演講資訊

摘要：

Massive stars end their lives as an explosive phenomenon called a core-collapse supernova (SN). SN ejecta and radiation can interact with circumstellar medium (CSM) which was released from the progenitor itself, as well as can produce observational signatures unique to CSM interaction. Thus, investigation of the properties of core-collapse SNe gives us opportunities to examine the mass-loss activities of massive stars before the explosion. Paying attention to the fact that synchrotron radio emission can robustly trace the density distribution of CSM, we have attempted theoretical and observational studies regarding radio SNe. We have shown that radio SNe have potential to infer the radial inhomogeneity of CSM density distribution, implying the time-variable mass-loss activity before the explosion. In addition, we have been interested in the origin of such time-variable mass-loss activities of SN progenitors, and we explored the possibility of whether binary interaction can yield the diverse structures of CSM. In this seminar, I will talk about our recent research results of radio SNe modeling and observations with the case studies, as well as discuss the possible origins of the time-variable (sometimes eruptive) mass-loss mechanism of SN progenitors including binary interaction.