SIMBAD references

We develop a detailed and self-consistent numerical model, assuming a poloidal magnetic field, for extremely magnetized white dwarfs, which have been proposed as progenitors of overluminous Type Ia supernovae. This model can describe fully consistent equilibria of magnetic stars in axial symmetry, with rotation, general relativistic effects and realistic equations of state (including electrostatic interactions and taking into account Landau quantization of electrons due to the magnetic field). We study the influence of each of these ingredients on to the white dwarf structure and, in particular, on their maximum mass. We perform an extensive stability analysis of such objects, with their highest surface magnetic fields reaching ∼10¹³ G (at which point the star adopts a torus-like shape). We confirm previous speculations that, although very massive strongly magnetized white dwarfs, could potentially exist, the onset of electron captures and pycnonuclear reactions may severely limit their stability. Finally, the emission of gravitational waves by these objects is addressed - our results suggest that detection by the currently planned space-based detector Laser Interferometer Space Antenna is unlikely.