Files in this item
The nonuniform magnetohydrodynamic nature of the solar atmosphere
Item metadata
dc.contributor.advisor | Priest, E. R. (Eric Ronald) | |
dc.contributor.author | De Ville, Andrew | |
dc.coverage.spatial | 214 p. | en_US |
dc.date.accessioned | 2018-06-14T13:47:57Z | |
dc.date.available | 2018-06-14T13:47:57Z | |
dc.date.issued | 1991 | |
dc.identifier.uri | https://hdl.handle.net/10023/14073 | |
dc.description.abstract | The nonuniform structure observed in the solar atmosphere, and in particular the corona, is thought to arise due to the interaction between the magnetic field and plasma. Using a linear theory, the nature of these interactions is investigated, and it is shown how coronal structure may be modelled in a simple way by extended standing disturbances. The effect of inertial forces in considered in both a Cartesian and cylindrical geometries, and a first correction due to gravity is calculated. The restrictions of a linear theory may be overcome by finding exact solutions. Solutions are presented which may model plasma flows in closed, partially open and open magnetic field line structures. A new method for finding particular classes of exact steady solutions in a gravitationally stratified, isothermal atmosphere is presented, along with some examples of possible solutions. | en_US |
dc.language.iso | en | en_US |
dc.publisher | University of St Andrews | en |
dc.subject.lcc | QA927.D3V5 | |
dc.subject.lcsh | Magnetohydrodynamics | en |
dc.title | The nonuniform magnetohydrodynamic nature of the solar atmosphere | en_US |
dc.type | Thesis | en_US |
dc.type.qualificationlevel | Doctoral | en_US |
dc.type.qualificationname | PhD Doctor of Philosophy | en_US |
dc.publisher.institution | The University of St Andrews | en_US |
This item appears in the following Collection(s)
Items in the St Andrews Research Repository are protected by copyright, with all rights reserved, unless otherwise indicated.