In the generation of the standard GRACE gravity fields, the K-Band Ranging (KBR) system data is used in its range-rate mode. Because time derivatives attenuate the gravity signal relative to the data noise at the lower frequencies, it is thought that solutions using range data might have better low-degree (low-frequency) characteristics. The purpose of this work is to detail the methods required to generate range-based solutions, to determine some of the properties of these solutions and then to compare them to range-rate based solutions. It is demonstrated that the range-based solutions are feasible. Different subarc lengths and parameterizations were considered. Although, the most effective combination of subarc lengths and parameterizations are not picked, it is concluded that estimating the mixed periodic term along with bias, bias-rate, bias-acceleration and periodic terms degrades the quality of the range based solution and therefore should not be used. Further study is necessary to pick the optimal combination of subarc length and parameterization which would be used in the time-series analysis. / text

The planet crossing asteroids in the inner solar system have strongly chaotic orbits and the distributions of their angular elements (longitude of ascending node, Ω; argument of perihelion, ω; and longitude of perihelion, ϖ) are often regarded as uniform random. In the last decade, the known population of these minor planets has increased by more than a factor of four, providing a sufficiently large dataset for statistical analysis of their distribution. By choosing the observationally complete set of bright objects, we quantified the level of intrinsic non-uniformities of the angular elements for the following dynamical subgroups of Near Earth Objects (NEOs) and Mars Crossing Objects (MCOs): three subgroups of NEOs (Atens, Apollos, and Amors) and two inclination subgroups of MCOs (high and low inclination MCOs, with the boundary at inclination of 15°). Using the methods of angular statistics, we found several statistically significant departures from uniform random angular distributions. We were able to link most of them with the effects of secular planetary perturbations. The distribution of the longitude of ascending node, Ω, for NEOs is slightly enhanced near the ascending node of Jupiter due to the secularly forced inclination vector. Apollos and high inclination MCOs have axial enhancement of ω due to secular dynamics associated with inclination-eccentricity-ω coupling; these enhancements show opposite trends in these two subgroups. The ϖ distributions of Amors and of MCOs are peaked towards the secularly forced eccentricity vector, close to the ϖ value of Jupiter. These non-uniform distributions of the angular elements may affect the asteroidal impact fluxes on the planets. We developed a new approach that accounts for the non-uniform angular elements of planet crossing asteroids to investigate the impact flux and its seasonal variation on the Earth, the Moon, and Mars. The calculation for this study was achieved by generating many clones of the observationally complete subset of bright planet-crossing objects, measuring the Minimum Orbit Intersection Distance (MOID) between the planet and the clones, and making use of the classical formulation of Wetherill (1967) for the collision probability of two objects on independent Keplerian orbits. We developed a novel method to calculate the collision probability for near-tangential encounters; this resolves a singularity in the Wetherill formulation. The impact flux of NEOs on the Earth-Moon system is found to be not affected significantly by the non-uniform distribution of angular elements of NEOs. The impact flux on Mars, however, is found to be reduced by a factor of about 2 compared to the flux that would obtain from the assumption of uniform random distributions of the angular elements of MCOs. Moreover, the impact flux on Mars has a strong seasonal variation, with a peak when the planet is near aphelion. We found that the amplitude of this seasonal variation is a factor of 4-5 times smaller compared to what would be obtained with a uniform random distribution of the angular elements of MCOs. We calculate that the aphelion impact flux on Mars is about three times larger than its perihelion impact flux. We also calculate the current Mars/Moon impact flux ratio as 2.9-5.0 for kilometer size projectiles.

The purpose of this study is to develop an understanding of the observability of small-scale dynamical Solar System features in meteor orbit radar data, particularly with reference to mean motion resonance effects. Particular focus is placed on the presence of `resonant swarms' in meteoroid streams: the resonant swarm at the 7:2 Jovian mean-motion resonance is used as an example, as it best satisfies radar observability criterion. Furthermore, evidence for this structure exists in visual meteor data. The radar dataset used for this study is that of the Canadian Meteor Orbit Radar (CMOR) as this dataset contains the largest number of meteoroid stream particles. The aim here is to determine whether the Taurid resonant swarm is observable in datasets produced by radars such as CMOR, or what improvements in individual orbital uncertainties are necessary for positive detection to be possible. The observability of the Taurid swarm in radar data depends on the limitations of the radar data (in terms of the individual measurement uncertainties); and on the properties of the resonance itself. Both aspects are investigated in this thesis. A statistical study is first conducted to assess whether evidence for the swarm exists in a dataset containing CMOR Northern and Southern Taurids from the years 2002 to 2007. It is found that the level of variations present is consistent with that expected due to random fluctuations: there is no evidence for a statistically significant resonant feature at the location of the 7:2 Jovian resonance. Additionally, the observability of various sizes of resonant peak for different sizes of dataset and for different levels of measurement uncertainties is investigated by addition of a modelled resonant feature to the data, followed by replacement of individual meteors by Gaussian profiles to simulate the effect of orbital uncertainties. It is clear that the level of broadening resulting from the uncertainties of the CMOR data used will not allow the observation of a resonant peak of the expected size. Detection is expected to be more likely in a `swarm encounter year' (a year in which the geometry between the resonant swarm and Earth is favourable to detection). The velocity uncertainties of a meteor orbit radar (similar to CMOR) need to be improved by a factor of 5 to 10 (relative to the CMOR uncertainties) in order to detect a resonant swarm that is composed of ~30% to ~5% (respectively) of the total number of observed Taurids in a swarm encounter year. An improvement significantly greater than a factor of ~10 is unlikely to result in a significant improvement in the ability to detect the resonant swarm. It is expected that a factor of 10 improvement in radar measurement uncertainties is achievable with the current techniques of radar systems and signal processing. These statistical tests require knowledge of the resonant width of the 7:2 Jovian resonance in semi-major axis, as this provides the size of the resonant feature of interest. Such resonant or libration widths can be determined analytically for orbits with low eccentricities. As Taurid orbits have high eccentricities (e~0.83), a hierarchical N-body integrator is used to examine the dynamics in the region of the 7:2 resonance, and determine a resonant width of (0.047±0.005) AU. To verify this method the standard analytic equations and a semi-analytic method are compared (at low eccentricities) with the numerical resonant width values: the agreement is within 10% for eccentricities below 0.4. It is important to know what proportion of radar Taurids are expected to be resonant in a swarm year in order to evaluate the observability of the swarm in radar data. One important factor that may affect this is the mass distribution of particles in the swarm. This is investigated by ejecting particles in multiple directions from three model comets: the first with a mass and orbit in agreement with those of the current 2P/Encke; the second with 2P/Encke mass and an orbit matching that of the proposed proto-Encke object; and a third with the mass and orbit of proto-Encke. The resulting orbits are examined to determine what proportion will land within the 7:2 resonance, for a range of particle masses and densities. The instantaneous effect of radiation pressure on the orbits of ejected particles is also considered. However, it is difficult to determine accurate capture percentage values due to the uncertainty surrounding cometary ejection mechanisms. Nevertheless, it is found that capture of Taurids into the 7:2 resonance by all comets is possible. Using comparisons between the percentages of visual-sized and radar-sized particles captured, it is determined that in weak swarm years (in which only 20% of visual meteoroids detected are resonant) only 4% to 5% of observed visual Taurids are expected to be resonant. Such a swarm would be on the edge of observability. However, in stronger swarm years (such as 2005), the resonant proportion will exceed that required for detection with a reduction in CMOR measurement uncertainties of a factor of ten.

Thesis (M.S.)--Worcester Polytechnic Institute. / Keywords: orbital trajectory, ion collection, turning point method, spherical probes, turning angle, ion scattering, cylindrical probes. Includes bibliographical references (p.60-63).

Made available in DSpace on 2014-06-11T19:25:29Z (GMT). No. of bitstreams: 0 Previous issue date: 2004-07Bitstream added on 2014-06-13T19:12:15Z : No. of bitstreams: 1 cruz_c_me_guara.pdf: 3366150 bytes, checksum: 08b399d3f2ebf41ec982fc0b5becc024 (MD5) / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) / Universidade Estadual Paulista (UNESP) / Neste trabalho propõe-se analisar a dinâmica do sistema Prometeu - Pandora - Anel F de Saturno, buscando soluções para alguns comportamentos anômalos observados em seus componentes. É realizada uma descrição geral, contextualizando este sistema dentro da estrutura de satélites e anéis de Saturno. A seguir, apresenta-se dados de interesse obtidos até o presente, a partir de observações realizadas pelas sondas espaciais Pioneer 11 e Voyager 1 e 2 e pelo Hubble Space Telescope, citando os pontos problemáticos deste sistema. A teoria necessária para a compreensão de alguns aspectos é colocada e discutida através de breves explanações. As principais publicações relacionadas ao tema são analisadas e comentadas, em ordem cronológica, demonstrando os avanços realizados no conhecimento deste sistema. Elabora-se uma proposta de investigação na tentativa de reproduzir os resultados mais importantes e através deles evoluir para a busca de novas informações que venham auxiliar no entendimento da dinâmica deste sistema, utilizando-se de ferramentas de simulação numérica, nas quais são acrescentados parâmetros e influências muitas vezes não-consideradas. Em trabalhos futuros, pretende-se realizar uma análise acurada dos resultados deste trabalho, introduzindo novas variáveis e elementos que possam enriquecer a teoria que vem sendo construída e que explique de maneira cada vez mais satisfatória os enigmas existentes no sistema Prometeu - Pandora - Anel F de Saturno. / In this work, we propose to analyze the dynamic of the Prometheus - Pandor - Saturn F ring system, searching for answers to the anomalous behavior of these bodies. We've made a general description, talking about this system and also about the ring and satellites structures of Saturn. Next, we show interesting data obtained until the moment from observations realized by the spacecrafts Pioneer 11 and 12 and Hubble Space Telescope, enumerating problematic points. We present the necessary theory to understand some aspects in evidence, discussing it through soon explanations. The main publications related to the topic are commented, in chronological order, showing advances in the understanding of this system. We've made an investigative offer to reproduce the most important results and through them develop new information to help the understanding of this dynamic system, using numerical simulations tools, in which we add new parameters and influences that wasn't consider. In future works, we'll try realize an accurate analyze of this work results, introducing new variables and elements to enrich the theory that has been built and to explain in a more clear manner the puzzle that exists in the Prometheus - Pandora - F ring system of Saturn.

Orientador: Antonio Maria Garcia Tommaselli / Banca: Aluir Porfírio Dal Poz / Banca: Antonio Machado e Silva / Resumo: A partir da década de 1970, com o início dos programas espaciais civis para fins de sensoriamento remoto, foi possível observar, fotografar e analisar a Terra a partir de dados gerados por plataformas orbitais. Atualmente, embora os sistemas orbitais sejam equipados com sensores de orientação direta (GNSS, giroscópios, sensores de estrelas, dentre outros), nem sempre as imagens corrigidas a partir dos dados (efemérides e atitude) provenientes destes sensores apresentam a acurácia requerida para certas aplicações. Para solucionar este problema é necessário orientar indiretamente estas imagens com elementos de controle no espaço objeto (pontos, retas e/ou áreas) ou corrigir os parâmetros orbitais a partir destes elementos de controle. O objetivo principal deste trabalho consiste em estudar, adaptar e avaliar experimentalmente modelos matemáticos rigorosos para a Fototriangulação de imagens orbitais utilizando pontos e retas como controle de campo. Os modelos matemáticos que relacionam os espaços objeto e imagem se baseiam nas condições de colinearidade (pontos) e coplanaridade (retas). Estes modelos foram implementados no programa TMS, seguindo a abordagem de triangulação multissensor com controle multi-feições. As entidades do espaço objeto (pontos e retas) foram levantadas em campo com o uso de um receptor GNSS de dupla frequência. Foram realizados experimentos com dados simulados e reais referentes ao sensor CBERS-2B HRC. Nos casos estudados, não houve melhora significativa nos resultados ao aplicar a Fototriangulação em bloco, quando comparado à orientação individual das imagens. Verificou-se também que a combinação dos modelos de colinearidade (pontos) e coplanaridade (retas)... (Resumo completo, clicar acesso eletrônico abaixo) / Abstract: Earth observation and analysis became feasible since the 70s with the civil spatial programs for remote sensing purpose. Nowadays, orbital imaging systems are equipped with direct orientation sensors. However, the images corrected using the orientation data (ephemeris and attitude) provided by these sensors are not always suitable for applications that require high metric accuracy. As a consequence, it is necessary to estimate indirectly the orientation elements of these images using ground control elements in the object space (points, lines and area), or to correct the orbital parameters using these control elements. The aim of this work is to study, adapt and experimentally assess rigorous bundle block adjustment models for orbital imagery using points and lines as control elements. The mathematical models relating object and image spaces are based on collinearity (points) and coplanarity (lines) conditions. The models were implemented in the in-house developed software TMS (Triangulation with Multiple Sensors), considering the multissensor triangulation with multifeatures control (points and lines) approach. The object space entities were surveyed with a dual-frequency GNSS receiver. Experiments with simulated and real data from the CBERS-2B HRC sensor were accomplished. The results showed that applying the bundle block adjustment... (Complete abstract click electronic access below) / Mestre

Made available in DSpace on 2014-06-11T19:22:25Z (GMT). No. of bitstreams: 0 Previous issue date: 2011-02-17Bitstream added on 2014-06-13T18:08:15Z : No. of bitstreams: 1 marcatojunior_j_me_prud.pdf: 903571 bytes, checksum: 62292812258f036e4d436b5a33074ae6 (MD5) / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) / Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) / A partir da década de 1970, com o início dos programas espaciais civis para fins de sensoriamento remoto, foi possível observar, fotografar e analisar a Terra a partir de dados gerados por plataformas orbitais. Atualmente, embora os sistemas orbitais sejam equipados com sensores de orientação direta (GNSS, giroscópios, sensores de estrelas, dentre outros), nem sempre as imagens corrigidas a partir dos dados (efemérides e atitude) provenientes destes sensores apresentam a acurácia requerida para certas aplicações. Para solucionar este problema é necessário orientar indiretamente estas imagens com elementos de controle no espaço objeto (pontos, retas e/ou áreas) ou corrigir os parâmetros orbitais a partir destes elementos de controle. O objetivo principal deste trabalho consiste em estudar, adaptar e avaliar experimentalmente modelos matemáticos rigorosos para a Fototriangulação de imagens orbitais utilizando pontos e retas como controle de campo. Os modelos matemáticos que relacionam os espaços objeto e imagem se baseiam nas condições de colinearidade (pontos) e coplanaridade (retas). Estes modelos foram implementados no programa TMS, seguindo a abordagem de triangulação multissensor com controle multi-feições. As entidades do espaço objeto (pontos e retas) foram levantadas em campo com o uso de um receptor GNSS de dupla frequência. Foram realizados experimentos com dados simulados e reais referentes ao sensor CBERS-2B HRC. Nos casos estudados, não houve melhora significativa nos resultados ao aplicar a Fototriangulação em bloco, quando comparado à orientação individual das imagens. Verificou-se também que a combinação dos modelos de colinearidade (pontos) e coplanaridade (retas)... / Earth observation and analysis became feasible since the 70s with the civil spatial programs for remote sensing purpose. Nowadays, orbital imaging systems are equipped with direct orientation sensors. However, the images corrected using the orientation data (ephemeris and attitude) provided by these sensors are not always suitable for applications that require high metric accuracy. As a consequence, it is necessary to estimate indirectly the orientation elements of these images using ground control elements in the object space (points, lines and area), or to correct the orbital parameters using these control elements. The aim of this work is to study, adapt and experimentally assess rigorous bundle block adjustment models for orbital imagery using points and lines as control elements. The mathematical models relating object and image spaces are based on collinearity (points) and coplanarity (lines) conditions. The models were implemented in the in-house developed software TMS (Triangulation with Multiple Sensors), considering the multissensor triangulation with multifeatures control (points and lines) approach. The object space entities were surveyed with a dual-frequency GNSS receiver. Experiments with simulated and real data from the CBERS-2B HRC sensor were accomplished. The results showed that applying the bundle block adjustment... (Complete abstract click electronic access below)

Made available in DSpace on 2016-06-02T19:12:36Z (GMT). No. of bitstreams: 1 5954.pdf: 27474055 bytes, checksum: eef4b5cada1fec33f5da8c25513efc8d (MD5) Previous issue date: 2014-01-28 / Motivated by increased consumption of abrasive grains and the need of the abrasive market to develop roughing, polishing and increasiling efficient cutting tools, this work aimed to understand the influence of titania in obtaining "blue fired" fused aluminum oxide. This is a material obtained from the brown fused aluminum oxide, which is subjected to a heat treatment and consequently gets higher physical properties than the conventional brown aluminum oxide sold. To ensure that the "blue fired" aluminum oxide acquires the physicochemical characteristics required by the market, it should have a blue color and a friability inferior than brown fused aluminum oxide. Given the strong market demand for this type of product, Elfusa Geral de Eletrofusão LTDA has been working on improving the technology for obtaining industrial scale "blue fired" aluminum oxide since 2009. In this context Elfusa proposed the Coordinator of Process Engineering and Development, Edmilson Ricelli dos Passos, a technological and systematic study on the production of "blue fired" aluminum oxide. Thus, this work discusses the process of electrofusion of bauxite to obtain the "blue fired" aluminum oxide, as well as a comparison of the mechanical properties of this material with conventional brown fused aluminum oxides. Both process variables as the influence of the chemical composition were analyzed during the study, using physical and chemical characterization techniques. It has been proved in this work that controlling for time, temperature and atmosphere variables is essential for the production of "blue fired" aluminum oxide. The blue coloration of the aluminum oxide is explained by electronic transition optical phenomena is the formation of aluminum titanate phase, as some explanations found in the technical literature state. / Motivado pelo aumento do consumo de grãos abrasivos e pela necessidade do mercado abrasivo em desenvolver ferramentas de desbaste, polimento e corte cada vez mais eficientes, este trabalho teve como objetivo entender a influência da titânia na obtenção do óxido de alumínio eletrofundido "blue fired". Este é um material obtido a partir do óxido de alumínio eletrofundido marrom, o qual é submetido a um tratamento térmico e por consequência adquire propriedades físicas superiores ao do óxido de alumínio marrom convencional comercializado. Para garantir que o óxido de alumínio blue fired adquira as características físico-químicas exigidas pelo mercado, o mesmo deve apresentar uma coloração azul e uma friabilidade inferior ao do óxido de alumínio eletrofundido marrom. Dada a forte procura do mercado por este tipo de produto, a Elfusa Geral de Eletrofusão LTDA vem desde 2009 trabalhando no aprimoramento da tecnologia para a obtenção em escala industrial do óxido de alumínio blue fired . Nesse contexto a Elfusa propôs ao Coordenador de Engenharia de Processo e Desenvolvimento, Edmilson Ricelli dos Passos, um estudo tecnológico e sistemático sobre a produção de óxido de alumínio blue fired . Desta forma, este trabalho aborda o processo de eletrofusão da bauxita até a obtenção do óxido de alumínio blue fired , assim como uma comparação das propriedades mecânicas deste material com os óxidos de alumínio eletrofundidos marrom convencionais. Tanto as variáveis de processo quanto a influência da composição química foram analisadas durante o trabalho, utilizando técnicas de caracterização físicas e químicas. Ficou provado nesse trabalho que o controle das variáveis tempo, temperatura e atmosfera são essenciais para a produção do óxido de alumínio blue fired . A coloração azul do óxido de alumínio é justificada por fenômenos óticos de transição eletrônica e não pela formação da fase titanato de alumínio, como algumas explicações encontradas na literatura técnica afirmam.

Orientador: Tadashi Yokoyama / Banca: Rodney da Silva Gomes / Banca: Nelson Callegari Junior / Resumo: Segundo Tsiganis et al (2005), no modelo de Nice os satélites regulares dos planetas gigantes seriam imunes aos efeitos da migraçãao sendo que os irregulares em geral seriam ejetados. Uma demonstraçãao clara e os cálculos que levam a isso, não são conhecidos. Neste trabalho estudaremos este problema, em especial para os casos dos sistemas de Urano e Saturno. Usamos o código de Gomes et al (2005) e tal com em Yokoyama et al (2008), o efeito do Sol e do achatamento do planeta será tomado, incluindo agora o disco planetesimal e a interação mútua dos satélites regulares. Os encontros próximos entre os satélites e planetesimais são tratados tal como em Nogueira (2008). Investigamos a possibilidade de existência de uma distância limite tal que satélites interiores a este limite resistam às instabilidades da migração. Neste sentido observa-se que Oberon e Titan, em geral, são os mais distantes (últimos) satélites que resistem á migração. Assim, em geral os objetos irregulares não resistem à migração. Por outro lado, as simulações mostram que embora os atuais satélites regulares sejam de fato primordiais, eventualmente podem ocorrer significativas instabilidades nesta região, que poderiam causar ejeção de algum satélite regular. Como resultado natural dos vários encontros, algumas capturas de satélites irregulares ocorrem. Neste sentido, um breve estudo de satélites capturados é mostrado / Abstract: According to Tsiganis et al (2005), in the Nice model, the regular satellites of the giant planets would be immune under the effects of the migration while the irregular ones would be ejected. A clear demonstration and the simulations showing that are not known. In this work we study this problem, in special for the cases of Uranus' and Saturn's systems. We use Gomes' code (GOMES et al,2005) and as in Yokoyama et al(2008), the effect of the Sun and of the oblateness of the planet are taken, but now including the planetesimal disk and the mutual interaction of the regular satellites. The close encounters between the satellites and the planetesimals are taken as in Nogueira (2008). We investigate the possibility of the existence of a limit distance such that satellites within this limit, resist the instabilities of the migration. In this sense we observe that, in general, Oberon and Titan are the outermost (last) that resist to the migration. Therefore, in general the irregular objects do not resist the migration. On the other hand, the simulations also show that although the current regular satellites are indeed primordial, eventually, some significant instabilities can occur in their region, leading to a possible ejection of some regular satellite. As a natural result of the several encounters, some captures of the irregular satellites occur. In this sense, a brief study of the captured satellites is shown / Mestre

abstract: Solar system orbital dynamics can offer unique challenges. Impacts of interplanetary dust particles can significantly alter the surfaces of icy satellites and minor planets. Impact heating from these particles can anneal away radiation damage to the crystalline structure of surface water ice. This effect is enhanced by gravitational focusing for giant planet satellites. In addition, impacts of interplanetary dust particles on the small satellites of the Pluto system can eject into the system significant amounts of secondary intra-satellite dust. This dust is primarily swept up by Pluto and Charon, and could explain the observed albedo features on Pluto's surface. In addition to Pluto, a large fraction of trans-neptunian objects (TNOs) are binary or multiple systems. The mutual orbits of these TNO binaries can range from very wide (periods of several years) to near-contact systems (less than a day period). No single formation mechanism can explain this distribution. However, if the systems generally formed wide, a combination of solar and body tides (commonly called Kozai Cycles-Tidal Friction, KCTF) can cause most systems to tighten sufficiently to explain the observed distributions. This KCTF process can also be used to describe the orbital evolution of a terrestrial-class exoplanet after being captured as a satellite of a habitable-zone giant exoplanet. The resulting exomoon would be both potentially habitable and potenially detectable in the full Kepler data set. / Dissertation/Thesis / Ph.D. Astrophysics 2013