City Research Online

Abstract

Understanding and characterising the dynamics inside the Sun is vital to in-terpret the large diversity of complex and variable magnetic phenomena that continually appear on the solar surface. Owing to the theory of magneto-hydrodynamics, many aspects of solar physics have been and continue to be investigated in order to unpuzzle the fundamental processes within the layers of the Sun. Of crucial importance, is the central role of convection that under-lies the structure and features we observe of the Sun. This thesis is devoted to develop mathematical and computational modelling frameworks for the purpose of exploring the interaction of magnetic fields with granular convection in the unobservable layers of the Sun, to better understand the distributions of field over the solar surface. In particular, I aim to address the influence of convective turbulence on the emergence of solar magnetic structures.

By conducting a series of idealised numerical experiments, I first explore how small-scale turbulent pumping in the convection zone can affect properties of the large-scale buoyancy-driven magnetic field. This investigation is pursued by an extension to account for more realistic turbulent pumping configurations, where the effect of turbulent convection and magnetic buoyancy are further examined. Finally, I focus on providing an insight into how the simplifying assumptions introduced in the general modelling of thermal convection can
alter the behaviour of a system.

Publication Type:	Thesis (Doctoral)
Subjects:	Q Science > QA Mathematics
Departments:	Doctoral Theses School of Science & Technology > School of Science & Technology Doctoral Theses School of Science & Technology > Mathematics

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