This study explores a new class of strange stars using the Durgapal IV interior solution within a \((2+1)\) dimensional framework while considering the BTZ Black Hole as the exterior solution. By examining the stability and conditions for physical acceptability, we identify constraints on mass-radius relationships for various values of the cosmological constant. Our model is applied to low-mass compact star candidates such as PSR B0943+10, PSR J1640-4631, and 1E 1207.4-5209, indicating that a negative cosmological constant on the order of \(10^{-3}\) (in the unit, \(\text {km}^{-2} \) ) or less is necessary. The research underscores the significance of the attractive anisotropic force in constraining the upper mass limit of stable configurations, with a maximum mass estimated at approximately \(0.338M_{\odot }\) . The criteria for equilibrium, fulfilment of energy constraints, and stability conditions further support our theoretical framework for low-mass strange stars.
