Pathway to type Iax supernovae

Type Ia supernovae (SNe Ia) are among the most common types of luminous astrophysical transients. They are thought to arise from the thermonuclear explosion of mass-accreting white dwarfs (WDs) in binary systems. Due to their consistent peak luminosities, SNe Ia are used as standarizable candles to measure the expansion rate of the universe. A subluminous subclass of these events, known as Type Iax supernovae, is believed to be result of a failed partial detonnation of the WDs. Pa 30 has recently been identified as the remnant of the historical supernovae SN 1181 was likely a sub-luminous event, classified as a Type Iax supernova, possibly originating from a merger between carbon-oxygen (C/O) and oxygen neon (O/Ne) WDs.In this thesis, we investigate failed detonations of Type Iax supernovae within the context of the double degenerate merger channel. Specifically, we consider a binary system consisting of a C/O WD and an O/NeWD. In this scenario, the secondary C/O WD is tidally disrupted and merges with the O/Ne WD, forming an accretion disk around the primary. Due to the instabilities within the disk, a carbon detonation is triggered on the accretion disk, while leaving the primary largely intact. The total nuclear energy released in this event is lower than that of normal SNe Ia, consistent with the properties of the SNe Iax. We further explore the detonation mechanism, the characteristics of the resulting remnant, and the broader implications of this model for understanding the physics of the Type Iax supernovae.