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This Ph.D. thesis in mathematical physics concerns systems of interacting fermions with strong correlations. For these systems the physical properties can only be described in terms of the collective behavior of the fermions. Moreover, they are often characterized by a close competition between fermion localization versus delocalization, which can result in complex and exotic physical phenomena. Strongly correlated fermion systems are usually modelled by many-body Hamiltonians for which the kinetic- and interaction energy have the same order of magnitude. This makes them challenging to study as the application of conventional computational methods, like mean field- or perturbation theory, often gives unreliable results. Of particular interest are Hubbard-type models, which provide minimal descriptions of strongly correlated fermions. The research of this thesis focuses on such models defined on two-dimensional square lattices. One motivation for this is the so-called high-Tc problem of the cuprate superconductors. A main hypothesis is that there exists an underlying Fermi surface with nearly flat parts, i.e. regions where the surface is straight. It is shown that a particular continuum limit of the lattice system leads to an effective model amenable to computations. This limit is partial in that it only involves fermion degrees of freedom near the flat parts. The result is an effective quantum field theory that is analyzed using constructive bosonization methods. Various exactly solvable models of interacting fermions in two spatial dimensions are also derived and studied. / QC 20111207

Thesis (Ph. D.)--University of Texas at Austin, 2008. / Vita. Includes bibliographical references.

Thesis (Ph. D.)--University of Washington, 1997. / Vita. Includes bibliographical references (p. [148]-178).

Thesis (Ph. D.)--University of Missouri-Columbia, 1997. / Typescript. Vita. Includes bibliographical references. Also available on the Internet.

Thesis (Ph. D.)--University of Missouri-Columbia, 1997. / Typescript. Vita. Includes bibliographical references. Also available on the Internet.

Thesis (Ph. D.)--Florida State University, 2004. / Advisor: Dr. Jorge Piekarewicz, Florida State University, College of Arts and Sciences, Dept. of Physics. Title and description from dissertation home page (Jan. 19, 2005). Includes bibliographical references.

Thesis (Ph.D.)--Memorial University of Newfoundland, 2000. / Restricted until June 2001. Bibliography: leaves 215-226.

Thesis (Ph. D.)--University of Washington, 2005. / Vita. Includes bibliographical references (p. 92-102).

L’étude des systèmes avec interactions gravitationnelles à l’aide des outils de la mécanique statistique repose jusqu’à présent sur l’utilisation d’une approximation de type champ moyen, qui néglige par construction les effets à courte portée de l’interaction. Pour commencer, je décris cette approximation dans son contexte historique, à savoir le modèle de la sphère isotherme. Puis, dans le cadre de la mécanique statistique du problème à N -corps, j’introduis un système de sphères dures massives, qui permet de s’affranchir de l’effondrement du système de points matériels. La validité de l’approche hydrostatique est discutée dans l’ensemble microcanonique, en introduisant une limite d’échelle adéquate.Cette étude permet de mettre en avant les critères de validité pour l’approche hydrostatique, et de constater qu’ils peuvent être mis en défaut dans les systèmes astrophysiques de type amas globulaire. Pour mieux les comprendre et les illustrer, je me concentre ensuite sur l’étude d’un modèle de bâtonnets durs massifs à une dimension, dont l’avantage est de permettre tous les calculs analytiques des différentes grandeurs statistiques. Ainsi, je mets en évidence comment l’approche de type champ moyen est mise en défaut pour certains états effondrés.Enfin, dans le but de tenter de décrire des amas globulaires, je développe un modèle comprenant des étoiles célibataires et des étoiles binaires. Ce modèle reproduit bien les effets qualitatifs attendus, et il constitue une première correction satisfaisante au modèle historique de la sphère isotherme. Je met aussi en évidence l’absence d’équilibre thermodynamique au sens strict pour les systèmes considérés. En conclusion, je réalise une discussion succincte de certains éléments dynamiques du problème. / The study of systems with gravitational interactions with the tools of mechanics statistics was based so far on the use of a mean-field approximation, which neglect by construction effects of the short-range interaction. To begin, I describe this approximation in its historical context, namely the model of isothermal sphere. Then, as part of statistical mechanics of many-body problem, I introduce a system of massive hard spheres, which overcomes the collapse of the point partcile system. The validity of the hydrostatic approach is discussed in the microcanonical ensemble, by introducing an appropriate scaling limit.This study helps to highlight conditions of validity of the the hydrostatic approach and show that those conditions may prove defective in astrophysical systems such globular clusters. To better understand and illustrate this point, I focus on the study of a model of massive hard sticks in one dimension, which has the advantage of allowing all analytical calculations of various statistical quantities. Thus, I highlight how the mean field type approach can be wrong for some collapsed states.Finally, in an attempt to describe globular clusters, I develop a model consisting of single stars and binaries stars systems. This model reproduces the expected qualitative effects, and is a good first correction of the historical model of the isothermal sphere. I also highlight the absence of thermodynamic equilibrium in the strict sense for the systems we study. In conclusion, I realize a brief discussion of some dynamical issues.