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Förslaget inkom 2011-10-06

Modelling of asymmetric solar wind-magnetosphere coupling

OBS! ANSÖKNINGSTIDEN FÖR DETTA EXJOBB HAR LÖPT UT.
The sun continuously emits a flow of plasma (ionized gas), which is called the solar wind. The solar wind also carries with it a magnetic field of solar origin, which is called the interplanetary magnetic field (IMF), at larger distances from the sun. When the solar wind encounters the region in space close to Earth, it interacts with the geomagnetic field, creating the region called the magnetosphere. This interaction can be modeled by several different methods, e.g. magnetohydrodynamics or kinetic theory. Of particular interest is to model how the IMF connects to the geomagnetic field. Here a simple superposition of the two fields can give a rough understanding of the interaction.

In models of the coupling between the solar wind plasma and magnetic field and the geomagnetic field, it is usually assumed that the variations in the solar wind are negligible on the scale of the magnetosphere. Therefore the solar wind parameters, including the IMF are taken to be constant at any given time. However, new results from the Cluster spacecraft indicate that at times the variations of the solar wind parameters can be of the order of the magnetosphere, or even smaller.

The goal of this thesis work is to model the interaction between the magnetosphere and the IMF, when the IMF varies over the magnetosphere. A simple superposition model of an existing magnetospheric model (the Tsyganenko model), and a non-uniform IMF will be used. Consequences for the magnetospheric topology, including the resulting position of the auroral zones, will be investigated.

It is important that the student has a good background in programming, in e.g. MATLAB.

Tutors: Tomas Karlsson, Anita Kullen


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