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所属期第14期（任期：2024年4月～）
グローバル型 -
専門astrophysics (天体物理学)
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研究内容Generational theoretical updates to pre-supernova mass loss in the era of high resolution observations and all-sky surveys
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受入先部署理学研究科
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直前所属京都大学 理学研究科
Most massive stars (heavier than 8 solar masses) end their lives in a spectacularly energetic and violent explosion— a core-collapse supernova.
While massive stars produce chemical elements as heavy as iron over their lifetime in successive nuclear burning phases, it is only during a supernova explosion that many heavier chemical elements in the universe can be created.
These bright cosmic explosions have been observed in our night sky for millennia. Despite advances in stellar evolution theory and numerical simulation it is still challenging today to connect explosion properties (luminosity, explosion geometry, chemical element production) with properties of both the massive star progenitor (mass, structure, and rotation) and the compact neutron star or black hole remnant (mass and spin) that is left behind.