论文标题
探索行星组成的随机模型I：天王星作为一个例子
Random Models for Exploring Planet Compositions I: Uranus as an Example
论文作者
论文摘要
对行星的内部进行建模很困难，因为少数测量参数不足以限制描述内部结构和组成所涉及的许多变量。一种解决方案是根据有关行星如何形成的论点来调用其他约束。但是，行星的实际结构和构图可能会符合其形成的线索，如果最初的假设不允许这种结构，这将丢失。因此，有趣的是探索允许的构图和结构的空间，以便更好地了解哪些宇宙限制绝对必要。为此，我们描述了一种适合给定质量，半径和惯性矩的随机，单调，密度分布（R）的代码。 整合静水平衡的方程在体内每个点都会给出压力P（r）。然后，我们提供了三种算法来生成单调温度分布，t（r）和相关组成，与Rho-P关系一致和状态方程是一致的。我们将此代码应用于天王星作为概念证明，并表明岩石与水的比率不能大于2。
Modeling the interior of a planet is difficult because the small number of measured parameters is insufficient to constrain the many variables involved in describing the interior structure and composition. One solution is to invoke additional constraints based on arguments about how the planet formed. However, a planet's actual structure and composition may hold clues to its formation which would be lost if this structure were not allowed by the initial assumptions. It is therefore interesting to explore the space of allowable compositions and structures in order to better understand which cosmogonic constraints are absolutely necessary. To this end, we describe a code for generating random, monotonic, density distributions, rho(r), that fit a given mass, radius, and moment of inertia. Integrating the equation of hydrostatic equilibrium gives the pressure, P(r), at each point in the body. We then provide three algorithms for generating a monotonic temperature distribution, T(r), and an associated composition that is consistent with the rho-P relation, and realistic equations of state. We apply this code to Uranus as a proof of concept, and show that the ratio of rock to water cannot be much larger than 2.
