Numerical simulation for cosmological fluid flows

Details Numerical simulation for cosmological fluid flows Numerical simulation for cosmological fluid flows

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...257..425d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 257, no. 2, p. 425-433.

Statistics

Computation

3

Computational Astrophysics, Computational Fluid Dynamics, Computerized Simulation, Cosmology, Space-Time Functions, Gravitational Collapse, Magnetohydrodynamics, Nuclear Fusion, Perturbation, Radiative Transfer, Thomson Scattering

Scientific paper

We describe a hydrodynamical simulation of the evolution of cosmological perturbations throughout recombination up to gravitational collapse. The cosmological model is the standard one with different values of the density parameter Omega0 and a nonbaryonic component. We follow the evolution of the mixture of radiation and matter by solving the radiation transfer and hydrodynamical equations. Thomson scattering is here the dominating process and we use a formalism close to the one proposed by Hsieh & Spiegel (1976). This fully nonlinear code allows us to give a coherent description from the initial prerecombination conditions until the formation of the first nonlinear gravitational objects, and shows the behavior of shocks before recombination.

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