Cosmology's century an inside history of our modern understanding of the Universe

Cosmology's century an inside history of our modern understanding of the Universe

Bibliographic Details
Main Author: Peebles, P. J. E. (Phillip James Edwin)
Format: eBook
Language:English
Published: Princeton Princeton University Press, 2020.
Subjects:
Cosmology > History.
EBSCO eBooks
Online Access:https://www.lib.tsu.ru/mminfo/2023/EBSCO/2324244.pdf
Table of Contents:
  • Cover
  • Contents
  • Preface and Acknowledgments
  • CHAPTER 1. Introduction
  • 1.1 The Science and Philosophy of Cosmology
  • 1.2 An Overview
  • CHAPTER 2. The Homogeneous Universe
  • 2.1 Einstein's Cosmological Principle
  • 2.2 Early Evidence of Inhomogeneity
  • 2.3 Early Evidence of Homogeneity: Isotropy
  • 2.4 Early Evidence of Homogeneity: Counts and Redshifts
  • 2.5 The Universe as a Stationary Random Process
  • 2.6 A Fractal Universe
  • 2.7 Concluding Remarks
  • CHAPTER 3. Cosmological Models
  • 3.1 Discovery of the Relativistic Expanding Universe
  • 3.2 The Relativistic Big Bang Cosmology
  • 3.3 The Steady-State Cosmology
  • 3.4 Empirical Assessments of the Steady-State Cosmology
  • 3.5 Nonempirical Assessments of the Big Bang Model
  • 3.5.1 Early Thinking
  • 3.5.2 Cosmological Inflation
  • 3.5.3 Biasing
  • 3.6 Empirical Assessments of the Big Bang Model
  • 3.6.1 Time Scales
  • 3.6.2 Cosmological Tests in the 1970s
  • 3.6.3 Mass Density Measurements: Introduction
  • 3.6.4 Mass Density Measurements: Hubble to the Revolution
  • 3.6.5 Mass Density Measurements: Assessments
  • 3.7 Concluding Remarks
  • CHAPTER 4. Fossils: Microwave Radiation and Light Elements
  • 4.1 Thermal Radiation in an Expanding Universe
  • 4.2 Gamow's Scenario
  • 4.2.1 Gamow's 1948 Papers
  • 4.2.2 Predicting the Present CMB Temperature
  • 4.2.3 The Alpher, Bethe, and Gamow Paper
  • 4.3 Helium and Deuterium from the Hot Big Bang
  • 4.3.1 Recognition of Fossil Helium
  • 4.3.2 Helium in a Cold Universe
  • 4.3.3 Developments in 1964 and 1965
  • 4.4 Sources of Microwave Radiation
  • 4.4.1 Interstellar Cyanogen
  • 4.4.2 Detection at Bell Laboratories
  • 4.4.3 Zel'dovich's Group
  • 4.4.4 Dicke's Group
  • 4.4.5 Recognition of the CMB
  • 4.5 Measuring the CMB Intensity Spectrum
  • 4.5.1 The Situation in the 1970s
  • 4.5.2 Alternative Interpretations
  • 4.5.3 The Submillimeter Anomalies
  • 4.5.4 Establishing the CMB Thermal Spectrum
  • 4.6 Nucleosynthesis and the Baryon Mass Density
  • 4.7 Why Was the Hot Big Bang Cosmology Reinvented?
  • CHAPTER 5. How Cosmic Structure Grew
  • 5.1 The Gravitational Instability Picture
  • 5.1.1 Lemaître's Solution
  • 5.1.2 Lifshitz's Perturbation Analyses
  • 5.1.3 Nongravitational Interaction of Baryons and the CMB
  • 5.1.4 The Jeans Mass
  • 5.2 Scenarios
  • 5.2.1 Chaos and Order
  • 5.2.2 Primeval Turbulence
  • 5.2.3 Gravitational Origin of Galaxy Rotation
  • 5.2.4 Explosions
  • 5.2.5 Spontaneously Broken Homogeneity
  • 5.2.6 Initial Conditions
  • 5.2.7 Bottom-Up or Top-Down Structure Formation
  • 5.3 Concluding Remarks
  • CHAPTER 6. Subluminal Mass
  • 6.1 Clusters of Galaxies
  • 6.2 Groups of Galaxies
  • 6.3 Galaxy Rotation Curves
  • 6.3.1 The Andromeda Nebula
  • 6.3.2 NGC 311525
  • 6.3.3 NGC 300
  • 6.3.4 NGC 2403
  • 6.3.5 The Burbidges's Program
  • 6.3.6 Challenges
  • 6.4 Stabilizing Spiral Galaxies
  • 6.5 Recognizing Subluminal Matter

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