Exploring density dependent B as a suitable parameter in higher dimensional approach with a non-linear equation of state

In this investigation, we present a singularity-free interior solution of the Einstein field equation for a class of anisotropic compact objects in dimensions [Formula: see text]. In accordance with the concept of Vaidya and Tikekar, the geometry of the physical [Formula: see text]-space of a star corresponding to [Formula: see text] hypersurface is assumed to be a [Formula: see text] spheroid. For the fulfilment of the causality condition, a bound on the spheroidal parameter ([Formula: see text]) is noted depending on the values of the amount of anisotropy ([Formula: see text]) and space-time dimensions ([Formula: see text]). We note that by switching off the extra parameters ([Formula: see text] and [Formula: see text]), the previously obtained limit of [Formula: see text] can be generated. To validate our findings, we compare the results obtained from our model with observational data of PSR J1614-2230 (mass=[Formula: see text], radius=[Formula: see text]) and PSR J0740+6620 (mass=[Formula: see text], radius= [Formula: see text]). It is noted that the best-fit equation of state corresponds to a polynomial equation of state of the order of five. We use this finding to develop a density-dependent B in the MIT bag model, which seems to be useful for the correct description of compact objects in our model. The mass radius relation shows that our model mimics a wide range of recently observed pulsars in four and higher dimensions. It is noted that, in the case of a superdense compact object, the number of space-time dimensions cannot be taken large, which is a different result from that of the braneworld model. However, with density-dependent B, the present model permits any number of space-time dimensions ([Formula: see text]) to describe a stellar configuration. Furthermore, we also found that our model exhibits stability according to the generalised TOV equation, the Herrera cracking condition, and the adiabatic index.