<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>I</mml:mi><mml:mo>?</mml:mo><mml:mi>Love</mml:mi><mml:mo stretchy="false">?</mml:mo><mml:mi>C</mml:mi></mml:mrow></mml:math> relation for an anisotropic neutron star

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