No description available.

Le signal thermique d'une exoplanète tellurique est une clé pour caractériser les propriétés physiques et chimiques de son atmosphère. La résolution spectrale, et donc la caractérisation spectrale que nous pouvons réaliser des planètes extrasolaires, est malheureusement très limité, en particulier pour les planètes similaires à la Terre. Dans cette thèse, j'ai étudié la possibilité de caractériser des exoplanètes telluriques par l'analyse de la variabilité de son émission infrarouge. L'émission thermique apparente est en effet modulée par les saisons, la rotation de la planète, le mouvement et la variabilité des nuages, la phase orbitale, et aussi par la présence des satellites naturels.Premièrement, nous avons étudié l' émission thermique de la Terre vue en tant que point-source distante, ainsi que la variabilité et la dépendance du signal de la géométrie d'observation. J'ai modélisé l'émission de la Terre à l'aide des données satellitaires et des données produites par des modèles de circulation général (GCMs) du Laboratoire de Météorologie Dynamique de Paris (LMD), en comparant les deux types de données afin de valider les simulations.Pendant la deuxième partie de mon travail, j'ai utilisé des donnés du GCM pour modéliser des planètes telluriques qui diffèrent de la Terre par seulement un ou deux paramètres tels que: la vitesse de rotation (y compris des planètes synchrones), une surface planétaire entièrement recouverte par la glace ou de l'eau, l'obliquité de l'axe de rotation ou l'excentricité de l'orbite. Pour toutes ces planètes virtuelles, j'ai étudié le climat, déduit les propriétés physiques de la planète, et produit et analysé les signaux intégrés associés à différentes géométries d'observation.La dernière partie de la thèse est un travail préliminaire qui consiste en ne plus considérer l'émission bolométrique mais le signal de bandes spectrales étroites, grâce à une nouvelle génération de GCM. Parce que chaque bande explore un niveau spécifique dans l'atmosphère, l'étude de la variation du spectre en comparant les variabilités photométriques entre les bandes, permet d'étudier la dynamique, la composition, la distribution et l'évolution de l'atmosphère de la planète, ce qui ouvre un champ encore inexploré pour la caractérisation des exoplanètes. / The thermal emission received from a planet is a key to characterize the physical and chemical properties of its atmosphere. The spectral resolution, and therefore the spectral characterization that we can achieve for extrasolar planets is unfortunately very limited in particular for terrestrial planets. In this thesis, we study the possibility to characterize an Earth-like exoplanet by the analysis of the broadband infrared emission variability. The apparent thermal emission is indeed modulated by the seasons, the rotation of the planet, the motion and variability of atmospheric patterns and clouds, the orbital phase, and even the presence of a moon. As a reference case, we have studied the thermal emission of the Earth seen as a distant point-source, as well as the variability and the dependency of the signal on the observation geometry. We have modeled the emission of the Earth using data derived from observations and data produced by a General Circulation Models (GCMs), comparing both types of data in order to validate our simulations.As a second part of our work, we have used the GCM to model Earth-like planets that differ from the Earth by a few parameters such as different rotation rates (including tidally-locked planets), a planetary surface completely covered by ice or water, different obliquities and eccentricities. For all these virtual planets, we have studied the climate derived from the physical properties and the photometric infrared signal associated with them.The last part of the thesis is a preliminary work that no longer consider the bolometric emission but the signal from narrow spectral bands, thanks to a new generation of GCMs. Because each band probes a specific level in the atmosphere, studying how the low resolution spectrum of the planets varies by comparing the photometric variabilities between bands, we can study the dynamics, composition, distribution and evolution of the atmosphere of the planet, which it opens a yet unexplored field for the characterization of exoplanets.

We present an innovative Bayesian method for estimation of statistical parameters of time series data. This method works by comparing coefficients of Karhunen-Lo\`{e}ve expansion of observed and synthetic data with known parameters. We show one new method for generating synthetic data with prescribed properties and we demonstrate on a numerical example how this method can be used for estimation of physically interesting features in power spectra calculated from observed light curves of some X-ray sources.

No description available.

Shape and attitude of near-Earth objects directly affect the orbit propagation via drag and solar radiation pressure. Obtaining information beyond the object states (position and velocity) is integral to identifying an object. It also enables tracing origin and can improve the orbit accuracy. For objects that have a significant distance to the observer, only non-resolved imaging is available, which does not show any details of the object. So-called non-resolved light curve measurements, i.e. photometric measurements over time can be used to determined the shape of space objects using a two step inversion scheme. It follows the procedure to first determine the Extended Gaussian Image and then going through the shape reconstruction process to retrieve the closed shape even while measurement noise is present. Furthermore, it is also possible to generate high confidence candidates when follow-up observations are provided through a multi-hypotheses process.

No description available.

Snow algae are psychrophilic microorganisms, that inhabit snow fields in mountains and polar regions, which creates colored snow in good conditions. Most species belong to order Chlamydomonadales (Chlorophyta) with complicated life cycles, containing flagellates and immobile stages (cysts). Extreme environment of snow is characteristed by low temperature, problems with availability of water and lack of nutrition. Depending on location and phase of life cycle, snow algae have to deal with excess or lack of solar radiation, the important component of which is also dangerous UV radiation. The light conditions differ substantially from open location above the forest level or polar regions to forest habitats. In the first part of this work I compared reactions of photosynthetic apparatus of snow algae strains from forest and forestless habitats to different intensity of radiation, then I dealt with assessing any changes related to long-term cultivation in laboratory. Based on measurement of rapid light curves on PAM fluorometer I have determined some characteristics of photosynthetic apparatus of individual strains (parameters α and Ik), which indicate adaptation to low or high light intensity. For some strains, it was possible to compare the results obtained at a three-year interval. In the second part...

Este trabalho tem como objetivo o ensino dos fundamentos da Astrofísica Estelar moderna a alunos do Ensino Médio através de uma abordagem empírica que usa como ferramentas principais da metodologia a observação, o registro, a análise e a interpretação das mudanças de brilho das estrelas variáveis ao longo do tempo. Mediante técnicas simples (fotometria visual) para a estimativa dos valores dos brilhos aparentes (magnitudes) dessas estrelas no decorrer de vários meses, o aluno coleta seus próprios dados observacionais. Em seguida, esses dados serão colocados em gráficos (curvas de luz), cuja análise permitirá a medida de seus períodos e amplitudes de variação, bem como a determinação de uma série de parâmetros que caracterizam as propriedades físicas das estrelas. O estudo é conduzido de uma forma que permite apresentar aos alunos vários dos grandes temas da Astrofísica contemporânea sem que eles percam o vínculo sensorial com a observação direta dos fenômenos celestes, seja com auxílio de instrumental modesto (binóculos ou pequenos telescópios), seja até mesmo a olho nu. O produto final de nosso trabalho é um Guia de Estudos intitulado Astrofísica Estelar para o Ensino Médio, em doze capítulos e mais de trezentas páginas, que está incluído em sua íntegra nesta monografia. O Guia foi desenvolvido tendo como alvos principais os alunos e professores do Ensino Médio formal. Não obstante, ele pode ser também utilizado por qualquer pessoa que tenha interesse no assunto e que possua os conceitos necessários de Matemática e Física do Ensino Médio; ou ainda em cursos do ensino não-formal que sejam ministrados, por exemplo, por planetários, museus de ciência e astrônomos amadores (situação essa testada com ótimos resultados pelo autor). Por fim, vale mencionar que, neste tipo de aprendizado (conhecido como research-based education, que poderíamos traduzir livremente como aprendizado vinculado à pesquisa), utilizamos intensivamente diversos recursos tecnológicos disponibilizados gratuitamente na internet pelas grandes entidades internacionais que se dedicam à pesquisa e ao estudo das estrelas variáveis tais como softwares específicos, bancos de dados, simulações e cartas para a estimativa das magnitudes. O uso dessa metodologia vinculada à pesquisa, em nossa experiência, se constitui em um fator valioso para desenvolver nos alunos a criatividade, o raciocínio crítico, a familiarização com o método científico e as habilidades para a pesquisa. / This work aims at teaching the fundamental aspects of Stellar Astrophysics to high school students through an empirical approach which uses variable stars observations, data collection, and the analysis and interpretation of brightness changes as key methodological tools. By using some simple techniques (visual photometry) to estimate the values of apparent brightness (magnitudes) of these stars over several months, the student collects his/her own observational data. Subsequently, that data will be plotted in graphs (light curves), whose analysis will in turn allow the determination of its periods and amplitudes of variation, as well as of a series of physical parameters that characterize the physical properties of the stars. The whole study is conducted in a way that shows students several of the major themes of contemporary Astrophysics without losing their sensory link with the direct observation of celestial phenomena - whether with the aid of modest instruments (binoculars or small telescopes) or even naked eye. The final product of our work is a Study Guide called \"Stellar Astrophysics for High School\" in twelve chapters and more than three hundred pages, which is included in their entirety in this monograph. The Guide was developed with the main targets being students and teachers of the formal high school level. Nevertheless, it can also be used by anyone who has an interest in the subject and who possesses the required concepts of high school Mathematics and Physics; or even in non-formal teaching courses that are taught, for example, by planetariums, science museums and amateur astronomers (a situation that has been tested with great results by the author). Last but not least, it is worth mentioning that in this type of learning (known as \"research-based education\") we intensively use various technological resources freely available on the internet from the great international entities that are dedicated to the research and study of variable stars such as specific softwares, databases, simulations and charts for estimating magnitudes. The use of research-based education, in our experience, is a valuable tool to foster and develop students creativity, critical thinking, and the familiarization with the scientific method and research skills.

Este trabalho tem como objetivo o ensino dos fundamentos da Astrofísica Estelar moderna a alunos do Ensino Médio através de uma abordagem empírica que usa como ferramentas principais da metodologia a observação, o registro, a análise e a interpretação das mudanças de brilho das estrelas variáveis ao longo do tempo. Mediante técnicas simples (fotometria visual) para a estimativa dos valores dos brilhos aparentes (magnitudes) dessas estrelas no decorrer de vários meses, o aluno coleta seus próprios dados observacionais. Em seguida, esses dados serão colocados em gráficos (curvas de luz), cuja análise permitirá a medida de seus períodos e amplitudes de variação, bem como a determinação de uma série de parâmetros que caracterizam as propriedades físicas das estrelas. O estudo é conduzido de uma forma que permite apresentar aos alunos vários dos grandes temas da Astrofísica contemporânea sem que eles percam o vínculo sensorial com a observação direta dos fenômenos celestes, seja com auxílio de instrumental modesto (binóculos ou pequenos telescópios), seja até mesmo a olho nu. O produto final de nosso trabalho é um Guia de Estudos intitulado Astrofísica Estelar para o Ensino Médio, em doze capítulos e mais de trezentas páginas, que está incluído em sua íntegra nesta monografia. O Guia foi desenvolvido tendo como alvos principais os alunos e professores do Ensino Médio formal. Não obstante, ele pode ser também utilizado por qualquer pessoa que tenha interesse no assunto e que possua os conceitos necessários de Matemática e Física do Ensino Médio; ou ainda em cursos do ensino não-formal que sejam ministrados, por exemplo, por planetários, museus de ciência e astrônomos amadores (situação essa testada com ótimos resultados pelo autor). Por fim, vale mencionar que, neste tipo de aprendizado (conhecido como research-based education, que poderíamos traduzir livremente como aprendizado vinculado à pesquisa), utilizamos intensivamente diversos recursos tecnológicos disponibilizados gratuitamente na internet pelas grandes entidades internacionais que se dedicam à pesquisa e ao estudo das estrelas variáveis tais como softwares específicos, bancos de dados, simulações e cartas para a estimativa das magnitudes. O uso dessa metodologia vinculada à pesquisa, em nossa experiência, se constitui em um fator valioso para desenvolver nos alunos a criatividade, o raciocínio crítico, a familiarização com o método científico e as habilidades para a pesquisa. / This work aims at teaching the fundamental aspects of Stellar Astrophysics to high school students through an empirical approach which uses variable stars observations, data collection, and the analysis and interpretation of brightness changes as key methodological tools. By using some simple techniques (visual photometry) to estimate the values of apparent brightness (magnitudes) of these stars over several months, the student collects his/her own observational data. Subsequently, that data will be plotted in graphs (light curves), whose analysis will in turn allow the determination of its periods and amplitudes of variation, as well as of a series of physical parameters that characterize the physical properties of the stars. The whole study is conducted in a way that shows students several of the major themes of contemporary Astrophysics without losing their sensory link with the direct observation of celestial phenomena - whether with the aid of modest instruments (binoculars or small telescopes) or even naked eye. The final product of our work is a Study Guide called \"Stellar Astrophysics for High School\" in twelve chapters and more than three hundred pages, which is included in their entirety in this monograph. The Guide was developed with the main targets being students and teachers of the formal high school level. Nevertheless, it can also be used by anyone who has an interest in the subject and who possesses the required concepts of high school Mathematics and Physics; or even in non-formal teaching courses that are taught, for example, by planetariums, science museums and amateur astronomers (a situation that has been tested with great results by the author). Last but not least, it is worth mentioning that in this type of learning (known as \"research-based education\") we intensively use various technological resources freely available on the internet from the great international entities that are dedicated to the research and study of variable stars such as specific softwares, databases, simulations and charts for estimating magnitudes. The use of research-based education, in our experience, is a valuable tool to foster and develop students creativity, critical thinking, and the familiarization with the scientific method and research skills.

The theory of stellar evolution and stellar structure relies on the observation of stars in di erent phases of their evolutionary cycle. The relation between observations and theory can be strengthened by obtaining observational data of a large sample of stars in a particular evolutionary phase. The search for Cephei stars, as conducted in this study, can contribute to the sample of known Cephei stars, where these interesting stars are massive non-supergiant early B-type stars, displaying pulsating behaviour which is not well understood. Stars tend to form in clusters where it can therefore be expected that young massive stars can be found in open clusters. For this reason two young southern open clusters were observed in order to search for B-type pulsating stars. The region of NGC 6204 and Hogg 22 was observed over a period of thirteen nights in Johnson B, V and I bands. NGC 6204 is believed to be the oldest cluster of the two at a distance of 0.8 kpc while the much younger Hogg 22 is more distant at 2.8 kpc. These two open clusters are located 6 arcminutes apart which made it possible to observe them simultaneously with a 12.8 12.8 arcminute eld of view. The observations were done with the newly installed 1600 telescope of the North-West University, South Africa. In order to do a variability search, periodic stars need to be identi ed from the cluster data, where a typical data set may contain thousands of scienti c images. In addition to the main motivation for this study, a pipeline was created in order to automate the photometry and data reduction processes. A Lomb-Scargle transform was applied to the stellar light curves in order to identify periodic sources. 354 signi cantly periodic stars were identi ed from the 3182 observed stars. Amongst them, two new possible Cephei stars were found together with a possible slowly pulsating B star (SPB), and numerous eclipsing binary systems. By using photometry of this region obtained by Forbes & Short (1996), instrumental magnitudes were transformed to a standard system in order to compare photometry results. From the constructed colour magnitude diagram of the two clusters, it could be seen that some stars, indicated by Forbes & Short (1996) to be cluster members, were in fact eld stars belonging to neither cluster. The reduction and photometry pipeline was implemented successfully on the data set, which also highlighted the importance of instrumentation and correct data analysis procedures. Possible improvements were identi ed in order to overcome di culties experienced during this study. / Thesis (MSc (Space Physics))--North-West University, Potchefstroom Campus, 2013