The instrumental blank of the Mars Science Laboratory alpha particle X-ray spectrometer

Campbell, John L.

doi:10.1016/j.nimb.2012.07.032

Cited by 6 publications

(6 citation statements)

References 14 publications

(23 reference statements)

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“…The APXS is located on the arm of the rover and is placed in close proximity or in direct contact with rock target surfaces, which enables the analysis of the elemental composition of rocks within a ~1.6 cm diameter circle. The composition of major, minor, and trace elements (Si, Ti, Al, Fe, Mg, Ca, Na, K, Mn, S, P, Cl, Br, Cr, Zn, Cu, and Ge) has been calibrated based on more than 450 geochemical reference materials that were analyzed within the APXS calibration chamber (Campbell, 2012; Gellert et al, 2013). During the first 750 sols, 112 rocks were analyzed by APXS, and their compositions were reported by Siebach et al (2017).…”

Section: Methodsmentioning

confidence: 99%

“…The second challenge in characterizing igneous rock types on Mars is obtaining a representative bulk composition for igneous classification. Terrestrial studies can use various approaches like small melt inclusions and/or large‐scale compositional surveys to determine magma compositions and classify igneous rocks, but Curiosity is limited to compositions obtained by the laser‐induced breakdown spectrometer (LIBS) from the ChemCam suite, which typically includes <20 points that are 350–550 μm in diameter on a given rock (Maurice et al, 2016), and the Alpha‐Particle X‐ray Spectrometer (APXS) instrument, which measures the surface composition of a circle of 1.6 cm diameter for each rock (Campbell, 2012). LIBS has the advantage of being able to blast away surface dust and any surface coatings, but the disadvantage of a small spot size that does not represent average chemistry, especially for heterogeneous rocks such as coarse‐grained cumulates (Cousin et al, 2017; Sautter et al, 2014).…”

Section: Introductionmentioning

confidence: 99%

“…LIBS has the advantage of being able to blast away surface dust and any surface coatings, but the disadvantage of a small spot size that does not represent average chemistry, especially for heterogeneous rocks such as coarse-grained cumulates (Cousin et al, 2017;Sautter et al, 2014). APXS integrates over a larger spot size than LIBS but it is sensitive to dust cover or surface alteration, especially for light elements (Campbell, 2012;Schmidt et al, 2018). Compounding these difficulties, the only candidate igneous rocks observed by Curiosity have been floats with few measurements per rock, and the most compelling are feldspathic cumulates, which are heterogeneous on a larger scale than available rover measurements ( Figure 1; Sautter et al, 2014Sautter et al, , 2015.…”

Section: Introductionmentioning

confidence: 99%

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Constraining Ancient Magmatic Evolution on Mars Using Crystal Chemistry of Detrital Igneous Minerals in the Sedimentary Bradbury Group, Gale Crater, Mars

et al. 2020

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Understanding magmatic processes is critical to understanding Mars as a system, but Curiosity's investigation of dominantly sedimentary rocks has made it difficult to constrain igneous processes. Igneous classification of float rocks is challenging because of the following: (1) the possibility that they have been affected by sedimentary processes or weathering, and (2) grain size heterogeneity in the observed rock textures makes the small‐scale compositions measured by rover instruments unreliable for bulk classification. We avoid these ambiguities by using detrital igneous mineral chemistry to constrain models of magmatic processes in the source region for the fluvio‐deltaic Bradbury group. Mineral chemistry is obtained from X‐ray diffraction of three collected samples and a new stoichiometric and visual filtering of ~5,000 laser induced breakdown spectroscopy (LIBS) spots to identify compositions of individual igneous minerals. Observed mineral chemistries are compared to those produced by MELTS thermodynamic modeling to constrain possible magmatic conditions. Fractionation of two starting primary melts derived from different extent of adiabatic decompression melting of a primitive mantle composition could result in the crystallization of all minerals observed. Crystal fractionation of a subalkaline and an alkaline magma is required to form the observed minerals. These results are consistent with the collection of alkaline and subalkaline rocks from Gale as well as clasts from the Martian meteorite Northwest Africa 7034 and paired stones. This new method for constraining magmatic processes will be of significant interest for the Mars 2020 mission, which will also investigate an ancient volcaniclastic‐sedimentary environment and will include a LIBS instrument.

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Section: Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Constraining Ancient Magmatic Evolution on Mars Using Crystal Chemistry of Detrital Igneous Minerals in the Sedimentary Bradbury Group, Gale Crater, Mars

et al. 2020

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“…Two emission spectroscopy instruments on the rover analyze the chemical composition of rocks and soils: the Chemistry Camera (ChemCam) and the Alpha‐Particle X‐ray Spectrometer (APXS) [ Campbell , ]. Major, minor, and trace elements are quantified by both instruments.…”

Section: Introductionmentioning

confidence: 99%

“…This very soluble element can be associated with both alkali and Mg-Fe phases such as pyroxene and feldspar. These observations of Li, Sr, Rb, and Ba mineralogical associations highlight their substitution with potassium and their incompatibility in magmatic melts.Two emission spectroscopy instruments on the rover analyze the chemical composition of rocks and soils: the Chemistry Camera (ChemCam) and the Alpha-Particle X-ray Spectrometer (APXS) [Campbell, 2012]. Major, minor, and trace elements are quantified by both instruments.…”

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confidence: 99%

Alkali trace elements in Gale crater, Mars, with ChemCam: Calibration update and geological implications

et al. 2017

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The Chemistry Camera (ChemCam) instrument onboard Curiosity can detect minor and trace elements such as lithium, strontium, rubidium, and barium. Their abundances can provide some insights about Mars' magmatic history and sedimentary processes. We focus on developing new quantitative models for these elements by using a new laboratory database (more than 400 samples) that displays diverse compositions that are more relevant for Gale crater than the previous ChemCam database. These models are based on univariate calibration curves. For each element, the best model is selected depending on the results obtained by using the ChemCam calibration targets onboard Curiosity. New quantifications of Li, Sr, Rb, and Ba in Gale samples have been obtained for the first 1000 Martian days. Comparing these data in alkaline and magnesian rocks with the felsic and mafic clasts from the Martian meteorite NWA7533—from approximately the same geologic period—we observe a similar behavior: Sr, Rb, and Ba are more concentrated in soluble‐ and incompatible‐element‐rich mineral phases (Si, Al, and alkali‐rich). Correlations between these trace elements and potassium in materials analyzed by ChemCam reveal a strong affinity with K‐bearing phases such as feldspars, K‐phyllosilicates, and potentially micas in igneous and sedimentary rocks. However, lithium is found in comparable abundances in alkali‐rich and magnesium‐rich Gale rocks. This very soluble element can be associated with both alkali and Mg‐Fe phases such as pyroxene and feldspar. These observations of Li, Sr, Rb, and Ba mineralogical associations highlight their substitution with potassium and their incompatibility in magmatic melts.

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Geochemical diversity in first rocks examined by the Curiosity Rover in Gale Crater: Evidence for and significance of an alkali and volatile‐rich igneous source

et al. 2014

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[1] The first four rocks examined by the Mars Science Laboratory Alpha Particle X-ray Spectrometer indicate that Curiosity landed in a lithologically diverse region of Mars. These rocks, collectively dubbed the Bradbury assemblage, were studied along an eastward traverse (sols 46-102). Compositions range from Na-and Al-rich mugearite Jake_Matijevic to Fe-, Mg-, and Zn-rich alkali-rich basalt/hawaiite Bathurst_Inlet and span nearly the entire range in FeO* and MnO of the data sets from previous Martian missions and Martian meteorites. The Bradbury assemblage is also enriched in K and moderately volatile metals (Zn and Ge). These elements do not correlate with Cl or S, suggesting that they are associated with the rocks themselves and not with salt-rich coatings. Three out of the four Bradbury rocks plot along a line in elemental variation diagrams, suggesting mixing between Al-rich and Fe-rich components. ChemCam analyses give insight to their degree of chemical heterogeneity and grain size. Variations in trace elements detected by ChemCam suggest chemical weathering (Li) and concentration in mineral phases (e.g., Rb and Sr in feldspars). We interpret the Bradbury assemblage to be broadly volcanic and/or volcaniclastic, derived either from near the Gale crater rim and transported by the Peace Vallis fan network, or from a local volcanic source within Gale Crater. High Fe and Fe/Mn in Et_Then likely reflect secondary precipitation of Fe 3+ oxides as a cement or rind. The K-rich signature of the Bradbury assemblage, if igneous in origin, may have formed by small degrees of partial melting of metasomatized mantle. , et al. (2014), Geochemical diversity in first rocks examined by the Curiosity Rover in Gale Crater: Evidence for and significance of an alkali and volatile-rich igneous source,

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The instrumental blank of the Mars Science Laboratory alpha particle X-ray spectrometer

Cited by 6 publications

References 14 publications

Constraining Ancient Magmatic Evolution on Mars Using Crystal Chemistry of Detrital Igneous Minerals in the Sedimentary Bradbury Group, Gale Crater, Mars

Constraining Ancient Magmatic Evolution on Mars Using Crystal Chemistry of Detrital Igneous Minerals in the Sedimentary Bradbury Group, Gale Crater, Mars

Alkali trace elements in Gale crater, Mars, with ChemCam: Calibration update and geological implications

Geochemical diversity in first rocks examined by the Curiosity Rover in Gale Crater: Evidence for and significance of an alkali and volatile‐rich igneous source

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