COMPARISON BETWEEN RHD SIMULATION OF SUPERCRITICAL ACCRETION FLOWS AND A STEADY MODEL WITH OUTFLOWS

	COMPARISON BETWEEN RHD SIMULATION OF SUPERCRITICAL ACCRETION FLOWS AND A STEADY MODEL WITH OUTFLOWS
	Jiao CL(焦承亮); Mineshige, S; Takeuchi, S; Ohsuga, K; Jiao CL(焦承亮)
刊名	ASTROPHYSICAL JOURNAL
	2015-06-10
卷号	806 期号:1
关键词	accretion black hole physics hydrodynamics accretion disks
ISSN号	0004-637X
通讯作者	Jiao, CL (reprint author), Chinese Acad Sci, Yunnan Observ, Kunming 650216, Yunnan, Peoples R China.
产权排序	第一完成单位
英文摘要	We apply our two-dimensional (2D), radially self-similar steady-state accretion flow model to the analysis of hydrodynamic simulation results of supercritical accretion flows. Self-similarity is checked and the input parameters for the model calculation, such as advective factor and heat capacity ratio, are obtained from time-averaged simulation data. Solutions of the model are then calculated and compared with the simulation results. We find that in the converged region of the simulation, excluding the part too close to the black hole, the radial distributions of azimuthal velocity v(phi), density rho and pressure p basically follow the self-similar assumptions, i.e., they are roughly proportional to r(-0.5), r(-n), and r(-(n+1)), respectively, where n similar to 0.85 for the mass injection rate of 1000L(E) lc(2), and n similar to 0.74 for 3000L(E) lc(2) . The distribution of vr and v(theta) agrees less with self-similarity, possibly due to convective motions in the r(theta) plane. The distribution of velocity, density, and pressure in the. direction obtained by the steady model agrees well with the simulation results within the calculation boundary of the steady model. Outward mass flux in the simulations is overall directed toward a polar angle of 0.8382 rad (similar to 48 degrees.0) for 1000L(E)lc(2) and 0.7852 rad (similar to 43 degrees.4) for 3000L(E)lc(2) and similar to 94% of the mass inflow is driven away as outflow, while outward momentum and energy fluxes are focused around the polar axis. Parts of these fluxes lie in the region that is not calculated by the steady model, and special attention should be paid when the model is applied.
学科主题	Astronomy & Astrophysics
类目[WOS]	Astronomy & Astrophysics
研究领域[WOS]	Astronomy & Astrophysics
关键词[WOS]	ADVECTION-DOMINATED ACCRETION ; RADIATION-MAGNETOHYDRODYNAMIC SIMULATIONS ; KERR BLACK-HOLES ; HOT ACCRETION ; SLIM DISKS ; NUMERICAL-SIMULATION ; VERTICAL STRUCTURE ; EMISSION-LINE ; SAGITTARIUS-A ; 2 DIMENSIONS
收录类别	SCI
原文出处	http://iopscience.iop.org/article/10.1088/0004-637X/806/1/93/meta
语种	英语
WOS记录号	WOS:000356810300093
公开日期	2016-05-03
内容类型	期刊论文
源URL	[http://ir.ynao.ac.cn/handle/114a53/7365]
专题	云南天文台_自由探索组云南天文台_中国科学院天体结构与演化重点实验室
通讯作者	Jiao CL(焦承亮)
推荐引用方式 GB/T 7714	Jiao CL,Mineshige, S,Takeuchi, S,et al. COMPARISON BETWEEN RHD SIMULATION OF SUPERCRITICAL ACCRETION FLOWS AND A STEADY MODEL WITH OUTFLOWS[J]. ASTROPHYSICAL JOURNAL,2015,806(1).
APA	焦承亮,Mineshige, S,Takeuchi, S,Ohsuga, K,&Jiao CL.(2015).COMPARISON BETWEEN RHD SIMULATION OF SUPERCRITICAL ACCRETION FLOWS AND A STEADY MODEL WITH OUTFLOWS.ASTROPHYSICAL JOURNAL,806(1).
MLA	焦承亮,et al."COMPARISON BETWEEN RHD SIMULATION OF SUPERCRITICAL ACCRETION FLOWS AND A STEADY MODEL WITH OUTFLOWS".ASTROPHYSICAL JOURNAL 806.1(2015).