Magnetized rotational neutron stars and mass-radius relations

Neutron stars are highly magnetized rotating compact stars.

It was reported in 2010 that a neutron star named PSR J1614-2230 making a binary system with a white dwarf has a mass of twice the solar mass (1.97±0.04M_☉). In 2013, a neutron star named PSR J0348+0432 with a mass of 2.01±0.04M_☉was observed. Such massive neutron stars give strong constraints on the equation of state (EoS) of neutron star matter. 

In this study, we calculate mass, radius, and eccentricity of magnetized and deformed rotational neutron stars, using a perturbative prescription. As for the EoS a relativistic mean field approach is utilized. We obtain neutron star masses more than 2 M_☉ from the mass-radius relation in a strong magnetic field.