Gabbroic and poikilitic shergottites are intrusive igneous rocks on Mars,providing significant insights into the igneous processes within the Martian crust.However,questions remain regarding the chemical signatures of...Gabbroic and poikilitic shergottites are intrusive igneous rocks on Mars,providing significant insights into the igneous processes within the Martian crust.However,questions remain regarding the chemical signatures of their source reservoirs and the petrogenetic links among shergottites of different subtypes.In this study,we present petrological and mineralogical analyses of the intermediate shergottite Northwest Africa(NWA)12241.Quantitative textural analysis and pyroxene chemistry indicate that,despite minor differences such as the accumulation of intermediate-sized olivine and smaller pyroxene oikocrysts,NWA 12241 has experienced a similar emplacement history as typical poikilitic and gabbroic shergottites.The estimated parent melt of NWA 12241 is consistent with derivation from an intermediate source reservoir,resulting from the mixing of enriched and depleted mantle end-members at depth,prior to magma ascent.Similar emplacement histories of variable poikilitic and gabbroic shergottites suggest the common presence of multiple staging magma chambers with different compositions at the crust–mantle boundary,coupled with prolonged ponding at this depth.Our study highlights that,in addition to magma mixing and assimilation,magmatic differentiation and cooling conditions at shallow depths are crucial processes leading to textural and compositional variations among shergottites of different subtypes.展开更多
Most basaltic shergottites are too Mg-rich to represent parent melt compositions because they contain some cumulus pyroxenes. However, basaltic shergottite Northwest Africa(NWA) 8656 with subophitic texture can be use...Most basaltic shergottites are too Mg-rich to represent parent melt compositions because they contain some cumulus pyroxenes. However, basaltic shergottite Northwest Africa(NWA) 8656 with subophitic texture can be used as the parent melt composition in petrogenetic studies because it contains no or rare cumulus pyroxenes. Its pyroxene cores(Mg# 66-68, the most magnesian) are in equilibrium with the bulk rock composition based on major(Fe-Mg) and trace elements(REE—rare earth elements).The patchy zoning of pyroxenes has been interpreted as reflecting a two-stage crystallization history: 1) crystallization of Mg-rich pyroxene cores at depth(50 km, the base of Martian crust), 2) crystallization of Fe-rich pyroxene rims at the shallow depth near the Martian surface with a fast cooling history. The crystallization of Fe-rich pyroxenes and the existence of different symplectites indicate that NWA 8656 underwent eruption. The oxygen fugacity of NWA 8656(QFM –0.9±0.5) suggests an oxidized condition at the late-stage crystallization process, and the CI-normalized REE patterns of different minerals show enrichment in LREE, compared to that of depleted shergottites. Both of these observations suggest a relatively ITE(incompatible trace elements)-enriched signature of NWA 8656, similar to those of other enriched shergottites. The REE compositions of augite core and rim and plagioclase can be successfully reproduced by progressive crystallization without exogenous components, which indicates a closed magmatic system for NWA 8656. Consequently, we conclude that the ITE-enriched signature of NWA 8656 is inherited from an enriched mantle source rather than caused by crustal assimilation. Moreover, partial melting of depleted Martian mantle could not directly yield magmas that have geochemical characteristics similar to enriched shergottite parent magmas, so the enriched and depleted shergottites are derived from distinct mantle sources, and the mantle source of enriched shergottites would be expected to contain ilmenite.展开更多
Depleted shergottites record unique information about the primary composition and differentiation of the mantle of Mars.Their petrology,geochemistry,and cosmic ray exposure and crystallization ages suggest that most o...Depleted shergottites record unique information about the primary composition and differentiation of the mantle of Mars.Their petrology,geochemistry,and cosmic ray exposure and crystallization ages suggest that most of them were excavated by a single young impact in the Amazonian-aged lava flows of the Tharsis and Elysium volcanic provinces.However,the difficulties of deriving consistent model ages for individual craters and inadequate evaluation of 3-7 km craters capable of ejecting martian meteorites have not been settled.Here we perform detailed geological investigations and crater statistics in patches of impact melt deposits for potential source craters of depleted shergottites with D>3 km,especially those in the Tharsis and Elysium volcanic provinces.By excluding the effect of heterogeneous textures across ejecta deposits,which hinder straightforward extraction of superposed production populations,our systematically updated model ages reveal that Chakpar crater at the northern flank of Ascraeus Mons is the best-fit candidate.The local context of this crater permits establishing a link between the meteorites and specific lava flows.The long-lived volcanic center here may experience an eruption and/or local deposition hiatus for about 1.8 billion years,and abundant subsurface water existed when the impact occurred at about 1.1 million years.展开更多
Reported in this paper are the petrology and mineral chemistry of GRV 020090, the second Martian meteorite collected from the Grove Mountains, Antarctica. This meteorite, with a mass of 7.54 g, is completely covered b...Reported in this paper are the petrology and mineral chemistry of GRV 020090, the second Martian meteorite collected from the Grove Mountains, Antarctica. This meteorite, with a mass of 7.54 g, is completely covered by a black and glazy fusion crust. It has two distinct textural regions. The interstitial region is composed of euhedral grains of olivine, pigeonite, and anhedral interstitial maskelynite, with minor chromite, augite, phosphates and troilite. The poikilitic region consists of three clasts of pyroxenes, each of which has a pigeonite core and an augite rim. A few grains of subhedral to rounded olivine and euhedral chromite are enclosed in the pyroxene oikocrysts. GRV 020090 is classified as a new member of lherzolitic shergottites based on the modal composition and mineral chemistry. This work will shed light on the composition of Martian crust and magmatism on the Mars.展开更多
基金supported by the National Natural Science Foundation of China(Nos.42473049,42241108,and 42273040)the Guangdong Basic and Applied Basic Research Foundation(No.2024A1515011311)the Open Project for Innovative Platform of Meteoritical Research,Shanghai Science and Technology Museum。
文摘Gabbroic and poikilitic shergottites are intrusive igneous rocks on Mars,providing significant insights into the igneous processes within the Martian crust.However,questions remain regarding the chemical signatures of their source reservoirs and the petrogenetic links among shergottites of different subtypes.In this study,we present petrological and mineralogical analyses of the intermediate shergottite Northwest Africa(NWA)12241.Quantitative textural analysis and pyroxene chemistry indicate that,despite minor differences such as the accumulation of intermediate-sized olivine and smaller pyroxene oikocrysts,NWA 12241 has experienced a similar emplacement history as typical poikilitic and gabbroic shergottites.The estimated parent melt of NWA 12241 is consistent with derivation from an intermediate source reservoir,resulting from the mixing of enriched and depleted mantle end-members at depth,prior to magma ascent.Similar emplacement histories of variable poikilitic and gabbroic shergottites suggest the common presence of multiple staging magma chambers with different compositions at the crust–mantle boundary,coupled with prolonged ponding at this depth.Our study highlights that,in addition to magma mixing and assimilation,magmatic differentiation and cooling conditions at shallow depths are crucial processes leading to textural and compositional variations among shergottites of different subtypes.
文摘Most basaltic shergottites are too Mg-rich to represent parent melt compositions because they contain some cumulus pyroxenes. However, basaltic shergottite Northwest Africa(NWA) 8656 with subophitic texture can be used as the parent melt composition in petrogenetic studies because it contains no or rare cumulus pyroxenes. Its pyroxene cores(Mg# 66-68, the most magnesian) are in equilibrium with the bulk rock composition based on major(Fe-Mg) and trace elements(REE—rare earth elements).The patchy zoning of pyroxenes has been interpreted as reflecting a two-stage crystallization history: 1) crystallization of Mg-rich pyroxene cores at depth(50 km, the base of Martian crust), 2) crystallization of Fe-rich pyroxene rims at the shallow depth near the Martian surface with a fast cooling history. The crystallization of Fe-rich pyroxenes and the existence of different symplectites indicate that NWA 8656 underwent eruption. The oxygen fugacity of NWA 8656(QFM –0.9±0.5) suggests an oxidized condition at the late-stage crystallization process, and the CI-normalized REE patterns of different minerals show enrichment in LREE, compared to that of depleted shergottites. Both of these observations suggest a relatively ITE(incompatible trace elements)-enriched signature of NWA 8656, similar to those of other enriched shergottites. The REE compositions of augite core and rim and plagioclase can be successfully reproduced by progressive crystallization without exogenous components, which indicates a closed magmatic system for NWA 8656. Consequently, we conclude that the ITE-enriched signature of NWA 8656 is inherited from an enriched mantle source rather than caused by crustal assimilation. Moreover, partial melting of depleted Martian mantle could not directly yield magmas that have geochemical characteristics similar to enriched shergottite parent magmas, so the enriched and depleted shergottites are derived from distinct mantle sources, and the mantle source of enriched shergottites would be expected to contain ilmenite.
基金funded by the National Natural Science Foundation of China(Grant Nos.42241108,423B2205,42273040,62227901)the Strategic Priority Research Program of Chinese Academy of Science(Grant No.XDB41000000)。
文摘Depleted shergottites record unique information about the primary composition and differentiation of the mantle of Mars.Their petrology,geochemistry,and cosmic ray exposure and crystallization ages suggest that most of them were excavated by a single young impact in the Amazonian-aged lava flows of the Tharsis and Elysium volcanic provinces.However,the difficulties of deriving consistent model ages for individual craters and inadequate evaluation of 3-7 km craters capable of ejecting martian meteorites have not been settled.Here we perform detailed geological investigations and crater statistics in patches of impact melt deposits for potential source craters of depleted shergottites with D>3 km,especially those in the Tharsis and Elysium volcanic provinces.By excluding the effect of heterogeneous textures across ejecta deposits,which hinder straightforward extraction of superposed production populations,our systematically updated model ages reveal that Chakpar crater at the northern flank of Ascraeus Mons is the best-fit candidate.The local context of this crater permits establishing a link between the meteorites and specific lava flows.The long-lived volcanic center here may experience an eruption and/or local deposition hiatus for about 1.8 billion years,and abundant subsurface water existed when the impact occurred at about 1.1 million years.
基金This work is supported by the National Natural Science Foundation of China(Grant No.40232026)the pilot project of knowledge innovation program of the Chinese Academy of Sciences(Grant No.KZCX3-SW-123).
文摘Reported in this paper are the petrology and mineral chemistry of GRV 020090, the second Martian meteorite collected from the Grove Mountains, Antarctica. This meteorite, with a mass of 7.54 g, is completely covered by a black and glazy fusion crust. It has two distinct textural regions. The interstitial region is composed of euhedral grains of olivine, pigeonite, and anhedral interstitial maskelynite, with minor chromite, augite, phosphates and troilite. The poikilitic region consists of three clasts of pyroxenes, each of which has a pigeonite core and an augite rim. A few grains of subhedral to rounded olivine and euhedral chromite are enclosed in the pyroxene oikocrysts. GRV 020090 is classified as a new member of lherzolitic shergottites based on the modal composition and mineral chemistry. This work will shed light on the composition of Martian crust and magmatism on the Mars.
