- •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
A |
Appendix A Summary of linear algebra |
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For the convenience of the student we collect those aspects of linear algebra that are important in our study. We hope that none of this is new to the reader.
Vec tor space
A collection of elements V = {A, B, . . .} forms a vector space over the real numbers if and only if they obey the following axioms (with a, b real numbers).
(1) V is an abelian group with operation + (A + B = B + A V) and identity
0(A + 0 = A).
(2)Multiplication of vectors by real numbers is an operation which gives vectors and which is:
(i)distributive over vector addition, a(A + B) = a(A) + a(B);
(ii)distributive over real number addition, (a + b)(A) = a(A) + b(A);
(iii)Associative with real number multiplication, (ab) (A) = a(b(A));
(iv)consistent with the real number identity, 1(A) = A.
This definition could be generalized to vector spaces over complex numbers or over any field, but we shall not need to do so.
A set of vectors {A, B, . . .} is said to be linearly independent if and only if there do not exist real numbers {a, b, . . . , f }, not all of which are zero, such that
aA + bB + · · · + fF = 0.
The dimension of the vector space is the largest number of linearly independent vectors we can choose. A basis for the space is any linearly independent set of vectors {A1, . . . , An}, where n is the dimension of the space. Since for any B the set {B, A1, . . . , An} is linearly dependent, it follows that B can be written as a linear combination of the basis vectors:
B = b1A1 + b2A2 + · · · + bnAn.
The numbers {b1, . . . , bn} are called the components of B on {A1, . . . , An}.
An inner product may be defined on a vector space. It is a rule associating with any pair of vectors, A and B, a real number A · B, which has the properties:
(1)A · B = B · A,
(2)(aA + bB) · C = a(A · C) + b(B · C).
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By (1), the map (A, B) → (A · B) is symmetric; by (2), it is bilinear. The inner product is called positive-definite if A · A > 0 for all A =0. In that case the norm of the vector A is |A| ≡ (A · A)1/2. In relativity we deal with inner products that are indefinite: A · A has one sign for some vectors and another for others. In this case the norm, or magnitude, is often defined as |A| ≡ |A · A|1/2. Two vectors A and B are said to be orthogonal if and only if
A · B = 0.
It is often convenient to adopt a set of basis vectors {A1, . . . , An} that are orthonormal: Ai · Aj = 0 if i =j and |Ak| = 1 for all k. This is not necessary, of course. The reader unfamiliar with nonorthogonal bases should try the following. In the two-dimensional Euclidean plane with Cartesian (orthogonal) coordinates x and y and associated Cartesian (orthonormal) basis vectors ex and ey, define A and B to be the vectors A = 5ex + ey, B = 3ey. Express A and B as linear combinations of the nonorthogonal basis {e1 = ex, e2 = ey − ex}. Notice that, although e1 and ex are the same, the 1 and x components of A and B are not the same.
M atrices
A matrix is an array of numbers. We shall only deal with square matrices, e.g.
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The dimension of a matrix is the number of its rows (or columns). We denote the elements of a matrix by Aij, where the value of i denotes the row and that of j denotes the column; for a 2 × 2 matrix we have
A = |
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A column vector W is a set of numbers Wi, for example |
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sions. (Column vectors form a vector space in the usual way.) The following rule governs multiplication of a column vector by a matrix to give a column vector V = A · W:
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V1 |
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Vi = |
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For n-dimensional matrices and vectors, this generalizes to |
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Notice that the sum is on the second index of A.
Matrices form a vector space themselves, with addition and multiplication by a number defined by:
A + B = C Cij = Aij + Bij.
aA = B Bij = aAij.
For n × n matrices, the dimension of this vector space is n2. A natural inner product may be defined on this space:
A · B = AijBij. i,j
We can easily show that this is positive-definite. More important than the inner product, however, for our purposes, is matrix multiplication. (A vector space with multiplication is called an algebra, so we are now studying the matrix algebra.) For 2 × 2 matrices, the product is
AB = C C21 |
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A21 |
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+ A12B21 |
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Generalizing to n × n matrices gives |
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k=1
Notice that the index summed on is the second of A and the first of B. Multiplication is associative but not commutative; the identity is the matrix whose elements are δij, the Kronecker delta symbol (δij = 1 if i = j, 0 otherwise).
The determinant of a 2 × 2 matrix is
det A = det |
A11 |
A12 |
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A21 |
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= A11A22 − A12A21.
Given any n × n matrix B and an element Blm (for fixed l and m), we call Slm the (n − 1) × (n − 1) submatrix defined by excluding row l and column m from B, and we call Dlm the determinant of Slm. For example, if B is the 3 × 3 matrix
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B32 |
B33 |
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then the submatrix S12 is the 2 × 2 matrix |
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and its determinant is |
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D12 = B21B33 − B23B31. |
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Then the determinant of B is defined as |
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det (B) = |
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In this expression we sum only over j for fixed i. The result is independent of which i was chosen. This enables us to define the determinant of a 3 × 3 matrix in terms of that of a 2 × 2 matrix, and that of a 4 × 4 in terms of 3 × 3, and so on.
Because matrix multiplication is defined, it is possible to define the multiplicative inverse of a matrix, which is usually just called its inverse;
(B−1)ij = (−1)i+jDji/ det (B)
The inverse is defined if and only if det (B) =0.