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Förslaget inkom 2009-08-06

Evolution of the ionospheric convection pattern

OBS! ANSÖKNINGSTIDEN FÖR DETTA EXJOBB HAR LÖPT UT.
The magnetosphere is a very dynamic system, driven by the solar wind flow past the Earth. When the solar wind magnetic field is southward, field lines with one end connected earth and one to the interplanetary magnetic field are created on the dayside of the magnetosphere through the process of magnetic reconnection. These field lines then convect tailward with the solar wind flow, and eventually reconnected in the magnetotail to form closed terrestrial field lines. This reconnection can either take place at a steady rate or impulsively in the form of substorms.

For steady solar wind conditions, the measured potential drop over the ionospheric polar cap, the cross-polar cap potential, can in general be viewed as a linear function of the solar wind electric field or other similar solar wind coupling functions. This however requires that the dayside and nightside reconnection are more or less in balance. The project aim is to investigate how the ionosphere responds to a southward turning of the interplanetary magnetic field, before it reaches steady state. The relation between the cross-polar cap potential and the solar wind behavior will be investigated, in order to estimate the balance between the dayside and nightside reconnection and the development of stable ionospheric convection patterns. The project will mainly use data from the DMSP F13 satellite, with the possible addition of data from global magnetospheric simulation models.

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