  We study radial oscillations in non-rotating neutron stars by considering the
unified equation of states (EoSs), which support the 2 M$_\odot$ star
criterion. We solve the Sturm-Liouville problem to compute 20 lowest radial
oscillation modes and their eigenfunctions for neutron star modelled with eight
selected unified EoSs from distinct Skyrme-Hartree Fock, Relativistic
Mean-Field and quarkyonic models. We compare the behavior of the computed
eigenfrequency for NS modelled with hadronic to that with quarkyonic EoSs while
varying central densities. The lowest order, f-mode frequency varies
substantially between the two classes of the of EoS at 1.4 M$_\odot$ but
vanishes at their respective maximum masses, consistent with the stability
criterion $\partial M/\partial\rho_c > 0$. Moreover, we also computed large
frequency separation and discovered that higher-order mode frequencies are
significantly reduced by incorporating crust in the EoS.
