Probing mass-radius and tidal properties of strange stars and GW190814 with the CFL phase equation of state

We propose a new class of compact star models by adopting the Durgapal IV metric potential for the temporal component g tt , together with a physically motivated anisotropic pressure distribution. To identify the conditions under which the interior matter configuration replicates the colour-flavour-locked (CFL) phase, we construct the corresponding equation of state (EoS) by incorporating corrections in strange quark mass (m s ) up to second order. For an appropriate choice of model parameters, the resulting interior EoS exhibits close agreement with the CFL EoS derived from thermodynamic considerations. Within the admissible parameter space, the model successfully reproduces key observational properties of compact stars, including their mass-radius relation, and tidal deformability Λ, and is consistent with constraints from gravitational wave events such as GW170817. Considering different values of the bag constant, we compute the energy per baryon (ℰ B ), thereby identifying the corresponding stability windows. The parameter α, for which the interior EoS mimics CFL matter, is utilised to study the important physical characteristics of the model. The TOV equations have been solved to obtain the mass-radius relation for different m s . The model supports a maximum mass of 2.96 M ⊙ for suitable choices of Δ, μ, m s , and B . An increase in m s leads to a reduction in the value of maximum mass, indicating a softening of the EoS. Moreover, the model meets all fundamental physical requirements-such as causality, energy conditions, and stability criteria-thereby confirming its viability as a realistic representation of compact stellar configurations.