4. Thermal and Magmatic Evolution of the Moon

Shearer, C. K.; Hess, P. C.; Wieczorek, M. A.; Pritchard, M. E.; Parmentier, E. Mark; Borg, L. E.; Longhi, J.; Elkins-Tanton, Linda T.; Neal, C. R.; Antonenko, I.; Canup, R. M.; Halliday, Alex N.; Grove, Tim L.; Hager, Bradford H.; Lee, D-C.; Wiechert, Uwe

doi:10.1515/9781501509537-008

Cited by 87 publications

(22 citation statements)

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“…The early Moon may have had a short-lived and episodic atmosphere due to magmatic degassing (Hui et al, 2018;Needham & Kring, 2017), which may interfere the interaction between the plasma particles and lunar soils. This atmosphere, however, must have been lost shortly after the main volcanism at 3.3-3.8 Ga on the Moon (Shearer et al, 2006). With limited interference of the lunar exosphere, the lunar soil grains could have recorded the implantation activities of plasma particles over the last several billion years.…”

Section: Testing Methods Of Hypothesismentioning

confidence: 99%

Implantation of Earth's Atmospheric Ions Into the Nearside and Farside Lunar Soil: Implications to Geodynamo Evolution

Wei

Zhong

Hui

et al. 2020

Geophysical Research Letters

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Earth's present dipolar magnetic field extends into the interplanetary space and interacts with the solar wind, forming a magnetosphere filled up with charged particles mostly originating from the Earth's atmosphere. In the elongated tail of the magnetosphere, the particles were observed to move either Earthward or tailward at different locations, even outside the Moon's orbit. We hypothesize that the lunar soil, on both the nearside and farside, should have been impacted by these particles during the geological history, and the impact was controlled by the size and morphology of the magnetosphere. We predict that the farside soil could also have the features similar to those in the nearside soil, e.g., 15N‐enrichment. Furthermore, we may infer the evolution of the magnetosphere and atmosphere by examining the implanted particles in the lunar soil from both sides. This hypothesis could provide an alternative way to study the evolution of Earth's dynamo and atmosphere.

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Section: Testing Methods Of Hypothesismentioning

confidence: 99%

Implantation of Earth's Atmospheric Ions Into the Nearside and Farside Lunar Soil: Implications to Geodynamo Evolution

Wei

Zhong

Hui

et al. 2020

Geophysical Research Letters

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“…We consider that the uniaxial pressure by collision with meteorites is similar to that by collision synthesis with super-high-energy ball milling. It is reported that geikielite-rich ilmenite rocks are important for the Moon's anomalies (33). It is considered that the anomalies in Mars require very large rock volumes over areas of hundreds of square kilometers and extending to depths of 20 to 30 km (34,35), where ilmenite exists as an accessory mineral.…”

Section: Discussionmentioning

confidence: 99%

Ferromagnetism and exchange bias in compressed ilmenite-hematite solid solution as a source of planetary magnetic anomalies

2022

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We propose a compressed ilmenite-hematite solid solution as a new potential source of Earth’s magnetic anomalies. The 0.5FeTiO 3 ·0.5Fe 2 O 3 solid solution compressed by collision synthesis with super-high-energy ball milling showed a decrease in molar volume of approximately 1.8%. Consequently, the sample showed a saturation magnetization of 1.5 ampere square meter per kilogram (Am 2 /kg) at 300 kelvin, a Curie temperature of 990 kelvin, and a magnetic exchange bias below 100 kelvin, e.g., 1.7 × 10 5 ampere per meter at 60 kelvin. Ilmenite-hematite solid solutions are common mineral systems in most mafic igneous and metamorphic rocks, and the compressive force in the rocks is generated by the high pressure in the upper mantle or by shock events with high pressure such as the collision of these rocks with meteorites. Therefore, we consider that the compressed ilmenite-hematite solid solution is an additional candidate source of other planetary magnetic anomalies including those in the Moon and Earth.

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“…We note however, that the data from olivine melt inclusions in Apollo 17 orange glass beads suggest a very small H 2 O fraction in the prefragmentation gas phase. Additionally, these values may not be representative of the bulk lunar mantle as the lunar glasses are believed to be generated from partial melting of differentiated and likely volatile enriched LMO material (Delano, 1986; Hess & Parmentier, 1995; Shearer et al., 2006), and the degree of partial melting is estimated to be 5%–10% (Saal,et al., 2008).…”

Section: Discussionmentioning

confidence: 99%

“…These glasses are thought to have been emplaced through Hawaiian‐like, fire‐fountaining eruptions (Wilson & Head, 2003) and include green (low‐Ti), yellow (intermediate Ti), and orange, red, and black glasses (high‐Ti). They represent quenched melts that are ultramafic in composition (Delano, 1986; Saal et al., 2008), crystal poor (Delano, 1986; Saal et al., 2008), were erupted as fine beads (<1 mm) (Delano, 1986; Heiken & McKay, 1977; Longhi, 1992; Saal et al., 2008; Weitz et al., 1998), and are believed to have been generated from magmas sourced at depths of 300–500 km (Delano, 1980; Delano & Lindsley, 1983; Elkins et al., 2000; Elkins‐Tanton et al., 2003; Longhi, 2006; Shearer & Papike, 1993; Shearer et al., 2006). For this reason, they have been used to probe the volatile content of parts of the lunar interior by virtue of melt inclusions, diffusion modeling, and through solubility experiments (Hauri et al., 2011; Rutherford et al., 2017; Saal et al., 2008, 2013).…”

Section: Introductionmentioning

confidence: 99%

Modeling Lunar Pyroclasts to Probe the Volatile Content of the Lunar Interior

et al. 2021

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Several models of lunar formation that have recently gained momentum in the planetary science community involve, to an extent, the giant impact theory (e.g., the terrestrial synestia model of Lock et al. (2018)). In this giant impact theory, the Moon is thought to have been formed from the coalescence of debris from a collision between an impactor and a proto-Earth (Canup, 2004), leading to the formation of a lunar magmatic ocean and the large-scale degassing of the Moon (Lucey et al., 2006). The depletion of hydrogen (e.g., in the form of OH/H 2 O, hereafter referred to simply as "water" or H 2 O) in volcanic samples returned from Luna and Apollo missions seemed to support this, but a growing body of research now suggests that the lunar mantle, or at least some parts of the lunar mantle, may not be as severely depleted in water as previously thought (

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4. Thermal and Magmatic Evolution of the Moon

Cited by 87 publications

References 0 publications

Implantation of Earth's Atmospheric Ions Into the Nearside and Farside Lunar Soil: Implications to Geodynamo Evolution

Implantation of Earth's Atmospheric Ions Into the Nearside and Farside Lunar Soil: Implications to Geodynamo Evolution

Ferromagnetism and exchange bias in compressed ilmenite-hematite solid solution as a source of planetary magnetic anomalies

Modeling Lunar Pyroclasts to Probe the Volatile Content of the Lunar Interior

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