Journal
ASTROPHYSICAL JOURNAL
Volume 804, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/804/2/101
Keywords
accretion, accretion disks; black hole physics; galaxies: jets; hydrodynamics
Categories
Funding
- National Basic Research Program of China (973 Program) [2014CB845800]
- Strategic Priority Research Program The Emergence of Cosmological Structures of CAS [XDB09000000]
- NSF of China [11103059, 11103061, 11121062, 11133005]
- NSF [AST1312651, TG-AST080026N]
- NASA [NNX14AB47G, NAS8-03060, NAS 5-26555]
- NASA through Einstein Postdoctotral Fellowship - Chandra X-ray Center [PF4-150126]
- NASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF2-51301.001-A]
- NASA via the High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center
- SHAO Super Computing Platform
- NASA [686658, NNX14AB47G] Funding Source: Federal RePORTER
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1312651] Funding Source: National Science Foundation
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Previous MHD simulations have shown that wind must exist in black hole hot accretion flows. In this paper, we continue our study by investigating the detailed properties of wind and the mechanism of wind production. For this aim, we make use of a 3D general relativistic MHD simulation of hot accretion flows around a Schwarzschild black hole. To distinguish real wind from turbulent outflows, we track the trajectories of the virtual Lagrangian particles from simulation data. We find two types of real outflows, i.e., a jet and a wind. The mass flux of wind is very significant, and its radial profile can be described by (M) over dot(wind) approximate to (M) over dot(BH) (r/20 r(s)), with (M) over dot(BH) being the mass accretion rate at the black hole horizon and r(s) being the Schwarzschild radius. The poloidal wind speed almost remains constant once they are produced, but the flux-weighted wind speed roughly follows v(p,wind) (r) approximate to 0.25v(k) (r), with v(k)(r) being the Keplerian speed at radius r. The mass flux of the. jet is much lower, but the speed is much higher, v(p, jet) similar to (0.3-0.4)c. Consequently, both the energy and momentum fluxes of the wind are much larger than those of the jet. The wind is produced and accelerated primarily by the combination of centrifugal force and magnetic pressure gradient, while the jet is mainly accelerated by the magnetic pressure gradient. Finally, we find that the wind production efficiency is an element of(wind) equivalent to (E) over dot(wind)/(M) over dot(BH)c(2) similar to 1/1000 2 is in good agreement with the value required from large-scale galaxy simulations with active galactic nucleus feedback.
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