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Information - ST15 The structure and dynamics of a planetary foreshock region (co-listed in PS)
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Event Information |
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The foreshock region is the first signature of the interaction of the solar wind with a planet's plasma environment when approaching its bow shock. Part of its structure and dynamic is determined by instabilities, which are created by the interaction of the solar wind with backstreaming ions. Prominent examples are the field aligned ion beams, specularly reflected, and the diffusive ions which have been extensively studied in the Earth's foreshock. The interaction of these reflected ions with the solar wind drives ion/ion beam instabilities, which generate waves that are then convected towards the shock by the solar wind. Subsequently they may mediate the shock structure and its reflection properties. Ion reflection, wave excitation by instabilities, shock and foreshock dynamic show therefore a close association. However, it is very difficult to determine the source and the physical mechanism creating these ions and the associated turbulence. Over the past year recent single and multi-spacecraft observations, theoretical considerations, and numerical simulations provided new insights to which physical processes determine the nature of the foreshock region.
For this session we therefore solicit contributions, which are in the broad context of the structure and dynamic of the foreshock region of planetary bow shocks. In particular we welcome contribution from spacecraft observation at Earth but also at other planets, including e.g., recent results at Mars or obtained by Cassini at Jupiter and Saturn, as well as theory and numerical modeling.
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