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1	Gaia : de la validation des données aux paramètres du Red Clump / Gaia : from the data validation to the Red Clump parameters Ruiz-Dern, Laura 08 November 2016 (has links) La mission Gaia de l'Agence Spatiale Européenne (ESA) a pour objectif de cartographier notre galaxie avec une précision astrométrique jamais atteinte auparavant. Il est donc particulièrement important que les données qui seront publiées soient rigoureusement validées afin d'assurer une qualité optimum au Catalogue. Ces validations sont faites par l'une des équipes de l'unité de coordination CU9 du Consortium Gaia DPAC (Data Processing and Analys Consortium) chargé par l'ESA de la production du Catalogue Gaia. Dans le cadre de cette thèse, nous avons mis en place toute l’infrastructure nécessaire à la validation du catalogue Gaia par comparaison avec des catalogues externes. Celle-ci gère toutes les interactions avec l'environnement global des validations et avec la base de données Gaia. Ensuite nous avons développé un ensemble de tests statistiques pour valider les données du premier catalogue Gaia (DR1). Ces tests concernent notamment l’homogénéité des données sur le ciel, la qualité des positions et de la photométrie de l'ensemble des étoiles de DR1 (plus d'un milliard d'étoiles, $V<20$) ainsi que celle des parallaxes et mouvements propres des étoiles de textit{Tycho-Gaia} Astrometric Solution (TGAS), environ deux millions d'étoiles communes aux catalogues Gaia et Tycho-2 ($V<12$). Ces tests statistiques sur la DR1 sont opérationnels et ont déjà été appliqués très récemment sur des données préliminaires. Cela a déjà permis d'améliorer ces données (donc la qualité du catalogue), et d'en caractériser les propriétés statistiques. Cette caractérisation est essentielle à une exploitation scientifique correcte des données. Le premier catalogue Gaia sera publié à la fin de l’été 2016. Parmi les objets observés par Gaia, il y a une population d'étoiles particulièrement intéressantes, les étoiles du Red Clump (RC), très utilisées comme étalons de distance. Nous avons développé et testé deux méthodes pour modéliser les relations couleur-couleur (CC) et température effective - couleur dans toutes les bandes photométriques, de l'ultraviolet au proche-infrarouge. Elles permettront de caractériser le RC dans la bande G de Gaia dès la publication du catalogue: 1. en utilisant des modèles théoriques, et 2. empiriquement, en se basant sur une méthode Monte Carlo Markov Chain (MCMC). Pour cela nous avons très rigoureusement sélectionné des échantillons d'étoiles avec une bonne qualité photométrique, une bonne métallicité, déterminée par spectroscopie, une température effective homogène et une faible extinction interstellaire. À partir de ces calibrations CC et température-couleur, nous avons ensuite développé une méthode par Maximum de Vraisemblance qui permet de déterminer les magnitudes absolues, les températures et les extinctions des étoiles du RC. Les couleurs et extinctions ainsi obtenues ont été testées sur des étoiles avec des températures effectives mesurées spectroscopiquement et une extinction déterminée par la mesure des Bandes Diffuses Interstellaires (DIB). Ces propriétés intrinsèques des étoiles du RC vont permettre de caractériser le Red Clump Gaia et de calibrer, dans la bande Gaia, la magnitude absolue de cet étalon de distance, premier échelon essentiel de la détermination des distances dans l'Univers. / The Gaia mission of the European Space Agency (ESA) aims to map our galaxy with an unprecedented astrometric precision. It is therefore very important that the data that will be published be rigorously validated to ensure an optimal quality in the Catalogue. These validations are done by one of the teams of the coordination unit CU9 of the Gaia DPAC Consortium (Data Processing and Analysis Consortium) commissioned by ESA of the Gaia catalogue production. As part of this thesis, we implemented all the necessary infrastructure to validate the Gaia catalogue by comparison with external catalogues. This last manages all the interactions with the global environment of validations and with the Gaia database. Then we developed a set of statistical tests to validate the data from the first Gaia catalogue (DR1). These tests relate in particular to the homogeneity of data on the sky, the quality of the positions and of photometry of all the stars of DR1 (more than a billion stars, $V <20$) as well as that of the parallaxes and proper motions for textit{Tycho-Gaia} Astrometric Solution (TGAS) stars, around two million stars in common in Gaia and Tycho-2 catalogues ($V <12$).These DR1 statistical tests are operational and were already applied very recently on preliminary data. This has improved the data (thus the quality of the catalog) as well as allowed to characterize the statistical properties. This characterisation is essential for a correct scientific exploitation of the data. The first Gaia catalogue will be released in late summer 2016.Among the objects that Gaia observes, there is a population of stars particularly interesting, the Red Clump (RC) stars, widely used for distance indicators. We developed and tested two methods to model the colour-colour (CC) and effective temperature - colour relations in all photometric bands, from the ultraviolet to the near infrared. They will allow us to characterize the RC in the Gaia G band upon publication of the catalogue: 1. using theoretical models, and 2. empirically, based on a Monte Carlo Markov Chain (MCMC) method. For this we have very carefully selected samples of stars with a good photometric quality, good metallicity determined by spectroscopy, an homogeneous effective temperature and a low interstellar extinction.From these CC and temperature-colour calibrations, we then developed a Maximum Likelihood method that allows to derive absolute magnitudes, temperatures and extinctions of the RC stars. Estimates of colours and extinctions are tested on stars with spectroscopically measured effective temperatures and an extinction determined by the measurement of Diffuse Interstellar Bands (DIB). These intrinsic properties of RC stars will allow to characterize the Gaia RC and calibrate, within the Gaia G band, the absolute magnitude of this standard candle, first essential step of determining distances in the Univers. Gaia Validation Étoiles du Red Clump Calibration photométrique Gaia Validation Red Clump stars Photometric calibration 520
2	Determination of Stellar Parameters through the Use of All Available Flux Data and Model Spectral Energy Distributions Ekanayake, Gemunu 01 January 2017 (has links) Basic stellar atmospheric parameters, such as effective temperature, surface gravity, and metallicity plays a vital role in the characterization of various stellar populations in the Milky Way. The Stellar parameters can be measured by adopting one or more observational techniques, such as spectroscopy, photometry, interferometry, etc. Finding new and innovative ways to combine these observational data to derive reliable stellar parameters and to use them to characterize some of the stellar populations in our galaxy is the main goal of this thesis. Our initial work, based on the spectroscopic and photometric data available in literature, had the objective of calibrating the stellar parameters from a range of available flux observations from far-UV to far-IR. Much effort has been made to estimate probability distributions of the stellar parameters using Bayesian inference, rather than point estimates. We applied these techniques to blue straggler stars (BSSs) in the galactic field, which are thought to be a product of mass transfer mechanism associated with binary stars. Using photometry available in SDSS and GALEX surveys we identified 85 stars with UV excess in their spectral energy distribution (SED) : indication of a hot white dwarf companion to BSS. To determine the parameter distributions (mass, temperature and age) of the WD companions, we developed algorithms that could fit binary model atmospheres to the observed SED. The WD mass distribution peaks at 0.4M , suggests the primary formation channel of field BSSs is Case-B mass transfer, i.e. when the donor star is in red giant phase of its evolution. Based on stellar evolutionary models, we estimate the lower limit of binary mass transfer efficiency β ~ 0.5. Next, we have focused on the Canis Major overdensity (CMO), a substructure located at low galactic latitude in the Milky Way, where the interstellar reddening (E(B-V )) due to dust is significantly high. In this study we estimated the reddening, metallicity distribution and kinematics of the CMO using a sample of red clump (RC) stars. The averageE(B-V)(~0.19)is consistent with that measured from Schlegel maps (Schlegal et.al. 1998). The overall metallicity and kinematic distribution is in agreement with the previous estimates of the disk stars. But the measured mean alpha element abundance is relatively larger with respect to the expected value for disk stars. Stellar parameters Kurucz models Blue straggler Canis Major Over- density Red clump
3	Les graphes asymétriques minimaux de longueur induite 3 Gagnon, Jérôme January 2006 (has links) Mémoire numérisé par la Direction des bibliothèques de l'Université de Montréal. Automorphisme Graphe asymétrique minimal Graphe sans involution minimal Longueur induite Clump
4	X-ray Emissions from Clump Bowshocks in Massive Star Winds Ignace, Richard, Waldron, W., Cassinelli, N. 01 January 2012 (has links) Clumped structures in wind flows have substantially altered our interpretations of multiwavelength data for understanding mass loss from massive stars. Embedded wind shocks have long been the favored explanation for the hot plasma production and X-ray generation in massive star winds. This contribution reports on line profile shapes fromthe clump bowshock model and summarizes the temperature and emission measure distributions throughout the wind for this model with a focus on results that can be tested against observations.The authors acknowledge funding support for this work from a NASA grant(NNH09CF39C X-ray Emissions Clump Bowshocks Massive Star Winds Physics and Astronomy Astrophysics and Astronomy
5	X-ray Emission Line Profiles from Wind Clump Bow Shocks in Massive Stars. Ignace, R., Waldron, W., Cassinelli, J., Burke, A. 01 May 2012 (has links) (PDF) The consequences of structured flows continue to be a pressing topic in relating spectral data to physical processes occurring in massive star winds. In a preceding paper, our group reported on hydrodynamic simulations of hypersonic flow past a rigid spherical clump to explore the structure of bow shocks that can form around wind clumps. Here we report on profiles of emission lines that arise from such bow shock morphologies. To compute emission line profiles, we adopt a two-component flow structure of wind and clumps using two “beta” velocity laws. While individual bow shocks tend to generate double-horned emission line profiles, a group of bow shocks can lead to line profiles with a range of shapes with blueshifted peak emission that depends on the degree of X-ray photoabsorption by the interclump wind medium, the number of clump structures in the flow, and the radial distribution of the clumps. Using the two beta law prescription, the theoretical emission measure and temperature distribution throughout the wind can be derived. The emission measure tends to be power law, and the temperature distribution is broad in terms of wind velocity. Although restricted to the case of adiabatic cooling, our models highlight the influence of bow shock effects for hot plasma temperature and emission measure distributions in stellar winds and their impact on X-ray line profile shapes. Previous models have focused on geometrical considerations of the clumps and their distribution in the wind. Our results represent the first time that the temperature distribution of wind clump structures are explicitly and self-consistently accounted for in modeling X-ray line profile shapes for massive stars. X-ray Emission Wind Clump Bow Shocks Massive Stars Physics and Astronomy Astrophysics and Astronomy
6	Epidemiology and management of the Indian peanut clump virus Delfosse, Philippe 28 January 2000 (has links) Groundnut or peanut (Arachis hypogaea L.) is an important legume cultivated in several developing countries in the tropics and subtropics. It plays a significant role as a food crop in regions with alarming population growth rates. The disease “peanut clump”, which is caused by viruses in the genus Pecluvirus, has been reported from India and from several countries of West Africa. In India, the causal agent is the Indian peanut clump virus (IPCV), which is transmitted by a soil-borne root parasite, Polymyxa graminis. The virus is also transmitted by infected seed and so far no economical method of control has been found. Therefore efforts have been concentrated on understanding the epidemiology of peanut clump disease with the aim of devising cultural methods of control. The work addressed in this thesis describes how investigation in various aspects of clump disease epidemiology, including identification of alternative hosts of the virus and the vector, and of factors that contribute to survival and spread of inoculum, has led to formulation of simple cultural practices that could reduce disease incidence. Seed transmission Arachis hypogaea Plasmodiophoromycetes Peanut Groundnut Pecluvirus Indian peanut clump virus IPCV PCV ELISA Serology Control Cultural practices Polymyxa graminis
7	Epidemiology and management of the Indian peanut clump virus Delfosse, Philippe 28 January 2000 (has links) Groundnut or peanut (Arachis hypogaea L.) is an important legume cultivated in several developing countries in the tropics and subtropics. It plays a significant role as a food crop in regions with alarming population growth rates. The disease “peanut clump”, which is caused by viruses in the genus Pecluvirus, has been reported from India and from several countries of West Africa. In India, the causal agent is the Indian peanut clump virus (IPCV), which is transmitted by a soil-borne root parasite, Polymyxa graminis. The virus is also transmitted by infected seed and so far no economical method of control has been found. Therefore efforts have been concentrated on understanding the epidemiology of peanut clump disease with the aim of devising cultural methods of control. The work addressed in this thesis describes how investigation in various aspects of clump disease epidemiology, including identification of alternative hosts of the virus and the vector, and of factors that contribute to survival and spread of inoculum, has led to formulation of simple cultural practices that could reduce disease incidence. Seed transmission Arachis hypogaea Plasmodiophoromycetes Peanut Groundnut Pecluvirus Indian peanut clump virus IPCV PCV ELISA Serology Control Cultural practices Polymyxa graminis
8	Gesteinsmechanische Versuche und petrophysikalische Untersuchungen – Laborergebnisse und numerische Simulationen Baumgarten, Lars 26 May 2016 (has links) (PDF) Dreiaxiale Druckprüfungen können als Einstufenversuche, als Mehrstufenversuche oder als Versuche mit kontinuierlichen Bruchzuständen ausgeführt werden. Bei der Anwendung der Mehrstufentechnik ergeben sich insbesondere Fragestellungen hinsichtlich der richtigen Wahl des Umschaltpunktes und des optimalen Verlaufs des Spannungspfades zwischen den einzelnen Versuchsstufen. Fraglich beim Versuch mit kontinuierlichen Bruchzuständen bleibt, ob im Versuchsverlauf tatsächlich Spannungszustände erfasst werden, welche die Höchstfestigkeit des untersuchten Materials repräsentieren. Die Dissertation greift diese Fragestellungen auf, ermöglicht den Einstieg in die beschriebene Thematik und schafft die Voraussetzungen, die zur Lösung der aufgeführten Problemstellungen notwendig sind. Auf der Grundlage einer umfangreichen Datenbasis gesteinsmechanischer und petrophysikalischer Kennwerte wurde ein numerisches Modell entwickelt, welches das Spannungs-Verformungs-, Festigkeits- und Bruchverhalten eines Sandsteins im direkten Zug- und im einaxialen Druckversuch sowie in dreiaxialen Druckprüfungen zufriedenstellend wiedergibt. Das Festigkeitsverhalten des entwickelten Modells wurde in Mehrstufentests mit unterschiedlichen Spannungspfaden analysiert und mit den entsprechenden Laborbefunden verglichen. Gesteinsprobe Prüfkörper Postaer Sandstein Laborprüfungen Petrophysikalische Untersuchungen Einaxialer Druckversuch Dreiaxialer Kompressionsversuch Einstufentest Mehrstufentechnik Spannungspfad Kontinuierliche Bruchzustände Continuous-Failure-State-Triaxial-Test Zugfestigkeitsprüfungen Scherversuch Spaltzugversuch Biegezugversuch Belastungsrichtung Ultraschalllaufzeitmessung Dehnwellen-Resonanzverfahren Kathodolumineszenz-Mikroskopie Gesteinkenngrößen Gesteinsmechanische Parameter Rohdichte Reindichte Porosität Dünnschliffanalyse Sphärizität Korngrößenverteilung Festigkeitskennwerte Höchstfestigkeit Spitzenfestigkeit Restfestigkeit Anisotropie Arbeitskurven Spannungs-Dehnungs-Verhalten Nachbruch Bruchbilder Verformungskennwerte Statischer Elastizitätsmodul Dynamischer Elastizitätsmodul Verformungsmodul Querdehnungszahl Impuls-Laufzeit Wellen-Ausbreitungsgeschwindigkeit Numerische Modellierung Simulationsrechnung PFC-3D Kugelmodell Clump Partikelarrangement Parameterkalibrierung Parallel Bond Mikrobruch Rissausbreitung elastische Wellen rock sample test specimen sandstone uniaxial compression test triaxial compression test unconfined compression test multiple failure state test continuous failure state test tensile splitting strength shear test bending test pulse velocity ultrasonic elastic constants Young’s modulus of elasticity modulus of deformation Poisson’s ratio post failure stress-strain behaviour real density apparent density grain-size distribution porosity flexural strength peak strength residual strength anisotropy fracture pattern micro-crack pulse-propagation velocity clump sphere model parallel bond crack propagation numerical modelling simulation elastic wave PFC-3D parameter calibration particle arrangement ddc:624 Posta Sandstein Gesteinsprobe Mechanische Eigenschaft Petrophysik Elastizität Werkstein Druckversuch Zugversuch Kennzahl Experiment Numerisches Modell
9	Gesteinsmechanische Versuche und petrophysikalische Untersuchungen – Laborergebnisse und numerische Simulationen Baumgarten, Lars 25 November 2015 (has links) Dreiaxiale Druckprüfungen können als Einstufenversuche, als Mehrstufenversuche oder als Versuche mit kontinuierlichen Bruchzuständen ausgeführt werden. Bei der Anwendung der Mehrstufentechnik ergeben sich insbesondere Fragestellungen hinsichtlich der richtigen Wahl des Umschaltpunktes und des optimalen Verlaufs des Spannungspfades zwischen den einzelnen Versuchsstufen. Fraglich beim Versuch mit kontinuierlichen Bruchzuständen bleibt, ob im Versuchsverlauf tatsächlich Spannungszustände erfasst werden, welche die Höchstfestigkeit des untersuchten Materials repräsentieren. Die Dissertation greift diese Fragestellungen auf, ermöglicht den Einstieg in die beschriebene Thematik und schafft die Voraussetzungen, die zur Lösung der aufgeführten Problemstellungen notwendig sind. Auf der Grundlage einer umfangreichen Datenbasis gesteinsmechanischer und petrophysikalischer Kennwerte wurde ein numerisches Modell entwickelt, welches das Spannungs-Verformungs-, Festigkeits- und Bruchverhalten eines Sandsteins im direkten Zug- und im einaxialen Druckversuch sowie in dreiaxialen Druckprüfungen zufriedenstellend wiedergibt. Das Festigkeitsverhalten des entwickelten Modells wurde in Mehrstufentests mit unterschiedlichen Spannungspfaden analysiert und mit den entsprechenden Laborbefunden verglichen. info:eu-repo/classification/ddc/624 ddc:624

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