Exploring gravitational-wave sources by numerical relativity

2016 Fiscal Year Final Research Report

• Project/Area Number: 24244028
• Research Category: Grant-in-Aid for Scientific Research (A)
• Allocation Type: Single-year Grants
• Section: 一般
• Research Field: Particle/Nuclear/Cosmic ray/Astro physics
• Research Institution: Kyoto University
• Principal Investigator: Shibata Masaru 京都大学, 基礎物理学研究所, 教授 (80252576)
• Co-Investigator(Kenkyū-buntansha): 田越 秀行 大阪大学, 理学(系)研究科(研究院), 助教 (30311765) ; 木内 建太 京都大学, 基礎物理学研究所, 研究員 (40514196) ; 関口 雄一郎 京都大学, 基礎物理学研究所, 研究員 (50531779)
• Project Period (FY): 2012-04-01 – 2016-03-31
• Keywords: 重力波 / 数値相対論 / 中性子星 / 中性子星連星 / ブラックホール / マクロノバ / 重元素合成 / 磁気流体

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.

Free Research Field

宇宙物理学、一般相対論、重力波、数値相対論、中性子星連星