The Double-TOP trap is a new type of magnetic trap for neutral atoms, and is suitable for Bose-Einstein condensates (BECs) and evaporatively cooled atoms. It combines features from two other magnetic traps, the Time-averaged Orbiting Potential (TOP) and Ioffe-Pritchard traps, so that a potential barrier can be raised in an otherwise parabolic potential. The cigar-like cloud of atoms (in the single-well configuration) is divided halfway along its length when the barrier is lifted. A theoretical model of the trap is presented. The double-well is characterised by the barrier height and well separation, which are weakly coupled. The accessible parameter space is found by considering experimental limits such as noise, yielding well separations from 230 [mu]m up to several millimetres, and barrier heights from 65 pK to 28 [mu]K (where the energies are scaled by Boltzmann�s constant). Potential experiments for Bose-Einstein condensates in this trap are considered. A Double-TOP trap has been constructed using the 3-coil style of Ioffe-Pritchard trap. Details of the design, construction and current control for these coils are given. Experiments on splitting thermal clouds were carried out, which revealed a tilt in the potential. Two independent BECs were simultaneously created by applying evaporative cooling to a divided thermal cloud. The Double-TOP trap is used to form a linear collider, allowing direct imaging of the interference between the s and d partial waves. By jumping from a double to single-well trap configuration, two ultra-cold clouds are launched towards a collision at the trap bottom. The available collision energies are centred on a d-wave shape resonance so that interference between the s and d partial waves is pronounced. Absorption imaging allows complete scattering information to be collected, and the images show a striking change in the angular distribution of atoms post-collision. The results are compared to a theoretical model, verifying that the technique is a useful new way to study cold collisions.

In General Relativity, the Einstein field equations allow us to study the evolution of a spacelike 3-manifold, provided that its metric and extrinsic curvature satisfy a system of geometric constraint equations. The so-called Einstein constraint equations, arise as a consequence of the fact that the 3-manifold in question is necessarily a submanifold of the spacetime its evolution defines. This thesis is devoted to a study of the structure of the Einstein constraint system in the special case when the spacelike 3-manifold also satisfies the quasispherical ansatz of Bartnik [B93]. We make no mention of the generality of this gauge; the extent to which the quasispherical ansatz applies remains an open problem. After imposing the quasispherical gauge, we give an argument to show that the resulting Einstein constraint system may be viewed as a coupled system of partial differential equations for the parameters describing the metric and second fundamental form. The hencenamed quasisperical Einstein constraint system, consists of a parabolic equation, a first order elliptic system and (essentially) a system of ordinary differential equations. The question of existence of solutions to this system naturally arises and we provide a partial answer to this question. We give conditions on the initial data and prescribable fields under which we may conclude that the quasispherical Einstein constraint system is uniquley solvable, at least in a region surrounding the unit sphere. The proof of this fact is centred on a linear iterative system of partial differential equations, which also consist of a parabolic equation, a first order elliptic system and a system of ordinary differential equations. We prove that this linear system consistently defines a sequence, and show via a contraction mapping argument, that this sequence must converge to a fixed point of the iteration. The iteration, however, has been specifically designed so that any fixed point of the iteration coincides with a solution of the quasispherical Einstein constraints. The contraction mapping argument mentioned above, relies heavily on a priori estimates for the solutions of linear parabolic equations. We generalise and extend known results 111 concerning parabolic equations to establish special a priori estimates which relate a useful property: the L2-Sobolev regularity of the solution of a parabolic equation is greater than that of the coefficients of the elliptic operator, provided that the initial data is sufficiently regular. This 'smoothing' property of linear parabolic equations along with several estimates from elliptic and ordinary differential equation theory form the crucial ingredients needed in the proof of the existence of a fixed point of the iteration. We begin in chapter one by giving a brief review of the extensive literature concerning the initial value problem in General Relativity. We go on, after mentioning two of the traditional methods for constructing spacetime initial data, to introduce the notion of a quasispherical foliation of a 3-manifold and present the Einstein constraint system written in terms of this gauge. In chapter two we introduce the various inequalities and tracts of analysis we will make use of in subsequent chapters. In particular we define the, perhaps not so familiar, complex differential operator 9 (edth) of Newman and Penrose. In chapter three we develop the appropriate Sobolev-regularity theory for linear parabolic equations required to deal with the quasispherical initial data constraint equations. We include a result due to Polden [P] here, with a corrected proof. This result was essential for deriving the results contained in the later chapters of [P], and it is for this reason we include the result. We don't make use of it explicitly when considering the quasispherical Einstein constraints, but the ideas employed are similar to those we use to tackle the problem of existence for the quasispherical constraints. Chapter four is concerned with the local existence of quasispherical initial data. We firstly consider the question of existence and uniqueness when the mean curvature of the 3-manifold is prescribed, then after introducing the notion of polar curvature, we also present another quasispherical constraint system in which we consider the polar curvature as prescribed. We prove local existence and uniqueness results for both of these alternate formulations of the quasispherical constraints. This thesis was typeset using LATEXwith the package amssymb.

An analysis of the Einstein Field Equations within a Robertson-Walker Cosmology. More specifically, what values of the cosmological constant will result in a Big Bang.

Dans cette thèse nous analysons la place logique que les principes ont occupée à la fin du XIXe et au début du XXe siècle dans la construction des théories relativistes. Après une présentation de caractère général et historique (chapitres 1-3) dans laquelle nous rappelons le statut des principes dans la tradition classique et dans les travaux de Newton, et dans laquelle nous tentons de montrer comment la théorie de la thermodynamique et les théories de la lumière ont pu remettre en cause cette tradition, le corpus de la thèse peut être divisé en deux grandes parties, une première (chapitres 4-6) consacrée à la relativité restreinte, et une deuxième (chapitres 7-9) consacrée à la théorie de la relativité générale. Le chapitre 1 est consacré à rappeler ce que sont les principes dans la tradition classique, d’Aristote à Galilée et Newton. Dans le deuxième chapitre nous évoquons la formulation des deux principes de la thermodynamique et nous montrons en quoi ils s’éloignent de la mécanique classique et peuvent être considérés comme deux principes d’un nouveau type. Dans le troisième chapitre nous présentons un panorama des théories physiques à la fin du XIXe siècle, afin de replacer dans leur contexte les réflexions qui ont conduit à la formulation de la théorie de la relativité restreinte. Les chapitres quatre et cinq sont consacrés au principe de relativité. Dans le chapitre quatre nous l’abordons de façon géométrique, en mettant en évidence les différences entre espace géométrique et espace physique et les problèmes liés à l’espace absolu. Au chapitre cinq nous analysons de plus près la formulation du principe de relativité dans les travaux de Poincaré de 1904-1905. Le chapitre six est consacré à la présentation de la relativité restreinte faite par Einstein la même année 1905. Les chapitres sept, huit et neuf sont consacrés à la relativité générale et aux principes qu’Einstein pose à sa base. Dans le chapitre sept nous analysons le principe d’équivalence et la première période de formulation de la théorie de la relativité générale (1907-1912). Le chapitre 8 reprend le thème de la géométrie et montre comment des considérations générales sur la non-validité de la géométrie euclidienne ont mis Einstein sur la voie de la théorie généralisée de la gravitation. Le chapitre 9 aborde un moment délicat de la construction de la théorie : les années 1913-1915, pendant lesquelles Einstein abandonne l’idée de covariance générale et essaie d’établir les équations de la théorie. Nous analysons les principes qui le guident dans ses recherches et ceux qu’il abandonne (même temporairement), pour montrer enfin comment Einstein est arrivé à la formulation de la théorie de la relativité générale.

In this thesis we consider the Einstein-Vlasov system, which models a system of particles within the framework of general relativity, and where collisions between the particles are assumed to be sufficiently rare to be neglected. Here the particles are stars, galaxies or even clusters of galaxies, which interact by the gravitational field generated collectively by the particles. The thesis consists of three papers, and the first two are devoted to cylindrically symmetric spacetimes and the third treats the spherically symmetric case. In the first paper the time-dependent Einstein-Vlasov system with cylindrical symmetry is considered. We prove global existence in the so called polarized case under the assumption that the particles never reach a neighborhood of the axis of symmetry. In the more general case of a non-polarized metric we need the additional assumption that the derivatives of certain metric components are bounded in a vicinity of the axis of symmetry to obtain global existence. The second paper of the thesis considers static cylindrical spacetimes. In this case we prove global existence in space and also that the solutions have finite extension in two of the three spatial dimensions. It then follows that it is possible to extend the spacetime by gluing it with a Levi-Civita spacetime, i.e. the most general vacuum solution of the static cylindrically symmetric Einstein equations. In the third and last paper, which is a joint work with C. Uggla and M. Heinzle, the static spherically symmetric Einstein-Vlasov system is studied. We introduce a new method by rewriting the system as an autonomous dynamical system on a state space with compact closure. In this way we are able to improve earlier results and enlarge the class of distribution functions which give rise to steady states with finite mass and finite extension.

Recently the phenomena of Bose-Einstein condensates have been observed in laboratories, and the related problems are extensively studied. In this paper we consider the nonlinear Schrödinger equation in the laser beam rotating magnetic field and compute its corresponding energy functional under the mass conservative condition. By separating time and space variables, factoring real part and image part, and discretizing via finite difference method, the original equation can be transformed to a large scale parametrized polynomial systems. We use continuation method to find the solutions that satisfy the mass conservative condition. We will also explore bifurcation points on the curves and other solutions lying on bifurcation branches. The numerical results show that when the rotating angular momentum is small, we can find the solutions by continuation method along some particular curves and these curves are regular. As the angular momentum is increasing, there will be more bifurcation points on curves.

Thèse de doctorat : Mathématiques : Paris Est : 2008. Thèse de doctorat : Mathématiques : Scuola Normale Superiore di Pisa : 2008. / Thèse soutenue en co-tutelle. Titre provenant de l'écran-titre.

Thèse de doctorat : Mathématiques : Tours : 2008. / Titre provenant de l'écran-titre.

Thesis (Ph. D.)--University of Washington, 2001. / Vita. Includes bibliographical references (leaves 75-83).

Thesis (Ph. D.)--University of Washington, 2003. / Vita. Includes bibliographical references (p. 205-211).