Welcome

• Maria Elena Innocenti (Ruhr University Bochum)

Introductory talk: Solar physics and space weather simulations

• Stefaan Poedts (University of Leuven)

MHD /1

• Jürgen Dreher

The MHD model of plasmas will be reviewed. Fundamental Finite-Difference schemes and a generic and robust Finite-Volume scheme for time-dependent fluid computations will be discussed.

MHD/ 2

• Jürgen Dreher

The MHD model of plasmas will be reviewed. Fundamental Finite-Difference schemes and a generic and robust Finite-Volume scheme for time-dependent fluid computations will be discussed.

Fluid/ MHD: Hands on exercises

• Rainer Grauer
• Jürgen Dreher

Explicit Particle-In-Cell

• Jérémy Dargent

In this lecture, we will introduce the Particle-In-Cell method, which consists into the coupling of a kinetic description of the plasma (macroparticles) with the projection on a grid of the fields, and develop the most basic method to implement it, e.g. the explicit description.

Implicit Particle-In-Cell

• Maria Elena Innocenti

In this lecture, we will introduce (semi-)implicit Particle-In-Cell methods, where the equations for the temporal update of fields and particles are discretised semi-implicitly. We will discuss how the increased algorithmic burden pays off in terms of relaxed stability constraints.

PIC: Hands on exercises

• Maria Elena Innocenti
• Jérémy Dargent

Finite elements and structure preserving Particle-In-Cell

• Katharina Kormann (Ruhr University Bochum)

In this lecture, we will introduce the framework of finite element exterior calculus which consists of a special type of finite elements that are adapted to the structure of Maxwell's equations and apply those to derive a structure-preserving particle-in-cell code of high accuracy order.

Relativistic Particle-In-Cell

• Kevin Schoeffler

Here we will explore how fully relativistic effects can be taken into account in the Particle-In-Cell method, take a look at several applications where that can take advantage of this such as systems with energetic non-thermal tails or plasmas in extreme conditions, and consider the differences between explicit and implicit implementations.

Particle In Cell: Hands on exercises

• Alfredo Micera
• Kevin Schoeffler

MuPhy: MultiPhysics framework

• Simon Lautenbach (University of Texas at Austin)

Collsionless astrophysical and space plasmas cover regions that typically display a separation of scales that exceeds any code's capabilities.The muphyII code utilizes a hierarchy of models with different inherent scales, unified in an adaptive framework that allows stand-alone use of models as well as a model-based dynamic and adaptive domain decomposition.This requires careful treatment of inner-domain model boundaries for model coupling, and robust time stepping algorithms, especially with the use of electron subcycling.

Turbulence and cosmic rays

• Rainer Grauer
• Horst Fichtner

Cosmic rays are important messengers providing information about various remote astrophysical systems. Therefore, it is of high interest to understand the transport of these high energetic particles in the turbulent plasma environments they traverse. Contemporary models of cosmic ray transport processes will be discussed along with strategies to model the turbulence that is determining the latter.

Cosmic ray propagation in turbulent fields: Hands on exercises

• Frederic Effenberger
• Jeremiah Lübke

We introduce a full-orbit test particle code that can propagate a large number of energetic particles in synthetic turbulence. Special emphasis is put on the turbulence geometry as either an isotropic or slab-2D composite model. Statistical analysis will be performed to determine the diffusion coefficients for different particle energies.

MuPhy: Hands on exercises

• Simon Lautenbach (University of Texas at Austin)
• Rainer Grauer

Cosmic rays propagation: CRPropa

• Sophie Aerdker

CRPropa is a modular open source cosmic-ray propagation framework. Particle transport can be treated in the single particle picture by solving the equation of motion or in an ensemble averaged approach, solving stochastic differential equations. Together with the implementation of all relevant loss processes and secondary production channels it forms a powerful tool to model cosmic rays and other messengers from GeV up to ZeV energies. In this lecture we will present the underlying concept of the Monte Carlo code and discuss some recent applications of the code to diffusive shock acceleration (DSA) and how it helped to distinguish the transport mode in the face-on galaxy M51. During the exercise you will learn how to set up and run different simulation from cosmogenic neutrino production to particle acceleration.

CRPropa: Hands on exercises

• Sophie Aerdker
• Julien Dörner