The Large-Scale Structure of the Universe

by P. J. E. Peebles

Overview

The classic account of the structure and evolution of the early universe from Nobel Prize–winning physicist P. J. E. Peebles

An instant landmark on its publication, The Large-Scale Structure of the Universe remains the essential introduction to this vital area of research. Written by one of the world's most esteemed theoretical cosmologists, it provides an invaluable historical introduction to the subject, and an enduring overview of key methods, statistical measures, and techniques for dealing with cosmic evolution. With characteristic clarity and insight, P. J. E. Peebles focuses on the largest known structures—galaxy clusters—weighing the empirical evidence of the nature of clustering and the theories of how it evolves in an expanding universe. A must-have reference for students and researchers alike, this edition of The Large-Scale Structure of the Universe introduces a new generation of readers to a classic text in modern cosmology.

Product Details

ISBN-13:	9780691206714
Publisher:	Princeton University Press
Publication date:	09/15/2020
Series:	Princeton Series in Physics , #96
Sold by:	Barnes & Noble
Format:	eBook
Pages:	448
File size:	56 MB
Note:	This product may take a few minutes to download.

About the Author

P. J. E. Peebles is a Nobel Prize–winning physicist whose books include Cosmology's Century, Principles of Physical Cosmology, and Quantum Mechanics (all Princeton). He is the Albert Einstein Professor of Science Emeritus in the Department of Physics at Princeton University.

Table of Contents

Preface xi

Acknowledgments xv

I Homogeneity and clustering 3

1 Homogeneity and clustering 3

2 Is the universe homogeneous? 3

3 Physical principles 11

4 How did galaxies and clusters of galaxies form? 18

5 Summary 35

II Behavior of irregularities in the distribution of matter: newtonian approximation 37

6 Newtonian approximation 37

7 Particle dynamics in expanding coordinates 41

8 The peculiar acceleration 43

9 Two models: the Vlasov equation and the ideal fluid 45

10 Linear perturbation approximation for δ 49

11 Solutions for δ(t): p = Λ = 0 51

12 Solutions for δ(t): effect of a uniform radiation background 56

13 Solutions for δ(t): models with Λ ≠ 0 59

14 The peculiar velocity field 63

15 Joining conditions for δ and υ 66

16 Critical Jeans length 68

17 Primeval magnetic field as a source for δρ/ρ 71

18 Second order perturbation theory for δρ/ρ 74

19 Spherical model 77

20 Homogeneous ellipsoid model 86

21 Caustics and pancakes 95

22 Expansion, vorticity, and shear 103

23 Origin of the rotation of galaxies 107

24 Cosmic energy equation 110

25 Spherical accretion model 115

26 Hierarchical clustering model 120

27 Fourier transform of the equations of motion 124

28 Coupling of density fluctuations 128

III n-Point correlation functions: descriptive statistics 138

29 Statistical measures of the galaxy distribution 138

30 Fair sample hypothesis 142

31 Two-point spatial correlation function ξ(r) 143

32 Two-point correlation function: another definition 145

33 Two-point correlation function: Poisson model 147

34 Three-point correlation function 148

35 Four-point correlation function 150

36 Moments of counts of objects 152

37 Constraints on ξ and ζ 156

38 Probability generating function 158

39 Estimates of P_N 160

40 Cluster model 163

41 Power spectrum 166

42 Power law model for the spectrum 169

43 Bispectrum 171

44 Cross correlation function 172

45 Angular two-point correlation function 174

46 Angular power spectrum 175

47 Estimating w(θ) 183

48 Statistical uncertainty in the estimate of w(θ) 187

49 Relation between angular and spatial two-point correlation functions 189

50 Small separation approximation and the scaling relation 191

51 Decoupling of magnitude and position 194

52 Relation between ξ and w: some examples 195

53 Inversion of the equation 200

54 Angular three-point correlation function 203

55 Angular four-point correlation function 209

56 Correction for curvature and expansion 213

57 Summary of numerical results 221

58 Power spectrum of the extragalactic light 225

59 Moments of the number of neighbors 230

60 Model for P_N 233

61 Clustering models 236

62 Continuous clustering hierarchy: Mandelbrot's prescription 243

63 The mass correlation functions 249

64 Clustering hierarchy: continuity speculation 253

65 Remarks on the observations 255

IV Dynamics and statistics 257

66 Goals 257

67 Definitions of variables and distribution functions 258

68 BBGKY hierarchy equations 259

69 Fluid limit 262

70 Evolution of the integral of ξ 264

71 Particle conservation equations 266

72 Relative peculiar velocity dispersion 272

73 Similarity solution 275

74 Cosmic energy equation 278

75 Cosmic virial theorem 280

76 Joint distribution in position and velocity 284

77 Behavior of the halo around a cluster of galaxies 291

78 Superclusters 299

79 Problems and prospects 301

V Relativistic theory of the behavior of irregularities in an expanding world model 304

80 Role of the relativistic theory 304

81 Time-orthogonal coordinates 306

82 The field equations for h_αβ 310

83 Gravitational waves 312

84 Newtonian approximation 313

85 Linear perturbation equations for the matter 317

86 Behavior of density perturbations at wavelength » ct 319

87 Spherical model 324

88 Evolution of acoustic waves 330

89 Nonlinear acoustic waves 333

90 Incompressible flow 341

91 Behavior of collisionless particles 345

92 Linear dissipation of adiabatic perturbations 352

93 Residual fluctuations in the microwave background 363

94 Isothermal perturbations 373

VI Scenarios 379

95 Nature of the universe at high redshift 379

96 Nature of protogalaxies and protoclusters 384

Appendix 395

97 Models and notation 395

List of abbreviations 401

References 402

Index 417

Editorial Reviews

James Peebles, Co-Winner of the Nobel Prize in Physics

From the Publisher