general relativistic magnetohydrodynamic simulations of relativistic jet formation and particle acceleration

2017 Fiscal Year Final Research Report

• Project/Area Number: 15K17670
• Research Category: Grant-in-Aid for Young Scientists (B)
• Allocation Type: Multi-year Fund
• Research Field: Particle/Nuclear/Cosmic ray/Astro physics
• Research Institution: Institute of Physical and Chemical Research
• Principal Investigator: Mizuta Akira 国立研究開発法人理化学研究所, 戎崎計算宇宙物理研究室, 研究員 (90402817)
• Project Period (FY): 2015-04-01 – 2018-03-31
• Keywords: ブラックホール / 宇宙ジェット / 降着円盤 / 磁気流体力学 / 一般相対性理論

Outline of Final Research Achievements

We have performed global general relativistic magneto-hydrodynamic simulations of accretion flows onto a black hole. We observed magnetic field amplification via magnetorotational instabilities (MRIs) and dissipation of magnetic fields in the accretion disks. The magnetic field amplification and dissipation repeatedly occur. The timescale of magnetic field amplification via MRI is consistent with linear theory. Alfven waves are emitted toward vertical direction from accretion disk to outside. Some of them propagate as relativistic alfven waves in the jet and will be converted to electromagnetic waves. For these waves we can apply theoretical acceleration models proposed by Ebisuzaki & Tajima (2014) for ultra high energy cosmic rays and non-thermal electrons which contributes to the high energy gamma-ray emissions from blazars. Our timescale of alfven waves are consistent with the observed timesclaes of gamma-ray flares of blazars.

Free Research Field

宇宙物理学