Monday, 07/24: Writing a pm-code - AIP

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equations summary 9 Cosmological simulations: equations summary • Equations of particle motion, the Poisson equation, the equations of gasdynamics above, along with the equation of state of the gas, form the set of basic equations solved in cosmological simulations: dx dt = u, du dt = −∇Φ ∇ 2 Φ = 4πGρ tot . ∂E ∂t ∂u ∂t ∂ρ ∂t + ∇ρu = 0, + (u · ∇)u = −∇Φ − ∇P ρ , + ∇ · [(E + P )u] = −ρu · ∇Φ, ε = f(ρ, P ).
equations summary 10 • Baryonic gas and dark matter are coupled by gravity, as they are both influenced by the same gravitational potential and they both contribute to the density in the Poisson equation. • Note that all of the equations we solve to describe the evolution of matter in the universe have their usual simple non-relativistic form. This is because most commonly the matter components relevant for late evolution move with non-relativistic velocities.
Page 1 and 2: Writing a PM code Andrey Kravtsov a
Page 3 and 4: equations I 2 Cosmological simulati
Page 5 and 6: N-body approach 4 Cosmological simu
Page 7 and 8: particle initial conditions 6 Cosmo
Page 9: equations of gasdynamics 8 Cosmolog
Page 13 and 14: dissipationless simulations 12 Part
Page 15 and 16: Model equations 14 Model equations
Page 17 and 18: Model equations 16 The quantities w
Page 19 and 20: Model equations 18 In dimensionless
Page 21 and 22: PM: main code blocks 20 Density Ass
Page 23 and 24: PM: main code blocks 22 In practice
Page 25 and 26: PM: main code blocks 24 Implementin
Page 27 and 28: PM: main code blocks 26 Solving the
Page 29 and 30: PM: main code blocks 28 ⇒ Given a
Page 31 and 32: PM: main code blocks 30 After n tim
Page 33 and 34: Zeldovich approximation (ZA) 32 Zel
Page 35 and 36: A test problem: 1D collapse of a pl
Page 41 and 42: Setting up cosmological ICs 40 The
Page 43 and 44: Setting up cosmological ICs 42 Appl
Page 45 and 46: project summary 44 Project summary
Page 47 and 48: References and links 46 PM in cosmo
Page 49 and 50: References and links 48 • Michael

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