The relativistic mean-field (RMF) models either with higher order couplings or density-dependent couplings can be used to explain neutron stars properties with and without kaon or baryons. The nuclear interactions are described by the exchange of the sigma, omega and rho mesons. RMF parameterizations consistent with the recently studied constraints related to nuclear matter, pure neutron matter and symmetry energy were used to calculate the equations of state of star. The properties of nonrotating and rotating neutron stars are considered for a set of equations of state.