Abstract
In 1181, “a guest star”, as bright as the planet Saturn was observed in the sky by Chinese and Japanese astronomers. A recent study (Ritter et al., 2021) has identified the star IRAS 00500 + 6713 as the remnant from the 1181 event, surrounded by the nebula “PA 30” and pointing to an unusual scenario where the explosion could have been caused by the double-degenerate merger of two white dwarfs (Oskinova et al., 2020) based on the neon abundance of the nebula. Initially identified as a possible planetary nebula, it was subsequently found associated with a very hot star (200,000 K) with an astounding 16,000 km/s velocity wind (Gvaramadze et al., 2019) and unique filamentary structure composed primarily of sulfur. Spectral analysis reveals an abundance of neon and magnesium and absence of hydrogen and helium (Fesen et al., 2023). Spectral analysis of the nebula reveals the presence of elements such as carbon, oxygen, neon, magnesium, and silicon in specific ionization states which pointed to a Type Iax event.(Lykou et al., 2023). Since we have observational results for both the central star and the nebula, comparing the results with a computational model helps in confirming if this is indeed a type 1ax event. In this thesis, I will present a 3D hydrodynamical simulation model for SNe Iax in the context of the double-degenerate channel of merging ONe- CO white dwarf binary and discuss the explosion mechanism, the characteristics of the remnant, and other implications of this model.