Oral Presentation

Modeling Supernova Explosions of Massive Stars and Predicting their Observational Signature

Author(s): Kai-An You (Department of Physics, NTHU); Ke-Jung Chen (Institute of Astronomy and Astrophysics, Academia Sinica); Sung-Han Tsai (Department of Physics, NTU); Po-Sheng Ou (Department of Physics, NTU)

Presenter: Kai-An You ((Department of Physics, NTHU))

Core-Collapse Supernovae (CCSNe) are the grandest explosions in the universe with much exploration in astrophysics. CCSNe are thought to originate from the death of massive stars which are powerful engines in driving the baryonic cycles in galaxies. However, the physics of massive star evolution and their CCSNe is still unclear. To advance the knowledge of CCSNe, we performed a large grid of stellar evolution models with the one-dimensional code, Modules for Experiments in Stellar Astrophysics (MESA). Our simulations evolved the massive stars from their zero-age main sequence (ZAMS) until their CCSNe. For this poster, we present the CCSNe models by considering various explosion energies, metallicities, angular momentum, and mass of the progenitor stars. We discuss how these physical parameters of stellar evolution impact on the CCSNe explosions and present their multi-color light curves. Our results can match the CCSNe observational data well and explain the physical origins of their progenitor stars.