Thesis (M.A. in Security Studies (Europe and Eurasia))--Naval Postgraduate School, June 2009. / Thesis Advisor(s): Abenheim, Donald. "June 2009." Description based on title screen as viewed on July 13, 2009. Author(s) subject terms: NASA, European Space Agency, ESA, International Cooperation, Transatlantic Relations, Nationalism, INTELSAT, Ulysses, Galileo, SOFIA, ISS, International Space Station, Constellation, Aurora, Vision for Space Exploration, Moon, Mars. Includes bibliographical references (p. 85-95). Also available in print.

Thesis (Ph.D.)--Memorial University of Newfoundland, Faculty of Medicine, 2000. / Includes bibliographical references.

abstract: Future robotic and human missions to the Moon and Mars will need in situ capabilities to characterize the mineralogy of rocks and soils within a microtextural context. Such spatially-correlated information is considered crucial for correct petrogenetic interpretations and will be key observations for assessing the potential for past habitability on Mars. These data will also enable the selection of the highest value samples for further analysis and potential caching for return to Earth. The Multispectral Microscopic Imager (MMI), similar to a geologist's hand lens, advances the capabilities of current microimagers by providing multispectral, microscale reflectance images of geological samples, where each image pixel is comprised of a 21-band spectrum ranging from 463 to 1735 nm. To better understand the capabilities of the MMI in future surface missions to the Moon and Mars, geological samples comprising a range of Mars-relevant analog environments as well as 18 lunar rocks and four soils, from the Apollo collection were analyzed with the MMI. Results indicate that the MMI images resolve the fine-scale microtextural features of samples, and provide important information to help constrain mineral composition. Spectral end-member mapping revealed the distribution of Fe-bearing minerals (silicates and oxides), along with the presence of hydrated minerals. In the case of the lunar samples, the MMI observations also revealed the presence of opaques, glasses, and in some cases, the effects of space weathering in samples. MMI-based petrogenetic interpretations compare favorably with laboratory observations (including VNIR spectroscopy, XRD, and thin section petrography) and previously published analyses in the literature (for the lunar samples). The MMI was also deployed as part of the 2010 ILSO-ISRU field test on the slopes of Mauna Kea, Hawaii and inside the GeoLab as part of the 2011 Desert RATS field test at the Black Point Lava Flow in northern Arizona to better assess the performance of the MMI under realistic field conditions (including daylight illumination) and mission constraints to support human exploration. The MMI successfully imaged rocks and soils in outcrops and samples under field conditions and mission operation scenarios, revealing the value of the MMI to support future rover and astronaut exploration of planetary surfaces. / Dissertation/Thesis / Ph.D. Geological Sciences 2012

Made available in DSpace on 2014-06-11T19:26:39Z (GMT). No. of bitstreams: 0 Previous issue date: 2007-06-20Bitstream added on 2014-06-13T20:54:55Z : No. of bitstreams: 1 jovchelevich_p_me_botfca.pdf: 499030 bytes, checksum: 7f5a990de9b5784be9e42359b9f390f9 (MD5) / Associacao Biodinamica / O presente trabalho teve como objetivo avaliar a influência dos diversos ritmos da Lua (sinódico, sideral, anomalístico, tropical e draconiano) sobre o rendimento, a qualidade e a conservação pós-colheita de cenoura, quando semeada em diferentes datas, sob as mesmas condições de manejo, em uma propriedade familiar com manejo biodinâmico no município de Botucatu-SP. O delineamento experimental utilizado foi o de blocos ao acaso com 31 tratamentos em 2005, e 14 tratamentos em 2006. A diferença entre tratamentos foi a data de semeadura, que variou de 5 de maio a 4 de junho em 2005, e de 25 de abril a 25 de maio em 2006, sempre entre 13 e 15hs. A colheita foi feita 82 dias depois de cada semeadura, equivalente a três ciclos da lua sideral, e no ponto que o consumidor de produtos orgânicos e biodinâmicos valoriza, segundo experiência do produtor. Para retirar o efeito da tendência dos dados na avaliação dos tratamentos, foi utilizada a metodologia de avaliação estatística do cálculo do Índice Estacional (IE). Foram avaliadas as seguintes características: massa fresca de raízes e folhas, massa seca, diâmetro, comprimento, teor de nitrogênio, fósforo e boro das raízes e perecibilidade das raízes com 30, 60 e 90 dias póscolheita. Nos dois períodos avaliados, a massa seca de raízes foi a única que, no contraste entre médias, apresentou diferença significativa nos ritmos sinódico tradicional e sinódico caboclo. No ritmo sinódico tradicional, a fase nova foi superior às fases crescente e cheia. No sinódico caboclo, a fase cheia foi inferior às demais. No contraste entre médias, o ritmo sinódico foi o que mais apresentou resultados significativos, e em menor proporção, os ritmos anomalístico, draconiano e sideral; O ritmo tropical (ascendente X descendente) e teor de nitrogênio não apresentaram resultados significativos... / The purpose of this work was to evaluate the influence of moon rhythms (synodic, sidereal, anomalistic, tropical and draconic) on yield, quality and postharvest storage of Daucus carota L. roots under biodynamic management sowed in different dates. The experiment was carried out over a two period on a biodynamic farm, in Botucatu, São Paulo State, Brazil. Rhythms were tested observing the effects of seeding at different planting dates. The experiment was performed with four randomized blocks and 31 treatments (different dates) in 2005 and fourteen treatments in 2006. The harvest occurred 82 days after the sowing, when carrot roots show the most desirable aspect for the organic and biodynamic consumers. The magnitudes of effects associated with planting at a specific lunar position were measured by the deviations from the trend curve. The following characteristics were evaluated: fresh mass of roots and leaves, dry mass, diameter, length, nitrogen, phosphorus and boron content of the roots and perishability of the roots at 30, 60 and 90 days post-harvest. Dry mass was the only one that in the contrast between averages showed significant results in the two periods of the experiment. Result was that the synodic new phase was superior to the first quarter, and full phases and in the caboclo synodic rhythm, the full phase was inferior to the other. It was clear that the synodic caboclo rhythm had the most significant influence followed by the traditional synodic one. The draconic, sideral and anomalistic had less influence and the tropical rhythm had no influence at all considering studied aspects. Nitrogen and tropical rhythm did not present any lunar influence. The two evaluated periods are still not conclusive related... (Complete abstract click electronic access below)

The Crescent Moon School (新月派Xinyue pai) is a Chinese intellectual group that was active from 1923 to 1934. Its members include Xu Zhimo 徐志摩(1897-1931), Hu Shi 胡适 (1891-1962), Liang Shiqiu 梁实秋(1903-1987), Wen Yiduo 闻一多(1899-1946), Luo Longji 罗隆基(1896-1965), and many other Anglo-American educated scholars in the Republican era. Although the group was engaged in various activities, poetry was their primary concern and their most notable practice. This thesis intends to solve two problems: 1) what common values or core spirit guided the various cultural practices of the group? 2) what are the poetic features and underlying poetics of the group as a whole? To answer the two questions, this thesis firstly examines the core spirit of the group by reviewing their activities and historical development. It argues that underlying the various activities and facts, there was a core spirit shared by the group. This core spirit, which I refer to as the “modern conservative spirit”, reflected a unique understanding of modernity that was different from that of the May Fourth discourse. They understood modernity not as a negation of tradition, but as a critical synthesis and mutual conformity between the old and the new, the local and the global. I show how the Crescent Moon intellectuals acquired this core spirit, and how it was displayed in their various activities. Secondly, this thesis provides detailed textual analysis of several Crescent Moon poems and reconstructs their poetics. It argues that their poetics demonstrated three faces, i.e. a romantic temperament, a classic ideal, and a modern consciousness. The three faces coexisted throughout the poetic practice of the group, although a certain face might have dominated in a certain period. I demonstrate how the three faces were unified under the guidance of the modern conservative spirit, and I argue that the simultaneousness of the three faces embodied the modern conservative intellectuals’ pursuit of literary modernity. By discussing the core spirit and poetics of the Crescent Moon School, this thesis concludes that the group was a missing link in Republican modern conservative trend, linking the late 1910s and early 1920s neotraditionalist thinkers with the mid-1930s Beijing School writers. The modern conservative intellectuals represented a dissenting voice in the Republican era, but they were also committed pursuers of modernity and cosmopolitanism.

abstract: Both volcanism and impact cratering produce ejecta and associated deposits incorporating a molten rock component. While the heat sources are different (exogenous vs. endogenous), the end results are landforms with similar morphologies including ponds and flows of impact melt and lava around the central crater. Ejecta from both impact and volcanic craters can also include a high percentage of melted rock. Using Lunar Reconnaissance Orbiter Camera Narrow Angle Camera (LROC NAC) images, crucial details of these landforms are finally revealed, suggesting a much more dynamic Moon than is generally appreciated. Impact melt ponds and flows at craters as small as several hundred meters in diameter provide empirical evidence of abundant melting during the impact cratering process (much more than was previously thought), and this melt is mobile on the lunar surface for a significant time before solidifying. Enhanced melt deposit occurrences in the lunar highlands (compared to the mare) suggest that porosity, target composition, and pre-existing topography influence melt production and distribution. Comparatively deep impact craters formed in young melt deposits connote a relatively rapid evolution of materials on the lunar surface. On the other end of the spectrum, volcanic eruptions have produced the vast, plains-style mare basalts. However, little was previously known about the details of small-area eruptions and proximal volcanic deposits due to a lack of resolution. High-resolution images reveal key insights into small volcanic cones (0.5-3 km in diameter) that resemble terrestrial cinder cones. The cones comprise inter-layered materials, spatter deposits, and lava flow breaches. The widespread occurrence of the cones in most nearside mare suggests that basaltic eruptions occur from multiple sources in each basin and/or that rootless eruptions are relatively common. Morphologies of small-area volcanic deposits indicate diversity in eruption behavior of lunar basaltic eruptions driven by magmatic volatiles. Finally, models of polar volatile behavior during impact-heating suggest that chemical alteration of minerals in the presence of liquid water is one possible outcome that was previously not thought possible on the Moon. / Dissertation/Thesis / Doctoral Dissertation Geological Sciences 2016

abstract: Affect is a domain of psychology that includes attitudes, emotions, interests, and values. My own affect influenced the choice of topics for my dissertation. After examining asteroid interiors and the Moon’s thermal evolution, I discuss the role of affect in online science education. I begin with asteroids, which are collections of smaller objects held together by gravity and possibly cohesion. These “rubble-pile” objects may experience the Brazil Nut Effect (BNE). When a collection of particles of similar densities, but of different sizes, is shaken, smaller particles will move parallel to the local gravity vector while larger objects will do the opposite. Thus, when asteroids are shaken by impacts, they may experience the BNE as possibly evidenced by large boulders seen on their surfaces. I found while the BNE is plausible on asteroids, it is confined to only the outer layers. The Moon, which formed with a Lunar Magma Ocean (LMO), is the next topic of this work. The LMO is due to the Moon forming rapidly after a giant impact between the proto-Earth and another planetary body. The first 80% of the LMO solidified rapidly at which point a floatation crust formed and slowed solidification of the remaining LMO. Impact bombardment during this cooling process, while an important component, has not been studied in detail. Impacts considered here are from debris generated during the formation of the Moon. I developed a thermal model that incorporates impacts and find that impacts may have either expedited or delayed LMO solidification. Finally, I return to affect to consider the differences in attitudes towards science between students enrolled in fully-online degree programs and those enrolled in traditional, in-person degree programs. I analyzed pre- and post-course survey data from the online astrobiology course Habitable Worlds. Unlike their traditional program counterparts, students enrolled in online programs started the course with better attitudes towards science and also further changed towards more positive attitudes during the course. Along with important conclusions in three research fields, this work aims to demonstrate the importance of affect in both scientific research and science education. / Dissertation/Thesis / Doctoral Dissertation Geological Sciences 2017

abstract: Water is a critical resource for future human missions, and is necessary for understanding the evolution of the Solar System. The Moon and Mars have water in various forms and are therefore high-priority targets in the search for accessible extraterrestrial water. Complementary remote sensing analyses coupled with laboratory and field studies are necessary to provide a scientific context for future lunar and Mars exploration. In this thesis, I use multiple techniques to investigate the presence of water-ice at the lunar poles and the properties of martian chloride minerals, whose evolution is intricately linked with liquid water. Permanently shadowed regions (PSRs) at the lunar poles may contain substantial water ice, but radar signatures at PSRs could indicate water ice or large block populations. Mini-RF radar and Lunar Reconnaissance Orbiter Camera Narrow Angle Camera (LROC NAC) products were used to assess block abundances where radar signatures indicated potential ice deposits. While the majority of PSRs in this study indicated large block populations and a low likelihood of water ice, one crater – Rozhdestvenskiy N – showed indirect indications of water ice in its interior. Chloride deposits indicate regions where the last substantial liquid water existed on Mars. Major ion abundances and expected precipitation sequences of terrestrial chloride brines could provide context for assessing the provenance of martian chloride deposits. Chloride minerals are most readily distinguished in the far-infrared (45+ μm), where their fundamental absorption features are strongest. Multiple chloride compositions and textures were characterized in far-infrared emission for the first time. Systematic variations in the spectra were observed; these variations will allow chloride mineralogy to be determined and large variations in texture to be constrained. In the present day, recurring slope lineae (RSL) may indicate water flow, but fresh water is not stable on Mars. However, dissolved chloride could allow liquid water to flow transiently. Using Thermal Emission Imaging System (THEMIS) data, I determined that RSL are most likely not fed by chloride-rich brines on Mars. Substantial amounts of salt would be consumed to produce a surface water flow; therefore, these features are therefore thought to instead be surface darkening due to capillary wicking. / Dissertation/Thesis / Doctoral Dissertation Geological Sciences 2017

abstract: Lunar Reconnaissance Orbiter (LRO) and MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft missions provide new data for investigating the youngest impact craters on Mercury and the Moon, along with lunar volcanic end-members: ancient silicic and young basaltic volcanism. The LRO Wide Angle Camera (WAC) and Narrow Angle Camera (NAC) in-flight absolute radiometric calibration used ground-based Robotic Lunar Observatory and Hubble Space Telescope data as standards. In-flight radiometric calibration is a small aspect of the entire calibration process but an important improvement upon the pre-flight measurements. Calibrated reflectance data are essential for comparing images from LRO to missions like MESSENGER, thus enabling science through engineering. Relative regolith optical maturation rates on Mercury and the Moon are estimated by comparing young impact crater densities and impact ejecta reflectance, thus empirically testing previous models of faster rates for Mercury relative to the Moon. Regolith maturation due to micrometeorite impacts and solar wind sputtering modies UV-VIS-NIR surface spectra, therefore understanding maturation rates is critical for interpreting remote sensing data from airless bodies. Results determined the regolith optical maturation rate on Mercury is 2 to 4 times faster than on the Moon. The Gruithuisen Domes, three lunar silicic volcanoes, represent relatively rare lunar lithologies possibly similar to rock fragments found in the Apollo sample collection. Lunar nonmare silicic volcanism has implications for lunar magmatic evolution. I estimated a rhyolitic composition using morphologic comparisons of the Gruithuisen Domes, measured from NAC 2-meter-per-pixel digital topographic models (DTMs), with terrestrial silicic dome morphologies and laboratory models of viscoplastic dome growth. Small, morphologically sharp irregular mare patches (IMPs) provide evidence for recent lunar volcanism widely distributed across the nearside lunar maria, which has implications for long-lived nearside magmatism. I identified 75 IMPs (100-5000 meters in dimension) in NAC images and DTMs, and determined stratigraphic relationships between units common to all IMPs. Crater counts give model ages from 18-58 Ma, and morphologic comparisons with young lunar features provided an additional age constraint of <100 Ma. The IMPs formed as low-volume basaltic eruptions significantly later than previous evidence of lunar mare basalt volcanism's end (1-1.2 Ga). / Dissertation/Thesis / Ph.D. Geological Sciences 2013

abstract: Impact craters are ubiquitous throughout the Solar System, formed by one of the principal processes responsible for surface modification of terrestrial planets and solid bodies (i.e., asteroids, icy moons). The impact cratering process is well studied, particularly on the Moon and Mercury, where the results remain uncomplicated by atmospheric effects, plate tectonics, or interactions with water and ices. Crater measurements, used to determine relative and absolute ages for geologic units by relating the cumulative crater frequency per unit area to radiometrically-determined ages from returned samples, are sensitive to the solar incidence angle of images used for counts. Earlier work is quantitatively improved by investigating this important effect and showing that absolute model ages are most accurately determined using images with incidence angles between 65&deg; and 80&deg;, and equilibrium crater diameter estimates are most accurate at ~80&deg; incidence angle. A statistical method is developed using crater size-frequencies to distinguish lunar mare age units in the absence of spectral differences. Applied to the Moon, the resulting areal crater densities confidently identify expansive units with >300&ndash;500 my age differences, distinguish non-obvious secondaries, and determine that an area >1&times;104 km2 provides statistically robust crater measurements. This areal crater density method is also applied to the spectrally-homogeneous volcanic northern smooth plains (NSP) on Mercury. Although crater counts and observations of embayed craters indicate that the NSP experienced at least two resurfacing episodes, no observable age units are observed using areal crater density measurements, so smooth plains emplacement occurred over a relatively short timescale (<500 my). For the first time, the distribution of impact melt on Mercury and the Moon are compared at high resolution. Mercurian craters with diameters &ge;30 km have a greater areal extent of interior melt deposits than similarly sized lunar craters, a result consistent with melt-generation model predictions. The effects of shaking on compositional sorting within a granular regolith are experimentally tested, demonstrating the possibility of mechanical segregation of particles in the lunar regolith. These results provide at least one explanation toward understanding the inconsistencies between lunar remote sensing datasets and are important for future spacecraft sample return missions. / Dissertation/Thesis / Ph.D. Geological Sciences 2013