numerical cosmology & galaxy formation€¦ · lecture 6: hydro schemes - grid codes. outline...
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Numerical Cosmology& Galaxy Formation
1
Benjamin Moster
Lecture 6: Hydro schemes - Grid codes
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Outline of the lecture course
• Lecture 1: Motivation & Historical Overview
• Lecture 2: Review of Cosmology
• Lecture 3: Generating initial conditions
• Lecture 4: Gravity algorithms
• Lecture 5: Time integration & parallelization
• Lecture 6: Hydro schemes - Grid codes
• Lecture 7: Hydro schemes - Particle codes
• Lecture 8: Radiative cooling, photo heating
• Lecture 9: Subresolution physics
• Lecture 10: Halo and subhalo finders
• Lecture 11: Semi-analytic models
• Lecture 12: Example simulations: cosmological box & mergers
• Lecture 13: Presentations of test simulations
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Computational Cosmology
• Cosmological model + initial conditions + simulation code = galaxies
SDSSCMB
generation theinitial conditions
running the simulation
analyzingthe data
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Why hydrodynamics?
• Everything we see is gas or made from gas
• Need to follow the hydrodynamics: To form galaxies and starsTo study the interstellar, intergalactic and intracluster medium
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The Bullet cluster
5
collisionlessdark matter
collisionlessdark matter
collisional gas
Numerical Cosmology & Galaxy Formation 6 25.05.2016
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Why hydrodynamics?
• Problems are so complex that analytical methods are inadequate.
• The solution is almost always sought using numerical methods
• No single numerical recipe for all hydrodynamic problems
• Each problem may involve different additional physics: e.g. radiation-hydrodynamics or magneto-hydrodynamics
• Two broad categories: Eulerian methods (fixed position) Lagrangian methods (fixed element)
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Eulerian vs Lagrangian methods
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The Euler equations
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On the blackboard…(see scanned notes)
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The Euler equations
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• The equations of hydrodynamics can be written in terms of
conserved quantities
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Advection on a grid
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• Let’s consider a simpler problem first and assuming u = const.
• discretize space into cells for numerical treatment
• need to advect the mass such that total mass is conserved➡ calculate mass fluxes at cell interfaces➡ remove mass from the cell on one side of the interface and add it to the cell on the other side (this ensures mass conservation)
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Advection on a grid
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Advection on a grid
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• next higher order: piecewise linear within cell
•
• average density at interface over time step Δt
• Flux:
Advection on a grid
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Advection on a grid
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Advection on a grid
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• Higher order schemes, such as the piecewise linear Lax-Wendroff
scheme shown here, produce oscillations near discontinuities
• Piecewise linear elements can have overshoots
• Successful method to prevent overshoots is the use of slope limitersModify the slope if this is necessary to prevent overshoots
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Characteristics
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• With a suitable advection scheme we can solvewith u = constant
• However, the full Euler equations are coupled:
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Characteristics
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• Can we decouple these equations?First we rewrite them (for simplicity in 1D) by defining:
• We then get
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Characteristics
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• The Euler equations in terms of q1,q2,q3 are then given by with
• Can be written more compact using the Jacobian
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Characteristics
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• Consider a simple system with A(q) = A = constant We get:
• The equations can then be decoupled by finding the eigensystem of
the matrix A
• Decompose the state q in the eigenbasisand find the equations for the individual components
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Characteristics
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• Using this decomposition with
• And therefore
• This is a simple advection equation with characteristic velocity λm
• We can thus solve the coupled set of equations by expanding the state vector in the eigenbasisadvecting each qm with its characteristic velocity recomputing the new state from the updated
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Characteristics
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• Each of these modes propagating with a characteristic velocity is
called a characteristic
• For the full Euler equations A(q) ≠ constant➙ eigenvectors depend on q (and thus position) ➙ no global decomposition of the state vector possible
• Locally we find:
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Characteristics
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• Decompose the state vector locally at each cell interface and advect
the components with their local characteristic velocities
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Riemann problems
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• What about shocks and contact discontinuities?➙ eigensystems differ significantly on both sides
• Consider the full Riemann problem e.g. for uL = uR = 0
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Riemann problems
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• Solutions are self-similar, i.e. they depend only on
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Godunov method
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• Assume piecewise constant fluid state
• Exactly solve Riemann problem at each interface(i.e. solve algebraic equations iteratively)
• Choose small enough time step, such that solutions of neighboring interfaces do not overlap
• Calculate new average of conserved quantities at end of time step
• Easy as flux f(q(x=x0)) is constant for self-similar q((x−x0)/(t−t0))
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Godunov method
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• Assume piecewise constant fluid state
• Exactly solve Riemann problem at each interface(i.e. solve algebraic equations iteratively)
• Choose small enough time step, such that solutions of neighboring interfaces do not overlap
• Calculate new average of conserved quantities at end of time step
• Easy as flux f(q(x=x0)) is constant for self-similar q((x−x0)/(t−t0))
For linear problems: same as advecting the components in the eigenbasis
But accounts for shocks and contact discontinuities
Cons: Diffusive as constant fluxes correspond to donor-cell advection
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The MUSCL-Hancock scheme
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• Create a 2nd order Godunov method by
- using a higher-order reconstruction(piecewise linear, piecewise parabolic)
- computing the left and right q values at the interface
- advance these values in half a time step
- use these values in the Riemann solver as if the state is constant on each side of the interface
- • used in many codes, e.g.: Ramses, Arepo
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Roe’s linearized Riemann solver
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• Exact Riemann solvers can be slow (e.g. for magneto-hydrodynamics)
• Alternatively linearise the problem at each interface by settingA(q) → A(qave) with qave: average value between left and right state
• A solution can then be found by decomposing the left and right
states into the eigenbasis of A(qave)
• And advecting the components with the corresponding characteristic
velocity➡ yields a solution in smooth parts of the flow ➡ every reasonable average value for qave should work there
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Roe’s linearized Riemann solver
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• It is possible to choose the average qave such that the linearized
Riemann solver also gives the correct propagation of contact
discontinuities and shocks
• Roe average:
• When using this average one can show that the “jump” corresponds
exactly to one eigenvector with a eigenvalue given by the correct
velocity (e.g. the shock velocity).
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Adaptive mesh refinement
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• In AMR the local resolution is adapted according to refinement
criteria (usually high density)
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Adaptive mesh refinement
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• In AMR the local resolution is adapted according to refinement
criteria (usually high density)
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Adaptive mesh refinement
29 Numerical Cosmology & Galaxy Formation 6 25.05.2016
• In AMR the local resolution is adapted according to refinement
criteria (usually high density)
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Moving-mesh hydrodynamics
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• Alternatively one can define a mesh based on a set of points using a Voronoi tessellation
• Points can be allowed to move, e.g. with the fluid ➙ then almost Lagrangian
• Procedure: use unspilt scheme transform to frame of moving interfacesolve Riemann problemtransform back
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Moving-mesh hydrodynamics
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Moving-mesh hydrodynamics
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Eulerian vs Lagrangian methods
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Eulerian vs Lagrangian methods
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Pros: accurate hydro, automatic automatic refinement on accurate hydro refinement on density, density, Galilean invar., Galilean invariant conserves angular mom.
Cons:needs AMR to overhead (~30%) for Often problems with get to high mesh construction contact discontinuities resolution slow convergence
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Up next
• Lecture 1: Motivation & Historical Overview
• Lecture 2: Review of Cosmology
• Lecture 3: Generating initial conditions
• Lecture 4: Gravity algorithms
• Lecture 5: Time integration & parallelization
• Lecture 6: Hydro schemes - Grid codes
• Lecture 7: Hydro schemes - Particle codes
• Lecture 8: Radiative cooling, photo heating
• Lecture 9: Subresolution physics
• Lecture 10: Halo and subhalo finders
• Lecture 11: Semi-analytic models
• Lecture 12: Example simulations: cosmological box & mergers
• Lecture 13: Presentations of test simulations
34 Numerical Cosmology & Galaxy Formation 6 25.05.2016