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martian mantle source

The new data implies that the martian mantle sources of shergottites have fO2 of −2.

Uniform oxygen fugacity of shergottite mantle sources and an oxidized martian lithosphere

martian mantle source

We investigated five of the twenty known nakhlites (Nakhla, Lafayette, Miller Range (MIL) 090032, Yamato 000593, and Yamato 000749) to determine whether these lavas show evidence of regolith assimilation, and to constrain the potential implications that this process has on chemical tracing of martian mantle source(s).

Syneruptive incorporation of martian surface sulphur in the nakhlite lava flows revealed by S and Os isotopes and highly siderophile elements : implication for mantle sources in Mars.

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10.1016/J.ICARUS.2021.114625

Therefore, we conclude from the observation of WR-formation ages that the Martian mantle was vastly active during the Noachian/Hesperian boundary and the intensity of the mantle activity decreased through time, giving rise to multiple pulses of regional volcano-tectonic events, as a part of thermal evolution over the Hesperian period.

A global investigation of wrinkle ridge formation events; Implications towards the thermal evolution of Mars

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10.5194/EGUSPHERE-EGU21-5745

Degree-1 convection in the Martian mantle and the origin of the hemispheric dichotomy.

Martian Dichotomy from a Giant Impact: Mantle Convection Models

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10.1126/science.abf8966

388 Data from the InSight mission on Mars help constrain the structure and properties of the martian mantle.

Thickness and structure of the martian crust from InSight seismic data

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10.31223/x5xw48

35 log units below the iron–wüstite 29 buffer to produce a Martian mantle with the observed Hf/W ratio.

Timing of Martian Core Formation from Models of Hf–W Evolution Coupled with N-body Simulations

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10.1016/j.gca.2020.10.024

Shergottite meteorites are ultramafic to mafic igneous rocks derived from partial melting of distinct regions of the martian mantle.

Highly siderophile elements in shergottite sulfides and the sulfur content of the martian mantle

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10.1016/J.GCA.2021.05.011

Shergottites were derived from mantle reservoirs through various magmatic processes, recording geochemical signatures of the martian mantle.

Heterogeneous martian mantle: Evidence from petrology, mineral chemistry, and in situ U-Pb chronology of the basaltic shergottite Northwest Africa 8653

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10.1016/J.PEPI.2019.106298

Phosphorus in Martian mantle is believed to be five to ten times more abundant than in Earth's mantle, and the distribution of this essential ingredient for life between different deep reservoirs is critical for understanding the habitability of the red planet.

Partition coefficient of phosphorus between liquid metal and silicate melt with implications for the Martian magma ocean

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10.1029/2019gl085234

Our mantle heat flow estimate is notably lower than the heat flow expected from a chondritic mantle suggesting the Martian mantle to be depleted in HPE.

Depletion of Heat Producing Elements in the Martian Mantle

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10.3390/min9090559

%) analog of Martian mantle in simplified MgO-Al2O3-FeO-SiO2-H2O (MAFSH) system between 15 and 21 GPa at 900–1500 °C using a multi-anvil apparatus.

Phase Relations in MAFSH System up to 21 GPa: Implications for Water Cycles in Martian Interior

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10.1016/J.GCA.2019.07.001

This study reveals that at least two sources are responsible for the enriched shergottites, and that the martian mantle is more heterogeneous than previously thought.

Petrology of the enriched poikilitic shergottite Northwest Africa 10169: Insight into the martian interior

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Martian Mantle - Therefore, we conclude from the observation of WR-formation ages that the Martian mantle was vastly active during the Noachian/Hesperian boundary and the intensity of the mantle activity decreased through time, giving rise to multiple pulses of regional volcano-tectonic events, as a part of thermal evolution over the Hesperian period. [1] Degree-1 convection in the Martian mantle and the origin of the hemispheric dichotomy. [2] 388 Data from the InSight mission on Mars help constrain the structure and properties of the martian mantle. [3] 35 log units below the iron–wüstite 29 buffer to produce a Martian mantle with the observed Hf/W ratio. [4] Shergottite meteorites are ultramafic to mafic igneous rocks derived from partial melting of distinct regions of the martian mantle. [5] Shergottites were derived from mantle reservoirs through various magmatic processes, recording geochemical signatures of the martian mantle. [6] Phosphorus in Martian mantle is believed to be five to ten times more abundant than in Earth's mantle, and the distribution of this essential ingredient for life between different deep reservoirs is critical for understanding the habitability of the red planet. [7] Our mantle heat flow estimate is notably lower than the heat flow expected from a chondritic mantle suggesting the Martian mantle to be depleted in HPE. [8] %) analog of Martian mantle in simplified MgO-Al2O3-FeO-SiO2-H2O (MAFSH) system between 15 and 21 GPa at 900–1500 °C using a multi-anvil apparatus. [9] This study reveals that at least two sources are responsible for the enriched shergottites, and that the martian mantle is more heterogeneous than previously thought. [10]

martian mantle source

The new data implies that the martian mantle sources of shergottites have fO2 of −2. [1] We investigated five of the twenty known nakhlites (Nakhla, Lafayette, Miller Range (MIL) 090032, Yamato 000593, and Yamato 000749) to determine whether these lavas show evidence of regolith assimilation, and to constrain the potential implications that this process has on chemical tracing of martian mantle source(s). [2]