在宇宙学模拟中实施压力调节、反馈调制恒星形成模型的探索：方法及其在 TNG 中的应用
Towards Implementation of the Pressure-Regulated, Feedback-Modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG
AI总结：
本文结合 TIGRESS 校准与 PRFM 理论，在 TNG50 中评估压力调节恒星形成模型，发现其与垂直平衡相符，并预测高密度、高红移下更短的气体耗竭时间。
摘要：
宇宙学星系形成模拟中采用的传统恒星形成子网格模型，例如 Springel 与 Hernquist（2003，以下简称 SH03）的模型，会使用可调参数以满足在局域宇宙中测得的约束。然而近年来，关于湍流、多相、恒星形成星际介质（ISM）的理论和空间分辨模拟已开始产生新的第一性原理模型；这些模型在充分发展后可以取代传统的子网格处方。该方法的优势在于具有物理动机和预测能力，而非经验调参，并允许环境条件变化，而非受制于局域宇宙条件。作为这种新方法的原型，通过将来自 TIGRESS 数值框架的校准与压力调节、反馈调制（PRFM）理论相结合，可以得到气体耗竭时间和有效状态方程的简单公式。以 TNG50 中的星系为对象，我们将“原生”模拟输出与 PRFM 的后处理预测进行比较。在 TNG50 分辨率下，总中平面压力几乎等于 ISM 总重量，表明 TNG50 中的星系接近满足垂直平衡。测得的气体标高也接近理论平衡预测。有效状态方程的斜率相似，但 SH03 的有效速度弥散归一化略高于当前 TIGRESS 模拟给出的值。由于这一点以及高压下 PRFM 反馈产率的降低，PRFM 模型预测在高密度和高红移处气体耗竭时间短于 SH03 模型。我们的结果代表了在宇宙学星系形成模拟中实施新的、经数值校准的子网格算法的第一步。
英文摘要：
Traditional star formation subgrid models implemented in cosmological galaxy formation simulations, such as that of Springel & Hernquist (2003, hereafter SH03), employ adjustable parameters to satisfy constraints measured in the local Universe. In recent years, however, theory and spatially-resolved simulations of the turbulent, multiphase, star-forming ISM have begun to produce new first-principles models, which when fully developed can replace traditional subgrid prescriptions. This approach has advantages of being physically motivated and predictive rather than empirically tuned, and allowing for varying environmental conditions rather than being tied to local Universe conditions. As a prototype of this new approach, by combining calibrations from the TIGRESS numerical framework with the Pressure-Regulated Feedback-Modulated (PRFM) theory, simple formulae can be obtained for both the gas depletion time and an effective equation of state. Considering galaxies in TNG50, we compare the "native" simulation outputs with post-processed predictions from PRFM. At TNG50 resolution, the total midplane pressure is nearly equal to the total ISM weight, indicating that galaxies in TNG50 are close to satisfying vertical equilibrium. The measured gas scale height is also close to theoretical equilibrium predictions. The slopes of the effective equations of states are similar, but with effective velocity dispersion normalization from SH03 slightly larger than that from current TIGRESS simulations. Because of this and the decrease in PRFM feedback yield at high pressure, the PRFM model predicts shorter gas depletion times than the SH03 model at high densities and redshift. Our results represent a first step towards implementing new, numerically calibrated subgrid algorithms in cosmological galaxy formation simulations.
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