论文标题
改善流体动力模拟中的黑洞积聚处理
Improving Black Hole Accretion Treatment in Hydrodynamical Simulations
论文作者
论文摘要
大银河尺度与许多数量级相连，通过喂食和反馈的情节循环，较小的超级质量黑洞（SMBH）尺度。主动银河核（AGN）由积聚到SMBH上的动力，在近伊德丁顿政权中，大多数AGN能量是在薄的SUB-PC增生盘中生产的。目前，很难建模在巨大不同尺度上发生的过程，范围从数十个处于数十的环糖气储存到数百个parsec，到<0.01 pc的积分盘量表。尽管在大规模或宇宙学模拟中使用的子网格处方能够再现大规模反馈，但我们建议在parsec尺度模拟中使用更现实的模型使用更现实的模型，在这种模拟中，重要的是要获得准确的时间表以了解反馈如何影响AGN AGN的气体动力学和恒星形成。为了测试我们的方法，我们在一组水动力模拟中，在与SPH Code Gadget-3类似的环境中，在与银河中心类似的环境中，在一组水动力模拟中，使用子分辨率的薄积分盘模型。与瞬时喂养处方相比，SMBH的椎间盘介导的摄食相对平滑且延迟。尽管在积聚盘和瞬时喂养模拟中都存在减少因反馈而产生的积聚，但仅在积聚盘中才能出现明显的中央空腔 - 暗示挥发性较小的增生阶段可能对周围气体产生更大的影响。
The large galactic scales are connected to the many orders of magnitude smaller supermassive black hole (SMBH) scales by an episodic cycle of feeding and feedback. Active galactic nuclei (AGN) are powered by accretion onto SMBH and the majority of AGN energy, in near-Eddington regime, is produced in thin sub-pc accretion discs. Currently, it is very difficult to model processes that occur on vastly different scales, ranging from the circumnuclear gas reservoirs at tens to hundreds of parsecs, down to the accretion disc scales at <0.01 pc. While sub-grid prescriptions used in large-scale or cosmological simulations are able to reproduce large-scale feedback, we propose using a more realistic model in parsec-scale simulations, where it is important to get accurate timescales to understand how feedback affects gas dynamics and star formation in the vicinity of the AGN. To test our approach we use a sub-resolution thin accretion disc model, coupled to the SMBH, in a set of hydrodynamical simulations of a retrograde collision between a gas ring and a molecular cloud in an environment similar to the Galactic centre using the SPH code Gadget-3. The disc-mediated feeding of the SMBH is relatively smooth and delayed compared to an instantaneous feeding prescription. While the reduction of accretion due to feedback is present in both accretion disc and instantaneous feeding simulations, a clear central cavity appears only in accretion disc runs - hinting that a less volatile accretion phase could have a greater impact on the surrounding gas.
