| Budget Amount *help |
¥44,980,000 (Direct Cost: ¥34,600,000、Indirect Cost: ¥10,380,000)
Fiscal Year 2015: ¥8,840,000 (Direct Cost: ¥6,800,000、Indirect Cost: ¥2,040,000)
Fiscal Year 2014: ¥12,350,000 (Direct Cost: ¥9,500,000、Indirect Cost: ¥2,850,000)
Fiscal Year 2013: ¥11,440,000 (Direct Cost: ¥8,800,000、Indirect Cost: ¥2,640,000)
Fiscal Year 2012: ¥12,350,000 (Direct Cost: ¥9,500,000、Indirect Cost: ¥2,850,000)
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| Outline of Final Research Achievements |
By numerical relativity simulations, the following facts on the merger of neutron-star binaries are found: (i) Massive neutron stars (MNS) formed typically after the merger of binary neutron stars depend strongly on neutron-star equations of state. (ii) During the merger of binary neutron stars, neutron-rich matter with mass about 0.1~1% of the solar mass is ejected and it could produce a variety of heavy elements via the so-called r-process nucleosynthesis. We indicate that the abundance pattern of the heavy elements could agree with the solar abundance pattern. (iii) During tidal disruption of neutron stars in black hole-neutron star binaries, a fraction of matter is ejected in an anisotropic manner and associated with this, characteristic signals of gravitational waves and electromagnetic waves would be emitted. (iv) By high-resolution magnetohydrodynamics simulations, we show that after the merger of binary neutron stars, magnetic-field strength the formed MNS is highly amplified.
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