COMPUTATIONAL METHODS IN COSMOLOGY

Although the formation of the structures in the universe is mainly driven by large scale gravitational instabilities, our understanding of the evolution of galaxies and galaxy clusters is tightly coupled to the complex galaxy formation physics, which is highly non-linear and where various aspects still are poorly understood. Therefore advanced computer simulations with large dynamical range have to be performed, following simultaneously various physical processes across different scales. This series of lectures will give insight into modern numerical simulation techniques. The hands on tutorials will provide a first hand experience in the simple numerical challenges inherited in simulation n-body systems.

• Chapter I (90 min, Notes):
  Methods for Cosmological Simulations (N-Body/Hydro/Initial-conditions)
• Chapter II (90 min, Notes):
  Numerical Treatment of Physical Processes (Star-Formation and Black-Holes, Magnetic-Fields, Transport-Processes)
• Hands on I (90 min, Details):
  Numerical Integration (Euler and Leapfrog)
• Hands on II (90 min, Details):
  Treating N-Bodies (Central potential and self-gravity)

Literature:

• Simulation Techniques for Cosmological Simulations, Space Science Review, Dolag et al. 2009a
• Non-Thermal Processes in Cosmological Simulations, Space Science Review, Dolag et al. 2009b
• See also Volume 2 of The Encyclopedia of Cosmology, especially Chapter 3 and Chapter 9
• The hands on tutorials are based on the Gravitational Dynamics lecture at LMU

Hands On preparation