Abstract
The birth and growth of cosmic structures is a highly nonlinear phenomenon that needs to be investigated with suitable numerical simulations. Themain goal of these simulations is to provide robust predictions, which, once compared to the present and future observations, allows us to constrain the main cosmological parameters. Different techniques have been proposed to follow both the gravitational interaction inside cosmological volumes and the variety of physical processes acting on the baryonic component only. In this chapter, we review the main characteristics of the numerical schemes most commonly used in the literature, discuss their pros and cons, and summarize the results of their comparison.
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Moscardini, L., Dolag, K. (2011). Cosmology with Numerical Simulations. In: Matarrese, S., Colpi, M., Gorini, V., Moschella, U. (eds) Dark Matter and Dark Energy. Astrophysics and Space Science Library, vol 370. Springer, Dordrecht. https://doi.org/10.1007/978-90-481-8685-3_4
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DOI: https://doi.org/10.1007/978-90-481-8685-3_4
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