Coframes, Spinors and Torsion
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1 HESTENES' TETRAD and SPIN CONNECTIONS Frank
HESTENES’ TETRAD AND SPIN CONNECTIONS Frank Reifler and Randall Morris Lockheed Martin Corporation MS2 (137-205) 199 Borton Landing Road Moorestown, New Jersey 08057 ABSTRACT Defining a spin connection is necessary for formulating Dirac’s bispinor equation in a curved space-time. Hestenes has shown that a bispinor field is equivalent to an orthonormal tetrad of vector fields together with a complex scalar field. In this paper, we show that using Hestenes’ tetrad for the spin connection in a Riemannian space-time leads to a Yang-Mills formulation of the Dirac Lagrangian in which the bispinor field Ψ is mapped to a set of × K ρ SL(2,R) U(1) gauge potentials Fα and a complex scalar field . This result was previously proved for a Minkowski space-time using Fierz identities. As an application we derive several different non-Riemannian spin connections found in the literature directly from an arbitrary K linear connection acting on the tensor fields (Fα ,ρ) . We also derive spin connections for which Dirac’s bispinor equation is form invariant. Previous work has not considered form invariance of the Dirac equation as a criterion for defining a general spin connection. 1 I. INTRODUCTION Defining a spin connection to replace the partial derivatives in Dirac’s bispinor equation in a Minkowski space-time, is necessary for the formulation of Dirac’s bispinor equation in a curved space-time. All the spin connections acting on bispinors found in the literature first introduce a local orthonormal tetrad field on the space-time manifold and then require that the Dirac Lagrangian be invariant under local change of tetrad [1] – [8]. -
Arxiv:1907.02341V1 [Gr-Qc]
Different types of torsion and their effect on the dynamics of fields Subhasish Chakrabarty1, ∗ and Amitabha Lahiri1, † 1S. N. Bose National Centre for Basic Sciences Block - JD, Sector - III, Salt Lake, Kolkata - 700106 One of the formalisms that introduces torsion conveniently in gravity is the vierbein-Einstein- Palatini (VEP) formalism. The independent variables are the vierbein (tetrads) and the components of the spin connection. The latter can be eliminated in favor of the tetrads using the equations of motion in the absence of fermions; otherwise there is an effect of torsion on the dynamics of fields. We find that the conformal transformation of off-shell spin connection is not uniquely determined unless additional assumptions are made. One possibility gives rise to Nieh-Yan theory, another one to conformally invariant torsion; a one-parameter family of conformal transformations interpolates between the two. We also find that for dynamically generated torsion the spin connection does not have well defined conformal properties. In particular, it affects fermions and the non-minimally coupled conformal scalar field. Keywords: Torsion, Conformal transformation, Palatini formulation, Conformal scalar, Fermion arXiv:1907.02341v1 [gr-qc] 4 Jul 2019 ∗ [email protected] † [email protected] 2 I. INTRODUCTION Conventionally, General Relativity (GR) is formulated purely from a metric point of view, in which the connection coefficients are given by the Christoffel symbols and torsion is set to zero a priori. Nevertheless, it is always interesting to consider a more general theory with non-zero torsion. The first attempt to formulate a theory of gravity that included torsion was made by Cartan [1]. -
On Dark Energy Models of Single Scalar Field
Home Search Collections Journals About Contact us My IOPscience On dark energy models of single scalar field This content has been downloaded from IOPscience. Please scroll down to see the full text. JCAP04(2012)003 (http://iopscience.iop.org/1475-7516/2012/04/003) View the table of contents for this issue, or go to the journal homepage for more Download details: IP Address: 140.112.101.4 This content was downloaded on 06/11/2014 at 07:57 Please note that terms and conditions apply. ournal of Cosmology and Astroparticle Physics JAn IOP and SISSA journal On dark energy models of single scalar field JCAP04(2012)003 Mingzhe Li,a,f Taotao Qiu,b,c Yifu Caid and Xinmin Zhange aDepartment of Physics, Nanjing University, Nanjing 210093, P.R. China bDepartment of Physics and Center for Theoretical Sciences, National Taiwan University, Taipei 10617, Taiwan cLeung Center for Cosmology and Particle Astrophysics, National Taiwan University, Taipei 106, Taiwan dDepartment of Physics, Arizona State University, Tempe, AZ 85287, U.S.A. eInstitute of High Energy Physics, Chinese Academy of Sciences, P.O. Box 918-4, Beijing 100049, P.R. China f Joint Center for Particle, Nuclear Physics and Cosmology, Nanjing University — Purple Mountain Observatory, Nanjing 210093, P.R. China E-mail: [email protected], [email protected], [email protected], [email protected] Received January 2, 2012 Accepted March 7, 2012 Published April 2, 2012 Abstract. In this paper we revisit the dynamical dark energy model building based on single scalar field involving higher derivative terms. By imposing a degenerate condition on the higher derivatives in curved spacetime, one can select the models which are free from the ghost mode and the equation of state is able to cross the cosmological constant boundary smoothly, dynamically violate the null energy condition. -
Cosmología De Tiempo Tardío Para Un Campo Escalar Con
Cosmolog´ıa de Tiempo Tard´ıo para un Campo Escalar con Acoplamientos Cinetico´ y de Gauss-Bonnet Edwin Loaiza Acuna˜ Tesis doctoral presentada como requisito parcial para optar al t´ıtulo de Doctor en Ciencias - F´ısica Director: Luis Norberto Granda Velasquez´ Universidad del Valle Facultad de Ciencias Naturales y Exactas Programa Academico´ de postgrado en F´ısica Julio 2016 Abstract In this thesis we study late-time cosmological solutions for a scalar field model with kinetic coupling to curvature and the scalar field coupled to the Gauss-Bonnet inva- riant, in order to explain the late-time accelerated expansion of the universe. Initially, exact cosmological solutions that show the phases of decelerated expansion, accelera- ted expansion and transition to the phantom phase have been found. These phases are necessary for the satisfactory explanation of the early inflation, and the current acce- lerated (super accelerated) expansion of the universe. These solutions have been found by imposing appropriate restrictions on the Gauss-Bonnet and kinetic couplings, ba- sed on the asimptotic limits of the Friedmann equations. Solutions with Big Rip and without Big Rip singularities have been studied. An especific choice of the Gauss- Bonnet coupling, where the squared of the Hubble parameter is proportional to the kinetic term, allows the reconstruction of the model for an appropriate cosmological evolution. The new found solution can describe the three cosmological phases that go from the power-law expansion, that describes a matter dominated universe, to the scalar field dominated phantom phase. For this solution and according to the values of the equation of state parameter during di↵erent epochs, the parameters of the solution can be adjusted in order to obtain di↵erent scenarios with and without Big Rip singularities. -
3. Introducing Riemannian Geometry
3. Introducing Riemannian Geometry We have yet to meet the star of the show. There is one object that we can place on a manifold whose importance dwarfs all others, at least when it comes to understanding gravity. This is the metric. The existence of a metric brings a whole host of new concepts to the table which, collectively, are called Riemannian geometry.Infact,strictlyspeakingwewillneeda slightly di↵erent kind of metric for our study of gravity, one which, like the Minkowski metric, has some strange minus signs. This is referred to as Lorentzian Geometry and a slightly better name for this section would be “Introducing Riemannian and Lorentzian Geometry”. However, for our immediate purposes the di↵erences are minor. The novelties of Lorentzian geometry will become more pronounced later in the course when we explore some of the physical consequences such as horizons. 3.1 The Metric In Section 1, we informally introduced the metric as a way to measure distances between points. It does, indeed, provide this service but it is not its initial purpose. Instead, the metric is an inner product on each vector space Tp(M). Definition:Ametric g is a (0, 2) tensor field that is: Symmetric: g(X, Y )=g(Y,X). • Non-Degenerate: If, for any p M, g(X, Y ) =0forallY T (M)thenX =0. • 2 p 2 p p With a choice of coordinates, we can write the metric as g = g (x) dxµ dx⌫ µ⌫ ⌦ The object g is often written as a line element ds2 and this expression is abbreviated as 2 µ ⌫ ds = gµ⌫(x) dx dx This is the form that we saw previously in (1.4). -
Spinor Quintom Cosmology with Intrinsic Spin
Hindawi Publishing Corporation Advances in High Energy Physics Volume 2016, Article ID 3740957, 10 pages http://dx.doi.org/10.1155/2016/3740957 Research Article Spinor Quintom Cosmology with Intrinsic Spin Emre Dil DepartmentofPhysics,SinopUniversity,Korucuk,57000Sinop,Turkey Correspondence should be addressed to Emre Dil; [email protected] Received 5 October 2016; Revised 5 November 2016; Accepted 7 November 2016 Academic Editor: Dandala R. K. Reddy Copyright © 2016 Emre Dil. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The publication of this article was funded by SCOAP3. We consider a spinor quintom dark energy model with intrinsic spin, in the framework of Einstein-Cartan-Sciama-Kibble theory. After constructing the mathematical formalism of the model, we obtain the spin contributed total energy-momentum tensor giving the energy density and the pressure of the quintom model, and then we find the equation of state parameter, Hubble parameter, deceleration parameter, state finder parameter, and some distance parameter in terms of the spinor potential. Choosing suitable potentials leads to the quintom scenario crossing between quintessence and phantom epochs, or vice versa. Analyzing three quintom scenarios provides stable expansion phases avoiding Big Rip singularities and yielding matter dominated era through the stabilization of the spinor pressure via spin contribution. The stabilization in spinor pressure leads to neglecting it as compared to the increasing energy density and constituting a matter dominated stable expansion epoch. 1. Introduction which is also named as a ghost [17]. -
ROTATION: a Review of Useful Theorems Involving Proper Orthogonal Matrices Referenced to Three- Dimensional Physical Space
Unlimited Release Printed May 9, 2002 ROTATION: A review of useful theorems involving proper orthogonal matrices referenced to three- dimensional physical space. Rebecca M. Brannon† and coauthors to be determined †Computational Physics and Mechanics T Sandia National Laboratories Albuquerque, NM 87185-0820 Abstract Useful and/or little-known theorems involving33× proper orthogonal matrices are reviewed. Orthogonal matrices appear in the transformation of tensor compo- nents from one orthogonal basis to another. The distinction between an orthogonal direction cosine matrix and a rotation operation is discussed. Among the theorems and techniques presented are (1) various ways to characterize a rotation including proper orthogonal tensors, dyadics, Euler angles, axis/angle representations, series expansions, and quaternions; (2) the Euler-Rodrigues formula for converting axis and angle to a rotation tensor; (3) the distinction between rotations and reflections, along with implications for “handedness” of coordinate systems; (4) non-commu- tivity of sequential rotations, (5) eigenvalues and eigenvectors of a rotation; (6) the polar decomposition theorem for expressing a general deformation as a se- quence of shape and volume changes in combination with pure rotations; (7) mix- ing rotations in Eulerian hydrocodes or interpolating rotations in discrete field approximations; (8) Rates of rotation and the difference between spin and vortici- ty, (9) Random rotations for simulating crystal distributions; (10) The principle of material frame indifference (PMFI); and (11) a tensor-analysis presentation of classical rigid body mechanics, including direct notation expressions for momen- tum and energy and the extremely compact direct notation formulation of Euler’s equations (i.e., Newton’s law for rigid bodies). -
Spin in Relativistic Quantum Theory∗
Spin in relativistic quantum theory∗ W. N. Polyzou, Department of Physics and Astronomy, The University of Iowa, Iowa City, IA 52242 W. Gl¨ockle, Institut f¨urtheoretische Physik II, Ruhr-Universit¨at Bochum, D-44780 Bochum, Germany H. Wita la M. Smoluchowski Institute of Physics, Jagiellonian University, PL-30059 Krak´ow,Poland today Abstract We discuss the role of spin in Poincar´einvariant formulations of quan- tum mechanics. 1 Introduction In this paper we discuss the role of spin in relativistic few-body models. The new feature with spin in relativistic quantum mechanics is that sequences of rotationless Lorentz transformations that map rest frames to rest frames can generate rotations. To get a well-defined spin observable one needs to define it in one preferred frame and then use specific Lorentz transformations to relate the spin in the preferred frame to any other frame. Different choices of the preferred frame and the specific Lorentz transformations lead to an infinite number of possible observables that have all of the properties of a spin. This paper provides a general discussion of the relation between the spin of a system and the spin of its elementary constituents in relativistic few-body systems. In section 2 we discuss the Poincar´egroup, which is the group relating inertial frames in special relativity. Unitary representations of the Poincar´e group preserve quantum probabilities in all inertial frames, and define the rel- ativistic dynamics. In section 3 we construct a large set of abstract operators out of the Poincar´egenerators, and determine their commutation relations and ∗During the preparation of this paper Walter Gl¨ockle passed away. -
Weyl's Spin Connection
THE SPIN CONNECTION IN WEYL SPACE c William O. Straub, PhD Pasadena, California “The use of general connections means asking for trouble.” —Abraham Pais In addition to his seminal 1929 exposition on quantum mechanical gauge invariance1, Hermann Weyl demonstrated how the concept of a spinor (essentially a flat-space two-component quantity with non-tensor- like transformation properties) could be carried over to the curved space of general relativity. Prior to Weyl’s paper, spinors were recognized primarily as mathematical objects that transformed in the space of SU (2), but in 1928 Dirac showed that spinors were fundamental to the quantum mechanical description of spin—1/2 particles (electrons). However, the spacetime stage that Dirac’s spinors operated in was still Lorentzian. Because spinors are neither scalars nor vectors, at that time it was unclear how spinors behaved in curved spaces. Weyl’s paper provided a means for this description using tetrads (vierbeins) as the necessary link between Lorentzian space and curved Riemannian space. Weyl’selucidation of spinor behavior in curved space and his development of the so-called spin connection a ab ! band the associated spin vector ! = !ab was noteworthy, but his primary purpose was to demonstrate the profound connection between quantum mechanical gauge invariance and the electromagnetic field. Weyl’s 1929 paper served to complete his earlier (1918) theory2 in which Weyl attempted to derive electrodynamics from the geometrical structure of a generalized Riemannian manifold via a scale-invariant transformation of the metric tensor. This attempt failed, but the manifold he discovered (known as Weyl space), is still a subject of interest in theoretical physics. -
Spin Connection Resonance in Gravitational General Relativity∗
Vol. 38 (2007) ACTA PHYSICA POLONICA B No 6 SPIN CONNECTION RESONANCE IN GRAVITATIONAL GENERAL RELATIVITY∗ Myron W. Evans Alpha Institute for Advanced Study (AIAS) (Received August 16, 2006) The equations of gravitational general relativity are developed with Cartan geometry using the second Cartan structure equation and the sec- ond Bianchi identity. These two equations combined result in a second order differential equation with resonant solutions. At resonance the force due to gravity is greatly amplified. When expressed in vector notation, one of the equations obtained from the Cartan geometry reduces to the Newton inverse square law. It is shown that the latter is always valid in the off resonance condition, but at resonance, the force due to gravity is greatly amplified even in the Newtonian limit. This is a direct consequence of Cartan geometry. The latter reduces to Riemann geometry when the Cartan torsion vanishes and when the spin connection becomes equivalent to the Christoffel connection. PACS numbers: 95.30.Sf, 03.50.–z, 04.50.+h 1. Introduction It is well known that the gravitational general relativity is based on Rie- mann geometry with a Christoffel connection. This type of geometry is a special case of Cartan geometry [1] when the torsion form is zero. There- fore gravitation general relativity can be expressed in terms of this limit of Cartan geometry. In this paper this procedure is shown to produce a sec- ond order differential equation with resonant solutions [2–20]. Off resonance the mathematical form of the Newton inverse square law is obtained from a well defined approximation to the complete theory, but the relation between the gravitational potential field and the gravitational force field is shown to contain the spin connection in general. -
Entanglement on Spin Networks Loop Quantum
ENTANGLEMENT ON SPIN NETWORKS IN LOOP QUANTUM GRAVITY Clement Delcamp London - September 2014 Imperial College London Blackett Laboratory Department of Theoretical Physics Submitted in partial fulfillment of the requirements for the degree of Master of Science of Imperial College London I would like to thank Pr. Joao Magueijo for his supervision and advice throughout the writ- ing of this dissertation. Besides, I am grateful to him for allowing me to choose the subject I was interested in. My thanks also go to Etera Livine for the initial idea and for introducing me with Loop Quantum Gravity. I am also thankful to William Donnelly for answering the questions I had about his article on the entanglement entropy on spin networks. Contents Introduction 7 1 Review of Loop Quantum Gravity 11 1.1 Elements of general relativity . 12 1.1.1 Hamiltonian formalism . 12 1.1.2 3+1 decomposition . 12 1.1.3 ADM variables . 13 1.1.4 Connection formalism . 14 1.2 Quantization of the theory . 17 1.2.1 Outlook of the construction of the Hilbert space . 17 1.2.2 Holonomies . 17 1.2.3 Structure of the kinematical Hilbert space . 19 1.2.4 Inner product . 20 1.2.5 Construction of the basis . 21 1.2.6 Aside on the meaning of diffeomorphism invariance . 25 1.2.7 Operators on spin networks . 25 1.2.8 Area operator . 27 1.2.9 Physical interpretation of spin networks . 28 1.2.10 Chunks of space as polyhedra . 30 1.3 Explicit calculations on spin networks . 32 2 Entanglement on spin networks 37 2.1 Outlook . -
Infeld–Van Der Waerden Wave Functions for Gravitons and Photons
Vol. 38 (2007) ACTA PHYSICA POLONICA B No 8 INFELD–VAN DER WAERDEN WAVE FUNCTIONS FOR GRAVITONS AND PHOTONS J.G. Cardoso Department of Mathematics, Centre for Technological Sciences-UDESC Joinville 89223-100, Santa Catarina, Brazil [email protected] (Received March 20, 2007) A concise description of the curvature structures borne by the Infeld- van der Waerden γε-formalisms is provided. The derivation of the wave equations that control the propagation of gravitons and geometric photons in generally relativistic space-times is then carried out explicitly. PACS numbers: 04.20.Gr 1. Introduction The most striking physical feature of the Infeld-van der Waerden γε-formalisms [1] is related to the possible occurrence of geometric wave functions for photons in the curvature structures of generally relativistic space-times [2]. It appears that the presence of intrinsically geometric elec- tromagnetic fields is ultimately bound up with the imposition of a single condition upon the metric spinors for the γ-formalism, which bears invari- ance under the action of the generalized Weyl gauge group [1–5]. In the case of a spacetime which admits nowhere-vanishing Weyl spinor fields, back- ground photons eventually interact with underlying gravitons. Nevertheless, the corresponding coupling configurations turn out to be in both formalisms exclusively borne by the wave equations that control the electromagnetic propagation. Indeed, the same graviton-photon interaction prescriptions had been obtained before in connection with a presentation of the wave equations for the ε-formalism [6, 7]. As regards such earlier works, the main procedure seems to have been based upon the implementation of a set of differential operators whose definitions take up suitably contracted two- spinor covariant commutators.