  Although barotropic matter does not constitute a realistic model for magnetic
stars, it would be interesting to confirm a recent conjecture that states that
magnetized stars with a barotropic equation of state would be dynamically
unstable (Reisenegger 2009). In this work we construct a set of barotropic
equilibria, which can eventually be tested using a stability criterion. A
general description of the ideal MHD equations governing these equilibria is
summarized, allowing for both poloidal and toroidal magnetic field components.
A new finite-difference numerical code is developed in order to solve the
so-called Grad-Shafranov equation describing the equilibrium of these
configurations, and some properties of the equilibria obtained are briefly
discussed.
