- •Contents
- •Preface to the second edition
- •Preface to the first edition
- •1 Special relativity
- •1.2 Definition of an inertial observer in SR
- •1.4 Spacetime diagrams
- •1.6 Invariance of the interval
- •1.8 Particularly important results
- •Time dilation
- •Lorentz contraction
- •Conventions
- •Failure of relativity?
- •1.9 The Lorentz transformation
- •1.11 Paradoxes and physical intuition
- •The problem
- •Brief solution
- •2 Vector analysis in special relativity
- •Transformation of basis vectors
- •Inverse transformations
- •2.3 The four-velocity
- •2.4 The four-momentum
- •Conservation of four-momentum
- •Scalar product of two vectors
- •Four-velocity and acceleration as derivatives
- •Energy and momentum
- •2.7 Photons
- •No four-velocity
- •Four-momentum
- •Zero rest-mass particles
- •3 Tensor analysis in special relativity
- •Components of a tensor
- •General properties
- •Notation for derivatives
- •Components
- •Symmetries
- •Circular reasoning?
- •Mixed components of metric
- •Metric and nonmetric vector algebras
- •3.10 Exercises
- •4 Perfect fluids in special relativity
- •The number density n
- •The flux across a surface
- •Number density as a timelike flux
- •The flux across the surface
- •4.4 Dust again: the stress–energy tensor
- •Energy density
- •4.5 General fluids
- •Definition of macroscopic quantities
- •First law of thermodynamics
- •The general stress–energy tensor
- •The spatial components of T, T ij
- •Conservation of energy–momentum
- •Conservation of particles
- •No heat conduction
- •No viscosity
- •Form of T
- •The conservation laws
- •4.8 Gauss’ law
- •4.10 Exercises
- •5 Preface to curvature
- •The gravitational redshift experiment
- •Nonexistence of a Lorentz frame at rest on Earth
- •The principle of equivalence
- •The redshift experiment again
- •Local inertial frames
- •Tidal forces
- •The role of curvature
- •Metric tensor
- •5.3 Tensor calculus in polar coordinates
- •Derivatives of basis vectors
- •Derivatives of general vectors
- •The covariant derivative
- •Divergence and Laplacian
- •5.4 Christoffel symbols and the metric
- •Calculating the Christoffel symbols from the metric
- •5.5 Noncoordinate bases
- •Polar coordinate basis
- •Polar unit basis
- •General remarks on noncoordinate bases
- •Noncoordinate bases in this book
- •5.8 Exercises
- •6 Curved manifolds
- •Differential structure
- •Proof of the local-flatness theorem
- •Geodesics
- •6.5 The curvature tensor
- •Geodesic deviation
- •The Ricci tensor
- •The Einstein tensor
- •6.7 Curvature in perspective
- •7 Physics in a curved spacetime
- •7.2 Physics in slightly curved spacetimes
- •7.3 Curved intuition
- •7.6 Exercises
- •8 The Einstein field equations
- •Geometrized units
- •8.2 Einstein’s equations
- •8.3 Einstein’s equations for weak gravitational fields
- •Nearly Lorentz coordinate systems
- •Gauge transformations
- •Riemann tensor
- •Weak-field Einstein equations
- •Newtonian limit
- •The far field of stationary relativistic sources
- •Definition of the mass of a relativistic body
- •8.5 Further reading
- •9 Gravitational radiation
- •The effect of waves on free particles
- •Measuring the stretching of space
- •Polarization of gravitational waves
- •An exact plane wave
- •9.2 The detection of gravitational waves
- •General considerations
- •Measuring distances with light
- •Beam detectors
- •Interferometer observations
- •9.3 The generation of gravitational waves
- •Simple estimates
- •Slow motion wave generation
- •Exact solution of the wave equation
- •Preview
- •Energy lost by a radiating system
- •Overview
- •Binary systems
- •Spinning neutron stars
- •9.6 Further reading
- •10 Spherical solutions for stars
- •The metric
- •Physical interpretation of metric terms
- •The Einstein tensor
- •Equation of state
- •Equations of motion
- •Einstein equations
- •Schwarzschild metric
- •Generality of the metric
- •10.5 The interior structure of the star
- •The structure of Newtonian stars
- •Buchdahl’s interior solution
- •10.7 Realistic stars and gravitational collapse
- •Buchdahl’s theorem
- •Quantum mechanical pressure
- •White dwarfs
- •Neutron stars
- •10.9 Exercises
- •11 Schwarzschild geometry and black holes
- •Black holes in Newtonian gravity
- •Conserved quantities
- •Perihelion shift
- •Post-Newtonian gravity
- •Gravitational deflection of light
- •Gravitational lensing
- •Coordinate singularities
- •Inside r = 2M
- •Coordinate systems
- •Kruskal–Szekeres coordinates
- •Formation of black holes in general
- •General properties of black holes
- •Kerr black hole
- •Dragging of inertial frames
- •Ergoregion
- •The Kerr horizon
- •Equatorial photon motion in the Kerr metric
- •The Penrose process
- •Supermassive black holes
- •Dynamical black holes
- •11.6 Further reading
- •12 Cosmology
- •The universe in the large
- •The cosmological arena
- •12.2 Cosmological kinematics: observing the expanding universe
- •Homogeneity and isotropy of the universe
- •Models of the universe: the cosmological principle
- •Cosmological metrics
- •Cosmological redshift as a distance measure
- •The universe is accelerating!
- •12.3 Cosmological dynamics: understanding the expanding universe
- •Critical density and the parameters of our universe
- •12.4 Physical cosmology: the evolution of the universe we observe
- •Dark matter and galaxy formation: the universe after decoupling
- •The early universe: fundamental physics meets cosmology
- •12.5 Further reading
- •Appendix A Summary of linear algebra
- •Vector space
- •References
- •Index
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5.3 Tensor calculus in polar coordinates |
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Divergence and Laplacian |
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Before doing any more theory, let us link this up with things we have seen before. In |
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Cartesian coordinates the divergence of a vector Vα is Vα ,α . This is the scalar obtained |
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by contracting Vα ,β on its two indices. Since contraction is a frame-invariant operation, |
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the divergence of V can be calculated in other coordinates {xμ } also by contracting the |
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components of V on their two indices. This results in a scalar with the value Vα ;α . It is |
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important to realize that this is the same number as Vα ,α in Cartesian coordinates: |
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Vα ,α ≡ Vβ ;β , |
(5.54) |
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where unprimed indices refer to Cartesian coordinates and primed refer to the arbitrary |
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system. |
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For polar coordinates (dropping primes for convenience here)
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∂Vα |
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Vα ;α = |
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+ α μα Vμ. |
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∂xα |
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Now, from Eq. (5.45) we can calculate |
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θ r+ |
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θ θ θ= |
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α θ α |
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r |
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(5.55) |
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α rα |
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rrr |
θ rθ |
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1/r, |
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+ |
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Therefore we have |
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∂Vr |
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∂Vθ |
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1 |
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Vα ;α = |
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+ |
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Vr, |
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∂r |
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r |
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1 ∂ |
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∂ |
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Vθ . |
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(5.56) |
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∂θ |
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This may be a familiar formula to the student. What is probably more familiar is the Laplacian, which is the divergence of the gradient. But we only have the divergence of vectors, and the gradient is a one-form. Therefore we must first convert the one-form to a vector. Thus, given a scalar φ, we have the vector gradient (see Eq. (5.53) and the last part of § 5.2 above) with components (φ,r, φ,θ /r2). Using these as the components of the vector in the
divergence formula, Eq. (5.56) gives |
φ = r ∂r |
r ∂r |
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∂θ 2 . |
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(5.57) |
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1 ∂ |
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This is the Laplacian in plane polar coordinates. It is, of course, identically equal to |
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φ = |
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(5.58) |
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∂x2 |
∂y2 |
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Derivatives of one -forms and tensors of higher t ypes
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Since a scalar φ depends on no basis vectors, its derivative dφ is the same as its covariant derivative φ. We shall almost always use the symbol φ. To compute the derivative of a one-form (which as for a vector won’t be simply the derivatives of its components), we use
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Preface to curvature |
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˜ |
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the property that a one-form and a vector give a scalar. Thus, if p is a one-form and V is an |
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arbitrary vector, then for fixed β, |
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β V is a vector, and |
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β p is also a one-form, |
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p, V |
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is a scalar. In any (arbitrary) coordinate system this scalar is just |
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φ = pα Vα . |
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(5.59) |
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Therefore β φ is, by the product rule for derivatives, |
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∂pα |
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β φ = φ,β = |
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But we can use Eq. (5.50) to replace ∂Vα /∂xβ in favor of Vα ;β , which are the components |
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of β V: |
∂pα |
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β φ = |
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Vα + pα Vα ;β − pα Vμ α μβ . |
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∂xβ |
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Rearranging terms, and relabeling dummy indices in the term that contains the Christoffel symbol, gives
β φ = |
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Vα + pα Vα ;β . |
(5.62) |
∂xβ |
Now, every term in this equation except the one in parentheses is known to be the compo-
nent of a tensor, for an arbitrary vector field V. Therefore, since multiplication and addition of components always gives new tensors, it must be true that the term in parentheses is also the component of a tensor. This is, of course, the covariant derivative of p˜:
( β p˜)α := ( p˜)αβ := pα;β = pα,β − pμ μαβ . |
(5.63) |
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Then Eq. (5.62) reads |
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β (pα Vα ) = pα;β Vα + pα Vα ;β . |
(5.64) |
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Thus covariant differentiation obeys the same sort of product rule as Eq. (5.60). It must do this, since in Cartesian coordinates is just partial differentiation of components, so Eq. (5.64) reduces to Eq. (5.60).
Let us compare the two formulae we have, Eq. (5.50) and Eq. (5.63):
Vα ;β = Vα ,β + Vμ α μβ , pα;β = pα,β − pμ μαβ .
There are certain similarities and certain differences. If we remember that the derivative index β is the last one on , then the other indices are the only ones they can be without raising and lowering with the metric. The only thing to watch is the sign difference. It may help to remember that α μβ was related to derivatives of the basis vectors, for then it is reasonable that − μαβ be related to derivatives of the basis one-forms. The change in sign means that the basis one-forms change ‘oppositely’ to basis vectors, which makes sense