| Budget Amount *help |
¥4,810,000 (Direct Cost: ¥3,700,000、Indirect Cost: ¥1,110,000)
Fiscal Year 2016: ¥1,300,000 (Direct Cost: ¥1,000,000、Indirect Cost: ¥300,000)
Fiscal Year 2015: ¥1,560,000 (Direct Cost: ¥1,200,000、Indirect Cost: ¥360,000)
Fiscal Year 2014: ¥1,950,000 (Direct Cost: ¥1,500,000、Indirect Cost: ¥450,000)
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| Outline of Final Research Achievements |
The formation of supermassive stars (SMSs) via rapid mass accretion and their direct collapse into black holes (BHs) is a promising pathway for sowing seeds of supermassive BHs in the early universe. We calculated the evolution of rapidly accreting SMSs including general relativistic (GR) effects up to the onset of the collapse. We found that such SMSs have a less concentrated structure than a non-accreting ones. This effect stabilizes the stars against GR instability even above the classical upper mass limit around 100,000 Msun. We found that the final masses for dM/dt = 0.1, 0.3, 1.0 and 10 Msun/yr are 1.2, 1.9, 3.5 and 8.0 times 100,000Msun, respectively. We also found that the GR instability does not occur for the dM/dt=0.1 model. On the other hand, the instability occurs during He-burning stage for the dM/dt=0.3 and 1.0 models, and during H-burning stage for the dM/dt=10 model. And the reasons for these reseluts were discussed.
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