原始气体巨行星上的星子吸积
Planetesimal Accretion onto Growing Proto-Gas-Giant Planets
摘要：
太阳和太阳外的气体巨星似乎有不同的内部结构和金属丰度。我们研究的背景下，传统的连续吸积形成的情况下，这些分散体的潜在原因。原则上，气体吸积到质量低于地球几倍的核心上，会被残余星子撞击释放的能量所抑制。我们发现，这些星子一般不能通过的核心的平均运动共振，和星子轰击率的抑制，使核心吸积气体很少中断。在从核心到原行星的生长过程中，由于共振相互重叠，被捕获的星子变得动态不稳定，它们的偏心率激发强烈增强。随后的气体阻力导致微行星迁移并与原行星碰撞。这一过程导致了在原行星生长的高级阶段，星子轰击的恢复和激增。这一机制可能解释了木星、土星和凌日系外行星的金属丰度分布之间的核包层结构差异。
英文摘要：
The solar and extra solar gas giants appear to have diverse internal structure and metallicities. We examine a potential cause for these dispersions in the context of the conventional sequential accretion formation scenario. In principle, gas accretion onto cores with masses below several times that of the Earth is suppressed by the energy released from the bombardment of residual planetesimals. We show that these planetesimals generally cannot pass through the mean motion resonances of the cores, and the suppression of planetesimal bombardment rate enables the cores to accrete gas with little interruption. During growth from the cores to protoplanets, as the resonances overlap with each other, the trapped planetesimals become dynamically unstable and their eccentricity excitation is strongly enhanced. Subsequent gas drag induces the planetesimals to migrate and collide with the protoplanet. This process leads to the resumption and a surge of planetesimal bombardment during the advanced stage of the protoplanet growth. This mechanism may account for the diversity of the core-envelope structure between Jupiter, Saturn and the metallicity dispersion inferred from the transiting extra solar planets.
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。
