We study the properties of neutron stars using the complete relativistic equation of state based on the relativisticmean field theory. The complete relativistic equation of state covers a wide density range from 10-7 to 1.2 fm-3for the use of describing both the interior region and the crusts of neutron stars. We include the ∧, ∑, and hyperons which may appear as new degrees of freedom at high densities. We also examine the sensibility of the results to the choice of hyperon couplings.