
Contents
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1. Homogeneity and Clustering 1. Homogeneity and Clustering
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2. Is the Universe Homogeneous? 2. Is the Universe Homogeneous?
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3. Physical Principles 3. Physical Principles
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A. Prediction of homogeneity? A. Prediction of homogeneity?
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B. The cosmological principle B. The cosmological principle
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C. The instability of the universe C. The instability of the universe
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4. How did Galaxies and Clusters of Galaxies Form? 4. How did Galaxies and Clusters of Galaxies Form?
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A. The role of gravity A. The role of gravity
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B. Clustering without preferred quantities B. Clustering without preferred quantities
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C. Cosmological parameters, fluid dynamics, and the primeval fireball C. Cosmological parameters, fluid dynamics, and the primeval fireball
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D. Primeval turbulence D. Primeval turbulence
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E. Alternative scenarios E. Alternative scenarios
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5. Summary 5. Summary
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I. Homogeneity and Clustering
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Published:September 2020
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Abstract
This chapter traces the history of the development of ideas on the large-scale structure of the universe. Modern discussions of the nature of the large-scale matter distribution can be traced back to three central ideas. In 1917, Albert Einstein argued that a closed homogeneous world model fits very well into general relativity theory and the requirements of Mach's principle. In 1926, Edwin Hubble showed that the large-scale distribution of galaxies is close to uniform with no indication of an edge or boundary. In 1927, Georges Lemaître showed that the uniform distribution of galaxies fits very well with the pattern of galaxy redshifts. The chapter then assesses several questions. The first is whether the universe really is homogeneous. Could the homogeneity of the universe have been deduced ahead of time from general principles? Or might it be a useful guide to new principles? It also asks how clustering evolves in an expanding universe, what its origin is, and what this reveals about the nature of the universe.
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