An essential component of the equation of state (EOS) of isospin asymmetric nuclear matter is nuclear symmetry energy. It influences the structure of neutron stars and finite nuclei. We perform qualitative investigations within chiral forces and do Brueckner-Hartree-Fock calculations for nuclear and neutron matter EOS in order to further our understanding of the influence of the symmetry energy on nuclear properties. We introduce N3LO, a nucleon-nucleon potential of chiral effective field theory, with various cutoff parameter values. The single particle potential's standard and continuous choices are both applied. To ensure the empirical saturation property, a phenomenological term based on chiral forces is introduced, modeling the three-body interaction. Both low and high values of the baryon density are specified in a generalized form for the equations of state. The Tolman-Oppenheimer-Volkov equations for comparable neutron stars are solved using these equations as input. The global parameters (masses, radii, and composition) of a neutron star are systematically studied using the obtained nuclear equations of state.