This thesis describes, with results to date, the establishment of a continuing programme of investigations into the nature of the solar coronal plasma. The diagnostic technique is that of measurement of optical emission lines in the x-ray, 1-25 u, region. The first chapter discusses the current state of knowledge of some of the properties of the corona, and chapter 2. examines the potential capabilities, and limitations, of x-ray measurement methods for study of coronal problems. A Bragg spectrometric technique is systematically selected in chapter 3. as an optimum measurement method, and a derivation of the necessary equations to describe the operation of the chosen equipment design is given. The properties and selection of Bragg analyser crystals are discussed in chapter 4. The next two chapters present the results and interpretation of the first two sets of observations, and the final chapter presents the current status of the programme. Results of more recent observations are presented and the objectives are discussed of new observations to be made towards the end of 1970. The work described has established a routine capability for the measurement of dozens of emission lines from spatially resolved regions of the solar corona, and has developed methods for characterising those regions of the plasma in terms of particle temperatures, number densities and elemental composition. New observing equipment, at present in preparation, will refine this characterisation by providing improved spatial definition, improved absolute energy flux calibration and adequate resolution to yield true line spectral profiles.
| Identifer | oai:union.ndltd.org:bl.uk/oai:ethos.bl.uk:674006 |
| Date | January 1970 |
| Creators | Evans, Kenton D. |
| Publisher | University of Leicester |
| Source Sets | Ethos UK |
| Detected Language | English |
| Type | Electronic Thesis or Dissertation |
| Source | http://hdl.handle.net/2381/35881 |
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