Mass-radius diagrams for a magnetized anisotropic neutron star

Abstract

We examine the relationship between the mass and radius of a magnetized neutron star with a polytropic equation of state $p_{r} = \kappa \rho^{2}$ and Bowers-Liang anisotropy. The mass we computed in the diagrams is the Tolman Whittaker mass, which is a proxy for the gravitational mass of an isolated object. The key effects of anisotropy and magnetic field are as follows: the mass grows with greater magnetic field and tangential pressures over the radial pressure at constant radii; stars with much stronger magnetic fields and tangential pressures may become unstable; and for each anisotropy, there is a critical magnetic field strength beyond which the stars lose stability. In most circumstances, the anisotropy has a higher effect on the mass of the star than the magnetic field.