Gas giant planet interactions with protoplanetary discs

行星是由原行星盘形成的。虽然年轻且质量巨大，但这些圆盘预计会在几个木星质量的气体团块上破碎。这些团块最终可能演变成气态巨行星、较小的行星或巨大的褐矮星。这两种结果中的哪一种会实现取决于圆盘与行星之间的相互作用。在这些相互作用中，行星和盘可能以气体和颗粒的形式交换质量，通过辐射交换能量，通过引力扭矩交换角动量。这些关键过程尚未得到详细研究，是本项目的主题。我们将通过三维碟形行星数值模拟和简化的二维模型来研究崩塌前气体团块上的卵石吸积。接下来，将采用对团块内部演化的放大模拟来了解行星状态下卵石吸积的结果。

Planets form out of protoplanetary discs. While young and massive, these discs are expected to fragment on gas clumps of a few Jupiter masses. The clumps may eventually evolve into gas giants, smaller planets or massive brown dwarfs. Which one of these outcomes is realised depends on the disc-planet interactions. In these interactions, the planet and the disc may exchange mass in both gas and grains, energy via radiation andangular momentum via gravitational torques. These key processes have not yet been studied in detail and are the subject of this project. We shall begin the study by looking at pebble accretion onto precollapse gas clumps via both 3D discplanet numerical simulations and simplified 2D models. Next, zoom-in simulations onto the internal evolution of clumps will be employed to understand the outcome of pebble accretion in the planetary regime.