Abstract
We investigate the structure of neutron stars with strong magnetic fields by using a density-dependent relativistic mean field model. The coupling constant between nucleons and the rho meson in the model is obtained by using the polytropic formula for the symmetry energy in the neutron star. With the density-dependent coupling constant, the effects of the symmetry energy on strongly-magnetized neutron stars are considered in detail for particle fractions and the equation of state. The consequent changes in the masses and the radii of the neutron star are discussed by using the roles of the symmetry energy in the neutron star.
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