- •Preface
- •Acknowledgements
- •Contents
- •1.1 Introduction
- •1.2 Classical Physics Between the End of the XIX and the Dawn of the XX Century
- •1.2.1 Maxwell Equations
- •1.2.2 Luminiferous Aether and the Michelson Morley Experiment
- •1.2.3 Maxwell Equations and Lorentz Transformations
- •1.3 The Principle of Special Relativity
- •1.3.1 Minkowski Space
- •1.4 Mathematical Definition of the Lorentz Group
- •1.4.1 The Lorentz Lie Algebra and Its Generators
- •1.4.2 Retrieving Special Lorentz Transformations
- •1.5 Representations of the Lorentz Group
- •1.5.1 The Fundamental Spinor Representation
- •1.6 Lorentz Covariant Field Theories and the Little Group
- •1.8 Criticism of Special Relativity: Opening the Road to General Relativity
- •References
- •2.1 Introduction
- •2.2 Differentiable Manifolds
- •2.2.1 Homeomorphisms and the Definition of Manifolds
- •2.2.2 Functions on Manifolds
- •2.2.3 Germs of Smooth Functions
- •2.3 Tangent and Cotangent Spaces
- •2.4 Fibre Bundles
- •2.5 Tangent and Cotangent Bundles
- •2.5.1 Sections of a Bundle
- •2.5.2 The Lie Algebra of Vector Fields
- •2.5.3 The Cotangent Bundle and Differential Forms
- •2.5.4 Differential k-Forms
- •2.5.4.1 Exterior Forms
- •2.5.4.2 Exterior Differential Forms
- •2.6 Homotopy, Homology and Cohomology
- •2.6.1 Homotopy
- •2.6.2 Homology
- •2.6.3 Homology and Cohomology Groups: General Construction
- •2.6.4 Relation Between Homotopy and Homology
- •References
- •3.1 Introduction
- •3.2 A Historical Outline
- •3.2.1 Gauss Introduces Intrinsic Geometry and Curvilinear Coordinates
- •3.2.3 Parallel Transport and Connections
- •3.2.4 The Metric Connection and Tensor Calculus from Christoffel to Einstein, via Ricci and Levi Civita
- •3.2.5 Mobiles Frames from Frenet and Serret to Cartan
- •3.3 Connections on Principal Bundles: The Mathematical Definition
- •3.3.1 Mathematical Preliminaries on Lie Groups
- •3.3.1.1 Left-/Right-Invariant Vector Fields
- •3.3.1.2 Maurer-Cartan Forms on Lie Group Manifolds
- •3.3.1.3 Maurer Cartan Equations
- •3.3.2 Ehresmann Connections on a Principle Fibre Bundle
- •3.3.2.1 The Connection One-Form
- •Gauge Transformations
- •Horizontal Vector Fields and Covariant Derivatives
- •3.4 Connections on a Vector Bundle
- •3.5 An Illustrative Example of Fibre-Bundle and Connection
- •3.5.1 The Magnetic Monopole and the Hopf Fibration of S3
- •The U(1)-Connection of the Dirac Magnetic Monopole
- •3.6.1 Signatures
- •3.7 The Levi Civita Connection
- •3.7.1 Affine Connections
- •3.7.2 Curvature and Torsion of an Affine Connection
- •Torsion and Torsionless Connections
- •The Levi Civita Metric Connection
- •3.8 Geodesics
- •3.9 Geodesics in Lorentzian and Riemannian Manifolds: Two Simple Examples
- •3.9.1 The Lorentzian Example of dS2
- •3.9.1.1 Null Geodesics
- •3.9.1.2 Time-Like Geodesics
- •3.9.1.3 Space-Like Geodesics
- •References
- •4.1 Introduction
- •4.2 Keplerian Motions in Newtonian Mechanics
- •4.3 The Orbit Equations of a Massive Particle in Schwarzschild Geometry
- •4.3.1 Extrema of the Effective Potential and Circular Orbits
- •Minimum and Maximum
- •Energy of a Particle in a Circular Orbit
- •4.4 The Periastron Advance of Planets or Stars
- •4.4.1 Perturbative Treatment of the Periastron Advance
- •References
- •5.1 Introduction
- •5.2 Locally Inertial Frames and the Vielbein Formalism
- •5.2.1 The Vielbein
- •5.2.2 The Spin-Connection
- •5.2.3 The Poincaré Bundle
- •5.3 The Structure of Classical Electrodynamics and Yang-Mills Theories
- •5.3.1 Hodge Duality
- •5.3.2 Geometrical Rewriting of the Gauge Action
- •5.3.3 Yang-Mills Theory in Vielbein Formalism
- •5.4 Soldering of the Lorentz Bundle to the Tangent Bundle
- •5.4.1 Gravitational Coupling of Spinorial Fields
- •5.5 Einstein Field Equations
- •5.6 The Action of Gravity
- •5.6.1 Torsion Equation
- •5.6.1.1 Torsionful Connections
- •The Torsion of Dirac Fields
- •Dilaton Torsion
- •5.6.2 The Einstein Equation
- •5.6.4 Examples of Stress-Energy-Tensors
- •The Stress-Energy Tensor of the Yang-Mills Field
- •The Stress-Energy Tensor of a Scalar Field
- •5.7 Weak Field Limit of Einstein Equations
- •5.7.1 Gauge Fixing
- •5.7.2 The Spin of the Graviton
- •5.8 The Bottom-Up Approach, or Gravity à la Feynmann
- •5.9 Retrieving the Schwarzschild Metric from Einstein Equations
- •References
- •6.1 Introduction and Historical Outline
- •6.2 The Stress Energy Tensor of a Perfect Fluid
- •6.3 Interior Solutions and the Stellar Equilibrium Equation
- •6.3.1 Integration of the Pressure Equation in the Case of Uniform Density
- •6.3.1.1 Solution in the Newtonian Case
- •6.3.1.2 Integration of the Relativistic Pressure Equation
- •6.3.2 The Central Pressure of a Relativistic Star
- •6.4 The Chandrasekhar Mass-Limit
- •6.4.1.1 Idealized Models of White Dwarfs and Neutron Stars
- •White Dwarfs
- •Neutron Stars
- •6.4.2 The Equilibrium Equation
- •6.4.3 Polytropes and the Chandrasekhar Mass
- •6.5 Conclusive Remarks on Stellar Equilibrium
- •References
- •7.1 Introduction
- •7.1.1 The Idea of GW Detectors
- •7.1.2 The Arecibo Radio Telescope
- •7.1.2.1 Discovery of the Crab Pulsar
- •7.1.2.2 The 1974 Discovery of the Binary System PSR1913+16
- •7.1.3 The Coalescence of Binaries and the Interferometer Detectors
- •7.2 Green Functions
- •7.2.1 The Laplace Operator and Potential Theory
- •7.2.2 The Relativistic Propagators
- •7.2.2.1 The Retarded Potential
- •7.3 Emission of Gravitational Waves
- •7.3.1 The Stress Energy 3-Form of the Gravitational Field
- •7.3.2 Energy and Momentum of a Plane Gravitational Wave
- •7.3.2.1 Calculation of the Spin Connection
- •7.3.3 Multipolar Expansion of the Perturbation
- •7.3.3.1 Multipolar Expansion
- •7.3.4 Energy Loss by Quadrupole Radiation
- •7.3.4.1 Integration on Solid Angles
- •7.4 Quadruple Radiation from the Binary Pulsar System
- •7.4.1 Keplerian Parameters of a Binary Star System
- •7.4.2 Shrinking of the Orbit and Gravitational Waves
- •7.4.2.1 Calculation of the Moment of Inertia Tensor
- •7.4.3 The Fate of the Binary System
- •7.4.4 The Double Pulsar
- •7.5 Conclusive Remarks on Gravitational Waves
- •References
- •Appendix A: Spinors and Gamma Matrix Algebra
- •A.2 The Clifford Algebra
- •A.2.1 Even Dimensions
- •A.2.2 Odd Dimensions
- •A.3 The Charge Conjugation Matrix
- •A.4 Majorana, Weyl and Majorana-Weyl Spinors
- •Appendix B: Mathematica Packages
- •B.1 Periastropack
- •Programme
- •Main Programme Periastro
- •Subroutine Perihelkep
- •Subroutine Perihelgr
- •Examples
- •B.2 Metrigravpack
- •Metric Gravity
- •Routines: Metrigrav
- •Mainmetric
- •Metricresume
- •Routine Metrigrav
- •Calculation of the Ricci Tensor of the Reissner Nordstrom Metric Using Metrigrav
- •Index
5.7 Weak Field Limit of Einstein Equations |
225 |
|
0 0 |
0 |
· · · |
· · · |
|
· · · |
|
|
|
0 |
|
|
|
|
|||||
|
0 0 |
0 |
· · · |
· · · |
|
· · · |
|
|
|
0 |
|
|
|
|
|
||||
|
|
0 0 |
γ |
33 |
γ |
34 |
|
|
γ |
3,m |
1 |
|
γ |
3,m |
|
|
|
||
|
|
|
|
· · · |
|
|
|
|
|
|
|||||||||
|
|
|
|
|
|
|
− |
|
|
|
|
|
|
|
|
||||
μν |
. . |
. |
|
. |
· . |
|
|
. − |
|
|
|
. |
|
|
|
|
|||
γ phys |
0 0 |
γ43 |
γ44 |
· · |
γ4,m |
1 |
|
γ4,m |
|
|
(5.7.25) |
||||||||
|
= . . |
. . . |
|
|
. |
|
|
|
. |
|
|
|
|
||||||
|
. . |
. . . |
|
|
. |
|
|
|
. |
|
|
|
|
||||||
|
. . |
. . . |
|
|
. |
|
|
|
. |
|
|
|
|
||||||
|
. . |
. . . |
|
|
. |
|
|
|
. |
|
|
|
|
||||||
|
. . |
. . . |
|
|
. |
|
|
|
. |
|
|
|
|
||||||
|
|
γ |
|
γ |
|
|
|
γ |
|
|
|
m |
1 |
γ |
|
|
|||
|
0 0 |
· · · |
|
|
|
− |
|
|
|
||||||||||
|
|
|
m3 |
m4 |
m,m−1 |
− i=3 |
|
ii |
|
||||||||||
The number of these degrees of freedom is easily calculated it is: |
|
||||||||||||||||||
|
|
|
|
|
|
|
= |
|
2 |
|
|
|
|
|
|
|
|
|
|
|
|
|
|
|
#d.o.f |
|
m(m − 3) |
|
|
|
|
|
|
|
(5.7.26) |
||||
|
|
|
|
|
|
|
|
|
|
|
|
|
In D = 4 space-time dimensions the degrees of freedom are 2 and the corresponding gauge fixed form of the γμν tensor is the following one:
|
|
|
|
0 |
0 |
0 |
|
0 |
|
|
γμνphys |
= |
(u) |
|
0 |
0 |
0 |
|
0 |
|
(5.7.27) |
0 |
0 |
a(u) |
b(u) |
|||||||
|
|
= |
|
|
|
|
|
|
|
|
|
|
|
|
0 |
0 |
b(u) |
− |
a(u) |
|
|
|
|
|
|
|
|
|
|
|
|
where the two functions a(u) and b(u) are arbitrary. We shall use this gauge-fixed form of the metric perturbation while studying the emission and propagation of gravitational waves (see Chap. 7 of this volume).
5.7.2 The Spin of the Graviton
Hence the gravitational waves, namely the small deformations of the Minkowski metric, propagate in Minkowski space-time and propagate at the speed of light since they obey the d’Alembertian equation. Moreover they are transverse waves since what varies in time along the line of flight is not the amplitude of the metric coefficient in that direction, rather all the metric coefficients in the space orthogonal to the line.
From the mathematical point of view the right way to approach this issue is from the point of view of the little group of invariance of the momentum vector. A planewave gravitational disturbance, like an electromagnetic one of the same type, is an object carrying momentum and this momentum is a light-like vector:
p(μwave) = :1, −1, 0, 0, · · · , 0; |
(5.7.28) |
m−2
The little group of invariance of any element v D belonging to the carrier vector space of a linear representation of some Lie group G is that subgroup G (v) G which leaves the vector v invariant:
226
Table 5.1 Degrees of freedom of the graviton in diverse dimensions
|
5 Einstein Versus Yang-Mills Field Equations |
|
D |
Little group |
# of d.o.f. |
11 |
SO(9) |
44 |
10 |
SO(8) |
35 |
9 |
SO(7) |
27 |
8 |
SO(6) |
20 |
7 |
SO(5) |
14 |
6 |
SO(4) |
9 |
5 |
SO(3) |
5 |
4 |
SO(2) |
2 |
3 |
— |
0 |
g G (v) : g · v = v |
(5.7.29) |
Typically the carrier space D is organized in orbits, under the action of G, whose little groups are different non-isomorphic subgroups of the G. In the case of the Lorentz group SO(1, m − 1) and its fundamental m-dimensional representation the relevant orbits are three corresponding to the time-like, space-like and null-like vectors. The corresponding little groups are Gtime = SO(m), Gspace = SO(1, m − 1) and Gnull = SO(m − 2). Therefore the degrees of freedom of the graviton correspond to the following irreducible representation of the little group SO(m − 2):
graviton ≡ |
|
|
|
(5.7.30) |
|
|
where the hat denotes the traceless nature of the symmetric tensor. The number of
independent components of such an irreducible representation is the number m(m−3)
2
quoted above. Given its relevance in modern multi-dimensional gravity theories and specifically in supergravities that are the low energy limits of superstring models, in Table 5.1 we list the number of graviton degrees of freedom for all space-time dimensions between D = 11 and D = 3.
In D = 3 the graviton disappears. There is no room for its propagation since there is no residual transverse group. Gravity in three space-time dimension allows only for the Newtonian potential and there are no local propagating degrees of freedom. In D = 4 the transverse group is SO(2), whose unitary irreducible representations are all two-dimensional, as we explained in Sect. 1.6.1. For this reason the graviton has the same number of degrees of freedom as the photon or a Yang-Mills gauge boson, namely 2. Yet although all two-dimensional, the irreducible representations of SO(2) are not all equivalent. According to the discussion of Sect. 1.6.1 they are characterized by an half integer number s that we name the spin of the corresponding particle. In the case of the graviton, just as for the photon, s is integer, but it is s = 2 rather than s = 1. Physically this means that we have two states, one of helicity s = 2 and one of helicity s = −2. The two states are pictorially described in Fig. 5.5.