TWO-DIMENSIONAL NUMERICAL SIMULATIONS OF SUPERCRITICAL ACCRETION FLOWS REVISITED
文献类型：期刊论文
| 作者 | Yang, Xiao-Hong1,2; Yuan, Feng1 ; Ohsuga, Ken3; Bu, De-Fu1
|
| 刊名 | ASTROPHYSICAL JOURNAL
 |
| 出版日期 | 2014 |
| 卷号 | 780期号:1页码:79 |
| 关键词 | accretion black hole physics hydrodynamics methods: numerical radiative transfer accretion disks |
| 通讯作者 | 袁峰 |
| 英文摘要 | We study the dynamics of super-Eddington accretion flows by performing two-dimensional radiation-hydrodynamic simulations. Compared with previous works, in this paper we include the T-theta phi component of the viscous stress and consider various values of the viscous parameter alpha. We find that when T-theta phi is included, the rotational speed of the high-latitude flow decreases, while the density increases and decreases at the high and low latitudes, respectively. We calculate the radial profiles of inflow and outflow rates. We find that the inflow rate decreases inward, following a power law form of M-in alpha r(s). The value of s depends on the magnitude of alpha and is within the range of similar to 0.4-1.0. Correspondingly, the radial profile of density becomes flatter compared with the case of a constant (M)Over dot (r). We find that the density profile can be described by p(r) alpha r(-p) and the value of p is almost same for a wide range of alpha ranging from alpha = 0.1 to 0.005. The inward decrease of inflow accretion rate is very similar to hot accretion flows, which is attributed to the mass loss in outflows. To study the origin of outflow, we analyze the convective stability of the slim disk. We find that depending on the value of alpha, the flow is marginally stable (when alpha is small) or unstable (when alpha is large). This is different from the case of hydrodynamical hot accretion flow, where radiation is dynamically unimportant and the flow is always convectively unstable. We speculate that the reason for the difference is because radiation can stabilize convection. The origin of outflow is thus likely because of the joint function of convection and radiation, but further investigation is required. |
| WOS标题词 | Science & Technology ; Physical Sciences |
| 类目[WOS] | Astronomy & Astrophysics |
| 研究领域[WOS] | Astronomy & Astrophysics |
| 关键词[WOS] | SLIM-DISK MODEL ; X-RAY SOURCES ; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS ; RADIATION-HYDRODYNAMIC CALCULATION ; BLACK-HOLE ; DOMINATED ACCRETION ; EDDINGTON LUMINOSITY ; 2 DIMENSIONS ; CONVECTION ; ADVECTION |
| 收录类别 | SCI |
| 语种 | 英语 |
| WOS记录号 | WOS:000328937100079 |
| 公开日期 | 2015-02-14 |
| 源URL | [http://119.78.226.72//handle/331011/15852]  |
| 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.Chongqing Univ, Dept Phys, Chongqing 400044, Peoples R China 3.Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan |
| 推荐引用方式 GB/T 7714 | Yang, Xiao-Hong,Yuan, Feng,Ohsuga, Ken,et al. TWO-DIMENSIONAL NUMERICAL SIMULATIONS OF SUPERCRITICAL ACCRETION FLOWS REVISITED[J]. ASTROPHYSICAL JOURNAL,2014,780(1):79. |
| APA | Yang, Xiao-Hong,Yuan, Feng,Ohsuga, Ken,&Bu, De-Fu.(2014).TWO-DIMENSIONAL NUMERICAL SIMULATIONS OF SUPERCRITICAL ACCRETION FLOWS REVISITED.ASTROPHYSICAL JOURNAL,780(1),79. |
| MLA | Yang, Xiao-Hong,et al."TWO-DIMENSIONAL NUMERICAL SIMULATIONS OF SUPERCRITICAL ACCRETION FLOWS REVISITED".ASTROPHYSICAL JOURNAL 780.1(2014):79. |
入库方式： OAI收割
来源：上海天文台
浏览0
下载0
收藏0
其他版本
除非特别说明，本系统中所有内容都受版权保护，并保留所有权利。