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【Abstract】

Radio emission from core-collapse supernovae (SNe) is attributed to synchrotron emission from electrons accelerated by an SN shock. The behavior of the SN shock sensitively reacts to the structure of the circumstellar medium (CSM), which can be tied to the mass-loss history of the progenitor. This indicates that radio SNe is a powerful tool for reconstructing the density structure of the CSM and even for inferring the activities of massive stars prior to the explosion. As we particularly focus on the initial phase of radio SNe, it becomes possible to trace the very final behavior of massive stars. This has been highlighted by recent transient surveys and rapid follow-up observations, suggesting the possible increase in the mass-loss rate of SN progenitors immediately before the explosion, against the current understanding of stellar evolution theory. We show that target of opportunity observations of radio SNe at high frequency (~100GHz) can serve as a robust diagnostic for the final moment of massive stars. In this seminar, we introduce our work related to the modeling of radio emission from infant SNe, including recent observational results and future prospects.