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

Abstract

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.