Asteroid 4 Vesta, the largest differentiated body in the asteroid belt, is a protoplanet, much like those that accreted to form the Earth. Understanding the geology of Vesta furthers understanding of early differentiation processes that occurred on Earth and helps define igneous processes occurring on other differentiated bodies in the early solar system. Howardite, eucrite and diogenite (HED) meteorites, which are thought to have originated from Vesta, can be analyzed to better understand the geology of that asteroid. Here my colleagues and I investigate the petrology and geochemistry of two groups of HEDs. This work is timely, in that the insights gained from these studies can be used to interpret data from the Dawn spacecraft, which has just been placed into orbit around Vesta. In the first four parts of this dissertation we investigate the origin of olivine in diogenites, which are ultramafic cumulates from Vesta. We discover that the majority of these samples are dimict (two-component) breccias, composed of harzburgitic and orthopyroxenitic lithologies. This is contrary to the traditional belief that all diogenites are orthopyroxenites with small amounts of cumulus olivine. Using bulk and in situ trace element chemistries, along with mineral major/minor element compositions, we demonstrate that these two lithologies were likely related through fractional crystallization. We also examine an anomalous achondritic dunite, and use geochemistry and petrology to demonstrate that it is the first recognized dunite belonging to the HED group. This sample likely also fractionated from a melt prior to the fractionation of harzburgitic and orthopyroxenitic diogenites. In the final part of this dissertation, we investigate compositional and textural heterogeneity in a large group of paired howardites, Vestan regolith breccias composed of diogenite and eucrite. We find significant compositional and textural variation within the group, and a preferential distribution of eucritic material in the finer grain sizes. This suggests an immature regolith, and has implications for interpretation of spectral data to be collected by the Dawn orbiter at Vesta.

No description available.

Le sujet de cette thèse est l'étude de la rotation à long terme des corps célestes.La première partie est consacrée à l’étude de la rotation à long terme de Cérès et Vesta, les deux corps les plus massifs de la ceinture principale d’astéroïdes. Ils sont l’objet d’étude de la sonde spatiale Dawn, qui a permis de déterminer précisément les caractéristiques physiques et de rotation nécessaires au calcul de leurs rotations. La distribution de glace sous et à la surface de Cérès dépend du mouvement de son axe de rotation par le biais de l’obliquité, inclinaison de l’équateur sur l’orbite. Les rotations de Cérès et Vesta étant rapides, l’évolution à long terme des axes de rotation de Cérès et Vesta a été obtenue à l'aide d'une intégration symplectique des équations de la rotation, où une moyenne a été réalisée sur la rotation propre rapide. La stabilité des axes de rotation de Cérès et Vesta a été étudiée en fonction des paramètres de la rotation avec un modèle séculaire semi-analytique, qui a permis de montrer que les axes de rotation ne présentaient pas de caractère chaotique.La seconde partie concerne le développement d'intégrateurs symplectiques dédiés au corps solide. L'intégration de la rotation propre d'un corps solide nécessite d’intégrer les équations issues du hamiltonien du corps solide libre. Ce hamiltonien est certes intégrable et présente une solution explicite nécessitant l’usage des fonctions elliptiques de Jacobi, cependant le coût numérique de ces fonctions est élevé. Lorsque le hamiltonien du corps solide libre est couplé avec une énergie potentielle, l’orientation du corps doit être calculée à chaque pas d’intégration, ce qui augmente le temps de calcul. Des intégrateurs symplectiques ont ainsi été précédemment proposés pour le corps solide libre. Dans ce travail, des intégrateurs spécifiques au corps solide ont été développés en utilisant les propriétés de l’algèbre de Lie du moment cinétique. / This thesis concerns the long-term rotation of celestial bodies.The first part is a study of the long-term rotation of Ceres and Vesta, the two heaviest bodies of the main asteroid belt. The spacescraft Dawn studied these two objects and determined the physical and rotational characteristics, which are necessary for the computation of their rotations. The ice distribution under and on the surface of Ceres depends on the evolution of the obliquity, which is the inclination of the equatorial plane on the orbital plane. As the rotations of Ceres and Vesta are fast, the long-term evolution of the spin axes of Ceres and Vesta was obtained by realizing a symplectic integration of the equations of the rotation averaged on the fast proper rotation. The stability of the spin axes of Ceres and Vesta was studied with respect to the parameters of the rotation with a secular and semi-analytical model, which allowed to show that the spin axes are not chaotic.The second part concerns the development of symplectic integrators dedicated to the rigid body. The integration of the proper rotation of a rigid body needs to integrate the equations given by the Hamiltonian of the free rigid body. This Hamiltonian is integrable and presents an explicit solution using the Jacobi elliptic functions. However, the numerical cost of these functions is high. When the Hamiltonian of the free rigid body is coupled to a potential energy, the orientation of the body is needed at each step, which increases the computation time. Symplectic integrators were then previously proposed for the free rigid body. In this work, symplectic integrators dedicated to the rigid body were developed using the properties of the Lie algebra of the angular momentum.

<p>The dynamical evolution of the spin axis direction due to gravitational and thermal factors is examined. It is found that the spin axis variations generally are regular and relatively small for the bodies in the asteroid main belt. There are also reasons to believe that this is the case for minor objects beyond the main belt. However, it is found that these regular variations are larger when the orbital inclination of the objects is increased. This effect may explain certain features in the spin vector distribution of the main belt asteroids, not possible to explain by collisional factors. The spin vector evolution of the asteroids in the inner solar system, including the Earth- and Mars-crossing objects, is often subjected to strong forces related to frequencies in the orbital evolution. The variations in the spin vector direction are then very large and often subjected to chaos. The larger frequency related obliquity zones of the Mars-crossers are usually regular while the zones of the Earth-Mars-crossers often are of a chaotic nature. The spin vector evolution of asteroids with comet-like orbits is often chaotic regardless of initial obliquity. For the inner solar system asteroids, it is often possible for an initial prograde spin to turn into a retrograde one, or vice versa, due to the frequency related phenomena. Though some spin vector directions seem to be more probable than other ones over time, there are no indications for an evolution towards a more prograde or a more retrograde spin vector distribution.</p><p>The effects on the spin vector evolution from the thermal Yarkovsky force are examined for objects with radii larger than 50 m. This force will affect the orbital evolution and thus indirectly affect the spin vector evolution. However, it is found that the studied effects are minor as compared to the gravitationally related ones. This is true both for the diurnal and the seasonal variants of the Yarkovsky force.</p>

The dynamical evolution of the spin axis direction due to gravitational and thermal factors is examined. It is found that the spin axis variations generally are regular and relatively small for the bodies in the asteroid main belt. There are also reasons to believe that this is the case for minor objects beyond the main belt. However, it is found that these regular variations are larger when the orbital inclination of the objects is increased. This effect may explain certain features in the spin vector distribution of the main belt asteroids, not possible to explain by collisional factors. The spin vector evolution of the asteroids in the inner solar system, including the Earth- and Mars-crossing objects, is often subjected to strong forces related to frequencies in the orbital evolution. The variations in the spin vector direction are then very large and often subjected to chaos. The larger frequency related obliquity zones of the Mars-crossers are usually regular while the zones of the Earth-Mars-crossers often are of a chaotic nature. The spin vector evolution of asteroids with comet-like orbits is often chaotic regardless of initial obliquity. For the inner solar system asteroids, it is often possible for an initial prograde spin to turn into a retrograde one, or vice versa, due to the frequency related phenomena. Though some spin vector directions seem to be more probable than other ones over time, there are no indications for an evolution towards a more prograde or a more retrograde spin vector distribution. The effects on the spin vector evolution from the thermal Yarkovsky force are examined for objects with radii larger than 50 m. This force will affect the orbital evolution and thus indirectly affect the spin vector evolution. However, it is found that the studied effects are minor as compared to the gravitationally related ones. This is true both for the diurnal and the seasonal variants of the Yarkovsky force.

Master’s thesis describes the design parameters of components of electrical and electronic circuits for the game lasetag. There are described the various components and suggested their connection.

No description available.

The maritime transport sector makes a significant contribution to greenhouse gas (GHG) emissions, playing a consistent and increasing part in global CO2 emissions. Electrification of marine transportation is a key and necessary step for achieving the goals of the Paris Agreement and for avoiding the worst consequences of climate change. Sweden is among the first countries pleading for zero-emission transportation within 2045. However, one of the key challenges facing the widespread adoption of electric boats is the availability and efficiency of charging infrastructure.  Wireless power transfer technology with more focus on inductive power transfer technology in the marine sector was investigated. The focus is wireless charging infrastructure for passenger ferries in Goteborg. Vesta was the ferry chosen for the case study and it operates on the Saltholmen to Vrångö route. The route, schedule, and ferry energy consumption were investigated to implement the wireless charging infrastructure. Swot analysis was performed to show the strengths, weaknesses, opportunities, and threats of the research. Based on this investigation, the power profile, energy storage, and adopted solution with its system were proposed.

No description available.

This master thesis presents a theoretical investigation of the energy and stability of interfaces in iron-carbide compounds, specifically focusing on the α-Fe/Cr7C3 system. The study aims to fill the gap in knowledge regarding the surface energetics of these interfaces using Density Functional Theory (DFT). Six different α-Fe/Cr7C3 interfaceswere constructed α-Fe(001)/Cr7C3(024), α-Fe(001)/Cr7C3(202), α-Fe(001)/Cr7C3(040),α-Fe(110)/Cr7C3(024), α-Fe(110)/Cr7C3(202) and α-Fe(110)/Cr7C3(040). Due to limited computational resources, only one of them was computationally analyzed to determine its interfacial energy value. The results revealed that the interfacial energy of the α-Fe(001)/Cr7C3(040) interface falls within the range of incoherent interfaces, indicating its stability. The computed interfacial energy values ranged from 0.94 to 3.39 J/m2, consistent with similar studies on other iron interfaces. The simulations also identified minimum and local minimum points in the interface energy curve, representing stable configurations at specific interface separation distances. The presence of a minimum point at an interface separation value of d = 1.3551 Å with an interfacial energy of 0.94 J/m2 indicates the most stable configuration, while a local minimum point at d = 2.27 Å with an interfacial energy of 2.12 J/m2 suggests another stable configuration for the interface. The conclusion that the computations were correctly performed with an interfacial energy value of 0.94 J/m2 for the most stable configuration at a supercell length (aSupercell ) of 22.23 Å is drawn. The findings of this research have significant implications for future investigations and applications. Firstly, this study fills the gap of the unresearched ferrite-carbide interfaces with theoretical data. Secondly, the knowledge gained from studying these interfaces contributes to understanding hydrogen interactions, which is fundamental for the transition towards a hydrogen economy. Additionally, the incoherent nature of the interface introduces challenges in understanding material behavior and properties, necessitating further investigations for designing efficient systems. Future work includes experimental validation of the α-Fe/Cr7C3 interface to compare the theoretical and experimental energies and stability. Investigating the remaining interfaces and examining the effects of introducing hydrogen atoms in these interfaces, along with calculating the corresponding hydrogen trapping energies, are important research areas. Further advancements in understanding these interfaces can be achieved through interface engineering, multiscale modeling, and studying other iron-carbide systems. / Detta examensarbete presenterar en teoretisk undersökning av energin och stabiliteten hos gränssnitt i järnkarbidföreningar och fokuserar specifikt på α-Fe/Cr7C3-systemet. Studien syftar till att fylla kunskaps tomrummet gällande ytegenskaperna hos dessa gränssnitt genom användning av densitetsfunktionalteori (DFT). Sex olika α-Fe/Cr7C3-gränssnitt konstruerades α-Fe(001)/Cr7C3(024), α-Fe(001)/Cr7C3(202), α-Fe(001)/Cr7C3(040), α-Fe(110)/Cr7C3(024), α-Fe(110)/Cr7C3(202) och α-Fe(110)/Cr7C3(040). På grund av begränsade beräkningsresurser analyserades endast ett av dem för att bestämma dess gränssnittsenergivärde. Resultaten visade att gränssnittsenergin för α-Fe(001)/Cr7C3(040)- gränssnittet ligger inom intervallet för inkoherenta gränssnitt, vilket indikerar dess stabilitet. De beräknade gränssnittsenergivärdena varierade mellan 0,94 och 3,39 J/m2 , vilket är i linje med liknande studier där järngränssnitt studeras. Minimi och lokala minimipunkter i gränssnittets energikurva, vilket representerar stabila konfigurationer vid specifika avstånd mellan gränssnittet. Förekomsten av en minimipunkt vid ett gränssnittsavstånd på d = 1,35 Å med en gränssnittsenergi på 0,94 J/m2 indikerar den mest stabila konfigurationen, medan en lokal minimipunkt vid d = 2,27 Å med en gränssnittsenergi på 2,12 J/m2 antyder en annan stabil konfiguration för gränssnittet. Slutsatsen dras att beräkningarna utfördes korrekt med ett gränssnittsenergivärde på 0,94 J/m2 för den mest stabila konfigurationen vid en supercellslängd (aSupercell) på 22,23 Å. Fynden från denna forskning har betydande implikationer för framtida undersökningar och tillämpningar. För det första fyller denna studie kunskapsgapet gällande de otillräckligt utforskade ferrit-karbidgränssnitten med teoretisk data. För det andra bidrar den erhållna kunskapen från studiet av dessa gränssnitt till förståelsen av väteinteraktioner, vilket är grundläggande för övergången till en väteekonomi. Dessutom innebär gränssnittets inkoherenta natur utmaningar när det gäller att förstå materialbeteende och egenskaper, vilket kräver ytterligare undersökningar för att utforma effektiva system. Framtida arbete inkluderar experimentell validering av gränssnittet mellan α-Fe/Cr7C3 för att jämföra teoretiska och experimentella energier och stabilitet. Att undersöka återstående gränssnitt och undersöka effekterna av att introducera väteatomer i dessa gränssnitt och beräkna motsvarande vätefällningsenergier är viktiga forskningsområden. Gränssnittsdesign, flerskalig modellering och studier av andra järnkarbid-system kan ytterligare främja förståelsen av dessa gränssnitt.