| Budget Amount *help |
¥32,110,000 (Direct Cost: ¥24,700,000、Indirect Cost: ¥7,410,000)
Fiscal Year 2020: ¥7,540,000 (Direct Cost: ¥5,800,000、Indirect Cost: ¥1,740,000)
Fiscal Year 2019: ¥7,670,000 (Direct Cost: ¥5,900,000、Indirect Cost: ¥1,770,000)
Fiscal Year 2018: ¥9,880,000 (Direct Cost: ¥7,600,000、Indirect Cost: ¥2,280,000)
Fiscal Year 2017: ¥7,020,000 (Direct Cost: ¥5,400,000、Indirect Cost: ¥1,620,000)
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| Outline of Final Research Achievements |
In order to investigate the multi-dimensional evolution of massive stars prior to collapse, we have developed 3D hydrodynamics code including an in-situ nuclear burning network calculation. By performing 3D simulations of typical massive stars (22 and 27 solar masses) over a hundred of second before collapse, we have found that the global turbulence develops in the oxygen-silicon layers with a typical Mach number of 0.1. This turbulence is expected to be favorable for the onset of the neutrino-driven supernova explosions. Besides, we have updated our 3D supernova code in such a way to implement the state-of-the-art neutrino opacities. By performing the 3D self-consistent core-collapse simulations, we obtain some major findings including the correlation between the progenitor’s core compactness and the kick velocity of the neutron stars and the new neutrino and gravitational signatures, for the formation of which spiral modes that develop in rapidly rotating cores play a vital role.
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