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.