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dc.contributor.advisorHood, Alan W.
dc.contributor.authorMacTaggart, David
dc.coverage.spatial142en_US
dc.date.accessioned2011-03-17T11:47:52Z
dc.date.available2011-03-17T11:47:52Z
dc.date.issued2011
dc.identifier.urihttp://hdl.handle.net/10023/1692
dc.description.abstractMagnetic flux emergence is the subject of how magnetic fields from the solar interior can rise and expand into the atmosphere to produce active regions. It is the link that joins dynamics in the convection zone with dynamics in the atmosphere. In this thesis, we study many aspects of magnetic flux emergence through mathematical modelling and computer simulations. Our primary aim is to understand the key physical processes that lie behind emergence. The first chapter introduces flux emergence and the theoretical framework, magnetohydrodynamics (MHD), that describes it. In the second chapter, we discuss the numerical techniques used to solve the highly non-linear problems that arise from flux emergence. The third chapter summarizes the current literature. In the fourth chapter, we consider how changing the geometry and parameter values of the initial magnetic field can affect the dynamic evolution of the emerging magnetic field. For an initial toroidal magnetic field, it is found that its axis can emerge to the corona if the tube’s initial field strength is large enough. The fifth chapter describes how flux emergence models can produce large-scale solar eruptions. A 2.5D model of the breakout model, using only dynamic flux emergence, fails to produce any large scale eruptions. A 3D model of toroidal emergence with an overlying magnetic field does, however, produce multiple large-scale eruptions and the form of these is related to the breakout model. The sixth chapter is concerned with signatures of flux emergence and how to identify emerging twisted magnetic structures correctly. Here, a flux emergence model produces signatures found in observations. The signatures from the model, however, have different underlying physical mechanisms to the original interpretations of the observations. The thesis concludes with some final thoughts on current trends in theoretical magnetic flux emergence and possible future directions.en_US
dc.language.isoenen_US
dc.publisherUniversity of St Andrews
dc.subjectMagnetohydrodynamicsen_US
dc.subjectFlux emergenceen_US
dc.subjectNumerical MHDen_US
dc.subjectMagnetic eruptionsen_US
dc.subject.lccQB539.M23M82
dc.subject.lcshSolar magnetic fields--Mathematical modelsen_US
dc.subject.lcshMagnetic fluxen_US
dc.subject.lcshMagnetohydrodynamicsen_US
dc.subject.lcshSun--Active regionsen_US
dc.titleTheoretical magnetic flux emergenceen_US
dc.typeThesisen_US
dc.type.qualificationlevelDoctoralen_US
dc.type.qualificationnamePhD Doctor of Philosophyen_US
dc.publisher.institutionThe University of St Andrewsen_US


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