- •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
7.3 Emission of Gravitational Waves |
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where: |
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7.3.3 Multipolar Expansion of the Perturbation
The next step in our elaboration of the general solution (7.3.3) for the metric perturbation consists of its systematic multipolar expansion. This will enable us to single out the contributions to the wave from the various angular momentum components of the source deformation. Since these contributions have a faster and faster distance decay at increasing angular momentum , it follows that for weak fields only the first non-vanishing multipole needs to be considered. Due to the spin of the graviton which is s = 2 the first contributing multipole turns out to be the quadrupole as opposed to the case of electromagnetic radiation where the spin s = 1 of the photon selects the dipole as first non-vanishing and dominant contribution.
To implement the above outlined programme we begin by performing a partial Fourier (see Fig. 7.9) transform of the metric perturbation with respect to the time coordinate:
γμν (ω, x) = √1 2π
Inserting this in (7.3.3) we get:
γμν (ω, x) = −4G
The Hilbert gauge condition implies:
+∞ dt eiωt γμν (t, x) |
(7.3.40) |
−∞ |
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d3r eiω|r−r | Tμν (ω, r ) |
(7.3.41) |
|r − r | |
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∂0γ0ν = iωγ0ν = ∂i γiν |
(7.3.42) |
and since γμν is symmetric we can conclude:
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Hence it suffices to determine the spatial components γij . The others are easily retrieved from these.
7.3.3.1 Multipolar Expansion
Let us consider the spatial part of the Green function, which apart from a factor 4π is just the Green function of the Laplace operator discussed in Sect. 7.2.1:
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7 Gravitational Waves and the Binary Pulsars |
Fig. 7.9 Jean Baptiste Joseph Fourier (March 21, 1768–May 16, 1830) is one among the incredibly large number of scientific geniuses giving fundamental contributions to the development of Modern Physics, Mathematics and Chemistry contributed by the Revolutionary and Napoleonic France. Other members of that group are Laplace, Lagrange, Monge, Carnot (father and son), to mention some. Born at Auxerre, Fourier was educated in a monastery and studied mathematics. He took prominent part in the Revolution and was appointed professor first at the Ecole Normale Superieure, then at the Ecole Polytechnique where he inherited the chair of Laplace. He served as officer in the Napoleonic Army and was even appointed governor of Egypt. Fourier was elected member of the French Academy of Sciences in 1817. Besides the introduction of the Fourier series and of the Fourier transform, Fourier discovered the equation of heat propagation and was the first to point out the green-house effect of the atmosphere. He died in Paris at the age of sixty-two
G x − x ≡ |
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by means of a trivial manipulation we can rewrite it as follows:
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Defining: |
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that we can develop into power series of 1/R:
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(7.3.45)
(7.3.46)
(7.3.47)
(7.3.48)
(7.3.49)
(7.3.50)
7.3 Emission of Gravitational Waves |
293 |
The next step is to reorganize the terms of order R−3 and of order R−5. In this way we obtain:
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(7.3.57) |
The first three lines in the above equation respectively define:
(a)the monopole moment,
(b)the dipole moment,
(c)the quadrupole moment.
To see this let us reconsider the general solution of the potential problem in Newtonian theory provided by (7.2.15) and let us insert into it the development (7.3.54) of the kernel. We obtain:
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294 |
7 Gravitational Waves and the Binary Pulsars |
Fig. 7.10 The radiation region
Equipped with this lore let us return to the case of our relativistic wave. We expand the phase factor according to:
exp iω x |
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exp iωR |
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iω x · x |
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Next we define the radiation zone by means of the following two inequalities:
ωR - 1; ω|x | 1 |
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namely the distance is very large compared to the wave-length and the extension of the source is small compared to the wave-length (see Fig. 7.10).
In the radiation region, which is the region far a way from the source, the phase factor can be well approximated by exp[iωR] and put out of the integral. Correspondingly we get:
γij (ω, x) |
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4G |
exp[iωR] |
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ω, x |
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