Magma Ascent and Eruption Triggered by Cratering on the Moon

Michaut, Chloé; Pinel, Virginie

doi:10.1029/2018gl078150

Cited by 25 publications

(24 citation statements)

References 30 publications

(92 reference statements)

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“…Impact cratering and volcanism also act on each other as well. On the one hand, impact cratering produced stress conditions in the crust that favor the ascent of the magma (Michaut & Pinel, ). On the other hand, lavas might either partially or completely bury a previously formed impact crater depending on the thickness of the flow and the height of the crater rim.…”

Section: Introductionmentioning

confidence: 99%

Thickness of Lunar Mare Basalts: New Results Based on Modeling the Degradation of Partially Buried Craters

Wieczorek

et al. 2019

JGR Planets

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Partially buried craters on the Moon are those craters whose distal ejecta are covered by lava flows and where the crater rim crest still protrudes above the mare plain. Based on the difference in rim heights between a partially buried crater and an unburied crater, previous studies estimated the thicknesses of the lunar mare basalts. However, these studies did not consider the erosion of the crater rim height, which can result in an overestimate in the derived thickness. By using recent high‐resolution topographic data, we report a basalt thickness estimation method based on numerically modeling the topographic degradation of partially buried craters. We identified 661 buried craters over the lunar surface, and their spatial distribution suggests a preferential occurrence along the mare‐highland boundaries. An elevation model of fresh lunar craters was derived, and the topographic diffusion equation was used to model crater degradation. By modeling the formation, degradation, and flooding of partially buried craters, basalt thicknesses were estimated for 41 mare craters whose rims are completely exposed. The resulting mare basalt thicknesses vary from 33 to 455 m, with a median value of 105 m that is 95 m smaller than that derived when not considering crater degradation. The estimated eruption rate of lunar mare basalts is found to have peaked at 3.4 Ga and then decreased with time, indicating a progressive cooling of the lunar interior. As a by‐product from the crater degradation model, our results suggest that the topographic diffusivity of lunar craters increases with diameter.

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Section: Introductionmentioning

confidence: 99%

Thickness of Lunar Mare Basalts: New Results Based on Modeling the Degradation of Partially Buried Craters

Wieczorek

et al. 2019

JGR Planets

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“…The huge underlying feeder dike identified by gravity gradients [43] bordering the PKT would be conducive to the magma ascent of either the Gardner volcano [15] or the Mare Tranquillitatis. The shield-building eruptions of domes could come directly from the mantle, driven by basin or crater loading-induced stress in dikes [44], or from shallow magma bodies created by intrusion-trapping loading stresses (e.g., [45]).…”

Section: Multi-stage Volcanic Activities Revealed By the Clustered Domesmentioning

confidence: 99%

Unsupervised Machine Learning on Domes in the Lunar Gardner Region: Implications for Dome Classification and Local Magmatic Activities on the Moon

et al. 2021

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Lunar volcanic domes are essential windows into the local magmatic activities on the Moon. Classification of domes is a useful way to figure out the relationship between dome appearances and formation processes. Previous studies of dome classification were manually or semi-automatically carried out either qualitatively or quantitively. We applied an unsupervised machine-learning method to domes that are annularly or radially distributed around Gardner, a unique central-vent volcano located in the northern part of the Mare Tranquillitatis. High-resolution lunar imaging and spectral data were used to extract morphometric and spectral properties of domes in both the Gardner volcano and its surrounding region in the Mare Tranquillitatis. An integrated robust Fuzzy C-Means clustering algorithm was performed on 120 combinations of five morphometric (diameter, area, height, surface volume, and slope) and two elemental features (FeO and TiO2 contents) to find the optimum combination. Rheological features of domes and their dike formation parameters were calculated for dome-forming lava explanations. Results show that diameter, area, surface volume, and slope are the selected optimum features for dome clustering. 54 studied domes can be grouped into four dome clusters (DC1 to DC4). DC1 domes are relatively small, steep, and close to the Gardner volcano, with forming lavas of high viscosities and low effusion rates, representing the latest Eratosthenian dome formation stage of the Gardner volcano. Domes of DC2 to DC4 are relatively large, smooth, and widely distributed, with forming lavas of low viscosities and high effusion rates, representing magmatic activities varying from Imbrian to Eratosthenian in the northern Mare Tranquillitatis. The integrated algorithm provides a new and independent way to figure out the representative properties of lunar domes and helps us further clarify the relationship between dome clusters and local magma activities of the Moon.

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“…Jull & MacKenzie, 1996) [well understood], magma transport towards the surface (e.g. Michaut and Pinel, 2018) [well understood], and the stability of crustal magma storage zones (Sigmundsson et al, 2010, Sigmundsson et al, 2013 [well understood]. As a counterpart to ice-retreat, sea-level rise (Fasullo and Nerem, 2018) may also decrease mantle melting rates and carbon outgassing at mid-ocean ridges on glacial timescales (Crowley et al, 2015;Tolstoy, 2015;Boulahanis et al, 2020) [hypothesised].…”

Section: Ii-advances Made In Exploring Climate-volcano Impacts Over the Last Two Decadesmentioning

confidence: 99%

Impact of climate change on volcanic processes: current understanding and future challenges

Aubry¹,

Farquharson²,

Rowell³

et al. 2021

Preprint

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The impacts of volcanic eruptions on climate are increasingly well understood, but the mirror question of how climate changes affect volcanic systems and processes, which we term “climate-volcano impacts”, remains understudied. Accelerating research on this topic is critical in view of rapid climate change driven by anthropogenic activities. Over the last two decades, we have improved our understanding of how mass distribution on the Earth’s surface, in particular changes in ice and water distribution linked to glacial cycles, affects mantle melting, crustal magmatic processing and eruption rates. New hypotheses on the impacts of climate change on eruption processes have also emerged, including how eruption style and volcanic plume rise are affected by changing surface and atmospheric conditions, and how volcanic sulfate aerosol lifecycle, radiative forcing and climate impacts are modulated by background climate conditions. Future improvements in past climate reconstructions and current climate observations, volcanic eruption records and volcano monitoring, and numerical models will contribute to boost research on climate-volcano impacts. Important mechanisms remain to be explored, such as how changes in atmospheric circulation and precipitation will affect the volcanic ash lifecycle. Fostering a holistic and interdisciplinary approach to climate-volcano impacts is critical to gain a full picture of how ongoing climate changes may affect the environmental and societal impacts of volcanic activity.

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Magma Ascent and Eruption Triggered by Cratering on the Moon

Cited by 25 publications

References 30 publications

Thickness of Lunar Mare Basalts: New Results Based on Modeling the Degradation of Partially Buried Craters

Thickness of Lunar Mare Basalts: New Results Based on Modeling the Degradation of Partially Buried Craters

Unsupervised Machine Learning on Domes in the Lunar Gardner Region: Implications for Dome Classification and Local Magmatic Activities on the Moon

Impact of climate change on volcanic processes: current understanding and future challenges

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