A positive feedback between magmatism and mantle upwelling in terrestrial planets: Implications for the Moon

Ogawa, Masaki

doi:10.1002/2014je004717

Cited by 13 publications

(7 citation statements)

References 45 publications

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“…In models where the uppermost mantle is locally more enriched in HPEs, the partially molten regions observed in there persist for more than 3 Gyr (Laneuville et al., 2013, 2014, 2018). Volcanism, however, extracts HPEs from the mantle leading to the decline of subsequent volcanic activity (Cassen & Reynolds, 1973; Cassen et al., 1979; Ogawa, 2014, 2018a). In particular, Ogawa (2018a) suggests that partially molten regions disappear within 2 Gyr since the beginning of the calculated history, too short to be a model of the lunar mare volcanism, owing to the extraction of HPEs by magmatism.…”

Section: Discussionmentioning

confidence: 99%

The Volcanic and Radial Expansion/Contraction History of the Moon Simulated by Numerical Models of Magmatism in the Convective Mantle

Kameyama,

Ogawa

2023

JGR Planets

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To understand the evolution of the Moon, we numerically modeled mantle convection and magmatism in a two‐dimensional polar rectangular mantle. Magmatism occurs as an upward permeable flow of magma generated by decompression melting through the convecting matrix. The mantle is assumed to be initially enriched in heat‐producing elements (HPEs) and compositionally dense ilmenite‐bearing cumulates (IBC) at its base. Here, we newly show that magma generation and migration play a crucial role in the calculated volcanic and radial expansion/contraction history. Magma is generated in the deep mantle by internal heating for the first several hundred million years. A large volume of the generated magma ascends to the surface as partially molten plumes driven by melt buoyancy; the magma generation and ascent cause a volcanic activity and radial expansion of the Moon with the peak at 3.5–4 Gyr ago. Eventually, the Moon begins to radially contract when the mantle solidifies by cooling from the surface boundary. As the mantle is cooled, the activity of partially molten plumes declines but continues for billions of years after the peak because some basal materials enriched in the dense IBC components hold HPEs. The calculated volcanic and radial expansion/contraction history is consistent with the observed history of the Moon. Our simulations suggest that a substantial fraction of the mantle was solid, and there was a basal layer enriched in HPEs and the IBC components at the beginning of the history of the Moon.

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Section: Discussionmentioning

confidence: 99%

The Volcanic and Radial Expansion/Contraction History of the Moon Simulated by Numerical Models of Magmatism in the Convective Mantle

Kameyama,

Ogawa

2023

JGR Planets

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“…It is a challenging issue to construct a model of mantle evolution in Mercury that is consistent with these observations. Here I extend my earlier models of coupled magmatism‐mantle convection system developed for Mars [ Ogawa and Yanagisawa , ] and the Moon [ Ogawa , ] (hereinafter called Papers 1 and 2, respectively) to Mercury to shed light on this issue.…”

Section: Introductionmentioning

confidence: 99%

Evolution of the interior of Mercury influenced by coupled magmatism-mantle convection system and heat flux from the core

Ogawa

2016

J. Geophys. Res. Planets

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To discuss mantle evolution in Mercury, I present two‐dimensional numerical models of magmatism in a convecting mantle. Thermal, compositional, and magmatic buoyancy drives convection of temperature‐dependent viscosity fluid in a rectangular box placed on the top of the core that is modeled as a heat bath of uniform temperature. Magmatism occurs as a permeable flow of basaltic magma generated by decompression melting through a matrix. Widespread magmatism caused by high initial temperature of the mantle and the core makes the mantle compositionally stratified within the first several hundred million years of the 4.5 Gyr calculated history. The stratified structure persists for 4.5 Gyr, when the reference mantle viscosity at 1573 K is higher than around 1020 Pa s. The planet thermally contracts by an amount comparable to the one suggested for Mercury over the past 4 Gyr. Mantle upwelling, however, generates magma only for the first 0.1–0.3 Gyr. At lower mantle viscosity, in contrast, a positive feedback between magmatism and mantle upwelling operates to cause episodic magmatism that continues for the first 0.3–0.8 Gyr. Convective current stirs the mantle and eventually dissolves its stratified structure to enhance heat flow from the core and temporarily resurrect magmatism depending on the core size. These models, however, predict larger contraction of the planet. Coupling between magmatism and mantle convection plays key roles in mantle evolution, and the difficulty in numerically reproducing the history of magmatism of Mercury without causing too large radial contraction of the planet warrants further exploration of this coupling.

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“…However, according to numerical simulations by Ogawa (), there is a possibility that basaltic material layers with 15 wt% ilmenite could have formed in the upper part of a partial melt zone (the blue zones of fig. i in Ogawa ) during Phase‐1 volcanism (Figs. d and e).…”

Section: Discussionmentioning

confidence: 99%

“…The second scenario is that the basaltic material layer predicted by the numerical simulations of mantle evolution by Ogawa () was re‐melted during Phase‐2 volcanism. In his model, basaltic melts generated in the partial melt zone in the upper mantle rose as permeable flows due to their lower density and formed a basaltic material layer under the lunar crust.…”

Section: Discussionmentioning

confidence: 99%

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Magma source transition of lunar mare volcanism at 2.3 Ga

Kato

Morota

Yamaguchi

et al. 2017

Meteorit & Planetary Scien

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Mare basalts provide insights into the composition and thermal history of the lunar mantle. The ages of mare basalts suggest a first peak of magma activity at 3.2-3.8 Ga and a second peak at~2 Ga. In this study, we reassess the correlation between the titanium contents and the eruption ages of mare basalt units using the compositional and chronological data updated by SELENE (Kaguya). Using morphological and geological criteria, we calculated the titanium content of 261 mare units across a representative area of each mare unit. In the Procellarum KREEP Terrane, where the latest eruptions are located, an increase in the mean titanium content is observed during the Eratosthenian period, as reported by previous studies. We found that the increase in the mean titanium content occurred within a relatively short period near approximately 2.3 Ga, suggesting that the magma source of the mare basalts changed at this particular age. Moreover, the high-titanium basaltic eruptions are correlated with a second peak in volcanic activity near 2 Ga. The high-titanium basaltic eruptions occurring during the last volcanic activity period can be explained by the three possible scenarios (1) the ilmenite-bearing cumulate rich layer in the core-mantle boundary formed after the mantle overturn, (2) the basaltic material layers beneath the lunar crust formed through upwelling magmas, and (3) ilmenite-bearing cumulate blocks remained in the upper mantle after the mantle overturn.

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A positive feedback between magmatism and mantle upwelling in terrestrial planets: Implications for the Moon

Cited by 13 publications

References 45 publications

The Volcanic and Radial Expansion/Contraction History of the Moon Simulated by Numerical Models of Magmatism in the Convective Mantle

The Volcanic and Radial Expansion/Contraction History of the Moon Simulated by Numerical Models of Magmatism in the Convective Mantle

Evolution of the interior of Mercury influenced by coupled magmatism-mantle convection system and heat flux from the core

Magma source transition of lunar mare volcanism at 2.3 Ga

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