行星的耦合SPH和热化学模型：方法学和火星大小物体的例子
Coupling SPH and thermochemical models of planets: Methodology and example of a Mars-sized body
摘要：
巨大的撞击被认为可以解释类地行星及其卫星的各种特征。然而，到目前为止，大多数模型只考虑了碰撞的直接影响，而没有研究被撞击行星的长期内部演化。在这里，我们提出了一种新的方法，结合三维冲击物理碰撞计算与三维热化学内部演化模型。我们应用相结合的方法，一个巨大的火星大小的身体上的影响示范的例子，使用典型的碰撞参数从以前的研究。虽然在撞击模拟中使用的材料参数（状态方程、流变模型）可能对长期演变产生一定影响，但我们发现，撞击角度是新形成地壳空间分布的最关键参数。结果表明，在正面碰撞之后可以形成二分的地壳格局，而在考虑更可能的擦肩碰撞时，情况并非如此。我们的研究结果强调，整个过程的端到端的3-D计算需要在未来研究大规模影响行星内部演化的影响。
英文摘要：
Giant impacts have been suggested to explain various characteristics of terrestrial planets and their moons. However, so far in most models only the immediate effects of the collisions have been considered, while the long-term interior evolution of the impacted planets was not studied. Here we present a new approach, combining 3-D shock physics collision calculations with 3-D thermochemical interior evolution models. We apply the combined methods to a demonstration example of a giant impact on a Mars-sized body, using typical collisional parameters from previous studies. While the material parameters (equation of state, rheology model) used in the impact simulations can have some effect on the long-term evolution, we find that the impact angle is the most crucial parameter for the resulting spatial distribution of the newly formed crust. The results indicate that a dichotomous crustal pattern can form after a head-on collision, while this is not the case when considering a more likely grazing collision. Our results underline that end-to-end 3-D calculations of the entire process are required to study in the future the effects of large-scale impacts on the evolution of planetary interiors.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
