One of the great challenges in the study of planetary interiors is to understand the generation of magnetic fields in the interiors of the giant gas planets. Wieland Dietrich and Chris Jones from the University of Leeds have been addressing this problem through high resolution magnetohydrodynamic models, with the novel feature of incorporating realistic radially-dependent profiles for the electrical conductivity (Icarus 305 (2018) 15-32). This allows the study of a range of models in which the conductivity ranges from Jupiter-like, with only a thin outer non-conducting shell to Saturn-like, with a thick non-conducting shell. They find Jupiter-like steady dipolar fields, quadrupolar dynamos for profiles between those of Jupiter and Saturn, and dipolar fields again for Saturn-like profiles. The non-axisymmetric components of the Saturn model are, though, more pronounced than in Saturn itself, prompting the suggestion that a stably stratified region – postulated to exist in Saturn, but not yet incorporated in the model – may be of significance.