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Cosmic strings and the formation of galaxies and clusters of galaxies
Physical Review D, 1986As many speakers have discussed at this meeting, recent observations of the universe on very large scales have revealed a great deal of structure. Large voids, filaments and sheets with dimensions of 50-100 h-1Mpc stand out in the observed distribution of galaxies. Rich clusters of galaxies are significantly clumped on scales of at least 100 h-1Mpc.
, Turok, , Brandenberger
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Galaxy Manifolds and Galaxy Formation
1992We are witnessing the emergence of a physical classification of galaxies. New methods of inquiry, including multivariate statistical analysis of galaxy manifolds, scaling laws and correlations provide important clues towards understanding the formative mechanisms and evolutionary histories of galaxies.
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New Astronomy Reviews, 2001
Abstract The basic framework for a successful theory of large-scale structure is provided by the cold dark matter hypothesis. It works surprisingly well, and has led to predictions, such as the clustering of gas and galaxies as a function of redshift, that have been observationally tested.
Joseph Silk, Rychard Bouwens
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Abstract The basic framework for a successful theory of large-scale structure is provided by the cold dark matter hypothesis. It works surprisingly well, and has led to predictions, such as the clustering of gas and galaxies as a function of redshift, that have been observationally tested.
Joseph Silk, Rychard Bouwens
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1987
The formation of galaxies from density perturbations is discussed, and it is shown that the Galaxy could have grown from a typical isolated peak in the now-fashionable “cold dark matter” model; most of its properties are correctly predicted by such a model.
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The formation of galaxies from density perturbations is discussed, and it is shown that the Galaxy could have grown from a typical isolated peak in the now-fashionable “cold dark matter” model; most of its properties are correctly predicted by such a model.
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Symposium - International Astronomical Union, 1967
From observations it is deduced that the disk and halo were formed about the same time and that most of the previously gaseous Galaxy became stars then. Dimensional analysis indicates that the flattening of a galaxy is related to its energy,E, angular momentum,H, and mass,M, by the dimensionless number - 2EH2/G5M5.
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From observations it is deduced that the disk and halo were formed about the same time and that most of the previously gaseous Galaxy became stars then. Dimensional analysis indicates that the flattening of a galaxy is related to its energy,E, angular momentum,H, and mass,M, by the dimensionless number - 2EH2/G5M5.
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2011
In the hierarchical model, small galaxies form first and merge together into more massive objects. In addition, numerical simulations recently emphasized the role of smooth gas accretion. Using state-of-the-art cosmological hydrodynamical multi-zoom simulations, we studied the formation and evolution of galaxies in a dense environment.
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In the hierarchical model, small galaxies form first and merge together into more massive objects. In addition, numerical simulations recently emphasized the role of smooth gas accretion. Using state-of-the-art cosmological hydrodynamical multi-zoom simulations, we studied the formation and evolution of galaxies in a dense environment.
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