AI 中文总结
研究早期宇宙尘埃丰度超模型预测的情况，通过考虑尘埃冷却等因素，针对不同初始温度和金属丰度研究气体等容冷却，揭示尘埃对气体冷却的影响及颗粒尺寸分布、气体不均匀性等因素的作用。
AI 中文摘要
早期宇宙中观测到的尘埃丰度显著超过假设其在超新星冲击波前有效破坏的模型预测。我们研究了冲击波后尘埃对气体冷却的影响，考虑了各种星际尘埃模型的尘埃冷却和尘埃颗粒的热溅射。针对不同初始温度（从3×10⁵K到3×10⁷K）和金属丰度（从10⁻²Z⊙到2Z⊙）考虑了气体元素的等容冷却。结果表明，在金属丰度低于0.1Z⊙时，尘埃对气体冷却的影响可忽略不计。一些模型中小颗粒的丰度在温度低于10⁶K时显著加速冷却，而大颗粒在高温（>3×10⁶K）时主导冷却。对于初始温度Tg,0>3×10⁶K，某些初始尺寸分布模型中不到10%的尘埃质量存活。颗粒尺寸分布最浅的模型实现了最大存活率（在Tg,0 = 3×10⁶K和太阳金属丰度下高达20%）。还讨论了气体不均匀性的作用：冲击波使尘埃从云中剥离既可以缩短云的寿命，也有助于形成尘埃尾，其中热气体的冷却加速，从而提高尘埃存活率。
英文摘要
The observed dust abundance in the early Universe significantly exceeds the predictions of models assuming its efficient destruction at supernova shock wave fronts. We investigate the effect of dust on gas cooling behind the shock wave front, taking into account both dust cooling and thermal sputtering of dust grains for various interstellar dust models. Isochoric cooling of a gas element is considered for various initial temperatures (from $3\cdot 10^{5}$ K to $3\cdot 10^{7}$ K) and metallicities (from $10^{-2}$ Z$_{\odot}$ to 2 Z$_{\odot}$). It is shown that at metallicities below 0.1 Z$_{\odot}$, the effect of dust on gas cooling is negligible. The abundance of small grains in some models significantly accelerates cooling at temperatures below $10^{6}$ K, whereas large grains dominate cooling at high temperatures ($> 3\cdot 10^{6}$ K). For an initial temperature $T_{g,0} > 3\cdot 10^{6}$ K, less than 10% of the dust mass survives for some models of the initial size distribution. The maximum survival rate (up to 20% at $T_{g,0} = 3\cdot 10^{6}$ K and solar metallicity) is achieved for the model with the shallowest grain size distribution. The role of gas inhomogeneities is discussed: dust stripping from clouds by a shock wave can both decrease the cloud lifetime and contribute to the creation of dust tails, where the cooling of hot gas is accelerated, thereby increasing the dust survival rate.
Comments10 pages, 6 figures published in Astronomy Letters, vol.52, 5, (2026)
