The ultimate goal of this dissertation was to better understand what the Apollo sample collection tells us about the impact history of the Moon. My main research tool is a computer code called Cratered Terrain Evolution Model (CTEM). CTEM is a Monte Carlo landscape evolution code developed to model a planetary surface subjected to impacts. While the main effect of impact cratering that CTEM simulates is elevation changes of the landscape through the excavation process of craters and the deposition of ejecta, I worked to extend the capabilities of the code to study problems in material transport. As impact cratering is a dominant process on the surface of Moon, the stratigraphy of lunar geology is thought to be composed of stacks of impact-generated ejecta layers. Each individual impact generates ejecta that is sourced from varying depths of the subsurface. This ejecta contains a rich abundance of material containing information, including composition and datable impact products, such as impact glasses. The extensions to the CTEM code that I developed allows me to track all ejecta generated during a simulation and model the complex history of the lunar regolith.

Les travaux menés dans cette thèse se partagent entre la Lune et Mars, cibles privilégiées pour les missions d'exploration spatiales. La première partie porte sur l'instrument Interference Imaging Spectrometer (IIM) qui était à bord du satellite lunaire chinois Chang’e-1. Une méthode inédite utilisant l'angle spectrale et le concept de distance Euclidienne, et visant à supprimer les mauvais pixels de IIM, est proposée. Une nouvelle procédure de calibration est utilisée, et l'inter-étalonnage des données IIM avec des données télescopiques est amélioré. Ce nouveau jeu de données permet, après inversion, d'estimer l'abondance de FeO dans le sol lunaire. Les valeurs trouvées sont comparables aux observations du satellite américain Clementine et fournissent une nouvelle référence pour les études lunaires à venir. La seconde partie est consacrée à la modélisation du phénomène de tempêtes de poussière-fusée ("rocket dust storms") générées par des mouvements convectifs meso-echelle liés au chauffage solaire des poussières. L'objectif est de reproduire numériquement les couches de poussières détachées découvertes par l'instrument Mars Climate Sounder (NASA) dans le Modèle de Climat Global (GCM) du LMD. Les simulations montrent que, durant la saison des tempêtes de poussières (printemps et été austral), ce phénomène permet d'expliquer les couches détachées, et de reproduire les observations. Cependant, durant l'autre partie de l'année où il y a très peu de tempêtes de poussières, il semble nécessaire d'inclure dans le GCM un autre processus impliquant les vents de pente, capable de réinjecter les poussières en altitude pour maintenir les couches détachées. / Moon and Mars have been the important targets for deep space missions. The studies in this thesis include two parts. The first part is concerning Chang’e-1 Interference Imaging Spectrometer (IIM) data preprocessing and global lunar FeO inversion. In order to better preprocess the IIM data, a new method using spectral angle and Euclidean distance for removing bad pixels has been proposed. A new in-flight calibration has been conducted. And cross calibration of IIM data by using the telescopic data is improved. The processed IIM data have also been used to inverse lunar FeO abundance. The IIM-derived FeO is comparable to Clementine FeO results, and can be an alternative dataset for Moon studies. The second part is concerning parameterizing rocket dust storms and daytime slope winds in LMD (Laboratoire de Météorologie Dynamique) Mars GCM (Global Climate Model) to reproduce the detached dust layers (DDLs) observed by Mars Climate Sounder (MCS) on Mars. The simulations by the GCM including rocket dust storm parameterization show that, during the Martian dusty seasons, the rocket dust storms are the key factors to explain the observed DDLs. The formation and evolution of GCM simulated DDLs are in agreement with those of MCS observation. Meanwhile, the simulation also suggests that the large variation of the DDLs’ altitudes in dusty season are contributed by the deep convection induced by rocket dust storms. The simulations by the GCM including daytime slope winds parameterization show that with the help of daytime slope winds, the GCM can reproduce the detached dust layers in Martian clear seasons, which cannot be simulated by the rocket dust storm process.

Les météoroïdes, issus de petits corps du système solaire produisent des phénomènes lumineux (flashs d'impact) lorsqu'ils percutent le sol de la Lune. Ces événements lumineux transitoires sont observables depuis le sol en utilisant des télescopes de taille moyenne (typiquement > 200 mm de diamètre) à l'aide des caméras CCD rapides de haute sensibilité. Dans cette thèse, nous décrivons la configuration instrumentale, la procédure d'observation et d'analyse qui a été implémentée à l'Observatoire Universitaire de l'Oukaimden pour l'observation régulière des flashs lunaires. Les premiers impacts lunaires observés et confirmés depuis un observatoire situé en Afrique et dans le monde arabe sont analysés dans ce manuscrit. Nous discutons les caractéristiques de cinq flashs et les paramètres physiques attribués aux impacteurs associés. Nous présentons une première estimation du flux d'impact à l'issue de cette phase de surveillance des impacts lunaires depuis nos observatoires. Nous présentons également le développement et le test d'une stratégie pour déterminer avec précision les coordonnées des impacts observés depuis la Terre. Cette précision de séléno-localisation pourra être utilisée au profit de futures missions sismologiques qui utiliseront les impacts météoritiques pour explorer l'intérieur lunaire. / Meteoroids, coming from small bodies of the solar system, produce luminous phenomena (impact flashes) when they strike the lunar surface. These transient light events are observable from the ground using medium-sized telescopes (typically> 200 mm in diameter) by using high-speed CCD cameras. In this thesis, we describe the instrumental configuration, observation and analysis procedure that was implemented at the Oukaimden Observatory for regular observation of lunar flashes. The first lunar impacts observed and confirmed from an observatory located in Africa and the Arab world are analyzed in this manuscript. We discuss the characteristics of five flashes and the physical parameters attributed to the associated impactors. We present an initial estimate of the impact flux from this first phase of monitoring lunar impacts from our observatories. We also present the development and testing of a strategy to accurately determine the coordinates of impacts observed from Earth. This precision of seleno-localization can be used for future seismological missions that will use meteoroid impacts to explore the lunar interior.

Le but de ce travail est de développer un outil d'aide à l'analyse de mission pour un satellite artificiel autour de la Lune. Nous développons tout d'abord une théorie analytique qui décrit suffisamment bien la dynamique du satellite lunaire : nous considérons les quatre perturbations majeures de natures différentes qui l'influencent, ainsi que leurs différents couplages. Les résultats sont obtenus sous forme fermée, sans aucun développement en série de l'excentricité ni de l'inclinaison de l'orbite du satellite : la solution s'applique donc à une large gamme de valeurs. Nous utilisons la méthode des Transformées de Lie pour moyenniser deux fois l'Hamiltonien du problème, dans des variables canoniques, ce qui permet d'intégrer des orbites avec un temps de calcul réduit d'un facteur environ 200 000. Grâce à cela, nous produisons des cartes inédites d'espaces de phase (a,i) qui permettent de sélectionner les paramètres orbitaux selon les besoins de la mission lunaire. De nombreuses vérifications analytiques par rapport à la littérature ont été réalisées, et se sont avérées concluantes; la qualité des deux moyennisations a également été vérifiée. Le logiciel développé est souple et permet un traitement automatisé; les intégrations sont automatiquement vérifiées. Nous avons aussi apporté quelques améliorations significatives au manipulateur algébrique des FUNDP, comme l'ajout de fractions symboliques. Par ailleurs, nous résolvons le problème zonal complet du satellite artificiel, étudions l'effet de C22 sur l'inclinaison critique ainsi que l'effet de la Terre sur les durées de vie orbitales limitées de certains satellites lunaires. The aim of this work is to develop a tool helpful to mission analysis of a lunar artificial satellite. We first develop an analytical theory which sufficiently well describes the dynamics of the lunar satellite : we consider the four main perturbations of various kind which influence it, together with their several coupling. The results are obtained in closed form, without any series expansion in eccentricity nor inclination of the orbit of the satellite : so the solution applies for a wide range of values. We use the Lie Transform method for averaging twice the Hamiltonian of the problem, in canonical variables, which allows to integrate orbits with a CPU time reduced by a factor of about 200 000. Thanks to that, we produce unpublished (a,i) phase space maps from which the orbital parameters can be selected on the basis of the needs of the lunar mission. Many conclusive analytical checks with the literature have been performed, and both averaging processes have been checked. The software developed is flexible and allows an automated treatment; the integrations are automatically checked. We also improved significantly the algebraic manipulator of the FUNDP, like the inclusion of symbolic fractions. Moreover, we solve the complete zonal problem of the artificial satellite, we study the effect of C22 on the critical inclination, and also the effect of the Earth on the limited orbital lifetimes of some lunar satellites.

This thesis investigates autobiography from the standpoint of Native Americans, using Anita Endrezze¡¦s work as my anchor text. Drawing on Hertha Wong¡¦s critical position on Native American life writing, I argue that Anita Endrezze¡¦s autobiography, Throwing Fire at the Sun, Water at the Moon (2000), widens the scope of traditional generic limitations. The first chapter is the introduction, which delineates the theme of the thesis and introduces Yaqui history and Endrezze¡¦s family and cultural background. The second chapter analyzes what characterizes Native American autobiography by borrowing Hertha Wong¡¦s standpoint. Hertha Wong is one of the first theorists who yearn to widen the scope of the well-established generic limitations. She theorizes Native American autobiography by putting its etymology (¡§self,¡¨ ¡§life,¡¨ and ¡§writing¡¨) under scrutiny. Wong¡¦s critical base is the key thread of the chapter, and other critics¡¦ positions on Native American life writing are also provided as subsidizing points. Chapter Three revolves around how Endrezee conceptualizes ¡§the self¡¨ in her autobiographical narratives. Wong argues that Native Americans never regard the self as a separate entity from their community. Correspondingly, Endrezze consciously strives to construct a communal self in her personal narratives. To reach the aim, she relates herself to her relatives, her ancestors, and the present-day Yaquis. Besides, through her homing-in journey, she makes a direct connection to her ancestral homeland. Therefore, the representation of the self is not only community-based but also localized. Chapter Four aims to show that Endrezze¡¦s life narratives go beyond the realms of humans. That is, her autobiography resists anthropocentric narratives. She tells stories about the corn, the rain, and a wide variety of plants and animals. It is through the assistance of non-humans that human life is sustainable. Chapter Five aims to argue that Endrezze¡¦s autobiography shatters the fallacy that Native American culture is in demise. On the contrary, it is burgeoning. Endrezze uses her autobiography to fight back. Endrezze attempts to hybridize the languages to pose some reading obstacles to Euro-Americans. Besides, inserting her paintings at the end of autobiography is also a political act because it subverts traditional writing system. She mocks at the mono-dimensional narratives. Chapter Six is my conclusion, in which Endrezze¡¦s cultural and literary contributions are re-affirmed. It is my deep hope that Endrezze¡¦s book can, as her book title symbolizes, become another form of fire/water to continue the life of Yaquis.

In 2009, NASA's LCROSS mission impacted Cabeus Crater near the Lunar South Pole with the spent Centaur upper stage rocket. The impact was observed by the trailing sheperding spacecraft (S-S/C) that impacted the moon 250 seconds after the Centaur impact. The main objective of the LCROSS mission was to verify the existence of water ice in the lunar regolith---the subsequent analysis of the data confirmed water ice present in the crater. The analysis of the S-S/C instrument data suggested that the plume consisted of two components: a central "spike" component and a thin, outward "cone" component. A model has been developed at The University of Texas at Austin improve the analysis of the data obtained by the S-S/C. This model is created with a free-molecular ballistic grain code that involves simulating individual regolith grains in the debris plume through grain-heating and grain-movement models and then modeling the spectral radiance properties of the grains as observed by the S-S/C. Mie scattering theory is used to model scattering and absorption of incoming solar radiation by the particles in the plume assuming they are perfect spheres. The UT LCROSS code was utilized in a parametric study that evaluated the effect of variations in assumed model plume parameters on the modeling of S-S/C UV-VIS instrument observations. The plume parameters were chosen based on the assumption that the dust plume was split into two components: a central spike and a surrounding high angle cone. The following parameters were varied: the spike and cone angles, the spike and cone grain radius distributions, and the spike mass fraction. The following parameters could be varied but were given fixed values: ice fraction between plume components, ice grain purity, albedo, and ice fraction in plume. The impact of these plume parameters upon plume brightness and blue/red color ratio was determined. Two grain models were used. In the initial grain species model all grains have a soil core surrounded by a thin ice shell. In the second, two species model two grain types were utilized: a pure ice grain component and a pure soil grain component. / text

Mémoire numérisé par la Division de la gestion de documents et des archives de l'Université de Montréal

Water is of interest for understanding the formation history and habitability of past and present solar system environments. It also has potential as a resource - when split to its constituent oxygen and hydrogen - both in space and on the Earth. Determining the sources, evolution, and eventual fate of water on bodies easily reachable from Earth, especially Earth's moon, is thus of high scientific and exploration value to the private sector and government space agencies. Understanding how to efficiently split water with solar energy has potential to launch a hydrogen economy here on Earth and to power spacecraft more sustainably to far away destinations. To address the fundamental interactions of water with important surfaces relevant to space exploration and technology development, temperature programmed desorption (TPD) and water photolysis experiments under well controlled adsorbate coverages have been carried out and are described in detail in this thesis. TPD experiments under ultra-high vacuum (UHV) conditions were conducted on lunar surrogate materials and genuine lunar samples brought to Earth by the Apollo program. The TPD's were conducted to determine the desorption activation energies of water chemisorbed directly to the powder surfaces, knowledge of which can improve existing models of water evolution on Earth's moon and aid in interpreting data collected by spacecraft-based investigations at the Moon. The TPD experiments of molecular water interacting with two lunar surrogates (micronized JSC-1A and albite) in ultra-high vacuum revealed water desorption during initial heating to 750 K under ultra-high vacuum. Diffuse Reflectance Infrared Fourier Transform Spectroscopy (DRIFTS) indicated possible water formation during the initial heating via recombinative desorption of native hydroxyls above 425 ± 25K. Dissociative chemisorption of water (i.e., formation of surface hydroxyl sites) was not observed on laboratory time scales after controlled dosing of samples (initially heated above 750 K) with 0.2 - 500 L exposures of water. However, pre-heated samples of both types of surrogates were found to have a distribution of molecular water chemisorption sites, with albite having at least twice as many as the JSC-1A samples by mass. A fit to the TPD data yields a distribution function of desorption activation energies ranging from ~0.45 eV to 1.2 eV. Using the fitted distribution function as an initial condition, the TPD process was simulated on the timescale of a lunation. A preview of these results and their context was published in Icarus (2011) 213, 64, doi: 10.1016/j.icarus.2011.02.015 by lead author Charles Hibbitts and the full treatment of the results from the TPD on lunar surrogates (presented here in Chapter 2) has been published in the Journal of Geophysical Research – Planets (2013) 118, 105, doi: 10.1002/jgre.20025 by lead author Michael J Poston. The desorption activation energies for water molecules chemisorbed to Apollo lunar samples 72501 and 12001 were determined by temperature programmed desorption (TPD) experiments in ultra-high vacuum. A significant difference in both the energies and abundance of chemisorption sites was observed, with 72501 retaining up to 40 times more water (by mass) and with much stronger interactions, possibly approaching 1.5 eV. The dramatic difference between the samples may be due to differences in mineralogy, surface exposure age, and contamination of sample 12001 with oxygen and water vapor before it arrived at the lunar sample storage facility. The distribution function of water desorption activation energies for sample 72501 was used as an initial condition to mathematically simulate a TPD experiment with the temperature program matching the lunar day. The full treatment of the TPD results from these two lunar samples (presented here in Chapter 3) has been submitted with the title "Water chemisorption interactions with Apollo lunar samples 72501 and 12001 by ultra-high vacuum temperature programmed desorption experiments" to Icarus for publication in the special issue on lunar volatiles by lead author Michael J Poston. A new ultra-high vacuum system (described in Chapter 4) was designed and constructed for planned experiments examining the possible formation of hydrated species, including water, from interaction of solar wind hydrogen with oxygen in the lunar regolith and to examine the effects of the active radiation environment on water adsorption and desorption behavior on lunar materials. This system has been designed in close collaboration with Dr. Chris J Bennett. An examination of a unique system for water photolysis - zirconia nanoparticles for hydrogen production from water with ultra-violet photons - was performed to better understand the mechanism and efficiency of water splitting on this catalyst. Specifically, formation of H₂ from photolysis of water adsorbed on zirconia (ZrO₂) nanoparticles using 254 nm (4.9 eV) and 185 nm (6.7 eV) photon irradiation was examined. The H₂ yield was approximately an order of magnitude higher using monoclinic versus cubic phase nanoparticles. For monoclinic particles containing 2 monolayers (ML) of water, the maximum H₂ production rate was ~0.4 µmole hr⁻¹ m⁻² using 185 + 254 nm excitation and a factor of 10 lower using only 254 nm. UV reflectance reveals that monoclinic nanoparticles contain fewer defects than cubic nanoparticles. A H₂O coverage dependence study of the H₂ yield is best fit by a sum of interactions involving at least two types of adsorbate-surface complexes. The first dominates up to ~0.06 ML and is attributed to H₂O chemisorbed at surface defect sites. The second dominates at coverages up to a bilayer. H₂ formation is maximum within this bilayer and likely results from efficient energy transfer from the particle to the interface. Energy transfer is more efficient for the monoclinic ZrO₂ nanoparticles and likely involves mobile excitons. These results (presented in Chapter 5) have been submitted with the title "UV Photon-Induced Water Decomposition on Zirconia Nanoparticles" for publication in the Journal of Physical Chemistry C by lead author Michael J Poston. This paper has been reviewed and will be accepted after minor modification.

The cosmic “Dark Ages” is the cosmic era between the epochs of recombination of cosmic microwave background and the formation of the first stars. The only signal from this epoch is from neutral hydrogen, which could represent one of the richest data sets in cosmology. In order to extract this data, NASA/JPL has proposed a rover mission to the farside of the moon to deploy several radio arrays. Here the arrays would gather data undisturbed by human interference. This thesis examines the possibility of using photovoltaic and electric batteries as an energy solution for a rover on the moon. The requirement for such a system to survive on the moon is discussed in a literature study. A proof of concept simulation using a Simulink model has also been done. The thesis concludes that a rover can deploy the radio array using solar energy. It would be able to hibernate through the night using radioisotope heating. It would need to wait for its batteries to charge before each night. / I kosmologi kallas epoken mellan “rekombinationen till väte” och bildandet av de första stjärnorna för “den mörka tidsåldern”. Från denna tid finns endast spår i form av strålning från neutralt väte. Denna strålning kan enligt astronomer vara en viktigare källa till data om universums uppkomst än den kosmiska mikrovågsstrålningen. Därför arbetar NASA/JPL med att hitta metoder att observera denna rika källa till data. Den mest använda metoden är att använda lågfrekventa radioteleskop för att observera strålning med våglängder mellan 3-30 m och frekvenser mellan 10-100 Mhz. Ett stort problem med så kort strålning är den lätt störs ut av mänsklig påverkan och andra radiokällor, tillexempel solen. Ett sätt att undvika antropogen störning är att bygga ett radioteleskop på månens baksida. Eftersom månen är i en låst bana runt jorden vänder den alltid samma sida bort från planeten. Därför är platsen alltid i radioskugga från jorden ochstörs inte av mänsklighetens radiotrafik. JPL har lång erfarenhet av användandet av robotfarkoster för att utforska himlakroppar. År 2030 vill de sända en så kallad rover för att upprätta en grupp radioteleskop på månen med syftet att införskaffa data om “den mörka tidsåldern.” Högskolan i Halmstad erbjuder sedan 2013 studenter möjligheten att skriva sitt examensarbete i samarbete med NASA/JPL om konstruktionen av denna rover. Detta arbete har ämnat finna en lösning på rovens energiförsörjning genom att använda solceller och batterier. Slutsatsen har varit att det är möjligt att driva en rover på månen med solceller samt batterier. Ett krav är att rovern värms med radioisotoperunder natten för att minska energianvändningen.

Thesis (Ph. D.)--University of Hawaii at Manoa, 1991. / Includes bibliographical references (leaves 152-154) / Microfiche. / xvi,154 leaves, bound ill. 29 cm