Structure, Properties and Implications of Complex Minkowski Spaces
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Line Element in Noncommutative Geometry
Line element in noncommutative geometry P. Martinetti G¨ottingenUniversit¨at Wroclaw, July 2009 . ? ? - & ? !? The line element p µ ν ds = gµν dx dx is mainly useful to measure distance Z y d(x; y) = inf ds: x If, for some quantum gravity reasons, [x µ; x ν ] 6= 0 is one losing the notion of distance ? (annoying then to speak of noncommutative geo-metry). ? - . ? !? The line element p µ ν ds = gµν dx dx & ? is mainly useful to measure distance Z y d(x; y) = inf ds: x If, for some quantum gravity reasons, [x µ; x ν ] 6= 0 is one losing the notion of distance ? (annoying then to speak of noncommutative geo-metry). ? - !? The line element p µ ν ds = gµν dx dx . & ? ? is mainly useful to measure distance Z y d(x; y) = inf ds: x If, for some quantum gravity reasons, [x µ; x ν ] 6= 0 is one losing the notion of distance ? (annoying then to speak of noncommutative geo-metry). ? - The line element p µ ν ds = gµν dx dx . & ? ? is mainly useful to measure distance Z y !? d(x; y) = inf ds: x If, for some quantum gravity reasons, [x µ; x ν ] 6= 0 is one losing the notion of distance ? (annoying then to speak of noncommutative geo-metry). The line element p µ ν ds = gµν dx dx . & ? ? is mainly useful to measure distance ? -Z y !? d(x; y) = inf ds: x If, for some quantum gravity reasons, [x µ; x ν ] 6= 0 is one losing the notion of distance ? (annoying then to speak of noncommutative geo-metry). -
1 Electromagnetic Fields and Charges In
Electromagnetic fields and charges in ‘3+1’ spacetime derived from symmetry in ‘3+3’ spacetime J.E.Carroll Dept. of Engineering, University of Cambridge, CB2 1PZ E-mail: [email protected] PACS 11.10.Kk Field theories in dimensions other than 4 03.50.De Classical electromagnetism, Maxwell equations 41.20Jb Electromagnetic wave propagation 14.80.Hv Magnetic monopoles 14.70.Bh Photons 11.30.Rd Chiral Symmetries Abstract: Maxwell’s classic equations with fields, potentials, positive and negative charges in ‘3+1’ spacetime are derived solely from the symmetry that is required by the Geometric Algebra of a ‘3+3’ spacetime. The observed direction of time is augmented by two additional orthogonal temporal dimensions forming a complex plane where i is the bi-vector determining this plane. Variations in the ‘transverse’ time determine a zero rest mass. Real fields and sources arise from averaging over a contour in transverse time. Positive and negative charges are linked with poles and zeros generating traditional plane waves with ‘right-handed’ E, B, with a direction of propagation k. Conjugation and space-reversal give ‘left-handed’ plane waves without any net change in the chirality of ‘3+3’ spacetime. Resonant wave-packets of left- and right- handed waves can be formed with eigen frequencies equal to the characteristic frequencies (N+½)fO that are observed for photons. 1 1. Introduction There are many and varied starting points for derivations of Maxwell’s equations. For example Kobe uses the gauge invariance of the Schrödinger equation [1] while Feynman, as reported by Dyson, starts with Newton’s classical laws along with quantum non- commutation rules of position and momentum [2]. -
ASSIGNMENTS Week 4 (F. Saueressig) Cosmology 13/14 (NWI-NM026C) Prof
ASSIGNMENTS Week 4 (F. Saueressig) Cosmology 13/14 (NWI-NM026C) Prof. A. Achterberg, Dr. S. Larsen and Dr. F. Saueressig Exercise 1: Flat space in spherical coordinates For constant time t the line element of special relativity reduces to the flat three-dimensional Euclidean metric Euclidean 2 SR 2 2 2 2 (ds ) = (ds ) =const = dx + dy + dz . (1) − |t Use the coordinate transformation x = r sin θ cos φ, y = r sin θ sin φ , z = r cos θ , (2) with θ [0,π] and φ [0, √2 π[ to express the line element in spherical coordinates. ∈ ∈ Exercise 2: Distances, areas and volumes For constant time the metric describing the spatial part of a homogeneous closed Friedmann- Robertson Walker (FRW) universe is given by 2 2 dr 2 2 2 2 ds = + r dθ + sin θ dφ , r [ 0 , a ] . (3) 1 (r/a)2 ∈ − The scale factor a(t) depends on time only so that, for t = const, it can be considered as a fixed number. Compute from this line element a) The proper circumference of the sphere around the equator. b) The proper distance from the center of the sphere up to the coordinate radius a. c) The proper area of the two-surface at r = a. d) The proper volume inside r = a. Compare your results to the ones expected from flat Euclidean space. Which of the quantities are modified by the property that the line element (3) is curved? Exercise 3: The metric is covariantly constant In the lecture we derived a formula for the Christoffel symbol Γα 1 gαβ g + g g . -
Spacetime Structuralism
Philosophy and Foundations of Physics 37 The Ontology of Spacetime D. Dieks (Editor) r 2006 Elsevier B.V. All rights reserved DOI 10.1016/S1871-1774(06)01003-5 Chapter 3 Spacetime Structuralism Jonathan Bain Humanities and Social Sciences, Polytechnic University, Brooklyn, NY 11201, USA Abstract In this essay, I consider the ontological status of spacetime from the points of view of the standard tensor formalism and three alternatives: twistor theory, Einstein algebras, and geometric algebra. I briefly review how classical field theories can be formulated in each of these formalisms, and indicate how this suggests a structural realist interpre- tation of spacetime. 1. Introduction This essay is concerned with the following question: If it is possible to do classical field theory without a 4-dimensional differentiable manifold, what does this suggest about the ontological status of spacetime from the point of view of a semantic realist? In Section 2, I indicate why a semantic realist would want to do classical field theory without a manifold. In Sections 3–5, I indicate the extent to which such a feat is possible. Finally, in Section 6, I indicate the type of spacetime realism this feat suggests. 2. Manifolds and manifold substantivalism In classical field theories presented in the standard tensor formalism, spacetime is represented by a differentiable manifold M and physical fields are represented by tensor fields that quantify over the points of M. To some authors, this has 38 J. Bain suggested an ontological commitment to spacetime points (e.g., Field, 1989; Earman, 1989). This inclination might be seen as being motivated by a general semantic realist desire to take successful theories at their face value, a desire for a literal interpretation of the claims such theories make (Earman, 1993; Horwich, 1982). -
On a Complex Spacetime Frame : New Foundation for Physics and Mathematics
On a complex spacetime frame : new foundation for physics and mathematics Joseph Akeyo Omolo∗ Department of Physics and Materials Science, Maseno University P.O. Private Bag, Maseno, Kenya e-mail: [email protected] March 31, 2016 Abstract This paper provides a derivation of a unit vector specifying the tem- poral axis of four-dimensional space-time frame as an imaginary axis in the direction of light or general wave propagation. The basic elements of the resulting complex four-dimensional spacetime frame are complex four-vectors expressed in standard form as four-component quantities specified by four unit vectors, three along space axes and one along the imaginary temporal axis. Consistent mathematical operations with the complex four-vectors have been developed, which provide extensions of standard vector analysis theorems to complex four-dimensional space- time. The general orientation of the temporal unit vector relative to all the three mutually perpendicular spatial unit vectors leads to ap- propriate modifications of fundamental results describing the invariant length of the spacetime event interval, time dilation, mass increase with speed and relativistic energy conservation law. Contravariant and co- variant forms have been defined, providing appropriate definition of the invariant length of a complex four-vector and appropriate definitions of complex tensors within the complex four-dimensional spacetime frame, thus setting a new geometrical framework for physics and mathematics. 1 Introduction Four-dimensional space-time frame is the natural reference frame for de- scribing the general dynamics of physical systems. Its basic elements are ∗Regular Associate, Abdus Salam ICTP: 2001-2006 1 four-vectors, which are suitable for expressing field equations and associ- ated physical quantities in consistent forms. -
Spacetime As a Feynman Diagram: the Connection Formulation
Spacetime as a Feynman diagram: the connection formulation Michael P. Reisenberger Theoretical Physics Group, Blackett Laboratory, Imperial College, London, SW7 2BZ, UK. Center for Gravitational Physics and Geometry, The Pennsylvania State University, 104 Davey Lab, University Park, PA16802-6300, USA [email protected] Carlo Rovelli Physics Department, University of Pittsburgh, Pittsburgh, PA 15260, USA. Centre de Physique Th´eorique, CNRS Luminy, 13288 Marseille, France [email protected] March 3, 2000 Abstract Spin foam models are the path integral counterparts to loop quantized canonical theories. In the last few years several spin foam models of gravity have been proposed, most of which live on finite simplicial lattice spacetime. The lattice truncates the presumably infinite set of gravitational degrees of freedom down to a finite set. Models that can accomodate an infinite set of degrees of freedom and that are independent of any background simplicial structure, or indeed any a priori spacetime topology, can be obtained from the lattice models by summing them over all lattice spacetimes. Here we show that this sum can be realized as the sum over Feynman diagrams of a quantum 1 field theory living on a suitable group manifold, with each Feynman diagram defining a particular lattice spacetime. We give an explicit formula for the action of the field theory corresponding to any given spin foam model in a wide class which includes several gravity mod- els. Such a field theory was recently found for a particular gravity model [1]. Our work generalizes this result as well as Boulatov’s and Ooguri’s models of three and four dimensional topological field theo- ries, and ultimately the old matrix models of two dimensional systems with dynamical topology. -
Appendix a Tensor Mathematics
Appendix A Tensor Mathematics A.l Introduction In physics we are accustomed to relating quantities to other quantities by means of mathematical expressions. The quantities that represent physical properties of a point or of an infinitesimal volume in space may be of a single numerical value without direction, such as temperature, mass, speed, dist ance, specific gravity, energy, etc.; they are defined by a single magnitude and we call them scalars. Other physical quantities have direction as well and their magnitude is represented by an array of numerical values, their number corresponding to the number of dimensions of the space, three numerical values in a three-dimensional space; such quantities are called vectors, for example velocity, acceleration, force, etc., and the three numerical values are the components of the vector in the direction of the coordinates of the space. Still other physical quantities such as moment of inertia, stress, strain, permeability coefficients, electric flux, electromagnetic flux, etc., are repre sented in a three-dimensional space by nine numerical quantities, called components, and are known as tensors. We will introduce a slightly different definition. We shall call the scalars tensors of order zero, vectors - tensors of order one and tensors with nine components - tensors of order two. There are, of course, in physics and mathematics, tensors of higher order. Tensors of order three have an array of 27 components and tensors of order four have 81 components and so on. Couple stresses that arise in materials with polar forces are examples of tensors of order three, and the Riemann curvature tensor that appears in geodesics is an example of a tensor of order four. -
Noncommutative Quantum Gravity
Noncommutative Quantum Gravity J. W. Moffat Department of Physics, University of Toronto, Toronto, Ontario M5S 1A7, Canada Abstract The possible role of gravity in a noncommutative geometry is investi- gated. Due to the Moyal *-product of fields in noncommutative geometry, it is necessary to complexify the metric tensor of gravity. We first consider the possibility of a complex Hermitian, nonsymmetric gµν and discuss the problems associated with such a theory. We then introduce a complex symmetric (non-Hermitian) metric, with the associated complex connec- tion and curvature, as the basis of a noncommutative spacetime geometry. The spacetime coordinates are in general complex and the group of local gauge transformations is associated with the complex group of Lorentz transformations CSO(3, 1). A real action is chosen to obtain a consistent set of field equations. A Weyl quantization of the metric associated with the algebra of noncommuting coordinates is employed. 1 Introduction The concept of a quantized spacetime was proposed by Snyder [1], and has received much attention over the past few years [2-6]. There has been renewed interest recently in noncommutative field theory, since it makes its appearance in string theory, e.g. noncommutative gauge theories describe the low energy excitations of open strings on D-branes in a background two-form B field [5,7-12]. Noncommutative Minkowski space is defined in terms of spacetime coordinates xµ, µ =0, ...3, which satisfy the following commutation relations [xµ, xν ]= iθµν , (1) arXiv:hep-th/0007181v2 25 Sep 2000 where θµν is an antisymmetric tensor. In what follows, we can generally extend the results to higher dimensions µ =0, ...d. -
1 Special Relativity
1 Special relativity 1.1 Minkowski space Inertial frames and the principle of relativity Newton’s Lex Prima (or the Galilean law of inertia) states: Each force-less mass point stays at rest or moves on a straight line at constant speed. In a Cartesian inertial coordinate system, Newton’s lex prima becomes d2x d2y d2z = = = 0 . (1.1) dt2 dt2 dt2 Most often, we call such a coordinate system just an inertial frame. Newton’s first law is not just a trivial consequence of its second one, but may be seen as practical definition of those reference frames for which his following laws are valid. Since the symmetries of Euclidean space, translations a and rotations R, leave Eq. (1.1) invariant, all frames connected by x′ = Rx + a to an inertial frame are inertial frames too. Additionally, proper Galilean transformations x′ = x + vt connect inertial frames moving with relative speed v. The principle of relativity states that the physics in all inertial frames is the same. If we consider two frames with relative velocity along the x direction, then the most general linear transformation between the two frames is t′ At + Bx At + Bx ′ x Dt + Ex A(x vt) ′ = = − . (1.2) y y y ′ z z z Newtonian physics assumes the existence of an absolute time, t = t′, and thus A = 1 and B = 0. This leads to the “common sense” addition law of velocities. Time differences ∆t and space differences 2 2 2 2 ∆x12 = (x1 x2) + (y1 y2) + (z1 z2) (1.3) − − − are separately invariant. Lorentz transformations In special relativity, we replace the Galilean transformations as symmetry group of space and time by Lorentz transformations Λ. -
Metric Tensor & Chriostofell Symbols
MATHEMATICAL PHYSICS UNIT – 8 Metric Tensor & Chriostofell Symbols PRESENTED BY: DR. RAJESH MATHPAL ACADEMIC CONSULTANT SCHOOL OF SCIENCES U.O.U. TEENPANI, HALDWANI UTTRAKHAND MOB:9758417736,7983713112 STRUCTURE OF UNIT 8.1. INTRODUCTION 8.2. RIEMANNIAN SPACE: METRIC TENSOR jk 풋 8.3. FUNDAMENTAL TENSORS gjk, g AND 휹풌 8.4. CHRISTOFELL’S 3-INDEX SYMBOLS 8.5. GEODESICS 8.1. INTRODUCTION In the mathematical field of differential geometry, one definition of a metric tensor is a type of function which takes as input a pair of tangent vectors v and w at a point of a surface (or higher dimensional differentiable manifold) and produces a real number scalar g(v, w) in a way that generalizes many of the familiar properties of the dot product of vectors in Euclidean space. In the same way as a dot product, metric tensors are used to define the length of and angle between tangent vectors. Through integration, the metric tensor allows one to define and compute the length of curves on the manifold. A metric tensor is called positive-definite if it assigns a positive value g(v, v) > 0 to every nonzero vector v. A manifold equipped with a positive-definite metric tensor is known as a Riemannian manifold. On a Riemannian manifold, the curve connecting two points that (locally) has the smallest length is called a geodesic, and its length is the distance that a passenger in the manifold needs to traverse to go from one point to the other. Equipped with this notion of length, a Riemannian manifold is a metric space, meaning that it has a distance function d(p, q) whose value at a pair of points p and q is the distance from p to q. -
PHY103A: Lecture # 3 (Text Book: Intro to Electrodynamics by Griffiths, 3Rd Ed.)
Semester II, 2017-18 Department of Physics, IIT Kanpur PHY103A: Lecture # 3 (Text Book: Intro to Electrodynamics by Griffiths, 3rd Ed.) Anand Kumar Jha 08-Jan-2018 Notes • The first tutorial is tomorrow (Tuesday). • Updated lecture notes will be uploaded right after the class. • Office Hour – Friday 2:30-3:30 pm • Phone: 7014(Off); 962-142-3993(Mobile) [email protected]; [email protected] • Tutorial Sections have been finalized and put up on the webpage. • Course Webpage: http://home.iitk.ac.in/~akjha/PHY103.htm 2 3 Summary of Lecture # 2: 2 Gradient of a scalar 1 0 1 + + 2 ≡ � � � 3 3 2 1 0 1 2 3 Divergence of a vector 2 1 ⋅ = + + 0 ⋅ 1 Curl of a vector × 2 2 2 1 0 1 2 1 × = � � � 0 1 = + + 2 2 1 0 1 2 3 − � − � − � Integral Calculus: The ordinary integral that we know of is of the form: In vector calculus we encounter many other types of integrals. ∫ Line Integral: � ⋅ Vector field Infinitesimal Displacement vector Or Line element = + + If the path is a closed loop � then the� line �integral is written as • When do� we ⋅ need line integrals? Work done by a force along a given path involves line integral. 4 Example (G: Ex. 1.6) Q: = + ( + 1) ? What is the line integral from A to2 B along path (1) and (2)? � 2 � Along path (1) We have = + . (i) = ; =1; �= � = 1 (ii) = ; =2; = 4( 2 + 1) =10 � ∫ ⋅ ∫ 2 � ∫ ⋅ ∫1 Along path (2): = + ; = ; = = ( + 2 + ) =10 � � 2 2 2 ∫ ⋅ ∫1 2 =11-10=1 This means that if represented the force vector, ⋅ ∮ it would be a non-conservative force 5 Surface Integral: or � ⋅ � ⋅ Vector field Infinitesimal area vector Closed loop • For a closed surface, the area vector points outwards. -
AST1100 Lecture Notes
AST1100 Lecture Notes 9–10 The special theory of relativity: Four vectors and relativistic dynamics 1 Worldlines In the spacetime diagram in figure 1 we see the path of a particle (or any object) through spacetime. We see the different positions (x, t) in space and time that the particle has passed through. Such a path showing the points in spacetime that an object passed is called a worldline. We will now study two events A and B (on the worldline of a particle) which are separated by a small spacetime interval ∆s. These events could be the particle emitting two flashes of light or the particle passing through two specific points in space. The corresponding space and time intervals between these two events in the laboratory frame are called ∆t and ∆x. From the figure you see that ∆t > ∆x. You can see that this also holds for every small spacetime interval along the path. This has to be this way: The speed of the particle at a given instant is v = ∆x/∆t. If ∆x = ∆t then v = 1 and the particle travels at the speed of light. That ∆t > ∆x simply means that the particle travels at a speed v < c which it must. The worldline of a photon would thus be a line at 45◦ with the coordinate axes. The worldline of any material particle will therefore always make less than 45◦ with the time axis. Events which are separated by spacetime distances such that ∆t > ∆x are called timelike events. Timelike events may be causally connected since a particle with velocity v < c would have the possibility to travel from one of the events to the other event.