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  • 1
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    Paired nakhlites MIL 090030, 090032, 090136, and 03346: Insights into the Miller Range parent meteorite : Paired Miller Range nakhlites
    Wiley ; 2012
    In:  Meteoritics & Planetary Science Vol. 47, No. 10 ( 2012-10), p. 1575-1589
    Details
    In: Meteoritics & Planetary Science, Wiley, Vol. 47, No. 10 ( 2012-10), p. 1575-1589
    Type of Medium: Online Resource
    ISSN: 1086-9379
    URL: Article
    DOI: 10.1111/j.1945-5100.2012.01420.x
    Language: English
    Publisher: Wiley
    Publication Date: 2012
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  • 2
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    The effects of highly reduced magmatism revealed through aubrites
    Wiley ; 2022
    In:  Meteoritics & Planetary Science Vol. 57, No. 7 ( 2022-07), p. 1387-1420
    Details
    In: Meteoritics & Planetary Science, Wiley, Vol. 57, No. 7 ( 2022-07), p. 1387-1420
    Abstract: Enstatite‐rich meteorites, including the aubrites, formed under conditions of very low oxygen fugacity (ƒO 2 : iron‐wüstite buffer −2 to −6) and thus offer the ability to study reduced magmatism present on multiple bodies in our solar system. Elemental partitioning among metals, sulfides, and silicates is poorly constrained at low ƒO 2 ; however, studies of enstatite‐rich meteorites may yield empirical evidence of the effects of low ƒO 2 on elemental behavior. This work presents comprehensive petrologic and oxygen isotopic studies of 14 aubrites, including four meteorites that have not been previously investigated in detail. The aubrites exhibit a variety of textures and mineralogy, and their elemental zoning patterns point to slow cooling histories for all 14 samples. Oxygen isotope analyses suggest that the aubrite parent bodies may be more heterogeneous than originally reported or may have experienced incomplete magmatic differentiation. Contrary to the other classified aubrites and based on textural and mineralogical observations, we suggest that the Northwest Africa 8396 meteorite shows an affinity for an enstatite chondrite parentage. By measuring major elemental compositions of silicates, sulfides, and metals, we calculate new metal–silicate, sulfide–silicate, and sulfide–metal partition coefficients for aubrites that are applicable to igneous systems at low ƒO 2 . The geochemical behavior of elements in aubrites, as determined using partition coefficients, is similar to the geochemical behavior of elements determined experimentally for magmatic systems on Mercury. Enstatite‐rich meteorites, including aubrites, represent valuable natural petrologic analogues to Mercury and their study could further our understanding of reduced magmatism in our solar system.
    Type of Medium: Online Resource
    ISSN: 1086-9379 , 1945-5100
    URL: Issue
    URL: Article
    DOI: 10.1111/maps.v57.7
    DOI: 10.1111/maps.13823
    Language: English
    Publisher: Wiley
    Publication Date: 2022
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  • 3
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    The formation of volatile‐bearing djerfisherite in reduced meteorites
    Wiley ; 2024
    In:  Meteoritics & Planetary Science
    Details
    In: Meteoritics & Planetary Science, Wiley
    Abstract: Enstatite meteorites, both aubrites and enstatite chondrites, formed under exceptionally reducing conditions, similar to the planet Mercury. Despite being reduced, the MESSENGER mission showed that the surface of Mercury is more enriched in volatiles (e.g., S, Na, K, Cl) than previously thought. To better understand the mineral hosts of these volatiles and how they formed, this work examines the chemistry and petrographic settings of a rare, K‐bearing sulfide called djerfisherite within enstatite chondrites and aubrites. The petrographic settings of djerfisherite within aubrites suggest this critical host of Cl formed after both the crystallization of troilite and exsolution of daubréelite. Djerfisherite is commonly observed as a rim on other sulfides and in contact with metal. We present an alteration model for djerfisherite formation in aubrite meteorites, whereby troilite and Fe‐Ni metal are altered through anhydrous, alkali‐ and Cl‐rich fluid metasomatism on the aubrite parent body to produce secondary djerfisherite. Moreover, we observe a loss of volatiles in djerfisherite within impact melted regions of the Miller Range 07139 EH3 chondrite and the Bishopville aubrite and explore the potential for impact devolatilization changes to sulfide chemistry on other reduced bodies in the Solar System. Vapor or fluid phase interactions are likely important in the formation of volatile‐rich phases in reduced systems. While most Na and K on the mercurian surface is expected to be hosted in feldspar, djerfisherite is likely a minor, but critical, reservoir for K, Na, and Cl. Djerfisherite present on reduced bodies, such as Mercury, may represent sulfides formed via late‐stage, primary metasomatism.
    Type of Medium: Online Resource
    ISSN: 1086-9379 , 1945-5100
    URL: Article
    DOI: 10.1111/maps.14220
    Language: English
    Publisher: Wiley
    Publication Date: 2024
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  • 4
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    Petrogenesis of Northwest Africa 8686: A ferroan olivine‐phyric shergottite
    Wiley ; 2022
    In:  Meteoritics & Planetary Science Vol. 57, No. 5 ( 2022-05), p. 947-964
    Details
    In: Meteoritics & Planetary Science, Wiley, Vol. 57, No. 5 ( 2022-05), p. 947-964
    Abstract: Northwest Africa (NWA) 8686 is an olivine‐phyric shergottite containing up to ~500 μm long olivine crystals in a fine‐grained groundmass of augite, pigeonite, and maskelynite, with accessory merrillite, pyrrhotite, and oxides. Bulk rock and mineral major and trace element concentrations are reported for NWA 8686, along with bulk rock highly siderophile element (HSE: Os, Ir, Ru, Pt, Pd, Re) abundances and 187 Re‐ 187 Os data. Based on its mineralogy, texture, and bulk rock rare earth element (REE) abundances, NWA 8686 is classified as an intermediate olivine‐phyric shergottite. It is notable for having some of the most ferroan olivine macrocrysts (forsterite content = 51.5 ± 3.5) of any olivine‐phyric shergottite. Olivine is absent from the NWA 8686 groundmass, which is unique for olivine‐phyric shergottites, and the calculated groundmass composition is also not olivine normative. The bulk meteorite has a low Mg# of 59 yet has HSE in broadly chondritic proportions (~0.005 × CI chondrite). The bulk rock REE pattern for NWA 8686 shows depletions in both the light and heavy REE relative to the middle REE. Compiled olivine and bulk rock data for olivine‐phyric shergottites indicate that olivine macrocrysts in almost all these meteorites are the result of entrainment of antecrysts or xenocrysts. The combination of low Mg# and chondritic HSE signatures in NWA 8686 means that it may have been formed either from the mixing between an evolved lava and early‐formed HSE‐rich phases such as Os‐Ir alloys or by the melting of a low Mg# mantle source with chondritic HSE abundances. The elevated Gd/Yb ratio in both NWA 8686 and other intermediate olivine‐phyric shergottites indicates that garnet was involved as either a residual or fractionating phase in their petrogenesis.
    Type of Medium: Online Resource
    ISSN: 1086-9379 , 1945-5100
    URL: Issue
    URL: Article
    DOI: 10.1111/maps.v57.5
    DOI: 10.1111/maps.13805
    Language: English
    Publisher: Wiley
    Publication Date: 2022
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  • 5
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    Nickel–manganese variability in olivine and Al‐in‐olivine thermometry for olivine‐phyric shergottites
    Wiley ; 2021
    In:  Meteoritics & Planetary Science Vol. 56, No. 8 ( 2021-08), p. 1597-1618
    Details
    In: Meteoritics & Planetary Science, Wiley, Vol. 56, No. 8 ( 2021-08), p. 1597-1618
    Abstract: Olivine‐phyric shergottites represent primitive Martian magmas, but they commonly contain excess olivine and rarely represent primary mantle melts. Olivine chemistry, however, tracks magma evolution and preserves information on the original parent magma composition. Here, we investigate the applicability of the Al‐in‐olivine thermometer in tandem with olivine chemistry in a suite of 13 olivine‐phyric shergottites to constrain the compositions and conditions of their mantle sources and parental magmas. We show that the Al‐in‐olivine thermometer is a robust method for constraining crystallization temperatures in shergottites, yielding temperatures in agreement with experimental work. In contrast, we do not recommend olivine–spinel thermometry relying on Mg‐Fe in olivine, which underestimates crystallization temperatures by 160–380 °C. Olivine chemistry reveals distinct differences in Ni concentrations between shergottite groups, with enriched shergottites generally having higher Ni at a given forsterite (Fo) content. Nickel variations in terrestrial olivine are often accredited to contributions from a pyroxenite source; however, the same mechanism is not responsible for Ni variations in Martian olivine. Here, we favor a model for variable olivine modal abundance, caused by multiple melting episodes in the depleted mantle source, affecting Ni partitioning during melting to account for the Ni variations observed. In addition, we show that olivine Ni‐Mn variations in depleted shergottites indicate variable petrogenetic histories and parental magmas. Tissint contains elevated Ni in olivine more similar to the enriched shergottites whereas DaG 1037 has elevated Mn in olivine suggesting an Mn‐enriched parent magma relative to other depleted shergottites.
    Type of Medium: Online Resource
    ISSN: 1086-9379 , 1945-5100
    URL: Issue
    URL: Article
    DOI: 10.1111/maps.v56.8
    DOI: 10.1111/maps.13721
    Language: English
    Publisher: Wiley
    Publication Date: 2021
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  • 6
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    Investigating the igneous petrogenesis of Martian volcanic rocks using augite quantitative textural analysis of the Yamato nakhlites
    Wiley ; 2023
    In:  Meteoritics & Planetary Science Vol. 58, No. 1 ( 2023-01), p. 63-84
    Details
    In: Meteoritics & Planetary Science, Wiley, Vol. 58, No. 1 ( 2023-01), p. 63-84
    Abstract: To better understand volcanism on planetary bodies other than the Earth, the quantification of physical processes is needed. Here, the petrogenesis of the achondrite Martian Yamato (Y) nakhlites (Y 000593, Y 000749, and Y 000802) is reinvestigated via quantitative analysis of augite (high‐Ca clinopyroxene) phenocrysts: crystal size distribution (CSD), spatial distribution patterns (SDP), and electron backscatter diffraction (EBSD). Results from CSD and EBSD quantitative data sets show augite to have continuous uninterrupted growth resulting in calculated minimum magma chamber residence times of either 88–117 ± 6 yr or 9–12 yr. All samples exhibit low‐intensity S‐LS type crystallographic preferred orientation. Directional strain is observed across all samples with intracrystalline misorientation patterns indicative of (100)[001]:(001)[100] (Y 000593 and Y 000802) and {110} 〈 001 〉 or {110} 1 / 2 〈 110 〉 (Y 000749) slip systems. SDP results indicate phenocryst‐bearing crystal‐clustered rock signatures. Combined findings from this work show that the Yamato nakhlites formed on Mars as individual low‐viscosity lava flows or sills. This study shows that through combining these different quantitative techniques over multiple samples, one can more effectively compare and interpret resulting data to gain a more robust, geologically contextualized petrogenetic understanding of the rock suite being studied. The techniques used in this study should be equally applicable to igneous achondrites from other parent bodies.
    Type of Medium: Online Resource
    ISSN: 1086-9379 , 1945-5100
    URL: Issue
    URL: Article
    DOI: 10.1111/maps.v58.1
    DOI: 10.1111/maps.13934
    Language: English
    Publisher: Wiley
    Publication Date: 2023
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  • 7
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    Lithium isotopes and light lithophile element abundances in shergottites: Evidence for both magmatic degassing and subsolidus diffusion
    Wiley ; 2016
    In:  Meteoritics & Planetary Science Vol. 51, No. 1 ( 2016-01), p. 80-104
    Details
    In: Meteoritics & Planetary Science, Wiley, Vol. 51, No. 1 ( 2016-01), p. 80-104
    Abstract: Degassed magmatic water was potentially the major source of surficial water on Mars. We measured Li, B, and Be abundances and Li isotope profiles in pyroxenes, olivines, and maskelynite from four compositionally different shergottites—Shergotty, QUE 94201, LAR 06319, and Tissint—using secondary ion mass spectrometry ( SIMS ). All three light lithophile elements ( LLE ) are incompatible: Li and B are soluble in H 2 O‐rich fluids, whereas Be is insoluble. In the analyzed shergottites, Li concentration decreases and Be concentration increases from cores to rims in pyroxenes. However, B concentrations do not vary consistently with Li and Be abundances, except in QUE 94201 pyroxenes. Additionally, abundances of these three elements in olivines show a normal igneous‐fractionation trend consistent with the crystallization of olivine before magma ascent and degassing. We expect that kinetic effects would lead to fractionation of 6 Li in the vapor phase compared to 7 Li during degassing. The Li isotope profiles, with increasing δ 7 Li from cores to rims, as well as Li and B profiles indicate possible degassing of hydrous fluids only for the depleted shergottite QUE 94201, as also supported by degassing models. Conversely, Shergotty, LAR 06319, and Tissint appear to have been affected by postcrystallization diffusion, based on their LLE and Li isotope profiles, accompanied by diffusion models. This process may represent an overlay on a degassing pattern. The LLE profiles and isotope profiles in QUE 94201 support the hypothesis that degassing of some basaltic shergottite magmas provided water to the Martian surface, although evidence may be obscured by subsolidus diffusion processes.
    Type of Medium: Online Resource
    ISSN: 1086-9379 , 1945-5100
    URL: Issue
    URL: Article
    DOI: 10.1111/maps.2016.51.issue-1
    DOI: 10.1111/maps.12582
    Language: English
    Publisher: Wiley
    Publication Date: 2016
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  • 8
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    Petrogenesis of basaltic shergottite Northwest Africa 8657: Implications for f O 2 correlations and element redistribution during shock melting in shergottites
    Wiley ; 2018
    In:  Meteoritics & Planetary Science Vol. 53, No. 2 ( 2018-02), p. 249-267
    Details
    In: Meteoritics & Planetary Science, Wiley, Vol. 53, No. 2 ( 2018-02), p. 249-267
    Abstract: Northwest Africa ( NWA ) 8657 is an incompatible trace element‐enriched, low‐Al basaltic shergottite, similar in texture and chemistry to Shergotty, Zagami, and NWA 5298. It is composed of zoned pyroxene, maskelynite, merrillite, and Ti‐oxide minerals with minor apatite, silica, and pyrrhotite. Pyroxene grains are characterized by patchy zoning, with pigeonite or augite cores zoned to Fe‐rich pigeonite mantles. The cores have rounded morphologies and irregular margins. Combined with the low Ti/Al of the cores, the morphology and chemistry of the pyroxene grains are consistent with initial crystallization at depth (30–70 km) followed by partial resorption en route to the surface. Enriched rare earth element ( REE ) equilibrium melt compositions and calculated oxygen fugacities ( f O 2 ) conditions for pigeonite cores indicate that the original parent melts were enriched shergottite magmas that staged in chambers at depth within the Martian crust. NWA 8657 does not represent a liquid but rather entrained a proportion of pyroxene crystals from magma chambers where fractional crystallization was occurring at depth. Variation between f O 2 and bulk‐rock (La/Yb) N of the enriched and intermediate shergottites suggests that oxidation conditions and degree of incompatible element enrichment in the source may not be correlated, as thought previously. Shock melt pockets are characterized by an absence of phosphates and oxide minerals. It is likely that these phases were melted during shock. REEs were redistributed during this process into maskelynite and to a lesser extent the shock melt; however, the overall normalized REE profile of the shock melt is like that of the bulk‐rock, but at lower absolute concentrations. Overall, shock melting has had a significant effect on the mineralogy of NWA 8657, especially the distribution of phosphates, which may be significant for geochronological applications of this meteorite and other Martian meteorites with extensive shock melt.
    Type of Medium: Online Resource
    ISSN: 1086-9379 , 1945-5100
    URL: Issue
    URL: Article
    DOI: 10.1111/maps.2018.53.issue-2
    DOI: 10.1111/maps.12999
    Language: English
    Publisher: Wiley
    Publication Date: 2018
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  • 9
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    Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170
    Wiley ; 2017
    In:  Meteoritics & Planetary Science Vol. 52, No. 2 ( 2017-02), p. 391-409
    Details
    In: Meteoritics & Planetary Science, Wiley, Vol. 52, No. 2 ( 2017-02), p. 391-409
    Abstract: Olivine‐phyric shergottites represent primitive basaltic to picritic rocks, spanning a large range of Mg# and olivine abundances. As primitive olivine‐bearing magmas are commonly representative of their mantle source on Earth, understanding the petrology and evolution of olivine‐phyric shergottites is critical in our understanding of Martian mantle compositions. We present data for the olivine‐phyric shergottite Northwest Africa ( NWA ) 10170 to constrain the petrology with specific implications for magma plumbing‐system dynamics. The calculated oxygen fugacity and bulk‐rock REE concentrations (based on modal abundance) are consistent with a geochemically intermediate classification for NWA 10170, and overall similarity with NWA 6234. In addition, we present trace element data using laser ablation ICP ‐ MS for coarse‐grained olivine cores, and compare these data with terrestrial and Martian data sets. The olivines in NWA 10170 contain cores with compositions of Fo 77 that evolve to rims with composition of Fo 58 , and are characterized by cores with low Ni contents (400–600 ppm). Nickel is compatible in olivine and such low Ni content for olivine cores in NWA 10170 suggests either early‐stage fractionation and loss of olivine from the magma in a staging chamber at depth, or that Martian magmas have lower Ni than terrestrial magmas. We suggest that both are true in this case. Therefore, the magma does not represent a primary mantle melt, but rather has undergone 10–15% fractionation in a staging chamber prior to extrusion/intrusion at the surface of Mars. This further implies that careful evaluation of not only the Mg# but also the trace element concentrations of olivine needs to be conducted to evaluate pristine mantle melts versus those that have fractionated olivine (±pyroxene and oxide minerals) in staging chambers.
    Type of Medium: Online Resource
    ISSN: 1086-9379 , 1945-5100
    URL: Issue
    URL: Article
    DOI: 10.1111/maps.2017.52.issue-2
    DOI: 10.1111/maps.12799
    Language: English
    Publisher: Wiley
    Publication Date: 2017
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  • 10
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    Petrology and trace element geochemistry of Tissint, the newest shergottite fall
    Wiley ; 2015
    In:  Meteoritics & Planetary Science Vol. 50, No. 1 ( 2015-01), p. 63-85
    Details
    In: Meteoritics & Planetary Science, Wiley, Vol. 50, No. 1 ( 2015-01), p. 63-85
    Abstract: The fall and recovery of the Tissint meteorite in 2011 created a rare opportunity to examine a Martian sample with a known, short residence time on Earth. Tissint is an olivine‐phyric shergottite that accumulated olivine antecrysts within a single magmatic system. Coarse olivine grains with nearly homogeneous cores of Mg# 〉 80 suggest slow re‐equilibration. Many macroscopic features of this sample resemble those of LAR 06319, including the olivine crystal size distribution and the presence of evolved oxide and olivine compositions. Unlike LAR 06319, however, no magmatic hydrous phases were found in the analyzed samples of Tissint. Minor and trace element compositions indicate that the meteorite is the product of closed‐system crystallization from a parent melt derived from a depleted source, with no obvious addition of a LREE‐rich (crustal?) component prior to or during crystallization. The whole‐rock REE pattern is similar to that of intermediate olivine‐phyric shergottite EETA 79001 lithology A, and could also be approximated by a more olivine‐rich version of depleted basaltic shergottite QUE 94201. Magmatic oxygen fugacities are at the low end of the shergottite range, with log f O 2 of QFM‐3.5 to ‐4.0 estimated based on early‐crystallized minerals and QFM‐2.4 estimated based on the Eu in pyroxene oxybarometer. These values are similarly comparable to other depleted shergottites, including SaU 005 and QUE 94201. Tissint occupies a previously unsampled niche in shergottite chemistry: containing olivines with Mg# 〉 80, resembling the enriched olivine‐phyric shergottite LAR 06319 in its crystallization path, and comparable to intermediate olivine‐phyric shergottite EETA 79001A, depleted olivine‐phyric shergottite DaG 476, and depleted basaltic shergottite QUE 94201 in its trace element abundances and oxygen fugacity. The apparent absence of evidence for terrestrial alteration in Tissint (particularly in trace element abundances in the whole‐rock and individual minerals) confirms that exposure to the arid desert environment results in only minimal weathering of samples, provided the exposure times are brief.
    Type of Medium: Online Resource
    ISSN: 1086-9379 , 1945-5100
    URL: Issue
    URL: Article
    DOI: 10.1111/maps.2015.50.issue-1
    DOI: 10.1111/maps.12403
    Language: English
    Publisher: Wiley
    Publication Date: 2015
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