Winds versus jets: a comparison between black hole feedback modes in simulations of idealized galaxy groups and clusters
Winds versus jets: a comparison between black hole feedback modes in simulations of idealized galaxy groups and clusters
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风与喷流：理想化星系群和星团模拟中黑洞反馈模式的比较
DOI：
10.1093/mnras/stad3548
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发表时间：
2024
影响因子：
4.8
通讯作者：
Huško F
中科院分区：
文献类型：
--
作者：
Huško F
利用SWIFT模拟程序，我们比较了不同形式的活动星系核（AGN）反馈在理想星系群和星系团中的作用。我们首先提出了一个物理动机模型的黑洞（BH）的自旋演化和数值实现的热各向同性反馈（代表能量驱动的风的影响）和准直的动能射流，他们在不同的吸积率发射。我们发现，动力喷流反馈是更有效的淬火星星形成在最明亮的星系团（BCGs）比热各向同性反馈，同时产生较冷的核心内集群介质（ICM）。一个混合模型与两种类型的活动星系核反馈产生适度的星星形成率，同时具有最冷的核心。然后，我们考虑一个简化的实施AGN反馈固定的反馈效率和喷流方向，发现相同的一般结论成立。我们改变的反馈能量（反冲速度和加热温度），固定的效率和类型的能量（动力与热）在各向同性和射流的情况下。各向同性情况对这些变化基本上不敏感。另一方面，射流反馈必须是动力学的，以便有效地淬灭。我们还发现，它是更敏感的选择每个反馈事件的能量（射流速度），以及效率。前者表明在宇宙学模拟中需要仔细选择喷流速度，而后者则激发了BH自旋演化模型的使用。
Using theSWIFTsimulation code, we compare the effects of different forms of active galactic nuclei (AGNs) feedback in idealized galaxy groups and clusters. We first present a physically motivated model of black hole (BH) spin evolution and a numerical implementation of thermal isotropic feedback (representing the effects of energy-driven winds) and collimated kinetic jets that they launch at different accretion rates. We find that kinetic jet feedback is more efficient at quenching star formation in the brightest cluster galaxies (BCGs) than thermal isotropic feedback, while simultaneously yielding cooler cores in the intracluster medium (ICM). A hybrid model with both types of AGN feedback yields moderate star formation rates, while having the coolest cores. We then consider a simplified implementation of AGN feedback by fixing the feedback efficiencies and the jet direction, finding that the same general conclusions hold. We vary the feedback energetics (the kick velocity and the heating temperature), the fixed efficiencies and the type of energy (kinetic versus thermal) in both the isotropic and the jet case. The isotropic case is largely insensitive to these variations. On the other hand, jet feedback must be kinetic in order to be efficient at quenching. We also find that it is much more sensitive to the choice of energy per feedback event (the jet velocity), as well as the efficiency. The former indicates that jet velocities need to be carefully chosen in cosmological simulations, while the latter motivates the use of BH spin evolution models.