東華大學圖書館 |

Combining Sample and Data Science With Remote Sensing Observations to Constrain the Thermal Evolution of the Moon /

紀錄類型:	書目-電子資源 : Monograph/item
正題名/作者:	Combining Sample and Data Science With Remote Sensing Observations to Constrain the Thermal Evolution of the Moon // Alissa Madera.
作者:	Madera, Alissa,
面頁冊數:	1 electronic resource (262 pages)
附註:	Source: Dissertations Abstracts International, Volume: 87-04, Section: B.
Contained By:	Dissertations Abstracts International87-04B.
標題:	Petrology. -
電子資源:	https://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=32239667
ISBN:	9798297618718

Combining Sample and Data Science With Remote Sensing Observations to Constrain the Thermal Evolution of the Moon /
Madera, Alissa,

Combining Sample and Data Science With Remote Sensing Observations to Constrain the Thermal Evolution of the Moon /Alissa Madera. - 1 electronic resource (262 pages)

Source: Dissertations Abstracts International, Volume: 87-04, Section: B.

The Moon is a cornerstone for understanding the formation, differentiation, and evolution of rocky bodies within our solar system. Volcanism played a crucial role in the Moon's geologic evolution and rocks that sample these volcanic events provide valuable insight into the Moon's thermal history. Studies of relative age dating through remote sensing and crater-size frequency distributions (CSFD) have shown that lunar volcanism was active on the Moon between ~4.0 billion years ago to potentially <1.0 billion years ago. However, long-lived volcanism contradicts models of lunar evolution that suggest the interior of the Moon should have ceased melting early on in geologic history. The drivers and dynamics of prolonged lunar volcanism are not well understood but studying lithologic products generated from lunar volcanic events can help us to better constrain the structure and composition of the lunar mantle over geologic time, which in turn, places valuable constraints on the evolution of the second most accessible rocky body in our solar system, the Moon.Within this work, we aim to constrain the drivers and dynamics of late-stage mare basalt volcanism recorded by young, lunar basaltic meteorites in order to place better constraints on the Moon's thermal history. The majority of returned lunar volcanic samples (i.e., Apollo and Luna missions) have radiometric ages that overlap with early lunar thermal evolution (between ~4.0 to 3.1 billion years ago) with a small fraction of the remaining returned volcanic samples (i.e., Chang'e missions) representing late lunar thermal evolution (2.8 and 2.0 billion years ago). However, the returned samples do not represent a complete timeline of the Moon's thermal history as they have been sampling only very limited areas of the lunar surface. Additionally, most of these returned samples were collected in geochemically unique regions that are not representative of a global Moon and, consequently, are also not representative of a global lunar interior. Northwest Africa (NWA) 8632 is an unbrecciated basaltic lunar meteorite with preliminary radiometric ages younger than 3.0 Ga and thus represents a sample of prolonged lunar volcanism. We performed an in-depth petrologic study of NWA 8632 using both qualitative and quantitative analyses by Electronprobe Microanalysis (EPMA), Ionic Coupling Optical Emission Spectroscopy (ICP-OES)/Triple Quad Mass Spectroscopy (ICP-QQQ-MS), and Ar-Ar radiometric age dating in order to assess a new absolute age date for NWA 8632 and compare new bulk-rock chemistry, mineral chemistry, and texture with compositionally and texturally similar mare basalts. Our results show that NWA 8632 is a low-K, low-Al, low-Ti mare basalt with a Mg# [=(Mg/(Mg+Fe)] of 44.4. Our new Ar-Ar isotope radiometric ages indicate that NWA 8632 crystallized between 2.878 ± 0.025 Ga and 2.877 ± 0.034 Ga using the step-wise heating method and between 2.820 ± 0.100 Ga and 2.946 ± 0.094 Ga for measured isochrons with derived cosmic ray exposure ages (CRE) between 162 ± 15 Ma to 157 ± 13 Ma. These new crystallization ages of NWA 8632 overlap with the reported ages for the North-North-Lapaz (NNL) Clan meteorites, that include NWA 032, NWA 4734, and LaPaz Icefield (LAP) 02205. NWA 8632 has a porphyritic texture, modal mineral abundances most similar to NWA 032, and a rare earth element (REE) abundance more similar to Apollo 12 and 15 low-Ti mare basalt suites (e.g., olivine, ilmenite, and pigeonite). Minerals olivine, pyroxene, and spinel in NWA 8632 follow similar chemical and fractional crystallization trends as those reported in NWA 032, LAP 02205, and NWA 4734. The impact produced melt vein compositions in NWA 8632 overlap with the NNL clan meteorite bulk compositions in major oxides but are not representative of a bulk rock composition for NWA 8632. Olivine addition calculations using the lever rule and the most magnesian olivine (Mg# 71.8) within NWA 8632 that were then added to the bulk rock of NWA 032 show that between 8-12% olivine addition is necessary to match the bulk rock composition of NWA 8632. Thus, NWA 8632 and NWA 032 may be chemically related by olivine-fractionation of compositionally similar parent melts or at the least, are launch-paired samples from the same mare volcanic province.Next, we performed an in-depth mineralogic study of NWA 8632 using both qualitative and quantitative analyses by EPMA, Electron Back Scatter Diffraction (EBSD), and micro X-ray Computed Tomography (micro-XCT) in order to constrain the sequence of crystallization and the magmatic plumbing system of NWA 8632 by parametrizing the intrinsic and extrinsic influences on the magma from which NWA 8632 crystallized, including mineral residence times within the magma chamber, temperature, and oxygen fugacity. Our results show that NWA 8632 represents a primary melt composition that crystallized for upwards of 407 days within the lunar interior before eruption onto the lunar surface, based on estimates of residence times derived from the earliest crystallized olivine. Phosphorus (P) oscillatory zoning in second-generation olivine was dominated by diffusion-controlled growth at high degree of undercoolings of the melt, with an initial and rapid dendritic stage of primary and secondary branches enriched in incompatible P that was followed by a period of slow growth. Sector-zoning of major elements Mg, Ca and minor elements Al, Ti, Cr, and V in large, euhedral pyroxenes are in chemical equilibrium with the P-zoned olivine and was also dominated by diffusion-controlled growth at high supersaturation of the melt at near-chemical equilibrium conditions. The potential drivers for the onset of P-zoned and sector-zoned co-genetic minerals are a thermal gradient in the magma chamber from conductive cooling of the surrounding wall-rock and crystal settling of earlier crystallizing olivine. Increased undercooling and increased cooling rates drove the nucleation of highly disequilibrium crystal habits, such as elongated chains of pyroxenes, dendritic pyroxenes, and hopper olivine crystals during magma ascent and eruption onto the lunar surface. During rapid ascent to the lunar surface, the elongated chains of pyroxenes aligned along the b-crystallographic axis with the flow of the magma through the conduits, oscillatory zoning of minor elements Ti, Al, and Cr and epitaxial growth of augite mantling pigeonite in euhedral pyroxenes recorded the turbulent nature of a rapid ascending magma, and dehydrogenation of OH bound H exsolved from olivine grain structures which may have driven the formation of Type I symplectites. These findings confirm that dynamic and complex magma plumbing systems exist on the Moon and may provide the framework for understanding how large suites of geochemically distinct mare basalts, that erupted close in age, are connected. To identify the location of the mare volcanic province that NWA 8632 may be sourced from and to place it in its geologic context, we developed a program capable of comparing small-scale meteoritic geochemical analyses with macroscopic remote sensing observations. The Lunar-Sample-Provenance (LSP) program is an open-source code in the python programming language that utilizes orbital chemical maps derived from the Lunar Prospector - Gamma Ray Spectrometer (LP-GRS) and Lunar Reconnaissance Orbiter (LRO) - DIVINER Instruments. The LSP program was validated using returned lunar regolith samples from the Apollo, Luna, and Chang'e missions as well and representative breccias and single-lithologic rocks from the Apollo and Chang'e missions. Lastly, models of origin are explored for NWA 8632 and the hypothesized launch-paired meteorites NWA 032, NWA 4734, and LAP 02205 by comparing bulk-rock compositions, mineral chemistries, radiometric ages, ejection histories, and potential source regions. Results are used to evaluate the petrogenetic relationship shared between late-stage mare basalts and to place constraints on dynamics and structure of evolved lunar interior at 2.9 Ga. Geochemical, mineralogical, and ejection histories suggests that these meteorites are launch-paired from a common volcanic province, possibly Mare Serenitatis.

English

ISBN: 9798297618718Subjects--Topical Terms:

535210
Petrology.
Subjects--Index Terms:

Lunar petrology

Combining Sample and Data Science With Remote Sensing Observations to Constrain the Thermal Evolution of the Moon /
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520 $a The Moon is a cornerstone for understanding the formation, differentiation, and evolution of rocky bodies within our solar system. Volcanism played a crucial role in the Moon's geologic evolution and rocks that sample these volcanic events provide valuable insight into the Moon's thermal history. Studies of relative age dating through remote sensing and crater-size frequency distributions (CSFD) have shown that lunar volcanism was active on the Moon between ~4.0 billion years ago to potentially <1.0 billion years ago. However, long-lived volcanism contradicts models of lunar evolution that suggest the interior of the Moon should have ceased melting early on in geologic history. The drivers and dynamics of prolonged lunar volcanism are not well understood but studying lithologic products generated from lunar volcanic events can help us to better constrain the structure and composition of the lunar mantle over geologic time, which in turn, places valuable constraints on the evolution of the second most accessible rocky body in our solar system, the Moon.Within this work, we aim to constrain the drivers and dynamics of late-stage mare basalt volcanism recorded by young, lunar basaltic meteorites in order to place better constraints on the Moon's thermal history. The majority of returned lunar volcanic samples (i.e., Apollo and Luna missions) have radiometric ages that overlap with early lunar thermal evolution (between ~4.0 to 3.1 billion years ago) with a small fraction of the remaining returned volcanic samples (i.e., Chang'e missions) representing late lunar thermal evolution (2.8 and 2.0 billion years ago). However, the returned samples do not represent a complete timeline of the Moon's thermal history as they have been sampling only very limited areas of the lunar surface. Additionally, most of these returned samples were collected in geochemically unique regions that are not representative of a global Moon and, consequently, are also not representative of a global lunar interior. Northwest Africa (NWA) 8632 is an unbrecciated basaltic lunar meteorite with preliminary radiometric ages younger than 3.0 Ga and thus represents a sample of prolonged lunar volcanism. We performed an in-depth petrologic study of NWA 8632 using both qualitative and quantitative analyses by Electronprobe Microanalysis (EPMA), Ionic Coupling Optical Emission Spectroscopy (ICP-OES)/Triple Quad Mass Spectroscopy (ICP-QQQ-MS), and Ar-Ar radiometric age dating in order to assess a new absolute age date for NWA 8632 and compare new bulk-rock chemistry, mineral chemistry, and texture with compositionally and texturally similar mare basalts. Our results show that NWA 8632 is a low-K, low-Al, low-Ti mare basalt with a Mg# [=(Mg/(Mg+Fe)] of 44.4. Our new Ar-Ar isotope radiometric ages indicate that NWA 8632 crystallized between 2.878 ± 0.025 Ga and 2.877 ± 0.034 Ga using the step-wise heating method and between 2.820 ± 0.100 Ga and 2.946 ± 0.094 Ga for measured isochrons with derived cosmic ray exposure ages (CRE) between 162 ± 15 Ma to 157 ± 13 Ma. These new crystallization ages of NWA 8632 overlap with the reported ages for the North-North-Lapaz (NNL) Clan meteorites, that include NWA 032, NWA 4734, and LaPaz Icefield (LAP) 02205. NWA 8632 has a porphyritic texture, modal mineral abundances most similar to NWA 032, and a rare earth element (REE) abundance more similar to Apollo 12 and 15 low-Ti mare basalt suites (e.g., olivine, ilmenite, and pigeonite). Minerals olivine, pyroxene, and spinel in NWA 8632 follow similar chemical and fractional crystallization trends as those reported in NWA 032, LAP 02205, and NWA 4734. The impact produced melt vein compositions in NWA 8632 overlap with the NNL clan meteorite bulk compositions in major oxides but are not representative of a bulk rock composition for NWA 8632. Olivine addition calculations using the lever rule and the most magnesian olivine (Mg# 71.8) within NWA 8632 that were then added to the bulk rock of NWA 032 show that between 8-12% olivine addition is necessary to match the bulk rock composition of NWA 8632. Thus, NWA 8632 and NWA 032 may be chemically related by olivine-fractionation of compositionally similar parent melts or at the least, are launch-paired samples from the same mare volcanic province.Next, we performed an in-depth mineralogic study of NWA 8632 using both qualitative and quantitative analyses by EPMA, Electron Back Scatter Diffraction (EBSD), and micro X-ray Computed Tomography (micro-XCT) in order to constrain the sequence of crystallization and the magmatic plumbing system of NWA 8632 by parametrizing the intrinsic and extrinsic influences on the magma from which NWA 8632 crystallized, including mineral residence times within the magma chamber, temperature, and oxygen fugacity. Our results show that NWA 8632 represents a primary melt composition that crystallized for upwards of 407 days within the lunar interior before eruption onto the lunar surface, based on estimates of residence times derived from the earliest crystallized olivine. Phosphorus (P) oscillatory zoning in second-generation olivine was dominated by diffusion-controlled growth at high degree of undercoolings of the melt, with an initial and rapid dendritic stage of primary and secondary branches enriched in incompatible P that was followed by a period of slow growth. Sector-zoning of major elements Mg, Ca and minor elements Al, Ti, Cr, and V in large, euhedral pyroxenes are in chemical equilibrium with the P-zoned olivine and was also dominated by diffusion-controlled growth at high supersaturation of the melt at near-chemical equilibrium conditions. The potential drivers for the onset of P-zoned and sector-zoned co-genetic minerals are a thermal gradient in the magma chamber from conductive cooling of the surrounding wall-rock and crystal settling of earlier crystallizing olivine. Increased undercooling and increased cooling rates drove the nucleation of highly disequilibrium crystal habits, such as elongated chains of pyroxenes, dendritic pyroxenes, and hopper olivine crystals during magma ascent and eruption onto the lunar surface. During rapid ascent to the lunar surface, the elongated chains of pyroxenes aligned along the b-crystallographic axis with the flow of the magma through the conduits, oscillatory zoning of minor elements Ti, Al, and Cr and epitaxial growth of augite mantling pigeonite in euhedral pyroxenes recorded the turbulent nature of a rapid ascending magma, and dehydrogenation of OH bound H exsolved from olivine grain structures which may have driven the formation of Type I symplectites. These findings confirm that dynamic and complex magma plumbing systems exist on the Moon and may provide the framework for understanding how large suites of geochemically distinct mare basalts, that erupted close in age, are connected. To identify the location of the mare volcanic province that NWA 8632 may be sourced from and to place it in its geologic context, we developed a program capable of comparing small-scale meteoritic geochemical analyses with macroscopic remote sensing observations. The Lunar-Sample-Provenance (LSP) program is an open-source code in the python programming language that utilizes orbital chemical maps derived from the Lunar Prospector - Gamma Ray Spectrometer (LP-GRS) and Lunar Reconnaissance Orbiter (LRO) - DIVINER Instruments. The LSP program was validated using returned lunar regolith samples from the Apollo, Luna, and Chang'e missions as well and representative breccias and single-lithologic rocks from the Apollo and Chang'e missions. Lastly, models of origin are explored for NWA 8632 and the hypothesized launch-paired meteorites NWA 032, NWA 4734, and LAP 02205 by comparing bulk-rock compositions, mineral chemistries, radiometric ages, ejection histories, and potential source regions. Results are used to evaluate the petrogenetic relationship shared between late-stage mare basalts and to place constraints on dynamics and structure of evolved lunar interior at 2.9 Ga. Geochemical, mineralogical, and ejection histories suggests that these meteorites are launch-paired from a common volcanic province, possibly Mare Serenitatis.
520 $a Additionally, the bulk rock compositions of NWA 8632, NWA 032, NWA 4734, and LAP 02205 reflect derivation from a shared parent melt, suggesting that these four meteorites represent comagmatic basaltsthat experienced varying partial melting and crystallization histories prior to locally and temporally emplaced eruptions within a single volcanic complex, similar to the Apollo 12 and 15 low-Ti mare basalt suites. NWA 8632 appears to be closest in composition to the parent melt, with an estimated origin at 0.7 GPa and ~1300°C, possibly influenced by hydrous conditions rather than KREEP. Collectively, these works show how geochemically distinct lunar basalts can be linked as large, co-magmatic suites that were partially melted from the same cumulate source but ultimately experienced contrasting crystallization histories that diverge their chemistries. Additionally, the program developed to identify lunar meteorites source regions provides the planetary community with a new, open-source method that maximizes the scientific return from both sample and orbital science.
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