| Project/Area Number |
20740150
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| Research Category |
Grant-in-Aid for Young Scientists (B)
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| Allocation Type | Single-year Grants |
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| Research Field |
Particle/Nuclear/Cosmic ray/Astro physics
|
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| Research Institution | National Astronomical Observatory of Japan |
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Principal Investigator |
KOTAKE Kei National Astronomical Observatory of Japan, 理論研究部, 助教 (20435506)
|
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| Project Period (FY) |
2008 – 2010
|
| Project Status |
Completed (Fiscal Year 2010)
|
| Budget Amount *help |
¥2,860,000 (Direct Cost: ¥2,200,000、Indirect Cost: ¥660,000)
Fiscal Year 2010: ¥910,000 (Direct Cost: ¥700,000、Indirect Cost: ¥210,000)
Fiscal Year 2009: ¥780,000 (Direct Cost: ¥600,000、Indirect Cost: ¥180,000)
Fiscal Year 2008: ¥1,170,000 (Direct Cost: ¥900,000、Indirect Cost: ¥270,000)
|
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| Keywords | 超新星爆発 / ニュートリノ / 重力波 / 強磁場 / 輻射流体力学 / γ線バースト / 磁気流体数値計算 / ニュートリノ輻射輸送 / 中性子星 / ブラックホール・降着円盤 / 超新星 / マグネター / QCD相転移 / 強磁場コンパクト天体 |
|---|
| Research Abstract |
By performing three-dimensional (3D) hydrodynamic simulations which model neutrino-driven supernova explosions, we find that the emitted gravitational waves (GWs) change stochastically with time due to the interplay between the standing accretion shock instability (SASI) and convection. In order to estimate correctly the GWs originated from anisotropic neutrino emission, we propose a ray-tracing method. Our result show that the GW spectra have its peak around 100 Hz, which is found to be a typical timescale of the growth of SASI that assists the neutrino-driven explosion.
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