FOR 1048: Instabilities, Turbulence and Transport in Cosmic Magnetic Fields

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Magnetic fields play a fundamental role in many astrophysical systems. This is a consequence of the fact that the latter are most often composed of a dominant plasma component. Prominent examples of cosmic magnetic fields are the solar corona and wind or the interstellar and intergalactic plasma. In many cases the kinetic energy density of the plasma and the magnetic energy density are of the same order so that neither a test particle nor a test wave description can be justified but rather a self-consistent treatment has to be developed. Subject of the Research Unit is an analysis of the profound implications of the non-negligible mutual influences for the instabilities, the turbulence and the transport processes in cosmic magnetic fields. In the foreground is a study of fundamental physical processes by analytical, numerical as well as experimental means. The results will be applied to astrophysical systems.