The Resource The largescale structure of the universe, by P.J.E. Peebles
The largescale structure of the universe, by P.J.E. Peebles
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The item The largescale structure of the universe, by P.J.E. Peebles represents a specific, individual, material embodiment of a distinct intellectual or artistic creation found in University of MissouriSt. Louis Libraries.This item is available to borrow from 1 library branch.
Resource Information
The item The largescale structure of the universe, by P.J.E. Peebles represents a specific, individual, material embodiment of a distinct intellectual or artistic creation found in University of MissouriSt. Louis Libraries.
This item is available to borrow from 1 library branch.
 Summary
 Opinions on the largescale structure of the early universe range widely from primeval chaos to a wellordered 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. In Chapter One the author provides an historical introduction to the subject. Chapter Two contains a survey of methods used to deal with the Newtonian approximation to the theory of the evolution of the mass distribution. Recent progress in the use of statistical measures of the clustering is described in Chapter Three. Chapters Four and Five return to techniques for dealing with cosmic evolution, in the statistical measures of clustering and under general relativity theory. Lastly, in Chapter Six Professor Peebles assesses the progress in attempts to link theory and observation to arrive at a well established physical picture of the nature and evolution of the universe
 Language
 eng
 Extent
 xiii, 422 pages
 Contents

 Homogeneity and Clustering
 Is the universe homogeneous?
 Physical principles
 How did galaxies and clusters of galaxies form?
 Behavior of Irregularities in the Distribution of Matter: Newtonian Approximation
 Newtonian approximation
 Particle dynamics in expanding coordinates
 The peculiar acceleration
 Two models: the Vlasov equation and the ideal fluid
 Linear perturbation approximation for [delta]
 Solutions for [delta](t): p = [Lambda] = 0
 Solutions for [delta](t): effect of a uniform radiation background
 Solutions for [delta](t): models with [Lambda not equal] 0
 The peculiar velocity field
 Joining conditions for [delta] and [upsilon]
 Critical Jeans length
 Primeval magnetic field as a source for [delta rho] / [rho]
 Second order perturbation theory for [delta rho] / [rho]
 Spherical model
 Homogeneous ellipsoid model
 Caustics and pancakes
 Expansion, vorticity, and shear
 Origin of the rotation of galaxies
 Cosmic energy equation
 Spherical accretion model
 Hierarchical clustering model
 Fourier transform of the equations of motion
 Coupling of density fluctuations
 nPoint Correlation Functions: Descriptive Statistics
 Statistical measures of the galaxy distribution
 Fair sample hypothesis
 Twopoint spatial correlation function [xi](r)
 Twopoint correlation function: another definition
 Twopoint correlation function: Poisson model
 Threepoint correlation function
 Fourpoint correlation function
 Moments of counts of objects
 Constraints on [xi] and [zeta]
 Probability generating function
 Estimates of P[subscript N]
 Cluster model
 Power spectrum
 Power law model for the spectrum
 Bispectrum
 Cross correlation function
 Angular twopoint correlation function
 Angular power spectrum
 Estimating w([theta])
 Statistical uncertainty in the estimate of w([theta])
 Relation between angular and spatial twopoint correlation functions
 Small separation approximation and the scaling relation
 Decoupling of magnitude and position
 Relation between [xi] and w: some examples
 Inversion of the equation
 Angular threepoint correlation function
 Angular fourpoint correlation function
 Correction for curvature and expansion
 Summary of numerical results
 Power spectrum of the extragalactic light
 Moments of the number of neighbors
 Model for P[subscript N]
 Clustering models
 Continuous clustering hierarchy: Mandelbrot's prescription
 The mass correlation functions
 Clustering hierarchy: continuity speculation
 Remarks on the observations
 Dynamics and Statistics
 Goals
 Definitions of variables and distribution functions
 BBGKY hierarchy equations
 Fluid limit
 Evolution of the integral of [xi]
 Particle conservation equations
 Relative peculiar velocity dispersion
 Similarity solution
 Cosmic energy equation
 Cosmic virial theorem
 Joint distribution in position and velocity
 Behavior of the halo around a cluster of galaxies
 Superclusters
 Problems and prospects
 Relativistic Theory of the Behavior of Irregularities in an Expanding World Model
 Role of the relativistic theory
 Timeorthogonal coordinates
 The field equations for h[subscript alpha beta]
 Gravitational waves
 Newtonian approximation
 Linear perturbation equations for the matter
 Behavior of density perturbations at wavelength [characters not reproducible] ct
 Spherical model
 Evolution of acoustic waves
 Nonlinear acoustic waves
 Incompressible flow
 Behavior of collisionless particles
 Linear dissipation of adiabatic perturbations
 Residual fluctuations in the microwave background
 Isothermal perturbations
 Scenarios
 Nature of the universe at high redshift
 Nature of protogalaxies and protoclusters
 Models and notation
 Isbn
 9780691082394
 Label
 The largescale structure of the universe
 Title
 The largescale structure of the universe
 Statement of responsibility
 by P.J.E. Peebles
 Language
 eng
 Summary
 Opinions on the largescale structure of the early universe range widely from primeval chaos to a wellordered 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. In Chapter One the author provides an historical introduction to the subject. Chapter Two contains a survey of methods used to deal with the Newtonian approximation to the theory of the evolution of the mass distribution. Recent progress in the use of statistical measures of the clustering is described in Chapter Three. Chapters Four and Five return to techniques for dealing with cosmic evolution, in the statistical measures of clustering and under general relativity theory. Lastly, in Chapter Six Professor Peebles assesses the progress in attempts to link theory and observation to arrive at a well established physical picture of the nature and evolution of the universe
 Cataloging source
 DLC
 http://library.link/vocab/creatorName
 Peebles, P. J. E.
 Dewey number
 523.1/12
 Index
 index present
 LC call number
 QB857
 LC item number
 .P43
 Literary form
 non fiction
 Nature of contents
 bibliography
 Series statement
 Princeton series in physics
 http://library.link/vocab/subjectName

 Large scale structure (Astronomy)
 Galaxies
 Cosmology
 Cosmology
 Galaxies
 Large scale structure (Astronomy)
 Kosmologie
 Galaxias
 Galaxies
 Galaxies
 Cosmologie
 Label
 The largescale structure of the universe, by P.J.E. Peebles
 Bibliography note
 Includes bibliographical references (pages 402416) and index
 Carrier category
 volume
 Carrier category code

 nc
 Carrier MARC source
 rdacarrier
 Content category
 text
 Content type code

 txt
 Content type MARC source
 rdacontent
 Contents
 Homogeneity and Clustering  Is the universe homogeneous?  Physical principles  How did galaxies and clusters of galaxies form?  Behavior of Irregularities in the Distribution of Matter: Newtonian Approximation  Newtonian approximation  Particle dynamics in expanding coordinates  The peculiar acceleration  Two models: the Vlasov equation and the ideal fluid  Linear perturbation approximation for [delta]  Solutions for [delta](t): p = [Lambda] = 0  Solutions for [delta](t): effect of a uniform radiation background  Solutions for [delta](t): models with [Lambda not equal] 0  The peculiar velocity field  Joining conditions for [delta] and [upsilon]  Critical Jeans length  Primeval magnetic field as a source for [delta rho] / [rho]  Second order perturbation theory for [delta rho] / [rho]  Spherical model  Homogeneous ellipsoid model  Caustics and pancakes  Expansion, vorticity, and shear  Origin of the rotation of galaxies  Cosmic energy equation  Spherical accretion model  Hierarchical clustering model  Fourier transform of the equations of motion  Coupling of density fluctuations  nPoint Correlation Functions: Descriptive Statistics  Statistical measures of the galaxy distribution  Fair sample hypothesis  Twopoint spatial correlation function [xi](r)  Twopoint correlation function: another definition  Twopoint correlation function: Poisson model  Threepoint correlation function  Fourpoint correlation function  Moments of counts of objects  Constraints on [xi] and [zeta]  Probability generating function  Estimates of P[subscript N]  Cluster model  Power spectrum  Power law model for the spectrum  Bispectrum  Cross correlation function  Angular twopoint correlation function  Angular power spectrum  Estimating w([theta])  Statistical uncertainty in the estimate of w([theta])  Relation between angular and spatial twopoint correlation functions  Small separation approximation and the scaling relation  Decoupling of magnitude and position  Relation between [xi] and w: some examples  Inversion of the equation  Angular threepoint correlation function  Angular fourpoint correlation function  Correction for curvature and expansion  Summary of numerical results  Power spectrum of the extragalactic light  Moments of the number of neighbors  Model for P[subscript N]  Clustering models  Continuous clustering hierarchy: Mandelbrot's prescription  The mass correlation functions  Clustering hierarchy: continuity speculation  Remarks on the observations  Dynamics and Statistics  Goals  Definitions of variables and distribution functions  BBGKY hierarchy equations  Fluid limit  Evolution of the integral of [xi]  Particle conservation equations  Relative peculiar velocity dispersion  Similarity solution  Cosmic energy equation  Cosmic virial theorem  Joint distribution in position and velocity  Behavior of the halo around a cluster of galaxies  Superclusters  Problems and prospects  Relativistic Theory of the Behavior of Irregularities in an Expanding World Model  Role of the relativistic theory  Timeorthogonal coordinates  The field equations for h[subscript alpha beta]  Gravitational waves  Newtonian approximation  Linear perturbation equations for the matter  Behavior of density perturbations at wavelength [characters not reproducible] ct  Spherical model  Evolution of acoustic waves  Nonlinear acoustic waves  Incompressible flow  Behavior of collisionless particles  Linear dissipation of adiabatic perturbations  Residual fluctuations in the microwave background  Isothermal perturbations  Scenarios  Nature of the universe at high redshift  Nature of protogalaxies and protoclusters  Models and notation
 Control code
 6421704
 Dimensions
 24 cm.
 Extent
 xiii, 422 pages
 Isbn
 9780691082394
 Lccn
 79084008
 Media category
 unmediated
 Media MARC source
 rdamedia
 Media type code

 n
 Note
 UMKC: Gift purchased by the UMKC Friends of the Library.
 Other physical details
 graphs
 System control number
 (OCoLC)6421704
 Label
 The largescale structure of the universe, by P.J.E. Peebles
 Bibliography note
 Includes bibliographical references (pages 402416) and index
 Carrier category
 volume
 Carrier category code

 nc
 Carrier MARC source
 rdacarrier
 Content category
 text
 Content type code

 txt
 Content type MARC source
 rdacontent
 Contents
 Homogeneity and Clustering  Is the universe homogeneous?  Physical principles  How did galaxies and clusters of galaxies form?  Behavior of Irregularities in the Distribution of Matter: Newtonian Approximation  Newtonian approximation  Particle dynamics in expanding coordinates  The peculiar acceleration  Two models: the Vlasov equation and the ideal fluid  Linear perturbation approximation for [delta]  Solutions for [delta](t): p = [Lambda] = 0  Solutions for [delta](t): effect of a uniform radiation background  Solutions for [delta](t): models with [Lambda not equal] 0  The peculiar velocity field  Joining conditions for [delta] and [upsilon]  Critical Jeans length  Primeval magnetic field as a source for [delta rho] / [rho]  Second order perturbation theory for [delta rho] / [rho]  Spherical model  Homogeneous ellipsoid model  Caustics and pancakes  Expansion, vorticity, and shear  Origin of the rotation of galaxies  Cosmic energy equation  Spherical accretion model  Hierarchical clustering model  Fourier transform of the equations of motion  Coupling of density fluctuations  nPoint Correlation Functions: Descriptive Statistics  Statistical measures of the galaxy distribution  Fair sample hypothesis  Twopoint spatial correlation function [xi](r)  Twopoint correlation function: another definition  Twopoint correlation function: Poisson model  Threepoint correlation function  Fourpoint correlation function  Moments of counts of objects  Constraints on [xi] and [zeta]  Probability generating function  Estimates of P[subscript N]  Cluster model  Power spectrum  Power law model for the spectrum  Bispectrum  Cross correlation function  Angular twopoint correlation function  Angular power spectrum  Estimating w([theta])  Statistical uncertainty in the estimate of w([theta])  Relation between angular and spatial twopoint correlation functions  Small separation approximation and the scaling relation  Decoupling of magnitude and position  Relation between [xi] and w: some examples  Inversion of the equation  Angular threepoint correlation function  Angular fourpoint correlation function  Correction for curvature and expansion  Summary of numerical results  Power spectrum of the extragalactic light  Moments of the number of neighbors  Model for P[subscript N]  Clustering models  Continuous clustering hierarchy: Mandelbrot's prescription  The mass correlation functions  Clustering hierarchy: continuity speculation  Remarks on the observations  Dynamics and Statistics  Goals  Definitions of variables and distribution functions  BBGKY hierarchy equations  Fluid limit  Evolution of the integral of [xi]  Particle conservation equations  Relative peculiar velocity dispersion  Similarity solution  Cosmic energy equation  Cosmic virial theorem  Joint distribution in position and velocity  Behavior of the halo around a cluster of galaxies  Superclusters  Problems and prospects  Relativistic Theory of the Behavior of Irregularities in an Expanding World Model  Role of the relativistic theory  Timeorthogonal coordinates  The field equations for h[subscript alpha beta]  Gravitational waves  Newtonian approximation  Linear perturbation equations for the matter  Behavior of density perturbations at wavelength [characters not reproducible] ct  Spherical model  Evolution of acoustic waves  Nonlinear acoustic waves  Incompressible flow  Behavior of collisionless particles  Linear dissipation of adiabatic perturbations  Residual fluctuations in the microwave background  Isothermal perturbations  Scenarios  Nature of the universe at high redshift  Nature of protogalaxies and protoclusters  Models and notation
 Control code
 6421704
 Dimensions
 24 cm.
 Extent
 xiii, 422 pages
 Isbn
 9780691082394
 Lccn
 79084008
 Media category
 unmediated
 Media MARC source
 rdamedia
 Media type code

 n
 Note
 UMKC: Gift purchased by the UMKC Friends of the Library.
 Other physical details
 graphs
 System control number
 (OCoLC)6421704
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