Exploring the impact of dark energy on the equation of state, physical properties and stability of charged anisotropic neutron stars in higher dimension

This work focuses on studying the impact of higher-dimensional [Formula: see text] space-time and Dark Energy on the mass–radius relation and other physical properties of the massive Neutron stars under the present accelerating Universe. To solve the stellar equations, Einstein gravity has been employed and the Equation of State of the core matter has been acquired by applying Tolman–Kuchowicz metric potentials and considering the presence of some exotic matter. Modified Tolman–Oppenheimer–Volkoff equations have been solved numerically by considering the presence of modified Chaplygin gas inside the stars along with the field equations in D-dimensions. The incremental dimensionality supports the higher mass of the Neutron Stars but lowers the maximum mass limit. Due to pressure anisotropy, the stars become less compact obeying the modified Buchdahl limit. The exotic matter plays the fundamental role to produce anisotropy. The higher value of electric charge [Formula: see text] with anisotropic pressure reveals the existence of massive Neutron Stars in the lower mass gap (in between the mass range of [Formula: see text] to [Formula: see text]) with stability. The increasing value of [Formula: see text] supports the highly massive Neutron stars and also shows a small decrement in the maximum upper mass limit of the Neutron Stars. Due to the higher dimensions, the upper limit of the maximum mass decreases significantly. From our investigation in higher dimensions, the mass–radius curve supports a maximum allowable mass about [Formula: see text] at the maximum nuclear saturation density and the lowest possible radius about [Formula: see text].