Isotopic links between atmospheric chemistry and the deep sulphur cycle on Mars

Franz, H. B.; Kim, Sang‐Tae; Farquhar, James; Day, James M.D.; Economos, Rita C.; McKeegan, Kevin D.; Schmitt, Axel K.; Irving, A. J.; Hoek, Joost; Dottin, James W.

doi:10.1038/nature13175

Cited by 97 publications

(207 citation statements)

References 31 publications

(41 reference statements)

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“…Sulfur concentrations in Tissint and Zagami from this study agrees well with those from previous studies (Aoudjehane et al, 2012;Gibson et al, 1985). However, bulk S concentrations of Los Angeles and Zagami from this study are both higher than the total S reported in Franz et al (2014). Also bulk S concentration of Nakhla from this study is higher than most of the ones reported from previous studies (Banin et al, 1992;Burgess et al, 1989;Gibson et al, 1985).…”

Section: Comparison With Previous Bulk Sulfur Data Of Martian Meteoritessupporting

confidence: 90%

“…Our new measurements of shergottites' and nakhlites' bulk sulfur data fall in the range of bulk S from the previous studies (Banin et al, 1992;Burgess et al, 1989;Burghele et al, 1983;Dreibus et al, 1994Dreibus et al, , 1992Dreibus et al, , 1982Franz et al, 2014;Gibson et al, 1985;Lodders, 1998;McSween and Jarosewich, 1983;Sarbadhikari et al, 2009;Zipfel et al, 2000). Sulfur concentrations of Los Angeles, Zagami, Nakhla and Tissint have been measured in previous studies (Aoudjehane et al, 2012;Banin et al, 1992;Burgess et al, 1989;Franz et al, 2014;Gibson et al, 1985;Dreibus et al, 1982).…”

Section: Comparison With Previous Bulk Sulfur Data Of Martian Meteoritesmentioning

confidence: 65%

“…Sulfur concentrations of Los Angeles, Zagami, Nakhla and Tissint have been measured in previous studies (Aoudjehane et al, 2012;Banin et al, 1992;Burgess et al, 1989;Franz et al, 2014;Gibson et al, 1985;Dreibus et al, 1982). Sulfur concentrations in Tissint and Zagami from this study agrees well with those from previous studies (Aoudjehane et al, 2012;Gibson et al, 1985).…”

Section: Comparison With Previous Bulk Sulfur Data Of Martian Meteoritesmentioning

confidence: 95%

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New bulk sulfur measurements of Martian meteorites and modeling the fate of sulfur during melting and crystallization – Implications for sulfur transfer from Martian mantle to crust–atmosphere system

Ding

Dasgupta

Lee

et al. 2015

Earth and Planetary Science Letters

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Section: Comparison With Previous Bulk Sulfur Data Of Martian Meteoritessupporting

confidence: 90%

Section: Comparison With Previous Bulk Sulfur Data Of Martian Meteoritesmentioning

confidence: 65%

Section: Comparison With Previous Bulk Sulfur Data Of Martian Meteoritesmentioning

confidence: 95%

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New bulk sulfur measurements of Martian meteorites and modeling the fate of sulfur during melting and crystallization – Implications for sulfur transfer from Martian mantle to crust–atmosphere system

Ding

Dasgupta

Lee

et al. 2015

Earth and Planetary Science Letters

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“…The Δ 33 S (and Δ 36 S) values of the Earth, Moon, and Mars, which are indistinguishable from IAB iron meteorites/bulk chondrites (18,19,37,38), are intermediate between the 33 S-enriched and 33 S-depleted isotopic compositions observed in magmatic irons and achondrites. This implies that the complementary photolytic sulfur isotope signatures captured by these early-formed differentiated protoplanets were either diluted by the later addition of materials with isotopically normal (chondritic/IAB) sulfur or were recombined during the continued accretionary processes that formed the terrestrial planets.…”

Section: Resultsmentioning

confidence: 82%

Early inner solar system origin for anomalous sulfur isotopes in differentiated protoplanets

Antonelli

Kim

Peters

et al. 2014

Proc. Natl. Acad. Sci. U.S.A.

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Achondrite meteorites have anomalous enrichments in 33 S, relative to chondrites, which have been attributed to photochemistry in the solar nebula. However, the putative photochemical reactions remain elusive, and predicted accompanying 33 S depletions have not previously been found, which could indicate an erroneous assumption regarding the origins of the 33 S anomalies, or of the bulk solar system S-isotope composition. Here, we report wellresolved anomalous 33 S depletions in IIIF iron meteorites (<−0.02 per mil), and 33 S enrichments in other magmatic iron meteorite groups. The 33 S depletions support the idea that differentiated planetesimals inherited sulfur that was photochemically derived from gases in the early inner solar system (<∼2 AU), and that bulk inner solar system S-isotope composition was chondritic (consistent with IAB iron meteorites, Earth, Moon, and Mars). The range of mass-independent sulfur isotope compositions may reflect spatial or temporal changes influenced by photochemical processes. A tentative correlation between S isotopes and Hf-W core segregation ages suggests that the two systems may be influenced by common factors, such as nebular location and volatile content.iron meteorites | sulfur isotopes | protoplanetary disk | solar system | photochemistry O f all of the extraterrestrial materials found on Earth, iron meteorites have always been the most conspicuous. Socalled "magmatic" iron meteorites are likely to be samples from the cores of magmatically differentiated protoplanetary parent bodies (1), whereas "nonmagmatic" iron meteorites are commonly suggested to sample solidified melt pockets that formed via impacts onto nondifferentiated (chondritic) parent bodies (2). Individual members from an iron meteorite group are assumed to derive from a common parent body, based on shared chemical and isotopic characteristics (1-4). Chemical and isotopic differences among the different iron groups provide convincing evidence that different individual parent body planetesimals incorporated genetically distinct precursor materials (1-4).Recent observations that several achondrite meteorite groups possess small, mass-independent 33 S enrichments relative to chondrites (5) have led to the conclusion that sulfur isotopes were heterogeneously distributed among the materials that accreted to form early solar system planetesimals. This observation, coupled with the ancient 182 Hf-182 W ages (within 1-3 My of solar system formation) of magmatic irons (6-8), provides impetus to search for systematic variations in mass-independent sulfur isotope compositions among the iron groups. ResultsWe report high-precision δ 34 S, Δ 33 S, and Δ 36 S data (where Δ 33 S = 1000 × {δ 33 S -[(δ 34 S + 1) 0.515 − 1]} and Δ 36 S = 1000 × {δ 36 S -[(δ 34 S + 1) 1.9 − 1]}) for 61 troilite (FeS) nodules extracted from 58 different iron meteorites selected from eight different groups (IAB, IC, IIAB, IIE, IIIAB, IIIF, IVA, and IVB) (Fig. 1, Fig. S1, and Tables S1 and S2). All groups except for IAB and IIE have been classi...

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“…A recent study has revealed a restricted range in δ 34 S for mare basalts of +0.57 ± 0.09 [52], while work to identify mass-independent S fractionation in shergottites indicates an average δ 34 S for martian basalts of −0.05 ± 0.3 [53]. High-precision 34 S/ 32 S data have been obtained for terrestrial mid-ocean ridge basalts (MORB), giving an average δ 34 S of −0.98 ± 0.51 [54,55].…”

Section: Isotopic Fractionation Of Moderately Volatile Elements In Comentioning

confidence: 99%

Evaporative fractionation of volatile stable isotopes and their bearing on the origin of the Moon

Day

Moynier

2014

Phil. Trans. R. Soc. A.

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106

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The Moon is depleted in volatile elements relative to the Earth and Mars. Low abundances of volatile elements, fractionated stable isotope ratios of S, Cl, K and Zn, high μ ( 238 U/ 204 Pb) and long-term Rb/Sr depletion are distinguishing features of the Moon, relative to the Earth. These geochemical characteristics indicate both inheritance of volatile-depleted materials that formed the Moon and planets and subsequent evaporative loss of volatile elements that occurred during lunar formation and differentiation. Models of volatile loss through localized eruptive degassing are not consistent with the available S, Cl, Zn and K isotopes and abundance data for the Moon. The most probable cause of volatile depletion is global-scale evaporation resulting from a giant impact or a magma ocean phase where inefficient volatile loss during magmatic convection led to the present distribution of volatile elements within mantle and crustal reservoirs. Problems exist for models of planetary volatile depletion following giant impact. Most critically, in this model, the volatile loss requires preferential delivery and retention of late-accreted volatiles to the Earth compared with the Moon. Different proportions of late-accreted mass are computed to explain present-day distributions of volatile and moderately volatile elements (e.g. Pb, Zn; 5 to >10%) relative to highly siderophile elements (approx. 0.5%) for the Earth. Models of early magma ocean phases may be more effective in explaining the volatile loss. Basaltic materials (e.g. eucrites and angrites) from highly differentiated airless asteroids are volatile-depleted, like the Moon, whereas the Earth and Mars have proportionally greater volatile contents. Parent-body size and the existence of early atmospheres are therefore likely to represent fundamental controls on planetary volatile retention or loss.

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Isotopic links between atmospheric chemistry and the deep sulphur cycle on Mars

Cited by 97 publications

References 31 publications

New bulk sulfur measurements of Martian meteorites and modeling the fate of sulfur during melting and crystallization – Implications for sulfur transfer from Martian mantle to crust–atmosphere system

New bulk sulfur measurements of Martian meteorites and modeling the fate of sulfur during melting and crystallization – Implications for sulfur transfer from Martian mantle to crust–atmosphere system

Early inner solar system origin for anomalous sulfur isotopes in differentiated protoplanets

Evaporative fractionation of volatile stable isotopes and their bearing on the origin of the Moon

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