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We derive an equation of state for magnetized charge neutral nuclear matterrelevant for neutron star structure. The calculations are performed within aneffective chiral model based on generalization of sigma model with nonlinearself interactions of the sigma mesons along with vector mesons and a$\rho-\sigma$ cross-coupling term. The effective chiral model is extended byintroducing the contributions of strong magnetic field on the charged particlesof the model. The contributions arising from the effects of magnetic field onthe Dirac sea of charged baryons are also included. The resulting equation ofstate for the magnetized dense matter is used to investigate the neutron starproperties, like, mass-radius relation and tidal deformability. Thedimensionless tidal deformability of $1.4~{M}_\odot$ NS is found to be$\Lambda_{1.4}=526$, which is consistent with recent observation of GW170817.The maximum mass of neutron star in presence of strong magnetic field isconsistent with the observational constraints on mass of neutron star from PSR~J0348 - 0432 and the radius at $1.4~{M}_\odot$ mass of the neutron star iswithin the empirical bounds.

Impact of Magnetic field on neutron star properties