This work presents self-consistent, single-star, stellar evolution models for the progenitor of the planetary nebula NGC 40, from the main sequence to its final stages. We used MESA, a 1-d stellar evolution code to generate a grid of models for this star. The grid consisted of different models built given a parameter space based on values estimated by previous studies (such as initial mass and chemical composition). The parameter space was explored using a semi-automated procedure, until a set of models was found that best matched the current observational parameter constraints. We found that a fast rotating \(1.09\pm 0.30\) M\({}_{\odot}\) progenitor can reproduce reasonably well the luminosity , effective temperature, mass and surface gravity of the central star (CS), as well as the chemical abundances of the planetary nebula (PN). However, we did not achieve a single-star model that is able to match the chemical composition of both the PN and the CS. We also discuss evidence that the most likely progenitor that is able to reproduce an H-poor CS has \(3.11\pm 0.11\) M\({}_{\odot}\) and unphysical rotation speeds, given the observational constraints used. Therefore, we conclude that an average solar-mass star is not able to match the observations of the CS of NGC 40, unless there is an enhancement on the mass loss rate during the AGB phase or some extra mixing caused by an external factor, which could expose the H-poor core of the CS.