- •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
49 |
2.7 Photons |
2.7 P h o t o n s
No four-velocity
Photons move on null lines, so, for a photon path,
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Therefore dτ is zero and Eq. (2.31) shows that the four-velocity cannot be defined. Another way of saying the same thing is to note that there is no frame in which light is at rest (the second postulate of SR), so there is no MCRF for a photon. Thus, no e0 in any frame will be tangent to a photon’s world line.
Note carefully that it is still possible to find vectors tangent to a photon’s path (which, being a straight line, has the same tangent everywhere): dx is one. The problem is finding a tangent of unit magnitude, since they all have vanishing magnitude.
Four-momentum
The four-momentum of a particle is not a unit vector. Instead, it is a vector where the components in some frame give the particle energy and momentum relative to that frame. If a photon carries energy E in some frame, then in that frame p0 = E. If it moves in the x direction, then py = pz = 0, and in order for the four-momentum to be parallel to its world line (hence be null) we must have px = E. This ensures that
p · p = −E2 + E2 = 0. |
(2.37) |
So we conclude that photons have spatial momentum equal to their energy. |
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E = hν, |
(2.38) |
where ν is its frequency and h is Planck’s constant, h = 6.6256 × 10−34 J s.
This relation and the Lorentz transformation of the four-momentum immediately give us the Doppler-shift formula for photons. Suppose, for instance, that in frame O a photon
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This is generalized in Exer. 25, § 2.9.
50 |
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Vector analysis in special relativity |
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Zero rest-mass particles |
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Any particle whose four-momentum is null must have rest mass zero, and conversely. The only known zero rest-mass particle is the photon. Neutrinos are very light, but not massless. (Sometimes the ‘graviton’ is added to this list, since gravitational waves also travel at the speed of light, as we shall see later. But ‘photon’ and ‘graviton’ are concepts that come from quantum mechanics, and there is as yet no satisfactory quantized theory of gravity, so that ‘graviton’ is not really a well-defined notion yet.) The idea that only particles with zero rest mass can travel at the speed of light is reinforced by the fact that no particle of finite rest mass can be accelerated to the speed of light, since then its energy would be infinite. Put another way, a particle traveling at the speed of light (in, say, the x direction) has p1/p0 = 1, while a particle of rest mass m moving in the x direction has, from the equation p · p = −m2, p1/p0 = [1 − m2/(p0)2]1/2, which is always less than one, no matter how much energy the particle is given. Although it may seem to get close to the speed of light, there is an important distinction: the particle with m =0 always has an MCRF, a Lorentz frame in which it is at rest, the velocity v of which is p1/p0 relative to the old frame. A photon has no rest frame.
2.8 F u r t h e r re a d i n g
We have only scratched the surface of relativistic kinematics and particle dynamics. These are particularly important in particle physics, which in turn provides the most stringent tests of SR. See Hagedorn (1963) or Wiedemann (2007).
2.9 E xe rc i s e s
1 Given the numbers {A0 = 5, A1 = 0, A2 = −1, A3 = −6}, {B0 = 0, B1 = −2, B2 = 4,
B3 = 0}, {C00 = 1, C01 = 0, C02 = 2, C03 = 3, C30 = −1, C10 = 5, C11 = −2, C12 =
−2, C13 = 0, C21 = 5, C22 = 2, C23 = −2, C20 = 4, C31 = −1, C32 = −3, C33 = 0}, find:
(a) Aα Bα ; (b) Aα Cαβ for all β; (c) Aγ Cγ σ for all σ ; (d) Aν Cμν for all μ; (e) Aα Bβ for all α, β; (f) AiBi; (g) AjBk for all j, k.
2Identify the free and dummy indices in the following equations and change them into equivalent expressions with different indices. How many different equations does each
expression represent?
(a) Aα Bα = 5; (b) Aμ¯ = μ¯ ν Aν ; (c) TαμλAμCλγ = Dγ α ; (d) Rμν − 12 gμν R = Gμν .
3Prove Eq. (2.5).
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6In the t − x spacetime diagram of O, draw the basis vectors e0 and e1. Draw the corresponding basis vectors of the frame O¯ that moves with speed 0.6 in the positive x direction relative to O. Draw the corresponding basis vectors of O a frame that moves with speed 0.6 in the positive x direction relative to O¯ .
7(a) Verify Eq. (2.10) for all α, β.
(b)Prove Eq. (2.11) from Eq. (2.9).
8(a) Prove that the zero vector (0, 0, 0, 0) has these same components in all reference frames.
(b)Use (a) to prove that if two vectors have equal components in one frame, they have equal components in all frames.
9Prove, by writing out all the terms, that
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(a)Write down the matrix of ν μ¯ (−v).
(b)Find Aα¯ for all α¯ .
(c)Verify Eq. (2.18) by performing the indicated sum for all values of ν and α.
(d)Write down the Lorentz transformation matrix from O¯ to O, justifying each entry.
(e)Use (d) to find Aβ from Aα¯ . How is this related to Eq. (2.18)?
(f)Verify, in the same manner as (c), that
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14 The following matrix gives a Lorentz transformation from O to O¯ :
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(a)What is the velocity (speed and direction) of O¯ relative to O?
(b)What is the inverse matrix to the given one?
O →
(c) Find the components in of a vector A (1, 2, 0, 0).
O¯
15(a) Compute the four-velocity components in O of a particle whose speed in O is v in the positive x direction, by using the Lorentz transformation from the rest frame of the particle.
(b)Generalize this result to find the four-velocity components when the particle has arbitrary velocity v, with |v| < 1.
(c)Use your result in (b) to express v in terms of the components {Uα }.
(d)Find the three-velocity v of a particle whose four-velocity components are (2, 1, 1, 1).
16Derive the Einstein velocity-addition formula by performing a Lorentz transformation with velocity v on the four-velocity of a particle whose speed in the original frame
was W.
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Prove that any timelike vector U for which U0 > 0 and U · U = −1 is the |
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18(a) Show that the sum of any two orthogonal spacelike vectors is spacelike.
(b)Show that a timelike vector and a null vector cannot be orthogonal.
19A body is said to be uniformly accelerated if its acceleration four-vector a has constant spatial direction and magnitude, say a · a = α2 0.
53 |
2.9 Exercises |
(a)Show that this implies that a always has the same components in the body’s MCRF, and that these components are what one would call ‘acceleration’ in Galilean terms. (This would be the physical situation for a rocket whose engine always gave the same acceleration.)
(b)Suppose a body is uniformly accelerated with α = 10 m s−2 (about the acceleration of gravity on Earth). If the body starts from rest, find its speed after time t. (Be
sure to use the correct units.) How far has it traveled in this time? How long does it take to reach v = 0.999?
(c)Find the elapsed proper time for the body in (b), as a function of t. (Integrate dτ
along its world line.) How much proper time has elapsed by the time its speed is v = 0.999? How much would a person accelerated as in (b) age on a trip from
Earth to the center of our Galaxy, a distance of about 2 × 1020 m? 20 The world line of a particle is described by the equations
x(t) = at + b sin ωt, |
y(t) = b cos ωt, |
z(t) = 0, |bω| < 1, |
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in some inertial frame. Describe the motion and compute the components of the particle’s four-velocity and four-acceleration.
21 The world line of a particle is described by the parametric equations in some Lorentz frame
t(λ) = a sinh |
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22(a) Find the energy, rest mass, and three-velocity v of a particle whose four-momentum has the components (4, 1, 1, 0) kg.
(b)The collision of two particles of four-momenta
p1 →O (3, −1, 0, 0) kg, |
p2 →O (2, 1, 1, 0) kg |
results in the destruction of the two particles and the production of three new ones, two of which have four-momenta
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Find the four-momentum, energy, rest mass, and three-velocity of the third particle produced. Find the CM frame’s three-velocity.
23A particle of rest mass m has three-velocity v. Find its energy correct to terms of
order |v|4. At what speed |v| does the absolute value of 0(|v|4) term equal 12 of the kinetic-energy term 12 m|v|2?
24Prove that conservation of four-momentum forbids a reaction in which an electron and positron annihilate and produce a single photon (γ -ray). Prove that the production of two photons is not forbidden.
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25(a) Let frame O¯ move with speed v in the x-direction relative to O. Let a photon have
frequency ν in O and move at an angle θ with respect to O’s x axis. Show that its frequency in O¯ is
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ν/ν |
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(b)Even when the motion of the photon is perpendicular to the x axis (θ = π/2) there is a frequency shift. This is called the transverse Doppler shift, and arises because
of the time dilation. At what angle θ does the photon have to move so that there is no Doppler shift between O and O¯ ?
(c)Use Eqs. (2.35) and (2.38) to calculate Eq. (2.42).
26 Calculate the energy that is required to accelerate a particle of rest mass m =0 from speed v to speed v + δv (δv v), to first order in δv. Show that it would take an infinite amount of energy to accelerate the particle to the speed of light.
27 Two identical bodies of mass 10 kg are at rest at the same temperature. One of them is heated by the addition of 100 J of heat. Both are then subjected to the same force.
Which accelerates faster, and by how much? |
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28 Let |
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moving at speed v = 0.6 in the positive x direction relative to O, with its spatial axes
oriented parallel to O’s. |
A, B, and C in |
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A, B, and C as timelike, spacelike, or null. |
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29 Prove, using the component expressions, Eqs. (2.24) and (2.26), that |
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30 The four-velocity of a rocket ship is U O (2, 1, 1, 1). It encounters a high-velocity
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(300, 299, 0, 0) |
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10−27 kg. Compute the |
cosmic ray whose momentum is P |
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energy of the cosmic ray as measured by the rocket ship’s passengers, using each of the two following methods.
(a) Find the Lorentz transformations from O to the MCRF of the rocket ship, and use
it to transform the components of P.
(b)Use Eq. (2.35).
(c)Which method is quicker? Why?
31A photon of frequency ν is reflected without change of frequency from a mirror, with an angle of incidence θ . Calculate the momentum transferred to the mirror. What momentum would be transferred if the photon were absorbed rather than reflected?
32Let a particle of charge e and rest mass m, initially at rest in the laboratory, scatter a photon of initial frequency νi. This is called Compton scattering. Suppose the scattered photon comes off at an angle θ from the incident direction. Use conservation of four-momentum to deduce that the photon’s final frequency νf is given by
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2.9 |
Exercises |
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33Space is filled with cosmic rays (high-energy protons) and the cosmic microwave back-
ground radiation. These can Compton scatter off one another. Suppose a photon of energy hν = 2 × 10−4 eV scatters off a proton of energy 109mP = 1018 eV, energies measured in the Sun’s rest frame. Use Eq. (2.43) in the proton’s initial rest frame to
calculate the maximum final energy the photon can have in the solar rest frame after
the scattering. What energy range is this (X-ray, visible, etc.)?
A, B, and C are any vectors and α and β any real numbers, |
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34 Show that, if |
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35 Show that the vectors |
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obtained from |
eα |
by Eq. (2.15) satisfy eα |
all ¯ , ¯.
α β
· ¯ = |
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for |
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ηαβ |