Gotowa bibliografia na temat „Formation et évolution des systèmes planétaires”
Utwórz poprawne odniesienie w stylach APA, MLA, Chicago, Harvard i wielu innych
Spis treści
Zobacz listy aktualnych artykułów, książek, rozpraw, streszczeń i innych źródeł naukowych na temat „Formation et évolution des systèmes planétaires”.
Przycisk „Dodaj do bibliografii” jest dostępny obok każdej pracy w bibliografii. Użyj go – a my automatycznie utworzymy odniesienie bibliograficzne do wybranej pracy w stylu cytowania, którego potrzebujesz: APA, MLA, Harvard, Chicago, Vancouver itp.
Możesz również pobrać pełny tekst publikacji naukowej w formacie „.pdf” i przeczytać adnotację do pracy online, jeśli odpowiednie parametry są dostępne w metadanych.
Artykuły w czasopismach na temat "Formation et évolution des systèmes planétaires"
Baudoz, Pierre. "Les futures missions spatiales dédiées aux planètes extrasolaires". Photoniques, nr 95 (styczeń 2019): 34–38. http://dx.doi.org/10.1051/photon/20199534.
Pełny tekst źródłaRatté, Stéphane. "Les techniques de la documentation : un programme de formation collégiale en évolution". Documentation et bibliothèques 61, nr 2-3 (31.08.2015): 45–52. http://dx.doi.org/10.7202/1032808ar.
Pełny tekst źródłaVerdier, Éric. "L’éducation et la formation tout au long de la vie : une orientation européenne, des régimes d’action publique et des modèles nationaux en évolution". Sociologie et sociétés 40, nr 1 (3.12.2008): 195–225. http://dx.doi.org/10.7202/019478ar.
Pełny tekst źródłaFillat, Federico, Jérôme Morlet, Javier Aguirre i Danielle Lassalle. "Le pastoralisme dans les Pyrénées de Huesca. Systèmes traditionnels et perspectives". Sud-Ouest européen 16, nr 1 (2003): 25–36. http://dx.doi.org/10.3406/rgpso.2003.2836.
Pełny tekst źródłaRousseau, L., O. Français i G. Lissorgues. "Introduction aux micro et nano technologies pour la réalisation de capteurs pour application médicale". J3eA 21 (2022): 1011. http://dx.doi.org/10.1051/j3ea/20221011.
Pełny tekst źródłaBeauné, Aurélie. "Activités de formation des migrants en France : des transitions expansives ?" Revue internationale du CRIRES : innover dans la tradition de Vygotsky 4, nr 2 (22.12.2017): 1–18. http://dx.doi.org/10.51657/ric.v4i2.41013.
Pełny tekst źródłaT. Hoffman, Philip, Gilles Postel-Vinay i Jean-Laurent Rosenthal. "Révolution et évolution Les marchés du crédit notarié en France, 1780-1840". Annales. Histoire, Sciences Sociales 59, nr 2 (kwiecień 2004): 387–424. http://dx.doi.org/10.1017/s0395264900003863.
Pełny tekst źródłaBonnaud, Olivier. "Les enjeux industriels, économiques et académiques de la filière micro-électronique". J3eA 21 (2022): 2011. http://dx.doi.org/10.1051/j3ea/20222011.
Pełny tekst źródłaCerman, Markus. "Proto-industrialization in an urban environment: Vienna, 1750–1857". Continuity and Change 8, nr 2 (sierpień 1993): 281–320. http://dx.doi.org/10.1017/s0268416000002095.
Pełny tekst źródłaTyers, Dianne, i Judy Sillito. "Locating Continuing Professional Development within a Proposed Complex Dynamic Systems Model for Today's English Language Teaching Profession". TESL Canada Journal 35, nr 2 (31.12.2018): 179–93. http://dx.doi.org/10.18806/tesl.v35i2.1297.
Pełny tekst źródłaRozprawy doktorskie na temat "Formation et évolution des systèmes planétaires"
Philipot, Florian. "Vers une recherche exhaustive des planètes géantes autour des étoiles proches de type solaire". Electronic Thesis or Diss., Université Paris sciences et lettres, 2023. http://www.theses.fr/2023UPSLO008.
Pełny tekst źródłaThe detection of the first exoplanets in the 1990s opened a new era in the study of planets. Today, thanks to increasingly powerful instruments, several hundred exoplanets (hot Jupiters, Super-Earths, multiple systems...) are discovered every year. Thanks to this wide variety of exoplanets, it is possible to study the distribution (distance, mass, eccentricity...) of these objects in order to better constrain the formation and evolution models of planetary system. Nevertheless, each detection method has its own limitations and detection biases. One aim of this thesis was to identify the limitations of the various detection methods, in particular those related to radial velocities (RV), and to improve the characterization of companions detected by RV.As a first step, I tested the robustness of studies aimed at determining the radial distribution of giant planets. Analysis of RV data from stars hosting long-period planets, the impact of stellar activity and the hypothesis made in completeness calculations, allowed us to demonstrate that statistical RV studies were not robust beyond 7-8 AU. Subsequently, I combined RV data with available absolute and relative astrometry measurements to improve the characterization of long-period sub-stellar companions. This study allowed us to precisely constrain the orbital parameters and, above all, the mass of seven companions detected in RV. It also highlighted the importance of coupling RV data with other measurements to accurately determine the nature of a companion. Finally, I used measurements of stars' proper motion anomalies (PMa), derived from Hipparcos and Gaia absolute astrometry, to search for new sub-stellar companions in the HARPS/VLT spectrograph archive. This analysis enabled me to improve the characterization of 14 sub-stellar companions, and to discover three new brown dwarfs and seven new exoplanets. I also demonstrated the effectiveness of using PMa measurements to optimize the search for sub-stellar companions
Petit, Antoine. "Architecture et stabilité des systèmes planétaires". Thesis, Paris Sciences et Lettres (ComUE), 2019. http://www.theses.fr/2019PSLEO005.
Pełny tekst źródłaThe architecture of a planetary systems is a signpost of their formation and history.Moreover, the large number of recent and future exoplanets discoveries allows to study the exoplanet system population.Besides, the observations of exoplanet systems has enriched the diversity of planetary system architecture, revealing that the Solar System shape is far from being the norm.However, the organization of planetary systems is heavily affected by dynamical stability, making individual studies particularly challenging.Since planets dynamics are chaotic, a detailed stability analysis study is computationally expensive.In this thesis, I develop analytic stability criteria for planet dynamics.In the secular system, the conservation of the total angular momentum and semi-major axes imply the conservation of the Angular Momentum Deficit (AMD).The AMD is a measure of a system’s eccentricities and mutual inclinations and act as a dynamical temperature of the system.Based on this consideration, we make the simplifying assumption that the dynamics can be replaced by AMD exchanges between the planets.In the first chapter we define the concept of AMD-stability. The AMD-stability criterion allows to discriminate between a priori stable planetary systems and systems for which the stability is not granted and needs further investigations.We show how AMD-stability can be used to establish a classification of the multiplanet systems in order to exhibit theplanetary systems that are long-term stable because they are AMD-stable, and those that are AMD-unstable which then require someadditional dynamical studies to conclude on their stability. We classify 131 multiplanet systems from the exoplanet.eu database with sufficiently well-known orbital elements.While the AMD criterion is rigorous, AMD conservation is only granted in absence of mean-motion resonances (MMR).If the MMR islands overlap, the system experiences chaos leading to instability.In the second chapter, we extend the AMD-stability criterion to take into account the overlap of first-order MMR.I derive analytically a new overlap criterion for first-order MMR.This stability criterion unifies the previous criteria proposed in the literature and admits the criteria obtained for initially circular and eccentric orbits as limit cases.In the third chapter I explain how the Hill stability can be understood in the AMD framework.Widely used, the Hill stability is a topological stability criterion for the three body system.However, most studies only use the coplanar and circular orbit approximation.We show that the general Hill stability criterion can be expressed as a function of only semi-major axes, masses, and total AMD of the system.The proposed criterion is only expanded in the planets-to-star mass ratio and not in the orbital elements.When studying AMD-unstable system, numerical simulations are mandatory.However the long timescales in planet dynamics make necessary the use of symplectic methods.These methods provide very accurate and fast integration when a system is stable.Their downside is that they are limited to fixed time-step integration.For unstable systems, the integrator may fail to resolve a close encounter and become inaccurate.In the fourth chapter, I propose a time renormalization that allow to use high order symplectic integrator with adaptive time-step at close encounter.The algorithm is well-adapted to systems of few similar masses planets.In the final chapter, I revisit the planet formation toy model developed by J. Laskar.While the AMD is conserved in the secular dynamics, it decreases during planets collisions.Laskar's model can be solved analytically for the average outcome and numerical simulations are very quick allowing to build large system population.I show that this formation model is in good agreement with recent realistic planet formation simulations where the final architecture results from a giant impact phase
Fortin, Francis. "Systèmes binaire : formation, évolution et environnement". Thesis, Université de Paris (2019-....), 2019. http://www.theses.fr/2019UNIP7071.
Pełny tekst źródłaAccreting binary systems are stellar couples in which a compact object (white dwarf, neutron star, black hole) feeds on a regular star. This accretion phase in the life of a binary shows characteristic high-energy emission, and can cause the formation of relativistic jets as well as a transient behavior which goes from violent outbursts to quiescent periods. These objects contribute significantly to the X-ray and gamma radiation in the universe, and since 2015 we know they are the progenitors of spectacular collisions between compact objects, which at the end of their lives radiate gravitationnal waves. Because more than half of the stars in our Galaxy spend at least a part of their lives within a binary, studying these systems is key to better understand stellar evolution in general. This thesis starts from an intial questioning about the origin of binary systems, of their diversity and the different evolutionnary paths they take, as well as the intricacy of their local environment. The tools we use to adress these topics are mainly observation-oriented. In particular, we will try to make full use of the multi-wavelength properties of binaries in the studies we present. The first part is a general introduction which covers the basics of stellar evolution, the processes taking place within binary systems, and also introduces practical aspects about observations such as the messengers and the observables that are associated. The second part is about a project of census concerning accreting binaries. We correlate previous catalogues with the Centre de Données Astronomiques de Starsbourg to update some of the information about the binaries, and also try to find counterparts of high-mass X-ray binaries (HMXB) among the detections of the Gaia satellite. This census will be used in a project studying the natal kick of HMXBs and will also be the starting point to look for progenitors of compact binaries which will be detected by the gravitationnal satellite LISA. The third part aims to actively participate in the census of X-ray binaries by determining the nature of unidentified INTEGRAL sources (IGR). We present the analysis of spectrophotometric data in near-infrared acquired with VLT/ISAAC on 14 IGR sources. Among them, we identified 9 new accreting binaries and 5 active galactic nuclei. The fourth part focuses on a particular system. IGR J16318-4848 is an obscured supergiant B[e] high-mass X-ray binary, and posesses a complex environment which we aim to characterize. We report on spectroscopic acquisitions with VLT/X-Shooter which allow us to probe the dynamics of the stellar wind from the supergiant star, the orbital motion of the dusty circumbinary disk as well as its own metal-rich wind. By modeling the broadband spectral energy distribution down to the far-infrared (Spitzer, Herschel), we determine the temperature of the emitting media as well as their absolute scales. The fifth part is a study on a transient source, the microquasar Swift J1745-26, made of a low-mass star orbiting a black hole. It was detected in X-rays down to radio waves late 2012 during outburst, and was observed again five months later during its decay. We use photometric data from VLT/FORS2, ISAAC in optical and near-infrared as well as soft and hard X-ray measurements (Swift/BAT, XRT) in order to compare the broadband spectral energy distributions at these two epochs. The variations in luminosity can be especially explained by a change in the internal radius of an accretion disk around the black hole. We conclude this manuscript by doing a summary of the results we brought on these topics, and also do a short review of the future prospects in the field of accreting binaries
Lebreton, Jérémy. "Observations et modélisation des systèmes planétaires autour des étoiles proches". Phd thesis, Université de Grenoble, 2013. http://tel.archives-ouvertes.fr/tel-00952803.
Pełny tekst źródłaKielbasiewicz, Nicolas. "Dynamique gravitationnelle multi-echelle : formation et évolution des systèmes auto-gravitants non isolés". Palaiseau, Ecole polytechnique, 2009. http://www.theses.fr/2009EPXX0004.
Pełny tekst źródłaThe purpose of this PhD thesis is to study the formation process and properties of self-gravitating systems, isolated or not, using N-body simulations of gravitational collapse. In the first part, we summarize the major analytical results about the collisionless Boltzmann - Poisson coupled system of equations, modelling the dynamics of collisionless gravitational systems. We present a study of the influence of the external potential on these results and of some analytical solutions. In the second part, we present the software we used to perform the simulations and introduce some concepts of data and task parallelism, having some elements parallelized with the M. P. I. Library. In the third and final part, we present the results of the numerical simulations, according to two studies. The first one concerns the complementary study of initial conditions leading to Antonov instability, and the study of internal dynamics of isolated self-gravitating systems. The second one concerns the study of the influence of an external potential to the gravitational collapse process
Lanquetot, Aurélie. "Etude d'un modèle de formation aux relations humaines : systèmes d'interactions et évolution des mentalités". Tours, 1998. http://www.theses.fr/1998TOUR2030.
Pełny tekst źródłaBazot, Michaël. "Tests sismiques de l'abondance des éléments dans les étoiles de type solaire, avec et sans planètes : modélisation et observations". Toulouse 3, 2005. http://www.theses.fr/2005TOU30214.
Pełny tekst źródłaKooli, Chokri. "Transformation du système éducatif Omanais, quarante ans de formation de capital humain : évolution et performance". Thesis, Paris, EHESS, 2017. http://www.theses.fr/2017EHES0028.
Pełny tekst źródłaThe economic prosperity of many countries depends primarily on revenues of oil resources and derivatives. Since this type of resource is exhaustible, the question of protecting the economy of certain countries from the fluctuations of oil prices may raise. These countries need too, to ensure the prosperity of their local economy based on sustainable resources. The Sultanate of Oman has launched the challenges of the diversification of its economy. To achieve this, the political authorities have understood the usefulness of the development of human capital throughout the increase of the level of instruction and education of the population. Being aware that such investment in education is more productive than any other one, our goal consists to study and analyze the effectiveness of public decision to invest in education and its impact on the quality of human capital. Through the Omani model, we seek to measure the impact and contribution of forty years of massive investments in the education system and on the development of human capital of the Sultanate. Our research, aims to analyze how to balance between the utility of education as a development model and the effectiveness of investment in the education system? We will see how public decision to invest in human capital must take into account the quantitative and qualitative aspects of the educational process. The consequences of such investment model need to be examined through the Omani case
Benbakoura, Mansour. "Evolution des étoiles de faible masse en interaction : observations multi-techniques et modélisation des systèmes multiples". Thesis, Université de Paris (2019-....), 2019. http://www.theses.fr/2019UNIP7027.
Pełny tekst źródłaThis thesis is devoted to the study of low-mass stars having other stars or planets in their immediate environment. We focused on the influence of interactions with these companions on stellar evolution and their observable consequences.In the first part, we present the model of evolution of star–planet systems that we developed during this thesis, called ESPEM (French acronym for Evolution of Planetary Systems and Magnetism). This model incorporates ab-initio prescriptions to quantify the effects of magnetized stellar wind and tidal dissipation on stellar rotation and planetary orbit, simultaneously with the star's structural evolution. First, we use it to study the secular evolution of the rotation of planet-host stars and show that this evolution can be significantly different from that of isolated stars. Next, we examine the predictions of this model regarding the orbital architecture of star–planet systems. Our results suggest an interpretation to the observed distributions of orbital and stellar rotation periods.In the second part of the manuscript, we show how the observation of advanced binary stars allows us to test astrophysical theories, in particular asteroseismology and tidal interaction. First, we present the results of an observation program that we conducted for more than two years and that allowed us to characterize 16 eclipsing binary systems. Then, we compare these results with those obtained by analyzing this sample using asteroseismic tools to verify the accuracy of the latter. Finally, by extending the studied sample to 30 other advanced binary stars including an evolved primary, we test the theory of tidal evolution. This allows us both to validate the theory and to understand the evolution of the systems observed in this work.This work highlights two aspects of the specificity of multiple systems. First, it shows how the evolution of stars is affected by the presence of a stellar or planetary companion. Second, it emphasizes the interest of binary stars in testing astrophysical theories and reinforces the current understanding of stellar evolution
Neves, Vasco. "Étude sur les paramétres stellaires des naines M et leur lien à la formation planétaire". Thesis, Grenoble, 2013. http://www.theses.fr/2013GRENY082/document.
Pełny tekst źródłaAt the time of writing of this Thesis more than 900 planets have been announced and about 2700 planets from the Kepler space telescope are waiting to be confirmed. The very precise spectra and light curves obtained in Doppler and transit surveys, allows the in-depth study of the parameters of the host stars, and opens the possibility to investigate the star-plant correlations. Also, determining the stellar parameters with precision is critical for more precise determinations of the planetary parameters, namely, mass, radius, and density.In the case of the FGK dwarfs, the determination of stellar parameters is well established and can be used with confidence to study the star-planet relation as well as to obtain precise planetary parameters. However, this is not the case for M dwarfs, the most common stars in the Galaxy. Compared to their hotter cousins, M dwarfs are smaller, colder, and fainter, and therefore harder to study. The biggest challenge regarding M dwarfs is related to the presence of billions of molecular lines that depress the continuum making a classical spectral analysis almost impossible. Finding new and innovative ways to overcome this obstacle in order to obtain precise stellar parameters is the goal of this Thesis.To achieve this goal I focused my research into two main avenues: photometric and spectroscopic methods. My initial work had the objective of establishing a precise photometric metallicity calibration, but I could not reach this goal, as I did not have enough FGK+M binaries with good photometric data. However, it was possible, with the available data, to compare the already established photometric calibrations and slightly improve the best one, as described in Chapter 3.Then, I focused on spectroscopic approaches with the aim of obtaining precise M dwarf parame- ters. To this end I used HARPS high-resolution spectra and developed a method to measure the spectral lines disregarding the continuum completely. Using this method I established a new visible calibration with a precision of 0.08 dex for [Fe/H] and 80 K for Te f f . This work is detailed in Chapter 4.Finally, I also participated in the refinement of the parameters of the star GJ3470 and its planet, where my expertise in stellar parameters of M dwarfs had an important role. The details regarding this investigation are shown in Chapter 5
No momento em que escrevo esta Tese, o número de planetas anunciados já ultrapassou os 900 e os cerca de 2700 candidatos detectados pelo telescópio espacial Kepler esperam por confirmação. Os espectros e as curvas de luz obtidos nos programas de procura de planetas permitem, também, o estudo em profundidade dos parâmetros das estrelas com planetas e abrem a possibilidade de investigar a relação estrela-planeta. Neste contexto, a determinação com precisão dos parâmetros estelares é crítica na determinação precisa dos parâmetros planetários, nomeadamente, a massa, o raio e a densidade.No caso das anãs FGK, os métodos de determinação dos parâmetros estelares estão bem estabelecidos e podem ser usados com confiança no estudo da relação estrela-planeta, assim como na obtenção de parâmetros planetários precisos. No entanto, não é esse o caso para as anãs M, as estrelas mais comuns da nossa Galáxia. Ao contrário das suas primas, as estrelas M são mais pequenas, frias e ténues e, assim sendo, mais difíceis de estudar. O grande entrave no estudo das estrelas M está relacionado com a presença de biliões de linhas moleculares que deprimem o contínuo espectral, fazendo com que uma análise espectral clássica se torne quase impossível. A procura de métodos inovadores que possibilitem ultrapassar este obstáculo, tendo em vista a obtenção de parâmetros precisos, é o objectivo desta Tese.Tendo em conta esse objetivo, foquei os meus esforços em duas linhas principais de pesquisa, baseadas em métodos fotométricos e métodos espectroscópicos. O meu trabalho inicial tinha como objetivo o estabelecimento de uma calibração fotométrica para a metalicidade, mas não me foi possível atingir esse objetivo, pois não tinha sistemas binários FGK+M suficientes com bons dados fotométricos. No entanto, foi possível, com os dados disponíveis, comparar as calibrações fotométricas existentes e refinar ligeiramente a melhor delas, como descrito no Capítulo 3.Após este trabalho passei a concentrar-me em técnicas espectroscópicas de obtenção de parâmetros estelares em estrelas M. Tendo em mente esse objetivo, usei espectros HARPS de alta resolução para desenvolver um novo método de medição de linhas espectrais independente do contínuo espectral. Seguidamente, usei este método no desenvolvimento de uma nova calibração de metalicidade e temperatura efectiva em estrelas M na região do visível, através da qual consegui atingir uma precisão de 0.08 dex para a [Fe/H] e de 80 K para a temperatura. Este trabalho está descrito no Capítulo 4.Ao mesmo tempo colaborei na determinação com precisão dos parâmetros da estrela GJ3470 e do seu planeta, onde a minha proficiência na determinação de parâmetros estelares em anãs M teve um papel importante. Os detalhes relacionados com este trabalho de investigação estão descritos no Capítulo 5
Części książek na temat "Formation et évolution des systèmes planétaires"
"7 Formation et évolution des systèmes planétaires". W La révolution des exoplanètes, 89–108. EDP Sciences, 2020. http://dx.doi.org/10.1051/978-2-7598-2148-8-008.
Pełny tekst źródła"7 Formation et évolution des systèmes planétaires". W La révolution des exoplanètes, 89–108. EDP Sciences, 2020. http://dx.doi.org/10.1051/978-2-7598-2148-8.c008.
Pełny tekst źródłaLEQUEUX, James. "Système solaire et systèmes planétaires". W Le Système solaire 1, 47–99. ISTE Group, 2021. http://dx.doi.org/10.51926/iste.9033.ch2.
Pełny tekst źródła