Theoretical assessment of the upper limit of a star's mass is a difficult problem which lies at the frontier of astrophysical research. In this article we develop a simple and plausible argument to estimate this value. The value at which we arrive is ~228 solar masses; well within the range of predicted accepted theoretical values. Towards the end of the article, theoretical estimations are compared with observational evidence, and a brief overview of the current research is given. The article is aimed at non-graduate students of sciences and engineering and the only requirements are elemental algebra and general notions of classical physics.