Statistics – Computation
Scientific paper
Jan 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994phdt........15g&link_type=abstract
PhD Dissertation, Princeton Univ. NJ United States
Statistics
Computation
Cosmology, Dark Matter, Computational Grids, Lagrangian Function, Hydrodynamics, Cosmic Gases, Galaxies, Astronomical Models, Background Radiation, Time Dependence, Radiation Distribution, Computerized Simulation, Spatial Distribution, Galactic Evolution
Scientific paper
The evolution of the cosmological model that incorporates the cold dark matter and the cosmological constant (CDM + lambda) is studied numerically utilizing a highly developed numerical code. The numerical scheme is based on a new method in cosmological hydrodynamics that is called 'Softened Lagrangian Hydrodynamics' (or SLH). The SLH method is grid based like Eulerian methods and so allows numerical equations to be written in conservation form and can resolve shocks accurately. But the grid points move with the fluid (hence 'Lagrangian') except when doing so would incur a large numerical overhead due to excessive twisting or compression of cells; in such regions the code reverts to an Eulerian scheme (hence 'softened'). The derivation and development of the SLH method are presented in chapter 1, with the emphasis on detail testing of the code and comparing the SLH approach with other existing methods in cosmological hydrodynamics. The extensive tests show that the SLH approach outperforms other existing approaches in resolving hydrodynamic caustics, that are possible sites for galaxy formation. In chapter 2 methods for accurate simulating of all important radiative processes in cosmology including the time-dependent evolution of the background radiation field are incorporated into the code; besides, the galaxy formation algorithm based on solving virial equations for a fluid element is introduced to supplement the code. The code is then applied to study the galaxy formation process in the CDM + lambda cosmological model. Physical properties of radiation field, the cosmic gas and simulated galaxies and their cosmological evolution are discussed at length. Finally, chapter 3 considers the spatial distributions of the dark matter, the cosmic gas and the galaxies, and relationships between these distributions (i.e. biases) are quantified and discussed in full detail.
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