Giant Planet Formation

巨行星被观测到靠近它们的主星星，作为热彗星;远离它们的主星星，作为直接成像的巨行星;和更典型的类似于我们太阳系中木星的巨行星。我们知道，大约10%的恒星拥有一颗类似于海王星的行星，这些行星以一种未知的方式与更普遍的亚海王星相连。目前，关于巨行星的形成还有许多未解决的问题。特别是，我们不知道它们是如何达到最终质量的。例如，它们可能只是在特定的时间内吸积;然而，可能有一些基本的过程阻止了吸积。此外，在几个Au处观察到巨行星的堆积，目前还不清楚这是否是由于在这个位置更容易形成行星，或者迁移是否会导致这种堆积。在这个项目中，我们将使用流体动力学模拟和分析理论来研究巨行星的形成;旨在回答上述问题。

Giant planets are observed to appear close to their host star, as Hot Jupiters; far away from their host star, as directly imaged giant planets; and in as more typical giant planets similar to Jupiter in our Solar System. We know that about 10% of all stars host a Jupiter-like planet, and these are connected in an as-yet-unknown way to the more ubiquitous sub-Neptunes. Currently, there are many unsolved problems with regard to giant planet formation. In particular, it is unknown how they reach their final mass. For example, it could be they just accrete for a specific time; however, there could be some fundamental process that stops accretion. In addition, there is an observed pile up of giant planets at a few AU, and it is unknown whether this is due to planet formation occurring more easily at this location or if migration will cause this pile-up. In this project we will use hydrodynamic simulations and analytic theory to investigate giant planet formation; aiming to answer the questions above.