The solar system, planetary systems of stars, and sequential accretion theory

Ксанфомалити, Л. В.

doi:10.3103/s0884591310040070

“…Despite having similar sizes and origin, the broad crustal structure and composition of the terrestrial planets of the solar system (Earth, Venus and Mars) are starkly different [1,2]. In particular, the Earth's dynamics is dominated by horizontal plate tectonics, while Mars is a "single-lid" planet, without evidence of horizontal plate movement [3].…”

Section: We Find That the Martian Crust Can Be Divided By Depth Into ...mentioning

confidence: 99%

“…Head III 2 , Olivier Bachmann 1 1 Institute for Geochemistry and Petrology, Department of Earth Sciences, ETH Zürich, Switzerland. 2 S6: Calculation mineral volume fractions from MELTS results of Backstay starting composition; for different conditions of QFM-2.5 H2O 0.1wt%, QFM-1 H2O 0.1wt%, QFM-1 H2O 1wt% CO2 500ppm and QFM+1 H2O 0.5wt%; and at depths of 2.5kbar and 1.5kbar. Table S7: Calculation mineral volume fractions from MELTS results of Champagne starting composition; for different conditions of QFM-2.5 H2O 0.1wt%, QFM-1 H2O 0.1wt%, QFM-1 H2O 1wt% CO2 500ppm and QFM+1 H2O 0.5wt%; and at depths of 2.5kbar and 1.5kbar.…”

Section: Supplementary Informationmentioning

confidence: 99%

“…We further show that crustal rheology strongly controls this transition depth. Our results also support the possibility of deep-seated magmatism underneath the seismically active Cerberus Fossae, suggesting that magmatism continues to play a major role in shaping the Martian crust.Despite having similar sizes and origin, the broad crustal structure and composition of the terrestrial planets of the solar system (Earth, Venus and Mars) are starkly different [1,2]. In particular, the Earth's dynamics is dominated by horizontal plate tectonics, while Mars is a "single-lid" planet, without evidence of horizontal plate movement [3].…”

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confidence: 99%

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Magma chamber longevity on Mars and its controls on crustal structure and composition

Chatterjee,

Huber,

III

et al. 2024

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0

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In volcanically active planetary bodies, the depths and longevity of crustal magma storage critically control eruptibility and crustal composition. A paucity of observations has challenged our understanding of the development of crustal magma storage systems in Mars and its role behind the lack of evolved compositions. Here, we use numerical modelling, together with recent results from the InSight mission, to study the evolution of crustal magma chambers on Mars and conditions that promote their growth and eruptibility. We find that the Martian crust can be divided, by depth, into three major domains. At depths ≤15km (~1.5kbar), trapped magma pods are small, short-lived, with high diking potential, hindering the production of evolved compositions. While depths >25km (~2.5kbar) can host long-lived magma chambers, 15-25km (~2 ± 0.5kbar) marks a transition where magma chambers could grow while expelling magma. Interestingly, this narrow depth window overlaps with the depth of an intra-crustal discontinuity reported by InSight, suggesting a possible magmatic origin for the discontinuity. We further show that crustal rheology strongly controls this transition depth. Our results also support the possibility of deep-seated magmatism underneath the seismically active Cerberus Fossae, suggesting that magmatism continues to play a major role in shaping the Martian crust.

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“…Despite having similar sizes and origin, the broad crustal structure and composition of the terrestrial planets of the Solar System are starkly different (Chambers, 2004;Head & Solomon, 1981;Ksanfomaliti, 2010). In particular, Earth's dynamics is dominated by horizontal plate tectonics, while Mars is a "single-lid" planet, without evidence of horizontal plate movement (Stern et al, 2018).…”

Section: Introductionmentioning

confidence: 99%

Magma chamber longevity on Mars and its controls on crustal structure and composition

Chatterjee,

Huber,

III

et al. 2024

Preprint

0

View full text Add to dashboard Cite

In volcanically active planetary bodies, the depths and longevity of crustal magma storage critically control eruptibility and crustal composition. A paucity of relevant observations and models has challenged our understanding of the development of crustal magma storage systems in Mars and their role in the apparent lack of evolved compositions. Here, we use numerical modelling, together with recent results from the InSight mission, to study the evolution of crustal magma chambers on Mars and conditions that promote their growth and eruptibility. We find that the Martian crust can be divided, by depth, into three major domains. For Elysium Planitia (the InSight landing site), at depths ≤15km (~1.5kbar), trapped magma pods are small, short-lived, with high diking potential, hindering the production of evolved compositions. While depths >25km (~2.5kbar) can host long-lived magma chambers, 15-25km (~2 ± 0.5kbar) marks a transition where magma chambers could grow while concurrently expelling magma. Interestingly, this narrow depth window overlaps with the depth of an intra-crustal discontinuity reported by InSight, suggesting a possible magmatic origin for the discontinuity. We further show that the crustal thermal gradient strongly controls this transition depth, indicating the possible variability of the domain depths in different terrains. Our results also support the likelihood of deep-seated magmatism beneath the seismically active Cerberus Fossae, suggesting that magmatism continues to play a major role in shaping the Martian crust.

show abstract

Magma chamber longevity on Mars and its controls on crustal structure and composition

Chatterjee,

Huber,

III

et al. 2024

Preprint

0

View full text Add to dashboard Cite

In volcanically active planetary bodies, the depths and longevity of crustal magma storage critically control eruptibility and crustal composition. A paucity of relevant observations and models has challenged our understanding of the development of crustal magma storage systems in Mars and their role in the apparent lack of evolved compositions. Here, we use numerical modelling, together with recent results from the InSight mission, to study the evolution of crustal magma chambers on Mars and conditions that promote their growth and eruptibility. We find that the Martian crust can be divided, by depth, into three major domains. For Elysium Planitia (the InSight landing site), at depths ≤15km (~1.5kbar), trapped magma pods are small, short-lived, with high diking potential, hindering the production of evolved compositions. While depths >25km (~2.5kbar) can host long-lived magma chambers, 15-25km (~2 ± 0.5kbar) marks a transition where magma chambers could grow while concurrently expelling magma. Interestingly, this narrow depth window overlaps with the depth of an intra-crustal discontinuity reported by InSight, suggesting a possible magmatic origin for the discontinuity. We further show that the crustal thermal gradient strongly controls this transition depth, indicating the possible variability of the domain depths in different terrains. Our results also support the likelihood of deep-seated magmatism beneath the seismically active Cerberus Fossae, suggesting that magmatism continues to play a major role in shaping the Martian crust.

show abstract

The solar system, planetary systems of stars, and sequential accretion theory

Cited by 5 publications

References 30 publications

Magma chamber longevity on Mars and its controls on crustal structure and composition

Magma chamber longevity on Mars and its controls on crustal structure and composition

Magma chamber longevity on Mars and its controls on crustal structure and composition

Magma chamber longevity on Mars and its controls on crustal structure and composition

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