期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 441, 期 4, 页码 3177-3208出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu762
关键词
accretion; accretion discs; black hole physics; gravitation; hydrodynamics; MHD; methods: numerical
资金
- NSF [AST1312651]
- NASA through Einstein Fellowship Programme [PF3-140115]
- NICS Kraken and Nautilus [TG-PHY120005, TG-AST100040, TG-AST080026N]
- NASA via High-End Computing (HEC) Program through NASA Advanced Supercomputing (NAS) Division at Ames Research Center
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1312651] Funding Source: National Science Foundation
Black hole (BH) accretion flows and jets are dynamic hot relativistic magnetized plasma flows whose radiative opacity can significantly affect flow structure and behaviour. We describe a numerical scheme, tests, and an astrophysically relevant application using the M1 radiation closure within a new 3D general relativistic radiation magnetohydrodynamics (GRRMHD) massively parallel code called harmrad. Our 3D GRRMHD simulation of super-Eddington accretion (about 20 times Eddington) on to a rapidly rotating BH (dimensionless spin j = 0.9375) shows sustained non-axisymmemtric disc turbulence, a persistent electromagnetic jet driven by the Blandford-Znajek effect, a disc wind, and a polar radiation jet. The total accretion efficiency is of the order of 20 per cent, the large-scale electromagnetic jet efficiency is of the order of 10 per cent, the disc wind efficiency is less than 1 per cent, and the total radiative efficiency remains low at only of the order of 1 per cent (of order the Eddington luminosity). However, the radiation jet and the electromagnetic jet both emerge from a geometrically beamed polar region, with super-Eddington isotropic equivalent luminosities. Such simulations with harmrad can enlighten the role of BH spin versus discs in launching jets, help determine the origin of spectral and temporal states in X-ray binaries, help to understand how tidal disruption events work, provide an accurate horizon-scale flow structure for M87 and other active galactic nuclei (AGN), and isolate whether AGN feedback is driven by radiation or by an electromagnetic, thermal, or kinetic wind/jet. For example, the low radiative efficiency and weak BH spin-down rate from our simulation suggest that BH growth over cosmological times to billions of solar masses by redshifts of z similar to 6-8 is achievable even with rapidly rotating BHs and 10 M-aS (TM) BH seeds.
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