Masters of Science / The redistribution patterns of trace elements related to ore mineralisation in the secondary environment are the foundation of regolith exploration geochemistry. Understanding the controls of these element patterns is important for the detection of underlying ore deposits, especially in areas where bedrock is concealed by extensive regolith. The study area, which hosts PGE and gold deposits within the Stella Layered Intrusion is one such area. A major aim of this study was to use major element data to characterise the regolith materials enclosing the PGE mineralisation in the Stella Layered Intrusion to ascertain the degree of weathering that has occurred. Furthermore, the study aimed to relate the weathering patterns in regolith to the distribution of pathfinder elements of PGEs and gold in areas proximal and distal to the mineralised zones. The study was conducted using XRF data, which included major oxide and trace element data. These data were used to characterise regolith materials (scatter plots, K/Al versus Mg/Al plots) and calculating indices that determine the degree of weathering such as CIA and ICV indices as well as A-CN-K and A-CN-FM diagrams. Signatures of pathfinder/ trace elements were enhanced by hydroxylamine hydrochloride partial selective leach technique. The distribution patterns of the partial leach data were compared to the intensity of weathering and weathering products, e.g. manganese oxides, carbonates in areas proximal and distal to the ore zone. In the Serpens North Prospect, the major horizons that were identified include saprolith, stone line and aeolian sands. Incipient calcrete formation occurs in some parts of the Sirius Prospect, while in some parts, well developed, thick calcrete layers are found interlayered with the saprolith and aeolian sand.

No description available.

The purpose of the following research is to explore molten regolith electrolysis (MRE) methodology for in-situ resource utilization (ISRU) of Highlands lunar regolith, to be explored during the initial Artemis missions. An analysis of potential commercial launch providers for MRE-equipment based on technology-readiness level (TRL), payload mass support, and $ USD/kg payload price is provided. SpaceX is ultimately proposed as a launch provider of MRE equipment following multi-factorial analysis, with the SpaceX Starship human landing system (HLS) variant proposed for supporting MRE payload. Finally, customers of regolith-derived oxygen, aluminum, and silicon are distinguished to form the business case for operating MRE equipment on the lunar surface.

This study investigated an oxidation-reduction reaction involving a mixture of minerals, glass, and aluminum that exhibited thermite-type reaction behavior. Thermite reactions are a class of Self-propagating High-temperature Synthesis (SHS) reactions. Chemical reactions between raw minerals and a reducing agent, which exhibit thermite-type reaction behavior, are termed geothermite reactions by the author. Geothermite reactions have the potential for use in In-Situ Resource Utilization (ISRU) applications on the Earth, the Moon, Mars, and beyond. A geothermite reaction was shown to occur between two particle size distributions of lunar regolith simulant. Regolith simulant is a naturally occurring mixture of minerals and glass mined from a volcanic ash deposit. The chemical composition of the simulant is similar to actual lunar regolith found on the Moon. The product of the reaction was a ceramic-composite material. The effect of reactant stoichiometry, regolith simulant particle size, and reaction environment on phase formation, microstructure, and compressive strength of the reaction product was investigated. Reaction environments used in this study included a standard atmosphere and a vacuum environment of 0.600 Torr. In addition, the energy required to initiate each reaction using various reaction parameters was measured. X-ray diffraction (XRD) analysis of reaction products synthesized in a standard atmosphere and in vacuum typically indicated the presence of the chemical species: silicon, corundum (α -Al₂O₃), spinel (MgAl₂O₄), and grossite (CaAl₄O₇). Many additional chemical species were present; their occurrence depended on reaction parameters used during synthesis. Diffraction peaks were observed for phases of aluminum nitride within all reaction products formed in a standard atmosphere. Scanning Electron Microscopy (SEM) showed the presence of whisker networks throughout the microstructure for all reactions conducted in a standard atmosphere. Energy Dispersive Spectroscopy (EDS) indicated the presence of aluminum and nitrogen within many of the whiskers. It was hypothesized that many of the whisker networks were composed of phases of aluminum nitride. No whisker networks were observed in the vacuum synthesized reaction products. Maximum mean compressive strengths were found to be ~ 18 MPa and occurred in the coarse particle size distribution of simulant using the smallest quantity of aluminum. Reactant mixtures using a coarse particle size distribution of regolith simulant were found to require substantially more energy to initiate the reaction than the simulant with the fine particle size distribution. / Master of Science

The lunar space environment is shaped by the interaction between the Moon and the solar wind. In the present thesis, we investigate two aspects of this interaction, namely the interaction between solar wind protons and lunar crustal magnetic anomalies, and the interaction between solar wind protons and lunar regolith. We use particle sensors that were carried onboard the Chandrayaan-1 lunar orbiter to analyze solar wind protons that reflect from the Moon, including protons that capture an electron from the lunar regolith and reflect as energetic neutral atoms of hydrogen. We also employ computer simulations and use a hybrid plasma solver to expand on the results from the satellite measurements. The observations from Chandrayaan-1 reveal that the reflection of solar wind protons from magnetic anomalies is a common phenomenon on the Moon, occurring even at relatively small anomalies that have a lateral extent of less than 100 km. At the largest magnetic anomaly cluster (with a diameter of 1000 km), an average of ~10% of the incoming solar wind protons are reflected to space. Our computer simulations show that these reflected proton streams significantly modify the global lunar plasma environment. The reflected protons can enter the lunar wake and impact the lunar nightside surface. They can also reach far upstream of the Moon and disturb the solar wind flow. In the local environment at a 200 km-scale magnetic anomaly, our simulations show a heated and deflected plasma flow and the formation of regions with reduced or increased proton precipitation. We also observe solar wind protons reflected from the lunar regolith. These proton fluxes are generally lower than those from the magnetic anomalies. We find that the proton reflection efficiency from the regolith varies between ~0.01% and ~1%, in correlation with changes in the solar wind speed. We link this to a velocity dependent charge-exchange process occurring when the particles leave the lunar regolith. Further, we investigate how the properties of the reflected neutral hydrogen atoms depend on the solar wind temperature. We develop a model to describe this dependence, and use this model to study the plasma precipitation on the Moon when it is in the terrestrial magnetosheath. We then use the results from these and other studies, to model solar wind reflection from the surface of the planet Mercury. / Rymdmiljön runt månen formas av den växelverkan som sker mellan månen och solvinden. I den föreliggande avhandlingen undersöker vi två aspekter av denna växerverkan, nämligen växelverkan mellan solvindsprotoner och magnetiserade områden i månskorpan, och växelverkan mellan solvindsprotoner och månens ytdamm. Vi använder oss av partikelsensorer på månsatelliten Chandrayaan-1 för att analysera solvindsprotoner som reflekteras från månen, även de protoner som fångar upp en elektron från ytan och reflekteras som neutrala väteatomer. Vi använder oss också av datorsimuleringar för att bygga vidare på de uppmätta resultaten. Observationerna från Chandrayaan-1 visar att reflektion av solvindsprotoner från magnetiserade områden är ett vanligt förekommande fenomen på månen, som inträffar även vid magnetiseringar som är utbredda över mindre än 100 km. Vid det största magnetiserade området på månen (1000 km i diameter), reflekteras i genomsnitt ~10% av de infallande solvindsprotonerna. Våra datorsimuleringar visar att dessa protonflöden har globala effekter på månens plasmamiljö. De reflekterade protonerna kan nå månens nattsida. De kan också nå långt uppströms om månen och störa solvindsflödet. I den lokala plasmamiljön vid ett magnetiserat område av storleken 200 km visar våra simuleringar ett förändrat solvindsflöde, där det skapas områden som delvis skyddas från solvinden, likväl som områden som utsätts för mer solvind. Vi observerar även solvindsprotoner som reflekterats från ytdammet på månen. Dessa protonflöden är lägre än de från de magnetiska fälten. Reflektionen från ytan varierar mellan ~0.01% och 1% av solvindsflödet, i samband med förändringar i solvindshastigheten. Vi förklarar detta med att partiklarnas laddning bestäms av den hastighet de har när de lämnar måndammet. Vidare undersöker vi hur egenskaperna hos de reflekterade neutrala väteatomerna beror på solvindstemperaturen. Vi skapar en modell för att beskriva sambandet och använder sedan denna modell för att studera hur solvinden faller in mot månens yta när den befinner sig i jordens magnetoskikt, där jordens magnetfält orsakar en upphettning av solvindsflödet. Resultaten från dessa och andra studier använder vi sedan för att modellera solvindsreflektion från planeten Merkurius yta, för jämförelse med framtida observationer.

La disponibilité et la mobilité du chrome ont été étudiées sur quatre sols développés sur le complexe ultramafique de Niquelândia (état du Goiàs, Brésil), à l'aide d'expérimentations en laboratoire et in situ. La teneur totale en chrome de ces sols est particulièrement élevée, et sa compartimentation évolue avec la position dans la toposéquence et la profondeur du sol. La majorité du chrome est associée aux oxydes de fer bien cristallisés qui constituent la matrice solide des sols. Il est également présent au sein des chromites, et de phases mineures silicatées. La quantité de chrome extractible est importante et majoritairement sous sa forme toxique (CrVI). Cette fraction atteint 1000 mg kg-1 soit plus de 10% du chrome total; ces teneurs sont dix fois supérieures à celles observées en Nouvelle-Calédonie. Des cinétiques d'échange isotopique du chromate ont confirmé la labilité de cette fraction. Elles ont également mis en évidence une vitesse d'échange rapide entre les phases porteuses et la solution, ainsi qu'une capacité élevée de ces sols à maintenir une importante concentration de chromate en solution. L'ensemble des résultats indique que le Cr(VI) labile est désorbé depuis la fraction fine composée d'oxydes de fer qui contrôle ainsi sa disponibilité et sa mobilité. Les résultats suggèrent que le chromate labile est faiblement adsorbé aux phases porteuses. La disponibilité du chrome est très hétérogène à des échelles décimétrique et décamétrique. L'étude des eaux du sol et de surface à l'échelle du bassin versant a mis en évidence une mobilité importante du Cr(VI) et des concentrations en chromate supérieures aux teneurs considérées comme toxiques, suggérant un impact sur les organismes vivants du complexe et également les écosystèmes environnants. D'autre part, l'analyse des solutions du sol a confirmé la faible teneur en nutriments, le rapport défavorable Ca:Mg et la disponibilité de certains métaux (Cr, Ni) typiques de ces milieux. Ces trois caractéristiques sont souvent considérés comme responsable de la faible fertilité de ce type de sol et du particularisme de ces écosystèmes. Enfin, les résultats suggèrent que la disponibilité en Cr(VI) de ces sols résulte de leur capacité d'échange anionique et non d'oxydation du Cr(III)

<p>The properties of Mercury's regolith have been investigated at optical and near-infrared wavelengths with high-resolution imaging, photometric, and spectroscopic observations with the Swedish Vacuum Solar Telescope and the Nordic Optical Telescope. </p><p>A new global optical map at a spatial resolution of 200 km shows that the well known (from Mariner 10) and poorly known hemispheres are indistinguishable with respect to the distribution, number density, and morphological parameters of bright albedo features. This indicates a globally uniform recent (<3 Gyr) geologic evolution, a compositionally very homogeneous surface and the absence of a lunar-like mare–terrae albedo dichotomy.</p><p>It is found that the spectrum of Mercury is linear, strongly sloped, lacks detectable absorption features and displays a unique relation between the continuum slope and photometric geometry. Mercury has a photometrically smoother surface than the average near-side Moon, and is 10–15% fainter and 50% more back scattering in the V-band. Unlike the case for the Moon, the average single-particle backscattering anisotropy increases with wavelength.</p><p>Intimate regolith mixing models are used to determine a probable surface composition of predominantly Ca-rich labradorite plagioclase feldspar with minor low-iron enstatitic orthopyroxene, and rule out high-iron pyroxenes or olivines as other than insignificant constituents. Abundances of FeO ~1.2 wt%, TiO₂ ~0 wt%, and submicroscopic metallic iron ~0.1–0.3 wt% are found for the average surface. This implies an optically active grain size of 15–30 μm that is a factor of two smaller than for the Moon.</p><p>A numerical integration study shows that hermeocentric orbits with semi-major axes <30 mercurian radii for elliptic retrograde, and circular prograde, object are stable for durations in excess of 4.5 Myr. The weak gravitational scattering effect of Mercury indicates that re-impacting particles may have been important for the early evolution of its crust.</p>

The properties of Mercury's regolith have been investigated at optical and near-infrared wavelengths with high-resolution imaging, photometric, and spectroscopic observations with the Swedish Vacuum Solar Telescope and the Nordic Optical Telescope. A new global optical map at a spatial resolution of 200 km shows that the well known (from Mariner 10) and poorly known hemispheres are indistinguishable with respect to the distribution, number density, and morphological parameters of bright albedo features. This indicates a globally uniform recent (&lt;3 Gyr) geologic evolution, a compositionally very homogeneous surface and the absence of a lunar-like mare–terrae albedo dichotomy. It is found that the spectrum of Mercury is linear, strongly sloped, lacks detectable absorption features and displays a unique relation between the continuum slope and photometric geometry. Mercury has a photometrically smoother surface than the average near-side Moon, and is 10–15% fainter and 50% more back scattering in the V-band. Unlike the case for the Moon, the average single-particle backscattering anisotropy increases with wavelength. Intimate regolith mixing models are used to determine a probable surface composition of predominantly Ca-rich labradorite plagioclase feldspar with minor low-iron enstatitic orthopyroxene, and rule out high-iron pyroxenes or olivines as other than insignificant constituents. Abundances of FeO ~1.2 wt%, TiO2 ~0 wt%, and submicroscopic metallic iron ~0.1–0.3 wt% are found for the average surface. This implies an optically active grain size of 15–30 μm that is a factor of two smaller than for the Moon. A numerical integration study shows that hermeocentric orbits with semi-major axes &lt;30 mercurian radii for elliptic retrograde, and circular prograde, object are stable for durations in excess of 4.5 Myr. The weak gravitational scattering effect of Mercury indicates that re-impacting particles may have been important for the early evolution of its crust.

This study used images taken from the OSIRIS-REx spacecraft sample-return mission and projected onto a three-dimensional shape model to determine surface properties of the asteroid (101955) Bennu. Two major projects were completed. For the first project, images of the pre-sampled Nightingale site and post-sampled Nightingale were compared to determine how the TAGSAM sampling maneuver effected the surface of the asteroid directly at the sampling site and in the surrounding area. This analysis demonstrated how spacecraft can potentially affect a small body during this and future sample-return missions. For the second project, several craters on Bennu’s surface were selected and all of the boulders within their rims and up to one crater radius outward from their rims were counted and measured. The interior and exterior of all craters were compared which determined that there is a pattern that supports the existence of a subsurface layer of finer-grained material which could be responsible for cohesion on Bennu and potentially other rubble-pile asteroids

No description available.