- •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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5.5 Noncoordinate bases |
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β as component indices and α as a label giving the particular tensor referred to. There is one such tensor for each basis vector eα . However, this is not terribly useful, since under a change of coordinates the basis changes and the important quantities in the new system are the new tensors eβ which are obtained from the old ones eα in a complicated way: they are different tensors, not just different components of the same tensor. So the set
in one frame is not obtained by a simple tensor transformation from the set μ
of another frame. The easiest example of this is Cartesian coordinates, where α βμ ≡ 0, while they are not zero in other frames. So in many books it is said that μαβ are not components of tensors. As we have seen, this is not strictly true: μαβ are the (μ, β) com-
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ponents of a set of 11 |
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expressions like μ |
Vα are not components of a single tensor, either. The |
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Vβ ,α + Vμ β μα
isa component of a single tensor V.
5.5 N o n co o rd i n a t e b a s e s
In this whole discussion we have generally assumed that the non-Cartesian basis vectors were generated by a coordinate transformation from (x, y) to some (ξ , η). However, as we shall show below, not every field of basis vectors can be obtained in this way, and we shall have to look carefully at our results to see which need modification (few actually do). We will almost never use non-coordinate bases in our work in this course, but they are frequently encountered in the standard references on curved coordinates in flat space, so we should pause to take a brief look at them now.
Polar coordinate basis
The basis vectors for our polar coordinate system were defined by
eα = β α eβ ,
where primed indices refer to polar coordinates and unprimed to Cartesian. Moreover, we had
β α = ∂xβ /∂xα ,
where we regard the Cartesian coordinates {xβ } as functions of the polar coordinates {xα }. We found that
eα · eβ ≡ gα β =δα β ,
i.e. that these basis vectors are not unit vectors.
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Preface to curvature |
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Polar unit basis |
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Often it is convenient to work with unit vectors. A simple set of unit vectors derived from the polar coordinate basis is:
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with a corresponding unit one-form basis |
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so these constitute orthonormal bases for the vectors and one-forms. Our notation, which is fairly standard, is to use a ‘caret’ or ‘hat’, ˆ, above an index to denote an orthornormal basis. Now, the question arises, do there exist coordinates (ξ , η) such that
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eθ |
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If so, then er, e |
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basis; if such (ξ , η) can be shown not to exist, then these vectors are a noncoordinate basis. The question is actually more easily answered if we look at the basis one-forms. Thus, we
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sin θ dx |
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∂ |
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137 |
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5.5 Noncoordinate bases |
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or |
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This is certainly not true. Therefore ξ and η do not exist: we have a noncoordinate basis. |
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dr and dθ themselves.) |
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(If this manner of proof is surprising, try it on ˜ |
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In textbooks that deal with vector calculus in curvilinear coordinates, almost all use the |
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unit orthonormal basis rather than the coordinate basis. Thus, for polar coordinates, if a |
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vector has components in the coordinate basis PC, |
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then it has components in the orthonormal basis PO |
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So if, for example, the books calculate the divergence of the vector, they obtain, instead of our Eq. (5.56),
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The difference between Eqs. (5.56) and (5.87) is purely a matter of the basis for V.
General remarks on noncoordinate bases
The principal differences between coordinate and noncoordinate bases arise from the fol-
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lowing. Consider an arbitrary scalar field |
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dφ(e |
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But if no coordinates exist for {eμ}, then Eq. (5.89) must fail. For example, if we let Eq. (5.88) define φ,μˆ , then we have
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αˆ φ ≡ φ,αˆ = β |
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138 |
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Preface to curvature |
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The Christoffel symbols may be defined just as before |
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where |
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in a coordinate basis (partial derivatives commute) but is not true otherwise. Hence, also, |
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Eq. (5.75) for μαβ in terms of gαβ,γ applies only in a coordinate basis. More general |
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expressions are worked out in Exer. 20, § 5.8. |
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What is the general reason for the nonexistence of coordinates for a basis? If |
ωα¯ |
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is a |
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dxα |
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is |
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coordinate one-form basis, then its relation to another one {˜ |
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dxβ . |
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(5.94) |
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The key point is that α¯ β , which is generally a function of position, must actually be the partial derivative ∂xα¯ /∂xβ everywhere. Thus we have
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α¯ γ . |
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These ‘integrability conditions’ must be satisfied by all the elements α¯ β |
in order for ωα¯ |
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to be a coordinate basis. Clearly, we can always choose a transformation matrix for which this fails, thereby generating a noncoordinate basis.
Noncoordinate bases in this book
We shall not have occasion to use such bases very often. Mainly, it is important to understand that they exist, that not every basis is derivable from a coordinate system. The algebra of coordinate bases is simpler in almost every respect. We may ask why the standard treatments of curvilinear coordinates in vector calculus, then, stick to orthonormal bases. The reason is that in such a basis in Euclidean space, the metric has components δαβ , so the form of the dot product and the equality of vector and one-form components carry over directly from Cartesian coordinates (which have the only orthonormal coordinate basis!). In order to gain the simplicity of coordinate bases for vector and tensor calculus, we have to spend time learning the difference between vectors and one-forms!
5.6 L o o k i n g a h e a d
The work we have done in this chapter has developed almost all the notation and concepts we will need in our study of curved spaces and spacetimes. It is particularly important that the student understands §§ 5.2–5.4 because the mathematics of curvature will be developed