结构形成模拟中的金属和分子冷却
Metal and molecule cooling in simulations of structure formation
摘要：
冷却是导致气体在暗物质势阱中凝结的主要过程，从而导致恒星和结构的形成。在无金属的环境中，主要可用的冷却剂是H、He、H $_2$和HD;一旦气体富含金属，这些冷却剂在定义气体的冷却特性时也变得重要。我们讨论了在小工具-2的分子和金属冷却的温度低于$\rm10^4 K$，气体和污染的时间依赖性的性质从恒星演化。我们已经检查了我们的计划的有效性比较的一些测试运行的结果与以前的宇宙丰度演化和结构形成的计算，发现非常一致。我们还研究了在某些特定情况下分子和金属冷却的相关性，发现HD冷却的加入会导致气体在高红移时的聚集因子更高，而低温下的金属冷却会对冷物体的形成和演化产生显着影响。
英文摘要：
Cooling is the main process leading to the condensation of gas in the dark matter potential wells and consequently to star and structure formation. In a metal-free environment, the main available coolants are H, He, H$_2$ and HD; once the gas is enriched with metals, these also become important in defining the cooling properties of the gas. We discuss the implementation in Gadget-2 of molecular and metal cooling at temperatures lower that $\rm10^4 K$, following the time dependent properties of the gas and pollution from stellar evolution. We have checked the validity of our scheme comparing the results of some test runs with previous calculations of cosmic abundance evolution and structure formation, finding excellent agreement. We have also investigated the relevance of molecule and metal cooling in some specific cases, finding that inclusion of HD cooling results in a higher clumping factor of the gas at high redshifts, while metal cooling at low temperatures can have a significant impact on the formation and evolution of cold objects.
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