  One of the most common assumptions has been made that the pressure inside the
star is isotropic in nature. However, the pressure is locally anisotropic in
nature which is a more realistic case. In this study, we investigate certain
properties of anisotropic neutron stars with the scalar pressure anisotropy
model. Different perfect fluid conditions are tested within the star with the
relativistic mean-field model equation of states (EOSs). The anisotropic
neutron star properties such as mass ($M$), radius ($R$), compactness ($C$),
Love number ($k_2$), dimensionless tidal deformability ($\Lambda$), and the
moment of inertia ($I$) are calculated. The magnitude of the quantities as
mentioned above increases (decreases) with the positive (negative) value of
anisotropy except $k_2$ and $\Lambda$. The Universal relation $I-$Love$-C$ is
calculated with almost 58 EOSs spans from relativistic to non-relativistic
cases. We observed that the relations between them get weaker when we include
anisotropicity. With the help of the GW170817 tidal deformability limit and
radii constraints from different approaches, we find that the anisotropic
parameter is less than 1.0 if one uses the BL model. Using the universal
relation and the tidal deformability bound given by the GW170817, we put a
theoretical limit for the canonical radius, $R_{1.4}=10.74_{-1.36}^{+1.84}$ km,
and the moment of inertia, $I_{1.4} = 1.77_{-0.09}^{+0.17}\times10^{45}$ g
cm$^2$ with 90\% confidence limit for isotropic stars. Similarly, for
anisotropic stars with $\lambda_{\rm BL}=1.0$, the values are
$R_{1.4}=11.74_{-1.54}^{+2.11}$ km, $I_{1.4} = 2.40_{-0.08}^{+0.17}
\times10^{45}$ g cm$^2$ respectively.
