Type Ia supernovae (SNe Ia) are crucial cosmic events used for cosmology and understanding the universe's expansion. However, the precise progenitor systems and explosion mechanisms behind SNe Ia remain elusive and subject to ongoing research. This abstract critically assesses the limitations of current progenitor models employed to explain these intriguing stellar explosions. The Single Degenerate Model, involving the accretion of matter onto a white dwarf from a non-degenerate companion star, faces challenges in explaining the observed lack of post-explosion companion stars, known as the "Missing Companion Problem." The Double Degenerate Model, based on the merger of two white dwarfs, lacks a definitive understanding of the exact merger mechanisms and the parameter space for successful explosions. These limitations highlight the need for further theoretical advancements, observational constraints, and computational modeling to refine and expand our understanding of the progenitor systems of Type Ia supernovae. Future investigations will aim to identify the dominant pathways leading to Type Ia explosions, reconcile the inconsistencies among different models, and enhance the accuracy of SNe Ia as cosmological distance indicators.The whole idea of this paper is to show that the white dwarf progenitor of a Type Ia supernova contains a significant portion of dark matter that is attracted to the dwarf until the Chandrasekhar limit of the star is reached. In this model there is no need for a companion star to provide the extra mass needed to exceed the Chandrasekhar limit of the white dwarf.