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Literatura académica sobre el tema "Formation stellaire – Modèles mathématiques"
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Artículos de revistas sobre el tema "Formation stellaire – Modèles mathématiques"
Walch, Jean-paul y Solange Blaise. "Introduction aux modèles phyllotaxiques". Le Journal de botanique 97, n.º 1 (2021): 2–11. http://dx.doi.org/10.3406/jobot.2021.2342.
Texto completoBIDDULPH, George Elliot, Yannick Enock BOCKO, Pierre BOLA, Bart CREZEE, Greta DARGIE, Ovide EMBA, Selena GEORGIOU et al. "Connaissances actuelles et orientations futures des recherches sur le complexe de tourbières de la Cuvette centrale du Congo". BOIS & FORETS DES TROPIQUES 355 (1 de marzo de 2023): 73–86. http://dx.doi.org/10.19182/bft2023.355.a37152.
Texto completoAbboud, Maha. "Mathematics teachers in the time of digital technologies: a theoretical framework adapting the double approach to study their activity". Recherches en Didactique des Mathématiques Synthesis and perspectives in... (16 de mayo de 2024). http://dx.doi.org/10.46298/rdm.12910.
Texto completoKuzniak, Alain. "The teaching of mathematical modelling and the mathematical work: A dynamic that is problematic". Recherches en Didactique des Mathématiques Synthesis and perspectives in... (16 de mayo de 2024). http://dx.doi.org/10.46298/rdm.12907.
Texto completoLeonardo Javier, D’Andrea. "Indicadores referenciales asociados a la enseñanza y el aprendizaje del cálculo diferencial e integral en una variable para el desarrollo de competencias en ingeniería electrónica". RIDAA Tesis Unicen, 11 de julio de 2023. http://dx.doi.org/10.52278/3627.
Texto completoTesis sobre el tema "Formation stellaire – Modèles mathématiques"
Bruel, Tristan. "Les coalescences de trous noirs à l'interface de la formation stellaire globale et de l'évolution stellaire". Electronic Thesis or Diss., Université Côte d'Azur, 2024. http://www.theses.fr/2024COAZ5054.
Texto completoMore than a hundred binary black hole (BBH) merger candidates have now been reported by the LIGO-Virgo-KAGRA (LVK) Collaboration after their first three series of observations and during the current O4 run. Physical properties of these tight pairs of compact objects merging in the local Universe are becoming increasingly well constrained. However, the question of their astrophysical origin and the nature of the dominant mechanisms behind their formation has yet to be fully answered. The two main scenarios generally put forward to explain the existence of these systems are, on the one hand, a series of interactions between two massive stars in a binary system and, on the other, a large number of dynamical interactions between stars and black holes in star clusters. The relative contribution of each of these two channels to the overall population is still unknown. While in recent years a number of studies have focused on either one or the other scenario, it is extremely challenging to model them together and in a consistent way within a cosmological context.During my thesis, I focused on this question and sought to constrain the different properties of BBHs that result from the isolated evolution of stellar binaries and those that form in massive star clusters. To this end, I use cosmological simulations as realistic environments in which the formation of stars and of star clusters across cosmic time can be modelled consistently for the first time. I first present some predictions of binary stellar evolution leading to the formation of merging BBHs using the rapid binary population synthesis code COSMIC. Combined with simplified analytic models of star formation, I am able to produce synthetic populations of BBHs that can be compared with LVK observations. By adopting different hypotheses on the binary evolution of massive stars and on the formation rate density of stars in the Universe, I find that the uncertainties on these two aspects are still too large to constrain the formation environment of these systems in a robust way.With regard to the dynamical formation of BBHs, I have joined an international collaboration and developed a project to study the formation and evolution of massive star clusters in cosmological simulations of individual galaxies with a wide range of present-day physical properties. Using the properties of the giant molecular clouds present in each simulated galaxy associated with a cluster formation model built consistently, I am able to produce the very first populations of realistic star clusters formed in various galaxies across cosmic time. The massive star clusters are integrated forward in time with the code for cluster evolution CMC, taking into account their interactions with the galactic surrounding. By examining the merging BBHs formed dynamically in these dense environments, I am able to identify some of their physical properties that could help identify the formation channel of the most massive BBH mergers observed by LVK. I also find strong correlations between local peaks in the BBH merger rate, recent formation of massive star clusters, and intense episodes of star formation, sometimes linked to interactions between galaxies or even to galaxy mergers.Finally, I extend this method built on simulations of individual galaxies to a cosmological volume simulation containing thousands of galaxies. I find that massive Milky Way-like galaxies, despite their low number compared to the numerous low-mass dwarf galaxies, have the larger contribution to the overall population of merging BBHs formed dynamically in massive star clusters. By using jointly the rapid code for binary evolution COSMIC and the code for cluster evolution CMC applied to stellar binaries and star clusters located within a common cosmological simulation, I create a common framework to study the formation of merging BBHs following the two aforementioned channels in the most consistent way
Couture, Pierre. "Galaxies à sursauts de formation stellaire : Simulations pour la mission UVIT". Thesis, Université Laval, 2011. http://www.theses.ulaval.ca/2011/28432/28432.pdf.
Texto completoMarseille, Matthieu. "Observations et modélisations de proto-étoiles massives dans le cadre des observatoires Herschel". Thesis, Bordeaux 1, 2008. http://www.theses.fr/2008BOR13658/document.
Texto completoToday the formation of massive stars is still not well understood due to the huge interac- tion of these objects with their environment, leading to a theoretical limit in the ?nal mass that observations contradict. The future observatories, like the Herschel Space Observatory, will try to answer some of the questions linked to this topic, particularly through the water line emissions. The correct and precise analysis of the future data is then necessary and needs a full work linking the observations and the modelling of the objects that will be studied. Hence the main goal of this PhD Thesis was to elaborate a robust and global modeling method of the massive dense cores in which high-mass stars are forming. The method leaded to a physical description and a chemical study of multiple massive dense cores, opening new views on evolution aspects. In addition it gave some tweaks on the guaranteed-time key program WISH for the water line emissions and con?rmed the key role of this molecule for a better understanding of the high-mass star formation
Côté, Benoit. "Modèle de vents galactiques destiné aux simulations cosmologiques à grande échelle". Master's thesis, Université Laval, 2010. http://hdl.handle.net/20.500.11794/22281.
Texto completoAlibert, Yann. "De la physique stellaire à la physique galactique : formation, évolution et pulsations stellaires. Modèles galactiques". Lyon, École normale supérieure (sciences), 2002. http://www.theses.fr/2002ENSL0191.
Texto completoDuhamel, Jean. "Effets diffusionnels dans la formation d'excimères intermoléculaires". Vandoeuvre-les-Nancy, INPL, 1989. http://www.theses.fr/1989NAN10401.
Texto completoMeliani, Salha. "Etude asymptotique et numérique d'un modèle thermo-chimique de formation d'un matériau composite". Saint-Etienne, 2003. http://www.theses.fr/2003STET4009.
Texto completoWe consider a composite material constituted of carbon or glass fibres included in a resin which becomes solid when it is heated up (reaction of reticulation). The mathematical modelling of the cure process is given by a kinetic equation describing the evolution of the reaction of reticulation coupled with the heat eqaution. The geometry of the composite material is periodic, with a small period E > 0. First we prove the existence and uniqueness of a solution by using Schauder's fixed point theorem. Then, by using an asymptotic expansion, we decrive the homogenized problem which describes the macroscopic behaviour of the material. We prove the convergence of the solution of the problem to the solution of the homogenized problem when E tends to zero and we obtain an error estimation in a case of weak non-linearity. Finally we solve numerically the homogenized problem
Bagot, Philippe. "Modèles de formation de systèmes doubles d'étoiles à neutrons". Montpellier 2, 1996. http://www.theses.fr/1996MON20178.
Texto completoLi, Jianfei. "Modélisation de la formation des contraintes résiduelles dans les dépôts élaborés par projection thermique". Besançon, 2006. http://www.theses.fr/2005BESA2061.
Texto completoThermal spray processes consist in elaborating a coating on a workpiece in order to protect it against corrosion, wear or thermal fluxes for example. Since the coatings are formed by the flattening and solidification of molten droplets sprayed on the surface, they are affected by residual stresses during their elaboration. This study is devoted to the modelling of the residual stresses formation during the coating elaboration. These stresses have two major contributions: - quenching stresses appearing during the flattening, solidification and cooling of individual splats. - thermal stresses appearing during the workpiece overall cooling down. The finite element SYSWELD software was used in the present study. It is specialized in the modelling of stresses induced during welding applications. Since thermal aspects play an important role in the formation of stresses for thermally sprayed coatings, they were first considered. The influence of thermal fluxes transferred to different shape workpieces using different trajectories is hence first presented. Moreover, the stresses formation modelling is presented in the last chapter. The cases of alumina and molybdenum coatings sprayed on a steel substrate are considered. Numerical results show that the overall residual stress level may be modified by using cooling devices during the coating elaboration
Combet, Céline. "Etude analytique et numérique des flots autour des étoiles jeunes". Phd thesis, Université Paris Sud - Paris XI, 2006. http://tel.archives-ouvertes.fr/tel-00090716.
Texto completoLorsqu'une étoile se forme, alors que l'accrétion sur l'objet central se poursuit, de gigantesques éjections de matière se produisent sous forme de jets et flots moléculaires bipolaires. Après une
introduction donnant une vision globale de tous les éléments
impliqués dans la formation stellaire, nous présentons les modèles "standards" pour les flots moléculaires. Dans un
troisième temps, nous construisons un modèle alternatif et complémentaire aux approches standards~: le modèle de transit. Il s'agit d'un modèle MHD, autosimilaire et qui considère le renversement d'un partie de l'écoulement lorsque le gaz en chute
approche de l'objet central. Les résultats montrent notamment que le modèle permet de rendre compte des taux de masses observés lors de la formation des étoiles massives, taux que les modèles standards atteignent difficilement. Le modèle est étudié de façon
extensive grâce à une exploration Monte Carlo de l'espace des paramètres et la mise en évidence de deux grandes familles de solutions. Le modèle de transit donne une description à grande échelle de l'environnement proto-stellaire et montre une forte structuration du milieu autant en densité qu'en vitesse. C'est dans un tel milieu que le jet issu du disque d'accrétion se propage, et une étude numérique préliminaire de cette propagation montre que la morphologie et la cinématique du jet est fortement affectée par le milieu ambiant. Nous en déduisons l'importance d'avoir un bonne description de ce dernier et la nécessité de ne pas se contenter des milieux "uniformes et au repos" généralement considérés.
La seconde partie est consacrée à la partie nucléaire du rayonnement cosmique Galactique. Ce "rayonnement" est constitué de noyaux qui se sont propagés dans la Galaxie et son halo diffusif, après avoir été accélérés dans les chocs de supernovae. Certains de ces noyaux atteignent la Terre où ils
sont détectés. Comprendre la propagation de ces noyaux est essentiel pour remonter, à partir des mesures, aux abondances des noyaux dans les sources. Dans ce travail, nous nous intéressons spécifiquement au cas des noyaux lourds, en connection avec l'expérience UHCRE, et regardons comment la structure locale de la Galaxie, la "bulle locale", affecte la propagation des lourds. Nous trouvons que la sous-densité locale du voisinnage solaire joue effectivement un rôle dans la détermination des abondances sources et que l'effet tend à réduire les différences entre les abondances sources et les abondances solaires des noyaux. Nous donnons enfin dans un dernier chapitre quelques perspectives pour la poursuite de cette étude.
Libros sobre el tema "Formation stellaire – Modèles mathématiques"
(Firm), Knovel, ed. Well logging and formation evaluation. Amsterdam: Elsevier, 2005.
Buscar texto completo1955-, Chaube Rajesh y Kishi Toshiharu 1955-, eds. Modelling of concrete performance: Hydration, microstructure formation, and mass transport. London: E & FN Spon, 1999.
Buscar texto completoL, Commons Michael y Symposium on Quantitative Analyses of Behavior., eds. Behavioral approaches to pattern recognition and concept formation. Hillsdale, NJ: Erlbaum Associates, 1990.
Buscar texto completoL, Commons Michael y Symposium on Quantitative Analyses of Behavior. (8th : 1985 : Harvard University), eds. Computational and clinical approaches to pattern recognition and concept formation. Hillsdale, N.J: Lawrence Erlbaum Associates, 1990.
Buscar texto completoUpadhyay, Ranjit Kumar y Satteluri R. K. Iyengar. Spatial Dynamics and Pattern Formation in Biological Populations. Taylor & Francis Group, 2021.
Buscar texto completoUpadhyay, Ranjit Kumar y Satteluri R. K. Iyengar. Spatial Dynamics and Pattern Formation in Biological Populations. Taylor & Francis Group, 2021.
Buscar texto completoUpadhyay, Ranjit Kumar y Satteluri R. K. Iyengar. Spatial Dynamics and Pattern Formation in Biological Populations. Taylor & Francis Group, 2021.
Buscar texto completoUpadhyay, Ranjit Kumar y Satteluri R. K. Iyengar. Spatial Dynamics and Pattern Formation in Biological Populations. Taylor & Francis Group, 2021.
Buscar texto completoSpatial Dynamics and Pattern Formation in Biological Populations. Taylor & Francis Group, 2021.
Buscar texto completoKahan, James P. y Amnon Rapoport. Theories of Coalition Formation. Taylor & Francis Group, 2014.
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