Recent Advances in Understanding the Chandrasekhar Maximum Mass of White Dwarf Stars

The maximum mass of white dwarf stars, the final products of stellar evolution, is a crucial parameter in astrophysics. The Chandrasekhar limit, approximately 1.4 M⊙, is widely recognized as the upper limit. However, recent observations have revealed the existence of super-Chandrasekhar white dwarfs, which are believed to be precursors of bright type Ia supernovae. The origin and fundamental nature of these super-Chandrasekhar white dwarfs remain poorly understood, leading to extensive debate within the scientific community. This research paper reviews current understanding of the maximum mass limit of white dwarf stars, examining various models, including strong magnetic fields, rapid rotation, non-commutative geometry and modified theories of gravity. Furthermore, the criticisms and challenges encountered by these Models, such as electron captures, pycnonuclear reactions, general relativity, and observational limitations were analyzed. This analysis yielded a conclusion with the proposition of potential avenues for future exploration in this area of study.