There is strong evidence that water-ice is relatively abundant within permanently shadowed lunar surface materials, particularly at the poles. Evidence for water-ice has been observed within the impact plume of the LCROSS mission and is supported by data gathered from the Lunar Exploration Neutron Detector (LEND) and the Lunar Prospector Neutron Spectrometer (LPNS). Albedo neutrons from the Moon are used for detection of hydrogen, where the epi-thermal neutron flux decreases as hydrogen content increases. The origin on the concentration of water within permanently shadowed regions is not completely understood, and the Lunar Polar Hydrogen Mapper (LunaH-Map) mission is designed to provide a high-resolution spatial distribution of the hydrogen content over the southern pole using a highly elliptical, low perilune orbit. The LunaH-Map spacecraft is a 6U cubesat consisting of the Miniature Neutron Spectrometer (Mini-NS). Mini-NS is not collimated, requiring a low altitude to achieve a higher spatial resolution compared to previous missions. To develop a compact neutron detector for epi-thermal neutrons, the Mini-NS comprises of 2-cm thick slabs of CLYC (Cs2LiYCl6), which provide a sensitivity similar to a 10-atm, 5.7-cm diameter He-3 tubes, as used in LPNS. The Mini-NS digital processing electronics can discriminate by shape and height to determine signal (albedo neutrons) from background (cosmic rays). The Mini-NS achieves a total active sensing area of 200 cm(2) and is covered with a cadmium sheet to shield against thermal neutrons. The research and development on the detector modules show a robust design ready for space flight.

This thesis is concerned with ensuring high energy resolution from the swept charge device (SCD) CCD54, essentially a non-pixellated version of the charge coupled device (CCD), for use in the Chandrayaan-1 X-ray Spectrometer (C1XS). Of particular interest is the effect on performance due to the radiation damage, caused by protons, the CCD54s used in C1XS will receive during the transfer to the Moon and during the two years in lunar orbit. Chapter 2 reviews the atomic structure, the formation and detection of X-rays, and the operation of a CCD. Chapter 3 discusses the space radiation environment and the damaging effects it has on CCDs, for example increasing dark current and charge transfer inefficiency. Chapter 4 presents the basic laboratory equipment and procedure used during the experimental work, and details the initial optimisation and characterisation, the pre-flight characterisation of devices available for use in C1XS, the measurement of the depletion depth, and quantum efficiency of the CCD54. Chapter 5 details the results of the initial proton irradiation study, intended to demonstrate the ability of the CCD54 to provide excellent scientific data over the two years at the Moon. Chapter 6 describes a second irradiation study covering a more detailed investigation of the damage effects, investigating dark current, trap energy levels, and charge transfer inefficiency. Chapter 7 describes work conducted to assist the C1XS science team in the development of an X-ray fluorescence model, to be used with X-ray spectra provided by the X-ray solar monitor and the spectra detected by C1XS, to provide elemental abundance information of the lunar surface. It also presents the initial C1XS results from the Moon, and a brief comparison of the CCD54 with other semiconductor X-ray fluorescence detectors. Chapter 8 describes the final conclusions and recommendations for further work, including a study of the radiation damage effects during the two years at the Moon and the future development of SCD detectors for use in space.

The spins of planetary bodies are not stagnant; they evolve in response to both external and internal forces. One way a planet's spin can change is through true polar wander. True polar wander is the reorientation of a planetary body with respect to its angular momentum vector, and occurs when mass is redistributed within the body, changing its principal axes of inertia. True polar wander can literally reshape a world, and has important implications for a variety of processes—from the long-term stability of polar volatiles in the permanently shadowed regions of airless worlds like the Moon and Mercury, to the global tectonic patterns of icy worlds like Pluto. In this dissertation, we investigate three specific instances of planetary true polar wander, and their associated consequences. In Chapter 2 we investigate the classic problem of the Moon's dynamical figure. By considering the effects of a fossil figure supported by an elastic lithosphere, and the contribution of impact basins to the figure, we find that the lunar figure is consistent with the Moon's lithosphere freezing in when the Moon was much closer to the Earth, on a low eccentricity synchronous orbit. The South Pole-Aitken impact basin is the single largest perturbation to the Moon’s figure and resulted in tens of degrees of true polar wander after its formation. In Chapter 3 we continue our analyses of the lunar figure in light of the discovery of a lunar ”volatile" paleopole, preserved in the distribution of hydrogen near the Moon's poles. We find that the formation and evolution of the Procellarum KREEP Terrain significantly altered the Moon’s orientation, implying that some fraction of the Moon’s polar volatiles are ancient—predating the geologic activity within the Procellarum region. In Chapter 4 we investigate how the formation of the giant, basin-filling glacier, Sputnik Planitia reoriented Pluto. This reorientation is recorded in both the present- day location of Sputnik Planitia (near the Pluto-Charon tidal axis), and the tectonic record of Pluto. This reorientation likely reflects a coupling between Pluto’s volatile cycles and rotational dynamics, and may be active on other worlds with comparably large, mobile volatile reservoirs. Finally, in Chapter 5 we consider the broader context of these studies, and touch on future investigations of true polar wander on Mercury, Venus, Mars, Vesta, Ceres, and other worlds in our solar system.

The work deals with geopolitics of inner solar system with focus on extraterrestrial celestial bodies. First part deals with definitions, delimitation of researched territory, and definition of researched questions. Afterwards, we deal with basics of astrophysics which is necessary precondition for understanding specifics of astropolitics and the issue of space- faring actors. Here, both state and non-state actors, their capacities and ability to become colonizing actor, are assessed. The work continues with exploration of single celestial bodies - Earth's Moon, Mars and its moons, and smaller bodies like asteroids. The final chapter scratches the issues crucial for space colonization such as sovereignty and weaponization. Based on these factors, few models of space colonization are presented. Conclusion then sums up all our findings and geopolitical map of "blue planet's" neighbourhood is presented.

abstract: Water has shaped the surface of Mars, recording previous environments and inspiring the search for extinct life beyond Earth. While conditions on the Martian surface today are not conducive to the presence of liquid water, ancient erosional and depositional features indicate that this was not always so. Quantifying the regional and global history of water on Mars is crucial to understanding how the planet evolved, where to focus future exploration, and implications for water on Earth. Many sites on Mars contain layered sedimentary deposits, sinuous valleys with delta shaped deposits, and other indications of large lakes. The Hypanis deposit is a unique endmember in this set of locations as it appears to be the largest ancient river delta identified on the planet, and it appears to have no topographic boundary, implying deposition into a sea. I have used a variety of high-resolution remote sensing techniques and geologic mapping techniques to present a new model of past water activity in the region. I gathered new orbital observations and computed thermal inertia, albedo, elevation, and spectral properties of the Hypanis deposit. I measured the strike and dip of deposit layers to interpret the sedimentary history. My results indicate that Hypanis was formed in a large calm lacustrine setting. My geomorphic mapping of the deposit and catchment indicates buried volatile-rich sediments erupted through the Chryse basin fill, and may be geological young or ongoing. Collectively, my results complement previous studies that propose a global paleoshoreline, and support interpretations that Mars had an ocean early in its history. Future missions to the Martian surface should consider Hypanis as a high-value sampling opportunity. / Dissertation/Thesis / Doctoral Dissertation Geological Sciences 2019

京都大学 / 0048 / 新制・課程博士 / 博士(理学) / 甲第18084号 / 理博第3962号 / 新制||理||1571(附属図書館) / 30942 / 京都大学大学院理学研究科地球惑星科学専攻 / (主査)准教授 齊藤 昭則, 教授 余田 成男, 准教授 藤 浩明 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DGAM

<div>Evidence of past volcanic activity has been found on many planets and moons in our Solar System, and volcanism represents a common process that ties together the geologic history of planetary bodies. Volcanic eruptions are a unique geologic process that link the planet’s interior to the surface and the atmosphere/exosphere. A key planetary science objective described in the 2013-2022 Decadal Survey is to characterize planetary surfaces and understand their modification by geologic processes, including volcanism. The Earth, Moon, and Mars have evidence of past effusive and explosive volcanic eruptions, creating a range of volcanic edifices, landforms, flows, and pyroclastic deposits. This dissertation strives to understand the composition and eruption style of explosive volcanic deposits on the terrestrial bodies of the Earth, the Moon, and Mars. These deposits provide critical insights into the volcanic and volatile histories of the bodies and may provide in situ resources for future planetary explorers. I utilize data from orbital and laboratory spectrometers to analyze volcanic tephras across the solar system. My dissertation uses new techniques from lab studies to inform orbital spectroscopy and geomorphology comparisons of explosive volcanic deposits. By identifying glass and other igneous minerals in the visible/near-infrared and thermal infrared orbital spectra of volcanic deposits we can infer volcanic eruption style and constrain the history of explosive volcanism of planetary bodies. With remote sensing, I investigated a large and ancient volcanic complex, the Marius Hills, with significant implications for the early volcanic history of the Moon and the pyroclastic deposits of a single impact basin, Schrödinger, that has been selected as a landing site for robotic missions in 2024. This dissertation expands on the previous limited understanding of explosive vs effusive volcanism on the Moon, with the ability to further constrain eruption styles with remote sensing. The results presented in this dissertation are directly relevant to the future goals of NASA and the effort to return humans to the lunar surface and have increased the science return of lunar missions like the ISRO/NASA Moon Mineralogy Mapper. </div>

This study investigated the effectiveness of commonly used instructional methods for teaching the phases of the Moon to fifth and sixth grade students. The instructional methods investigated were the use of diagrams, animations, and models. The effectiveness of each method was tested by measuring students' understanding of Moon phases with a pre and post-assessment after receiving instruction with a specific method or combination of methods. These methods were then evaluated for their ability to help students learn essential concepts, reinforce relevant vocabulary and discourage misconceptions. Results showed that students had better scores with less prevalence of misconception when they were taught using two methods instead of one. Students taught with only computer animations had significantly lower scores and a higher prevalence of misconceptions when compared to the other methods. This may be due to some design errors in the animation used in this study. Even though students taught with only computer animations had significantly lower scores, students taught with computer animations followed by instruction with diagrams had significantly higher scores. Why this combination of instruction was more effective for student learning is a question that requires further research.

Human activities and unpredictable changes to environmental habitats impose a suite of stress and challenges to animal homeostatic function. Stress responses are often controlled by the release of glucocorticoids to mobilize energy, primarily corticosterone in small mammals, to help regulate homeostatic function such as heterothermy and changes to body condition, the latter of which serves as a proxy for energy reserves. Adaptive heterothermy is influenced by daily and seasonal patterns, heat produced from daily activity, and has been shown to increase in small mammals during times of environmental stress to conserve energy budgets. Body condition also changes in response to environmental perturbations, mobilization of energy by corticosterone, seasonal changes, and activity. My study aimed to disentangle the effects of environment and activity on homeostatic responses by pharmacologically manipulating corticosterone in kangaroo rats. Kangaroo rats are ecosystem engineers, heterothermic, and their activity periods are functions of their thermoregulatory patterns as well as environmental conditions thus making the species a great candidate for this form of study. I conducted two in-situ field experiments to assess for the effects of stress responses on thermoregulation, activity, and body condition. In my first experiment, I used body temperature (Tb) as a proxy for activity time and examined how pharmacologically increased corticosterone influenced kangaroo rat heterothermy responses to the moon phases and ambient temperatures. I also examined their fat, lean mass, and water content at the end of the study. Moon phase was a significant predictor of activity period as animals typically waited longer during the waxing moon phase to become active and cooled down below activity earlier in the night during the waning moon phase. As nights shortened, activity decreased despite environmental conditions becoming warmer. Corticosterone also significantly decreased total activity time and thus steadily increased heterothermy across the length of my experiment. These results indicate activity, not environment, are stronger drivers of heterothermy patterns. Total fat content (energy content) at the end of the study was not affected by corticosterone. The lack of change in fat content was presumably because kangaroo rat body condition was measured once at the end of the study and likely not a reflection of changed body condition over time. In my second experiment, I examined body condition across a longer period by measuring lean mass, fat content, and total body water across a 2-month period in the summer by pharmacologically increasing corticosterone to test the relationship between stress and body condition and to dissociate the two from environmental factors. Body condition indices generally increased across the summer, but corticosterone implantation did not significantly affect body any of the indices. The loss of heterothermic control and decrease in activity time across the summer suggests that animals are likely conserving energy budgets leading to preservation of condition. Further, banner-tailed kangaroo rats generally breed in the spring where body condition falls due to stress induced by increased competition and then increases across the summer as late summer monsoons promote the growth of primary resources utilized by animals thereby preserving body condition. This study suggests that body condition is driven more by life-history traits, activity time, and environment rather than stress responses.

The intent of this thesis is to explore the pressure-sinkage relationship for simulated lunar regolith (simulant). The simulants used in this experiment emulate the lunar highlands (LHS-1) and the lunar mare (LMS-1). The ultimate ability of a terrain or regolith to support a load without shear failure is vital to the planning and construction of permanent infrastructure. This relationship can be measured by applying a normal load to the regolith until shear failure, from which allowable and ultimate bearing capacity can be deduced. An understanding of the pressure-sinkage of lighter loads on the higher ‘fluffy' layer of regolith is of great importance to low mass projects. The experimental hardware consisted of a test bed filled with simulated lunar regolith. The focus was to create a mechanism to apply a known load to a simulant surface normal to a square box filled with a regolith simulant. A known mass of each simulant was placed into the bearing capacity box and gently agitated to encourage natural settling and the density was measured. The simulant was only packed as much as was caused by gravity and settling. Normal loads of increasing weight were put into the box, putting pressure on the simulant. It was determined that widely accepted models for pressure-sinkage reasonably anticipate sinkage in both LHS-1 and LMS-1, though this study recommends improvements to the experimental design.