- •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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2.2 Vector algebra |
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In the last line we use the summation convention (remember always to write the index on e as a subscript in order to employ the convention in this manner). The meaning of Eq. (2.11)
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A is the linear sum of four vectors A0e , A1e , etc. |
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Transformation of basis vectors
The discussion leading up to Eq. (2.11) could have been applied to any frame, so it is equally true in O¯ :
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A is also the sum of the four vectors A0¯ |
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e1, etc. These are not the same |
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This says that |
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four vectors as in Eq. (2.11), since they are parallel to the basis vectors of ¯ and not of |
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A. It is important to understand that the expressions |
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O, but they add up to the same vector |
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are not obtained from one another merely by relabeling dummy indices. |
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Aα eα |
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Barred and unbarred indices cannot be interchanged, since they have different meanings.
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eα |
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from {eα }. But, by definition, the two sums are the same: |
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Aα e |
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Aα¯ e |
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(2.12) |
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α = |
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and this has an important consequence: from it we deduce the transformation law for the basis vectors, i.e. the relation between {eα } and {eα¯ }. Using Eq. (2.7) for Aα¯ , we write Eq. (2.12) as
α¯ β Aβ eα¯ = Aα eα .
On the left we have two sums. Since they are finite sums their order doesn’t matter. Since the numbers α¯ β and Aβ are just numbers, their order doesn’t matter, and we can write
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Aβ α¯ |
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β α¯ |
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This equation must be true for all sets |
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A ( ¯ α e |
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eα ) 0 |
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we deduce |
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or |
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38 |
Vector analysis in special relativity |
This gives the law by which basis vectors change. It is not a component transformation: it gives the basis {eα } of O as a linear sum over the basis {eα¯ } of O¯ . Comparing this to the law for components, Eq. (2.7),
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α A , |
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we see that it is different indeed.
The above discussion introduced many new techniques, so study it carefully. Notice that the omission of the summation signs keeps things neat. Notice also that a step of key importance was relabeling the dummy indices: this allowed us to isolated the arbitrary Aα from the rest of the things in the equation.
An example
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Let ¯ move with velocity v in the x direction relative to |
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where we use the standard notation |
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(5, 0, 0, 2), we find its components in |
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by |
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Then, if |
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O
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A0 = 00A0 + 01A1 + · · ·
=γ · 5 + (−vγ ) · 0 + 0 · 0 + 0 · 2
=5γ .
Similarly,
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A1¯ = −5vγ , |
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A2¯ = 0, |
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A3¯ = 2. |
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Therefore, |
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The basis vectors are expressible as |
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eα |
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α e |
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β
or
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e0 = 00e¯ + 10e¯ + · · ·
0 1
= γ e¯ − vγ e¯ .
0 1
39 |
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2.2 Vector algebra |
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Similarly, |
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e1 = −vγ e0¯ + γ e1¯ , |
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This gives O’s basis in terms of O¯ ’s, so let us draw the picture (Fig. 2.1) in O¯ ’s frame: This transformation is of course exactly what is needed to keep the basis vectors pointing along the axes of their respective frames. Compare this with Fig. 1.5(b).
Inverse transformations
¯
The only thing the Lorentz transformation β α depends on is the relative velocity of the two frames. Let us for the moment show this explicitly by writing
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α (v). |
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Then |
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If the basis of O is obtained from that of O¯ by the transformation with velocity v, then the reverse must be true if we use −v. Thus we must have
eμ¯ = ν μ¯ (−v)eν . |
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In this equation I have used μ¯ and ν as indices to avoid confusion with the previous formula. The bars still refer, of course, to the frame O¯ . The matrix [ ν μ¯ ] is exactly the
matrix [ ¯ α ] except with changed to − . The bars on the indices only serve to indicate
β v
v
the names of the observers involved: they affect the entries in the matrix [ ] only in that the matrix is always constructed using the velocity of the upper-index frame relative to the
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Figure 2.1 |
Basis vectors of |
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and |
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O¯ |
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as drawn by . |
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Vector analysis in special relativity |
lower-index frame. This is made explicit in Eqs. (2.14) and (2.15). Since v is the velocity of O¯ (the upper-index frame in Eq. (2.14)) relative to O, then −v is the velocity of O (the upper-index frame in Eq. (2.15)) relative to O¯ . Exer. 11, § 2.9, will help you understand this point.
We can rewrite the last expression as
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v)eν . |
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equations, one for each value of |
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¯. In this form we can put it into the expression for eα |
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Eq. (2.14): |
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eα = β α (v)e ¯
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= β α (v) ν ¯ (−v)eν . (2.16)
β
In this equation only the basis of O appears. It must therefore be an identity for all v. On
the right there are two sums, one on |
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first, then the right is a sum over the basis {eν } in which each basis vector eν has coefficient
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Imagine evaluating Eq. (2.16) for some fixed value of the index α. If the right side of Eq. (2.16) is equal to the left, the coefficient of eα on the right must be 1 and all other coefficients must vanish. The mathematical way of saying this is
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β α (v) ν ¯ (−v) = δν α ,
β
where δν α is the Kronecker delta again. This would imply
eα = δν α eν ,
which is an identity.
Let us change the order of multiplication above and write down the key formula
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This expresses the fact that the matrix [ ν |
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sum on ¯ is exactly the operation we perform when we multiply two matrices. The matrix (δν α ) is, of course, the identity matrix.
The expression for the change of a vector’s components, |
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also has its inverse. Let us multiply both sides by ν |
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= δν α Aα
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