Magnetohydrodynamic equilibria in barotropic stars
arXiv:1305.0592 · doi:10.1017/S1743921314002646
Abstract
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.
Conference Proceedings, Magnetic Fields in the Universe IV (2013)
References in corpus (4)
- Modelling magnetically deformed neutron stars
- Twisted-torus configurations with large toroidal magnetic fields in relativistic stars
- Hall equilibria with toroidal and poloidal fields: application to neutron stars
- Axisymmetric and stationary structures of magnetized barotropic stars with extremely strong magnetic fields deep inside