flash -light on the ring : hydrodynamic simulations of expanding supernova shells near supermassive black holes
flash -light on the ring : hydrodynamic simulations of expanding supernova shells near supermassive black holes
复制标题
环上的闪光灯：超大质量黑洞附近膨胀的超新星壳的流体动力学模拟
DOI：
10.1093/mnras/stab3723
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发表时间：
2022
影响因子：
4.8
通讯作者：
Vermot, P
中科院分区：
文献类型：
--
作者：
Barna, B;Palouš, J;Ehlerová, S;Wünsch, R;Morris, M R;Vermot, P
银河系中心(GC)中的超大质量黑洞(SMBH)积累质量的方式尚未完全确定。在大尺度上，它是由星系相遇、连接到螺旋臂和旋杆的质量流入，或者是由于星系中心部分超新星(SN)爆炸而膨胀的壳层所控制的。对后一过程的研究需要一套广泛的气体动力学模拟，以探索构成这一现象所需的多维参数空间。本文的目的是扩展我们对SNE在SMBH上诱导吸积作用的重要性的研究，并将全流体动力学程序$\Scriptsize{\mathm{flash}}与使用薄壳近似的计算量小得多的程序$\ScriptSize{\mathm{ring}}$进行比较。我们模拟了具有各种均匀和湍流环境的3D膨胀壳在类似于GC的引力势中。在均匀介质中，我们发现在壳的形状和它们的等效半径在整个演化过程中令人信服地一致，直到它们变成亚音速。在高度不均匀、湍流的介质中，壳的形状和大小以及它们与中心1-PC球体首次接触的时间也有很好的一致性，在那里我们假设它们加入了吸积流。这一比较支持这样的命题，即发生在5hpC的半乳着丝点距离处的SN通常会将1-3mpC的⊙驱动到GC周围的中央1pc。
The way supermassive black holes (SMBHs) in Galactic Centres (GCs) accumulate their mass is not completely determined. At large scales, it is governed by galactic encounters, mass inflows connected to spirals arms and bars, or due to expanding shells from supernova (SN) explosions in the central parts of galaxies. The investigation of the latter process requires an extensive set of gas dynamical simulations to explore the multidimensional parameter space needed to frame the phenomenon. The aims of this paper are to extend our investigation of the importance of SNe for inducing accretion on to an SMBH and carry out a comparison between the fully hydrodynamic code $\scriptsize{\mathrm{FLASH}}$ and the much less computationally intensive code $\scriptsize{\mathrm{RING}}$, which uses the thin shell approximation. We simulate 3D expanding shells in a gravitational potential similar to that of the GC with a variety of homogeneous and turbulent environments. In homogeneous media, we find convincing agreement between $\scriptsize{\mathrm{FLASH}}$ and $\scriptsize{\mathrm{RING}}$ in the shapes of shells and their equivalent radii throughout their whole evolution until they become subsonic. In highly inhomogeneous, turbulent media, there is also a good agreement of shapes and sizes of shells, and of the times of their first contact with the central 1-pc sphere, where we assume that they join the accretion flow. The comparison supports the proposition that an SN occurring at a galactocentric distance of 5 pc typically drives 1–3 M⊙ into the central 1 pc around the GC.