The solar wind blows a bubble into the interstellar space which we call heliosphere. The physical properties of this bubble are primarily determined by the density and velocity of particles forming the solar wind, as well as the magnetic field frozen into the plasma. With the analysis of measurements by space probes we investigate the spatial and temporal variations of the solar wind and magnetic flux. We demonstrate the diverse properties of the fast and slow solar wind. Investigated also is the variations of the magnetic flux frozen into the solar wind in association with the solar cycle, including the polarity reversal of the solar magnetic field. We also touch the formation of structures related to coronal mass ejections and co-rotating fast solar wind streams, which is of importance from the point of view of geoeffectivity.
|Translated title of the contribution||Three-dimensional structure of the heliosphere|
|Number of pages||6|
|Publication status||Published - Dec 1 2012|
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