Magneto-thermal evolution in magnetars

Neutron stars are among the most extreme objects in the universe, with densities comparable to those found in atomic nuclei, and the strongest magnetic fields anywhere, up to 10^15 Gauss. Understanding the interior dynamics of neutron stars is of considerable interest for both astrophysics and physics generally, in terms of understanding the behaviour of matter at such extreme conditions.

Their magnetic field are among the few ways of linking their deep interiors with observations made by astronomers. This project involves high-resolution numerical modelling of some of the equations believed to govern the evolution of magnetic fields in the cores and crusts of neutron stars, modelling phenomena such as ambipolar diffusion in the core and the Hall effect in the crust.

Wherever possible, comparisons will be made with astronomical observations. We will also make connections with models of neutron star magnetospheres, and use the outputs of our numerical simulations as more realistic inputs for their models.