The extent of dynamical processes in the lower atmosphere of the Sun during solar flares is not fully understood. While it is widely accepted that the majority of the associated flare energy is deposited in the Sun's chromosphere, it is less clear how this energy is transported and how it influences the configuration of material flows. Current models of chromospheric evaporation and condensation assume an upwards expulsion of high-temperature plasma, with an accompanying downwards flow at cooler temperatures. In this thesis, the validity of these assumptions are tested using a combination of observations and modelling, with particular focus given to the Lyman lines of hydrogen.
| Identifer | oai:union.ndltd.org:bl.uk/oai:ethos.bl.uk:768729 |
| Date | January 2019 |
| Creators | Brown, Stephen Alistair |
| Publisher | University of Glasgow |
| Source Sets | Ethos UK |
| Detected Language | English |
| Type | Electronic Thesis or Dissertation |
| Source | http://theses.gla.ac.uk/40974/ |
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