Neill 2010 galactic cosmic ray model. In addition to galactic cosmic rays, five different solar energetic particle event spectra were considered. For all input radiation environments, radiation dose throughout the atmosphere and at the surface was investigated as a function of atmospheric dust loading. It is demonstrated that for galactic cosmic rays, the ionization depends strongly on the atmosphere profile. Moreover, it is shown that solar energetic particle events strongly increase the ionization throughout the atmosphere, including ground level, and can account for the radio blackout conditions observed by the Mars Advanced Radar for Subsurface and Ionospheric Sounding instrument on the Mars Express spacecraft. These results demonstrate that the cosmic rays' influence on the Martian surface chemistry is strongly dependent on solar and atmospheric conditions that should be taken into account for future studies.

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The Mars Science Laboratory Organic Check Material

Cited by 15 publications

References 12 publications

Abundances and implications of volatile‐bearing species from evolved gas analysis of the Rocknest aeolian deposit, Gale Crater, Mars

Abundances and implications of volatile‐bearing species from evolved gas analysis of the Rocknest aeolian deposit, Gale Crater, Mars

Science Potential from a Europa Lander

Influence of dust loading on atmospheric ionizing radiation on Mars

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