Chalcophile elements in Martian meteorites indicate low sulfur content in the Martian interior and a volatile element-depleted late veneer

Wang, Zaicong; Becker, Harry

doi:10.1016/j.epsl.2017.01.023

Cited by 47 publications

(49 citation statements)

References 87 publications

(190 reference statements)

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“…Similarly, we find positive Cu vs Ti correlations in shergottites ( Fig. A14), except for some anomalously high Cu/Ti samples (Cu/Ti > 0.005), and their average Cu/Ti value (0.0026 ± 0.0005) yields 2.6 ± 0.6 ppm Cu is in the BSM, which is comparable to the estimate by Wang and Becker (2017).…”

Section: Moderately Volatile Siderophile Elementssupporting

confidence: 87%

“…e Filiberto et al (2016); this study. f Wang and Becker (2017). g Taylor et al (2006a,b); this study.…”

Section: Conclusion and Implications For Future Worksupporting

confidence: 48%

“…Their average P/Y value in shergottites (0.021 ± 0.005) is used to estimate the P 2 O 5 at 0.17 ± 0.05 wt% in the BSM. Wang and Becker (2017) estimated Cu in the BSM abundance at 2.0 ± 0.4 ppm, based on Cu and MgO correlations in shergottites. Similarly, we find positive Cu vs Ti correlations in shergottites ( Fig.…”

Section: Moderately Volatile Siderophile Elementsmentioning

confidence: 99%

“…There is a wide range of estimates for the abundances of S-Se-Te in the BSM (Franz et al, 2019;Wang and Becker, 2017 and references therein). The limited variation in S/Se/Te ratios indicates little degassing loss of S, Se and Te, which lead Wang and Becker (2017) to derive the BSM abundance of these elements at 360 ± 120 ppm, 100 ± 27 ppb and 0.50 ± 0.25 ppb, respectively. Here we adopt their estimates.…”

Section: Moderately Volatile Chalcophile Elementsmentioning

confidence: 99%

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The composition of Mars

Yoshizaki

McDonough

2020

Geochimica et Cosmochimica Acta

150

154

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Comparing compositional models of the terrestrial planets provides insights into physicochemical processes that produced planet-scale similarities and differences. The widely accepted compositional model for Mars assumes Mn and more refractory elements are in CI chondrite proportions in the planet, including Fe, Mg, and Si, which along with O make up >90% the mass of Mars. However, recent improvements in our understandings on the composition of the solar photosphere and meteorites challenge the use of CI chondrite as an analog of Mars. Here we present an alternative model composition for Mars that avoids such an assumption and is based on data from Martian meteorites and spacecraft observations. Our modeling method was previously applied to predict the Earth's composition. The model establishes the absolute abundances of refractory lithophile elements in the bulk silicate Mars (BSM) at 2.26 times higher than that in CI carbonaceous chondrites. Relative to this chondritic composition, Mars has a systematic depletion in moderately volatile lithophile elements as a function of their condensation temperature. Given this finding, we constrain the abundances of siderophile and chalcophile elements in the bulk Mars and its core. The Martian volatility trend is consistent with ≤7 wt% S in its core, which is significantly lower than that assumed in most core models (i.e., >10 wt% S). Occurrence of ringwoodite at the Martian core-mantle boundary might have contributed to the partitioning of O and H into the Martian core.

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Section: Moderately Volatile Siderophile Elementssupporting

confidence: 87%

“…e Filiberto et al (2016); this study. f Wang and Becker (2017). g Taylor et al (2006a,b); this study.…”

Section: Conclusion and Implications For Future Worksupporting

confidence: 48%

Section: Moderately Volatile Siderophile Elementsmentioning

confidence: 99%

Section: Moderately Volatile Chalcophile Elementsmentioning

confidence: 99%

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The composition of Mars

Yoshizaki

McDonough

2020

Geochimica et Cosmochimica Acta

150

154

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“…Modeling investigations should consider hydrogen as a likely constituent of the core, which may affect the dynamical regimes for an iron/sulfur core (Davies & Pommier, 2018). Hydrogen substitutes for sulfur as a light element to match geodetic and dynamical constraints (Gudkova & Zharkov, 2004), which is perhaps desirable given evidence that sulfur could be less abundant than typically assumed (Wang & Becker, 2017)-closer to the <5 wt% expected for Earth's core from cosmochemical and mineral physics constraints (Dreibus & Palme, 1996;Mahan et al, 2017;Suer et al, 2017). Hydrogen also depresses the solidus (Shibazaki et al, 2011), helping to explain why the core remains at least partially liquid today (Gudkova & Zharkov, 2004;Yoder et al, 2003).…”

Section: Behavior Of Hydrogen In the Mantle And Corementioning

confidence: 99%

Hydrogenation of the Martian Core by Hydrated Mantle Minerals With Implications for the Early Dynamo

O’Rourke

Shim

2019

JGR Planets

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Mars lacks an internally generated magnetic field today. Crustal remanent magnetism and meteorites indicate that a dynamo existed after accretion but died roughly four billion years ago. Standard models rely on core/mantle heat flow dropping below the adiabatic limit for thermal convection in the core. However, rapid core cooling after the Noachian is favored instead to produce long‐lived mantle plumes and magmatism at volcanic provinces such as Tharsis and Elysium. Hydrogenation of the core could resolve this apparent contradiction by impeding the dynamo while core/mantle heat flow is superadiabatic. Here we present parameterized models for the rate at which mantle convection delivers hydrogen into the core. Our models suggest that most of the water that the mantle initially contained was effectively lost to the core. We predict that the mantle became increasingly ironrich over time and a stratified layer awaits detection in the uppermost core—analogous to the E′ layer atop Earth's core but likely thicker than alternative sources of stratification in the Martian core such as iron snow. Entraining buoyant, hydrogen‐rich fluid downward in the core subtracts gravitational energy from the total dissipation budget for the dynamo. The calculated fluxes of hydrogen are high enough to potentially reduce the lifetime of the dynamo by several hundred million years or longer relative to conventional model predictions. Future work should address the complicated interactions between the stratified, hydrogen‐rich layer and convection in the underlying core.

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Chemical Sample Processing for Combined Selenium Isotope and Selenium‐Tellurium Elemental Investigation of the Earth's Igneous Reservoirs

Yierpan

König

Labidi

et al. 2018

Geochem Geophys Geosyst

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The redox‐sensitive, chalcophile, and volatile Se stable isotope system offers new perspectives to investigate the origin and evolution of terrestrial volatiles and the roles of magmatic and recycling processes in the development of the redox contrast between Earth's reservoirs. Selenium isotope systematics become more robust in a well‐constrained petrogenetic context as can be inferred from Se‐Te elemental signatures of sulfides and igneous rocks. In this study, we present a high‐yield chemical sample processing method that allows the determination of Se‐Te concentrations and Se isotope composition from the same sample digest of silicate rocks by hydride generation isotope dilution (ID) quadrupole inductively coupled plasma mass spectrometry (ICP‐MS) and double spike (DS) multicollector (MC)‐ICP‐MS, respectively. Our procedure yields ∼80% Se‐Te recoveries with quantitative separation of relevant interfering elements such as Ge and HG‐buffering metals. Replicate analyses of selected international reference materials yield uncertainties better than 0.11‰ (2 s.d.) on δ82/76Se and 3% (r.s.d.) on Se concentration for DS MC‐ICP‐MS determinations for as low as ∼10 ng sample Se. The precision of Se‐Te concentration measurements by ID ICP‐MS is better than 3% and 5% (r.s.d.) for total amounts of ∼0.5–1 ng Se and ∼0.2–0.5 ng Te, respectively. The basaltic reference materials have variable Se‐Te contents, but their δ82/76Se values are rather uniform (on average 0.23 ± 0.14‰; 2 s.d.) and different from the chondritic value. This altogether provides the methodology and potential to extend the limited data set of coupled Se isotope and Se‐Te elemental systematics of samples relevant to study the terrestrial igneous inventory.

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Chalcophile elements in Martian meteorites indicate low sulfur content in the Martian interior and a volatile element-depleted late veneer

Cited by 47 publications

References 87 publications

The composition of Mars

The composition of Mars

Hydrogenation of the Martian Core by Hydrated Mantle Minerals With Implications for the Early Dynamo

Chemical Sample Processing for Combined Selenium Isotope and Selenium‐Tellurium Elemental Investigation of the Earth's Igneous Reservoirs

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