NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. III. REVISITING WIND PROPERTIES USING THE TRAJECTORY APPROACH

	NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. III. REVISITING WIND PROPERTIES USING THE TRAJECTORY APPROACH
	Yuan, Feng1 ; Gan, Zhaoming 1; Narayan, Ramesh 2; Sadowski, Aleksander 3; Bu, Defu1 ; Bai, Xue-Ning 2
刊名	ASTROPHYSICAL JOURNAL
	2015-05-10
卷号	804 期号:2 页码:1
关键词	accretion black hole physics galaxies: jets hydrodynamics accretion disks
英文摘要	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.
WOS标题词	Science & Technology ; Physical Sciences
类目[WOS]	Astronomy & Astrophysics
研究领域[WOS]	Astronomy & Astrophysics
关键词[WOS]	ADVECTION-DOMINATED ACCRETION ; ACTIVE GALACTIC NUCLEI ; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS ; SPINNING BLACK-HOLE ; SAGITTARIUS-A ; 2-DIMENSIONAL MODELS ; ELLIPTIC GALAXIES ; MASS OUTFLOWS ; 2 DIMENSIONS ; FEEDBACK
收录类别	SCI
语种	英语
WOS记录号	WOS:000354905000023
公开日期	2015-08-18
内容类型	期刊论文
源URL	[http://119.78.226.72/handle/331011/18336]
专题	上海天文台_星系宇宙学重点实验室
作者单位	1.Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China 2.Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA 3.MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA
推荐引用方式 GB/T 7714	Yuan, Feng,Gan, Zhaoming,Narayan, Ramesh,et al. NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. III. REVISITING WIND PROPERTIES USING THE TRAJECTORY APPROACH[J]. ASTROPHYSICAL JOURNAL,2015,804(2):1.
APA	Yuan, Feng,Gan, Zhaoming,Narayan, Ramesh,Sadowski, Aleksander,Bu, Defu,&Bai, Xue-Ning.(2015).NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. III. REVISITING WIND PROPERTIES USING THE TRAJECTORY APPROACH.ASTROPHYSICAL JOURNAL,804(2),1.
MLA	Yuan, Feng,et al."NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. III. REVISITING WIND PROPERTIES USING THE TRAJECTORY APPROACH".ASTROPHYSICAL JOURNAL 804.2(2015):1.