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This study presents a universal relation for anisotropic neutron stars,called the $I-f-C$ relation, which accounts for the local anisotropic pressureusing the Quasi-Local (QL) Model proposed by Horvat et al. \cite{QL_Model} todescribe the anisotropy inside the neutron star. This study analyzesapproximately 60 unified tabulated EoS-ensembles, spanning from relativistic tonon-relativistic mean-field models, that comply with multimessenger constraintsand cover a broad range of stiffness. The results indicate that therelationship between the parameters becomes more robust with positiveanisotropy, while it weakens with negative anisotropy. With the help of theGW170817 \& GW190814 tidal deformability limit, a theoretical limit for thecanonical $f$-mode frequency for both isotropic and anisotropic stars isestablished. For isotropic case the canonical $f$-mode frequency for eventGW170817 \& GW190814 is $f_{1.4} = 2.605^{+0.487} _ {-0.459}\ \mathrm{kHz}$ and$ f_{1.4} = 2.093^{+0.150} _ {-0.125} \ \mathrm{kHz}$ respectively. Theseestablished relationships have the potential to serve as a reliable tool tolimit the equation of state of nuclear matter when measurements of relevantobservables are obtained.

The Impact of Anisotropy on Neutron Star Properties: Insights from I-f-C Universal Relations