
Contents
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11.1 Cosmological simulations 11.1 Cosmological simulations
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11.1.1 General context 11.1.1 General context
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11.1.2 Periodic universes versus zoomed-in haloes 11.1.2 Periodic universes versus zoomed-in haloes
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11.1.3 Cosmological initial conditions 11.1.3 Cosmological initial conditions
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11.2 Dark matter as a collisionless fluid 11.2 Dark matter as a collisionless fluid
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11.2.1 The Vlasov–Poisson equations 11.2.1 The Vlasov–Poisson equations
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11.2.2 N-body techniques 11.2.2 N-body techniques
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11.2.3 Tree codes 11.2.3 Tree codes
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11.2.4 Adaptive particle–mesh 11.2.4 Adaptive particle–mesh
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11.3 High-performance computing 11.3 High-performance computing
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11.3.1 Moore’s law versus new algorithms 11.3.1 Moore’s law versus new algorithms
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11.3.2 Massively parallel computing 11.3.2 Massively parallel computing
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11.3.3 Towards exascale computing? 11.3.3 Towards exascale computing?
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11.4 Baryons as a collisional fluid 11.4 Baryons as a collisional fluid
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11.4.1 The Euler–Poisson equations 11.4.1 The Euler–Poisson equations
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11.4.2 Computational fluid dynamics 11.4.2 Computational fluid dynamics
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11.4.3 Radiative processes 11.4.3 Radiative processes
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11.4.4 Coupling radiation to hydrodynamics 11.4.4 Coupling radiation to hydrodynamics
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11.4.5 Radiative transfer techniques 11.4.5 Radiative transfer techniques
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11.5 Galaxy formation physics 11.5 Galaxy formation physics
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11.5.1 Star formation and stellar feedback 11.5.1 Star formation and stellar feedback
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11.5.2 Supermassive black hole feedback 11.5.2 Supermassive black hole feedback
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11.6 Beyond Planck: precision computational cosmology 11.6 Beyond Planck: precision computational cosmology
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11.6.1 Accuracy of N-body techniques 11.6.1 Accuracy of N-body techniques
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11.6.2 Modified gravity models 11.6.2 Modified gravity models
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11.6.3 The impact of baryons 11.6.3 The impact of baryons
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References References
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11 Computational cosmology
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Published:February 2015
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Abstract
This chapter gives an introduction to the main concepts of computational cosmology. It describes the equations governing the nonlinear dynamics of self-gravitating fluids evolving in the expanding universe, namely dark matter, baryons, and radiation. While the first of these is modelled using N-body techniques, the other two can be simulated using traditional fluid solvers. Basic numerical techniques are introduced and their limitations are discussed. The goal is to familiarize the reader with the terminology of computational cosmology, and to give insight into the strengths and weaknesses of cosmological simulations. Finally, the chapter discusses the future role of computational cosmology in the post-Planck era of high-precision cosmology.
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