Relativistic Bondi-Hoyle-Lyttleton accretion: A parametric study

被引:5
|
作者
Blakely, P. M. [1 ]
Nikiforakis, N. [1 ]
机构
[1] Univ Cambridge, Cavendish Lab, Dept Phys, Comp Sci Lab, Cambridge CB3 0HE, England
来源
ASTRONOMY & ASTROPHYSICS | 2015年 / 583卷
基金
英国工程与自然科学研究理事会;
关键词
methods: numerical; accretion; accretion disks; hydrodynamics; shock waves; black hole physics; MOVING BLACK-HOLE; HYDRODYNAMICS; SIMULATIONS; GRADIENTS; SYSTEMS;
D O I
10.1051/0004-6361/201525763
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Aims. We investigate Bondi-Eloyle-Lyttleton accretion onto a black hole for ultra-relativistic :flows, and how flow features are affected by density perturbations, upstream fluid velocity, and black hole spin. Methods. We use high-resolution shock-capturing (HRSC) schemes solved on curvilinear overlapping grids as demonstrated in a previous publication. Results. We demonstrate the quantitative dependence of the shock-angle and mass accretion rate on black hole spin, upstream fluid velocity, and density perturbations. We also demonstrate the qualitative dependence of the accretion region and flow features on the same parameters. Conclusions. We find that the mass accretion rate does not depend strongly on these parameters, and most of the difference in flow is seen in the shock angle and general flow patterns close to the black-hole, as previously predicted by lower-dimensional simulations. Moreover, we demonstrate independence of initial conditions in that a steady flow around a non-spinning black-hole which suddenly starts to spin will converge to the same flow pattern as if the black-hole had been spinning initially.
引用
收藏
页数:18
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