  We study the properties of the binary neutron star (BNS) systems in the
inspiral phase. To calculate the equation of state (EOS) of the neutron star
(NS), we take the relativistic mean-field (RMF) model. The RMF model, namely
NL3 (stiff) and two extended RMF model IOPB-I (less stiff) and G3 (soft) are
taken to explore the properties of the NS. We assume that the dark matter (DM)
particles are accreted inside the NS due to its enormous gravitational field.
Different macroscopic properties of the NS such as mass $M$, radius $R$, tidal
deformability $\lambda$ and dimensionless tidal deformability $\Lambda$ are
calculated at different DM fractions. With the addition of DM inside the NS,
the value of the quantities like $M$, $R$, $\lambda$ and $\Lambda$ decreases.
To explore the BNS properties in the inspiral phase, the post-Newtonian (PN)
formalism is considered because it is suitable up to the last orbits in the
inspiral phase. We calculated the strain amplitude of the polarization
waveforms $h_+$ and $h_\times$, (2,2) mode waveform $h_{22}$, orbital phase
$\Phi$, frequency of the gravitational wave $f$ and PN parameter $x$ with DM as
an extra candidate inside the NS. We find that the BNS with soft EOS sustains
more time in their inspiral phase as compare to stiff EOS. In the case of DM
admixed NS, the BNS with high DM fractions survives more time in the inspiral
phase than lesser fraction of DM. The magnitude of $f$, $\Phi$ and $x$ are
almost the same for all the assumed parameter sets, but their inspiral time in
the last orbit is different. We find a significant change in the BNS systems
properties in the inspiral phase with DM inside the NS.
