论文标题
由巨大影响形成的行星系统的轨道结构：恒星质量依赖性
Orbital structure of planetary systems formed by giant impacts: stellar mass dependence
论文作者
论文摘要
最近的系外行星调查显示，对于太阳能型恒星，近距离地球无处不在，其中许多都在多星际系统中。这些系统比太阳系的陆地行星更紧凑。但是，关于低质量恒星周围这种行星形成的理论研究很少。在标准模型中，陆地行星形成的最后阶段是巨大的冲击阶段，在该阶段，原始星et重力散射并相互碰撞，然后演变成稳定的行星系统。我们研究了恒星质量对巨大影响形成的行星系统结构的影响。我们在恒星周围进行{\ it n} - 体仿真，质量是太阳能质量的0.1--2倍。使用原始星网的隔离质量，我们从中央恒星中分布在0.05--0.15 au中的初始原始球星，并遵循最内向的原始球星的2亿轨道时期的进化。我们发现，对于给定的Protoplanet系统，随着恒星质量的减少，行星的质量增加，而行星数量减少。轨道的偏心和倾斜度以及相邻行星的轨道分离随着恒星质量的减少而增加。这是因为随着恒星质量的减小，行星散射的相对强度变得更加有效。我们还讨论了使用最小质量质量的星云模型在宜居区中形成的行星的特性。
Recent exoplanet surveys revealed that for solar-type stars, close-in Super-Earths are ubiquitous and many of them are in multi-planet systems. These systems are more compact than the Solar System's terrestrial planets. However, there have been few theoretical studies on the formation of such planets around low-mass stars. In the standard model, the final stage of terrestrial planet formation is the giant impact stage, where protoplanets gravitationally scatter and collide with each other and then evolve into a stable planetary system. We investigate the effect of the stellar mass on the architecture of planetary systems formed by giant impacts. We perform {\it N}-body simulations around stars with masses of 0.1--2 times the solar mass. Using the isolation mass of protoplanets, we distribute the initial protoplanets in 0.05--0.15 au from the central star and follow the evolution for 200 million orbital periods of the innermost protoplanet. We find that for a given protoplanet system, the mass of planets increases as the stellar mass decreases, while the number of planets decreases. The eccentricity and inclination of orbits and the orbital separation of adjacent planets increase with decreasing the stellar mass. This is because as the stellar mass decreases, the relative strength of planetary scattering becomes more effective. We also discuss the properties of planets formed in the habitable zone using the minimum-mass extrasolar nebula model.
