论文标题
关于完全相互作用系统的寡头增长
On the oligarchic growth in a fully interacting system
论文作者
论文摘要
在行星形成的最终组装阶段，Protoplanets通过行星和行星胚胎之间的碰撞发展。行星形成的效率可以由形成的原始星et与胚胎和行星的初始质量之间的质量比定义。在最终的组装行星形成模型中，由于计算困难，行星模拟之间的重力相互作用通常被忽略，即，以这种方式计算需要更少的资源。我们通过对胚胎和自我相互作用或非自我相互作用的行星模拟的行星形成效率进行建模来研究这种简化的效果。我们将自己开发的基于GPU的直接N体积分器Hiperion用于模拟。我们发现，如果在包含常用100个胚胎的模型中考虑了行星自身交互，则行星形成效率较高。观察到的效果可以通过行星偏心的自我重度来解释。如果胚胎的初始数量高于200，则非自我相互作用和自我相互作用模型在质量上显示出相同的结果。
Protoplanets develop via collisions between planetesimals and planetary embryos in the final assembly stage of planet formation. The efficiency of the planet formation can be defined by the mass ratio between formed protoplanets and the initial mass of embryos and planetesimals. In final assembly planet formation models, the gravitational interactions between planetesimals are usually neglected due to computational difficulties, namely, computations require fewer resources in this way. We investigated the effect of this simplification via modeling the planet formation efficiency in a circumstellar belt of embryos and self-interacting or non-self-interacting planetesimals. We used our own developed GPU-based direct N-body integrator, HIPERION, for the simulations. We found that planet formation efficiency is higher if the planetesimal self-interaction is taken into account in models that contain the commonly used 100 embryos. The observed effect can be explained by the damping of planetesimal eccentricities by their self-gravity. The non-self-interacting and self-interacting models show qualitatively the same results if the initial number of embryos is above 200.
