Oral Presentation

Three-dimensional hydrodynamical simulations toward linking supernova explosions to their supernova remnants

Author(s): Masaomi Ono (ASIAA)

Presenter: Masaomi Ono (ASIAA)

Nearby supernova remnants (SNRs), e.g., SN (SNR) 1987A and Cassiopeia A (Cas A), have been providing fruitful information thanks to their spatially resolved emissions. On the other hand, theories of the mechanisms of core-collapse supernovae (CCSNe) have suggested an aspherical nature in explosions. Historically, early SN 1987A observations have implied the necessity of a large-scale matter mixing. Therefore, consequential SNRs should reflect complicate physics and a three-dimensional long-term modeling of CCNSe is indispensable to disentangle the underlying physics and to elucidate the evolution of CCSNe.

Recent breakthrough observations of SN 1987A by ALMA have unveiled 3D distribution of the emission from the molecules, carbon monoxide (CO) and silicon monoxide (SiO), for the first time, which has also revealed an aspherical nature. Along with further ALMA observations of dust in the ejecta, such observations have been provided hints to understand the chemical evolution in the ejecta. Additionally, a hotspot found in the dust emission has insisted the existence of the undetected neutron star (NS) of SN 1987A.

We have performed three-dimensional (3D) hydrodynamical simulations from the explosion to a young SNR phase in an attempt to understand such long-term evolution from the explosion focusing on SN 1987A as the first target. From the estimated observables, e.g., [Fe II] lines and X-ray light curves, an aspherical explosion of a binary merger progenitor star has been suggested. Our attempt to model the chemical evolution in the ejecta based on the 3D models is also introduced; newly launched JWST has further motivated us to do such theoretical modeling. Analyses of X-ray spectrum have further supported the existence. Future thermal X-ray observations will provide constraints on the properties of the NS through theoretical models. Interesting observational properties of Cas A and 3D hydrodynamical simulations for it are also introduced in the talk, if time permits.