An accretion disc is a structure formed by plasma in orbital motion around a massive central body - normally a star or black hole. Such structures are often modelled by the Grad-Shafranov equation, which describes the balance of forced perpendicular to flow lines.
In toroidal magnetic confinement, the assumption of toroidal-axis symmetry also leads to the Grad-Shafranov equation, which in this case represents force alance perpendicular to magnetic field surfaces. Both treatments normally use polynomial representations for the constraints, and solve for the configuration using current-field iteration.
In this project we would compare the construction of accretion disc and magnetic configuration Grad-Shafranov problems, and apply a recently developed toroidal magnetic confinement equilibrium code to model an accretion disc. A focus of the project will be constraining free functions to observational data.