用PLUTO程序模拟辐射天体物理流：一个非平衡多组分冷却函数
Simulating radiative astrophysical flows with the PLUTO code: A non-equilibrium, multi-species cooling function
摘要：
随时间变化的冷却过程在天体物理学气态星云的演化过程中，特别是在存在辐射激波的情况下，是至关重要的。目前的工作介绍了一套必要的工具，可用于模拟辐射天体物理流动的光学薄等离子体的限制。我们的目标是提供可靠和准确的预测的发射线比和辐射冷却损失的天体物理模拟的冲击流。此外，我们讨论了数值实现方面，以方便未来的改进和实施在其他MHD数值代码。对于我们的等离子体条件，辐射冷却的最重要来源来自碰撞激发线辐射。我们发展了一个化学网络，包括29个离子物种，在非平衡条件下计算电离平衡。经过一系列的验证和测试，典型的天体物理设置在一维和二维模拟，采用本冷却模型和简化的。冷却模型对结构形态的影响可能变得重要，特别是对于发射线诊断目的。
英文摘要：
Time-dependent cooling processes are of paramount importance in the evolution of astrophysical gaseous nebulae and, in particular, when radiative shocks are present. The present work introduces a necessary set of tools that can be used to model radiative astrophysical flows in the optically-thin plasma limit. We aim to provide reliable and accurate predictions of emission line ratios and radiative cooling losses in astrophysical simulations of shocked flows. Moreover, we discuss numerical implementation aspects to ease future improvements and implementation in other MHD numerical codes. The most important source of radiative cooling for our plasma conditions comes from the collisionally-excited line radiation. We evolve a chemical network, including 29 ion species, to compute the ionization balance in non-equilibrium conditions. After a series of validations and tests, typical astrophysical setups are simulated in 1D and 2D, employing both the present cooling model and a simplified one. The influence of the cooling model on structure morphologies can become important, especially for emission line diagnostic purposes.
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