Applied Mathematics Seminar

Solar physics derives its continuing appeal from the existence of magnetic fields. These magnetic fields are generated by the convective motions below the solar surface.What happens below the solar surface is mostly hidden, and so our first real view of the fields is as they cross the photosphere (the layer where most of the Sun's light comes from).

A surprisingly large portion of the magnetic flux crossing the photosphere has been observed to be in concentrated elements, with magnetic energy densities typically ten times that of the local kinetic energy density (and comparable with the thermal energy densities). The mechanism which determines the strength of the magnetic concentrations has been studied in various limiting cases. In this talk we present a more general (numerical) treatment which is able to link these regimes and which reveals some new constraints.

(This is joint work with Dr Dave Galloway, University of Sydney.)