Submitted by Angela Maria de Oliveira (amolivei@uepg.br) on 2018-10-09T12:41:56Z No. of bitstreams: 2 license_rdf: 811 bytes, checksum: e39d27027a6cc9cb039ad269a5db8e34 (MD5) Jessica Mayara Eidam.pdf: 7618711 bytes, checksum: 8899a404c0b09be99db22ac7f334ae5b (MD5) / Made available in DSpace on 2018-10-09T12:41:56Z (GMT). No. of bitstreams: 2 license_rdf: 811 bytes, checksum: e39d27027a6cc9cb039ad269a5db8e34 (MD5) Jessica Mayara Eidam.pdf: 7618711 bytes, checksum: 8899a404c0b09be99db22ac7f334ae5b (MD5) Previous issue date: 2018-07-30 / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior / Buscando melhorar a estatística de parâmetros sismológicos de estrelas do tipoA,apresentamosnestetrabalhoaanálisededadosespectroscópicosefotométricos de oito estrelas observadas na direção do Pólo Galáctico durante a Campanha 8 da missão Kepler K2, proposto pelo nosso grupo de pesquisa. A observação fotométrica pelo satélite espacial Kepler ocorreu entre janeiro e março de 2016. A análise das frequências das oito curvas de luz foi feita usando o algoritmo CLEANEST e Period04. A espectroscopia de solo foi feita no OPD/LNA em outubro de 2015 com o telescópio Zeiss (0,6m) e em agosto de 2016 com o telescópio Perkin-Elmer (1,6m).Informaçõesespectroscópicascompletamosdadosdascurvasdeluzdosatélite, permitindo a caracterização da estrutura interna das estrelas. A determinação dos parâmetros estelares foi realizada por meio do Spectroscopy Made Easy (SME). Parâmetros como massa, raio e luminosidade foram obtidos usando as grades Code dÉvolution Stellaire Adaptatif et Modulaire (CESAM) e Porto Oscillations Code (POSC). Permitindo assim, gerar o modelo evolutivo para as oito estrelas. Estrelas dotipoespectralBmuitasvezessãoerroneamenteclassificadascomoestrelasdotipo espectralA,quandosomentedadosdefotometriasãoutilizadosparaaclassificação. Como exemplo, temos as estrelas: Epic220679442 e Epic220607132. Classificadas fotométricamente como tipo espectral A0, revelaram através da análise espectral, tratar-se do tipo espectral B9V. Epic220532854 é uma binária, Epic220466722 é uma δ e Epic220679442 possue variações fotométrica e, dados de espectroscopia revelam linha de Silício pronunciada (SiII λ4128), característica apresentada pela classe peculiar de estrelas Bp magnética. / Searching to improve the statistics of seismological parameters of stars of type A, we this work we present the analysis of spectroscopic and photometric data of eight stars observed in the direction of the Galactic Pole during the Kepler mission Campaign 8, proposed by our research group. The photometric observation occurred between January and March 2016. Frequency analysis of the eight light curves was made using the CLEANEST and Period04 algorithm. In addition to the photometric data, ground-based spectroscopy was done at the OPD/LNA in October 2015 with the Zeiss Telescope (0.6m) and in August 2016 with the Perkin-Elmer Telescope (1.6m). Spectroscopic information enhances the data from thesatellite’slightcurves,allowingthecharacterizationoftheinternalstellarstructure. Spectral characterization was done using Spectroscopy Made Easy (SME). Parameters such as mass, radius and luminosity were obtained using the Code d Évolution Stellaire Adaptatif et Modulaire (CESAM) and Porto Oscillations Code (POSC) grids, allowing to generate evolutionary models for the eight stars. Stars of spectral type B are often erroneously classified as stars of spectral type A, when only photometry data is used for classification. As an example, we have the stars: Epic220679442 and Epic220607132. Photometrically classified as spectral type A0, revealed through spectral analysis, to be spectral type B9V. Epic220532854 is a binary, Epic220466722 is a δ Scuti and Epic220679442 has photometric variations and spectroscopy data reveals pronounced silicon line (SiII λ4128), characteristic presented by the class peculiar stars Ap magnetic.

No description available.

Euclid's geometry is well-known for its theorems concerning triangles and circles. Less popular are the contents of the tenth book, in which geometry is a means to study quantity in general. Commensurability and rational quantities are first principles, and from them are derived at least eight species of irrationals. A recently republished work by Johannes Kepler contains examples using polygons to illustrate these species. In addition, figures having these quantities in their construction form solid shapes (polyhedra) having origins though Platonic philosophy and Archimedean works. Kepler gives two additional polyhedra, and a simple means for constructing the “divine” proportion is given.

Kepler is mainly known among historians of science due to his astronomical theories and his approaches to problems having to do with philosophy of science and ontology. This thesis attempts to contribute to Kepler studies by providing a comprehensive discussion of a topic hitherto not really considered, namely Kepler’s theory of the soul, a general theory of knowledge or epistemology whose central problem is what makes knowledge possible—rather than what makes knowledge true, as happens in the case of Descartes’s and Bacon’s epistemologies. Kepler’s theory consists of four issues: the theory of the different sorts of soul—i.e. the human soul, the animal soul, the vegetable soul, and the Earth soul—concerning their faculties, the differences and the resemblances that emerge among them, the relation they maintain with their own bodies and the world, and the distinction soul-world. The thesis discusses these issues from a historical perspective, that is, it reconstructs the way they appear in three periods of Kepler’s career: the period prior to the publication of the Mysterium Cosmographicum, the period going from 1596 to 1611, and the harmonic period. Finally, Kepler’s epistemology is briefly contrasted with Descartes’s and Bacon’s in order to suggest why Kepler’s is philosophically interesting and valuable. / October 2006

Texte remanié de: Doct. th. / Bibliogr. p. 233-271. Index.

Transiting planet candidates around rapidly rotating stars, a number of which have been found by the Kepler mission, are not amenable to follow-up via the usual radial velocity techniques due to their rotationally broadened stellar lines. An alternative method is Doppler tomography. In this method, the distortions of the stellar spectral lines due to subtracted light during the transit are spectroscopically resolved. This allows us to not only validate the transiting planet candidate but also to obtain the spin-orbit misalignment for the system. The spin-orbit misalignment is a powerful statistical tracer of the migration histories of planets. I discuss our project to perform Doppler tomographic observations of Kepler candidates and other transiting planets using the facilities at McDonald Observatory. I present our first transit detection, that of Kepler-13 b, and discuss some other recent results. / text

Kepler is mainly known among historians of science due to his astronomical theories and his approaches to problems having to do with philosophy of science and ontology. This thesis attempts to contribute to Kepler studies by providing a comprehensive discussion of a topic hitherto not really considered, namely Kepler’s theory of the soul, a general theory of knowledge or epistemology whose central problem is what makes knowledge possible—rather than what makes knowledge true, as happens in the case of Descartes’s and Bacon’s epistemologies. Kepler’s theory consists of four issues: the theory of the different sorts of soul—i.e. the human soul, the animal soul, the vegetable soul, and the Earth soul—concerning their faculties, the differences and the resemblances that emerge among them, the relation they maintain with their own bodies and the world, and the distinction soul-world. The thesis discusses these issues from a historical perspective, that is, it reconstructs the way they appear in three periods of Kepler’s career: the period prior to the publication of the Mysterium Cosmographicum, the period going from 1596 to 1611, and the harmonic period. Finally, Kepler’s epistemology is briefly contrasted with Descartes’s and Bacon’s in order to suggest why Kepler’s is philosophically interesting and valuable.

Kepler is mainly known among historians of science due to his astronomical theories and his approaches to problems having to do with philosophy of science and ontology. This thesis attempts to contribute to Kepler studies by providing a comprehensive discussion of a topic hitherto not really considered, namely Kepler’s theory of the soul, a general theory of knowledge or epistemology whose central problem is what makes knowledge possible—rather than what makes knowledge true, as happens in the case of Descartes’s and Bacon’s epistemologies. Kepler’s theory consists of four issues: the theory of the different sorts of soul—i.e. the human soul, the animal soul, the vegetable soul, and the Earth soul—concerning their faculties, the differences and the resemblances that emerge among them, the relation they maintain with their own bodies and the world, and the distinction soul-world. The thesis discusses these issues from a historical perspective, that is, it reconstructs the way they appear in three periods of Kepler’s career: the period prior to the publication of the Mysterium Cosmographicum, the period going from 1596 to 1611, and the harmonic period. Finally, Kepler’s epistemology is briefly contrasted with Descartes’s and Bacon’s in order to suggest why Kepler’s is philosophically interesting and valuable.

Submitted by ANTONIO DA SILVA MENDONÇA null (tonymendoncinha@hotmail.com) on 2016-01-22T03:29:34Z No. of bitstreams: 1 Dissertação de Mestrado_Antonio da Silva Mendonça.pdf: 2601605 bytes, checksum: 562d719c1ce663f9c2b34cf6b05642aa (MD5) / Approved for entry into archive by Juliano Benedito Ferreira (julianoferreira@reitoria.unesp.br) on 2016-01-25T15:20:03Z (GMT) No. of bitstreams: 1 mendonça_as_me_prud_par.pdf: 1006886 bytes, checksum: d88f93543cb3408b57b645b74eb6920f (MD5) / Made available in DSpace on 2016-01-25T15:20:03Z (GMT). No. of bitstreams: 1 mendonça_as_me_prud_par.pdf: 1006886 bytes, checksum: d88f93543cb3408b57b645b74eb6920f (MD5) Previous issue date: 2015-12-18 / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) / Cada vez mais professores do Ensino Médio se deparam com desafios em sua rotina de como de ensinar Física para pessoas com deficiência visual. O processo de inclusão vem crescendo, mas não tem sido acompanhado pela devida formação desses profissionais, que na maioria das vezes, não sabem como lidar e desenvolver atividades diversificadas que, de fato, incluam esse público no ambiente escolar. A inclusão é uma tarefa complexa que vai muito além de manter alunos cegos ou com baixa visão nas salas regulares convivendo com os demais alunos. Segundo alguns referenciais é possível ensinar Física a alunos deficientes visuais, desde que algumas precauções sejam tomadas, como o uso de adaptações em equipamentos que levem o aluno deficiente a construir significado daquilo que está sendo estudado através de outros sentidos como, por exemplo, o tato. O desenvolvimento de metodologias alternativas para o ensino de alunos cegos ou com baixa visão é muito importante para a melhoria da qualidade do ensino oferecido. Sendo assim, este estudo visa através de entrevistas intermediadas por questionários inicial e final, saber o que alunos com deficiência visual pensam e avaliam dos materiais (maquetes) construída com materiais de fácil acesso para trabalharem as Leis de Kepler. Nesse sentido, o objetivo desta Dissertação de Mestrado está relacionado à avaliação que os alunos com deficiência visual podem fazer dos materiais construídos, saber deles se os materiais são perceptivos, se são acessíveis tatilmente, se as dimensões são adequadas e se os conceitos podem ser construídos com auxílio da maquete. / More and more high school teachers are faced with challenges in their routine on physics teaching to people with visual impairment. The inclusion process is growing, but has not been accompanied by proper formation of these professionals who most often do not know how to handle and develop diversified activities that, in fact, include this public in the school environment. Inclusion is a complex task that goes far beyond keeping blind or low vision students in regular rooms in getting along with other students. According to some references it is possible to teach Physics to visually impaired students, as long as certain precautions are taken, such as using adaptations in equipment that take the visually impaired student to construct meaning of what is being studied by other senses, for example, the tact. In this sense, the development of alternative methodologies for teaching blind students and low vision is very important for improving the quality of education offered. Thus, this study aims through interviews carried out through initial and final questionnaires, know what students with visual impairment think and evaluate about the materials (models) built with easily and accessible materials to work Kepler's Laws. In this sense, the objective of this Master's Dissertation is related to the assessment that students with visual impairments can make about the materials built, know them if the materials are perceptive, if they are accessible tactually, if the dimensions are adequate and if the concepts can be constructed with model’s help.

The detection of exoplanets has rapidly evolved to one of the most important frontiers of astronomical and astrophysical research. The recent decades have seen the development of various techniques for detecting exoplanets. Of these approaches the transit method has received particular interest and has lead to the largest number of discoveries to date. The Kepler K2 mission is an ongoing observational survey, which has generated light curves for thousands of stars, a large fraction of which have yet to be fully explored. To discover and characterize the transiting planets hosted by the respective stars, extensive transit screens are required. However, implementing a pipeline for transit analyses is not straight forward, considering the light curve properties of different survey, the rapid changes brought by technological advancements, and the apparent lack of a golden standard with respect to the applied methodology. The project has reviewed several aspects of exoplanet detection via the transit method. Particular focus was placed on the identification of a suitable workflow covering the relevant steps to move from raw light curve files to a final prediction and characterization of transiting planetary candidates. Adhering to the identified strategy, the major part of the project then dealt with the implementation of a pipeline that integrates and executes all the different steps in a streamlined fashion. Of note, primary focus was placed on the actual selection and implementation of methods into an operational pipeline, but due to the given time constraints extensive optimizations of each individual processing step was outside the scope of this project. Nevertheless, the pipeline was employed to predict transit candidates for K2 campaigns C7, C8, C10, C11, and C12. A comparsion of the most conservative predictions from campaigns C7 and C10 with previously reported exoplanet candidates demonstrated that the pipeline was highly capable of discovering reliable transit candidates. Since campaigns C11 and C12 have not yet been fully explored, the respective candidates predicted for those campaigns in the current project might thus harbour novel planetary transit candidates that would be suitable for follow-up confirmation runs. In summary, the current project has produced a pipeline for performing transiting exoplanet searches in K2 data, which integrates the steps from raw light curve processing to transit candidate selection and characterization. The pipeline has been demonstrated to predict credible transit candidates, but future work will have to focus on additional optimizations of individual method parameters and on the analysis of transit detection efficiencies.