Rapid changes in relative helium abundance in solar wind are often attributed to the flux tube crossings - thus between solar wind streams coming from different parts of the solar corona. Recent studies however show, that the changes in relative helium abundance are not always correlated with changes in other parameters and therefore the relative helium abundance could be changed even during the propagation of solar wind inside a flux tube. The topic of this thesis is an analysis of rapid changes of solar wind parameters and their mutual connection. Using a multipoint (we use data from the SPEKTR-R, WIND and the THEMIS spacecraft) case study of interplanetary shocks, we show that a possible explanation of those changes could be a magnetosonic instability excited by the differential flow between helium and proton populations.
| Identifer | oai:union.ndltd.org:nusl.cz/oai:invenio.nusl.cz:331730 |
| Date | January 2015 |
| Creators | Cagaš, Petr |
| Contributors | Šafránková, Jana, Vandas, Marek |
| Source Sets | Czech ETDs |
| Language | Czech |
| Detected Language | English |
| Type | info:eu-repo/semantics/masterThesis |
| Rights | info:eu-repo/semantics/restrictedAccess |
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