The large-scale structure of the universe / by P. J. E. Peebles.

Format:

Book

Author/Creator:

Peebles, P. J. E. (Phillip James Edwin)

Series:

Princeton series in physics

Language:

English

Subjects (All):

Galaxies.

Cosmology.

Physical Description:

xiii, 422 pages ; 24 cm.

Place of Publication:

Princeton, N.J. : Princeton University Press, [1980]

Summary:

Opinions on the large-scale structure of the early universe range widely from primeval chaos to a well-ordered mass distribution. P.J.E. Peebles argues that the evolution proceeded from a nearly uniform initial state to a progressively more irregular and clumpy universe. The discussion centers on the largest known structures -- the clusters of galaxies, the empirical evidence of the nature of the clustering, and the theories of how the clustering evolves in an expanding universe.

Contents:

I. Homogeneity and Clustering 3

2. Is the universe homogeneous? 3

3. Physical principles 11

4. How did galaxies and clusters of galaxies form? 18

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 [delta] 49

11. Solutions for [delta](t): p = [Lambda] = 0 51

12. Solutions for [delta](t): effect of a uniform radiation background 56

13. Solutions for [delta](t): models with [Lambda not equal] 0 59

14. The peculiar velocity field 63

15. Joining conditions for [delta] and [upsilon] 66

16. Critical Jeans length 68

17. Primeval magnetic field as a source for [delta rho] / [rho] 71

18. Second order perturbation theory for [delta rho] / [rho] 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 [xi](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 [xi] and [zeta] 156

38. Probability generating function 158

39. Estimates of P[subscript 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([theta]) 183

48. Statistical uncertainty in the estimate of w([theta]) 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 [xi] 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[subscript 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 [xi] 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[subscript alpha beta] 310

83. Gravitational waves 312

84. Newtonian approximation 313

85. Linear perturbation equations for the matter 317

86. Behavior of density perturbations at wavelength [characters not reproducible] 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

97. Models and notation 395.

Notes:

Includes index.

Bibliography: pages 402-416.

ISBN:

0691082391 :

OCLC:

6421704