宇宙学模拟中的流体动力学方法与次网格模型

Thu, 25 Jun 2026 00:00:00 +0000

原文信息

出处：Numerical Simulations in Cosmology: Chapter 3 — Hydrodynamic methods and sub-resolution models for cosmological simulations

作者：Milena Valentini (Universitá degli Studi di Trieste / INAF), Klaus Dolag (LMU München / MPI for Astrophysics)

arXiv：arXiv:2502.06954 页数：61 页，14 幅图

翻译说明：

中文翻译，段落对照，上面是中文，下面是英文。
Chinese translation, paragraph by paragraph, with Chinese on top and English below.
虚线下划线为个人添加的注释或评论。文献引用如 ^[1] 可点击复制完整引用信息。

§3.3 基本方程与技术

Thu, 25 Jun 2026 00:00:00 +0000

过去几十年中，人们发展了多种数值方案来求解描述宇宙重子成分与无碰撞暗物质的耦合方程组。绝大多数重子（即气体）可被描述为理想流体，其演化由一组方程——即欧拉方程——所支配。积分上述方程的流体求解器可归为两大类，如Fig. 2所示：粒子方法（离散化质量，见^[47] 及其参考文献）和网格方法（离散化计算域，见^[48] 及其参考文献）。近年来又涌现出新的求解器：它们融合了两种方法的特征（见^[49] 及其参考文献），将在后续章节中详细讨论。

A variety of numerical schemes has been developed in the past decades to solve the coupled system of equations describing the baryonic content of the Universe and the collisionless DM. The majority of the baryons (i.e. gas) can be described as an ideal fluid, whose evolution is ruled by a set of equations, namely, the Euler equations. The hydro solvers which integrate the aforementioned equations fall into two main categories, that are summarized in Fig. 2: particle methods, which discretize mass (see ^[47] and references therein), and grid-based methods, which discretize the computational domain (see ^[48] and references therein). Recently, additional solvers have been developed: they combine characteristics of both methods (see ^[49] and references therein) and will be discussed in detail in the following sections.

Numerical:hydrodynamics:AMR on NumericAstronomy

宇宙学模拟中的流体动力学方法与次网格模型

§3.3 基本方程与技术