Cooling-driven coagulation

Cooling-driven coagulation
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冷却驱动凝固

DOI:
10.1093/mnras/stad1874
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发表时间:
2023
影响因子:
4.8
通讯作者:
Oh, S. Peng
Oh, S. Peng
中科院分区:
物理与天体物理2区
文献类型:
--
作者:
Gronke, Max;Oh, S. Peng

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天体物理气体,如星际、环银河或团内介质通常是多相的,这就提出了这些系统的结构问题。虽然有许多已知的过程导致嵌入在(湍流)热介质中的冷气体的破碎,但在这项工作中,我们专注于相反的过程:凝聚。这在风洞和剪切层模拟中经常看到,在这些模拟中,冷气体碎片自发地合并。使用二维和三维流体动力学模拟,我们发现,足够大的(cascstcool),扰动冷气体云发展脉动,确保冷气体质量增长在一段较长的时间(cascr/cs)。这种质量增长有效地加速了热气体,这反过来又可以夹带冷液滴,导致凝结。冷气滴之间的平方反比吸引力与重力有着有趣的相似之处;“重力”是表面积而不是质量。我们开发了一个简单的分析模型,再现我们的数值结果。
Astrophysical gases such as the interstellar-, circumgalactic-, or intracluster-medium are commonly multiphase, which poses the question of the structure of these systems. While there are many known processes leading to fragmentation of cold gas embedded in a (turbulent) hot medium, in this work, we focus on the reverse process: coagulation. This is often seen in wind-tunnel and shearing layer simulations, where cold gas fragments spontaneously coalesce. Using 2D and 3D hydrodynamical simulations, we find that sufficiently large (≫cstcool), perturbed cold gas clouds develop pulsations which ensure cold gas mass growth over an extended period of time (≫r/cs). This mass growth efficiently accelerates hot gas which in turn can entrain cold droplets, leading to coagulation. The attractive inverse square force between cold gas droplets has interesting parallels with gravity; the ‘monopole’ is surface area rather than mass. We develop a simple analytic model which reproduces our numerical findings.
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