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Multiphase Gas and the Fractal Nature of Radiative Turbulent Mixing Layers
The Astrophysical Journal Letters ( IF 7.9 ) Pub Date : 2020-05-12 , DOI: 10.3847/2041-8213/ab8d2c
Drummond B. Fielding 1 , Eve C. Ostriker 2 , Greg L. Bryan 1, 3 , Adam S. Jermyn 1
Affiliation  

A common situation in galactic and intergalactic gas involves cold dense gas in motion relative to hot diffuse gas. Kelvin–Helmholtz instability creates a turbulent mixing layer and populates the intermediate-temperature phase, which often cools rapidly. The energy lost to cooling is balanced by the advection of hot high enthalpy gas into the mixing layer, resulting in growth and acceleration of the cold phase. This process may play a major role in determining the interstellar medium and circumgalactic medium phase structure, and accelerating cold gas in galactic winds and cosmic filaments. Cooling in these mixing layers occurs in a thin corrugated sheet, which we argue has an area with fractal dimension D = 5/2 and a thickness that adjusts to match the hot phase mixing time to the cooling time. These cooling sheet properties form the basis of a new model for how the cooling rate and hot gas inflow velocity depend on the size L , cooling time of the mixed phase

中文翻译:

多相气体与辐射湍流混合层的分形性质

银河系和银河系间气体的常见情况涉及相对于热扩散气体运动的冷致密气体。开尔文-亥姆霍兹(Kelvin-Helmholtz)的不稳定性会形成湍流的混合层,并在中间温度阶段填充,该阶段通常会迅速冷却。冷却损失的能量通过热的高焓气体进入混合层的平流来平衡,从而导致冷相的生长和加速。这个过程可能在确定星际中和绕银河系中的相结构,以及在银河风和宇宙细丝中加速冷气体起主要作用。这些混合层中的冷却发生在薄瓦楞纸中,我们认为其分形维数D = 5/2,其厚度可以调整以使热相混合时间与冷却时间匹配。
更新日期:2020-05-12
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