AI 中文总结
本研究探讨行星形成早期不同pebble吸积隔离质量模型对超级地球最终性质的影响，发现现有模型无法同时匹配开普勒样本的所有可观测分布，需进一步研究初始条件等因素。
AI 中文摘要
开普勒任务已发现大量拥有超级地球大小行星的行星系统，这些系统呈现出诸多性质，从间距较大、具有不可忽略的偏心率和倾角的行星，到间距紧密、共面且近乎圆形的多行星系统，不一而足。这类系统的可观测性质，如行星-行星间距、多行星数量及轨道形态，会受到形成初期条件的强烈影响。这些条件会通过 pebble 和/或星子吸积影响气态盘阶段行星胚胎的早期生长，进而影响巨撞击阶段行星的最终生长。本研究探究行星形成早期不同极限胚胎隔离质量的假设如何影响内盘中超级地球的最终性质，将我们的模拟观测结果相互比较，并与开普勒样本进行对比。我们测试了 pebble 吸积隔离、流动隔离和迁移反馈隔离等多种 pebble 吸积隔离质量模型，其余参数均采用相同的气态盘参数。我们发现，尽管每个模型都能匹配开普勒星表中至少一种可观测分布，但即便进行极端重加权，它们也无法同时匹配所有分布。我们无法匹配所有观测结果，这表明模拟中我们固定的初始条件和/或建模效应需要进一步研究。本次探索揭示了行星系统的演化方式以及影响我们如今观测到的广泛系统参数的过程，有助于将我们自身的太阳系置于更广阔的背景中。
英文摘要
The Kepler Mission has discovered a plethora of planetary systems with super-Earth sized planets. These systems exhibit many properties, from widely-spaced planets with non-negligible eccentricities and inclinations, to tightly-spaced, coplanar, and nearly circular multi-planet systems. The observable properties of these systems, such as planet-planet spacings, multiplicity and orbital morphology, can be strongly influenced by the initial conditions of formation. These conditions affect the early growth of planetary embryos in the gas disk phase through pebble and/or planetesimal accretion, which then affects the final growth of planets during the giant impact stage. In this work, we investigate how assumptions of different limiting embryo isolation masses during early stages of planet formation affect the final properties of super-Earth planets within the inner disk, comparing our mock-observed results to each other, as well as to the Kepler sample. We test several models of pebble accretion isolation mass, including pebble isolation, flow isolation, and migration feedback isolation and otherwise adopt the same parameters for the gas disk. We find that while each model can match at least one distribution of observables in the Kepler catalog, they fall short of matching all distributions simultaneously, even with extreme reweighting. Our inability to match all observations suggests that the initial conditions and/or modeled effects in our simulations that we held fixed should be investigated. This exploration sheds light on how planetary systems evolve and the processes that influence the wide range of system parameters we observe today, helping place our own Solar System in context.
Comments26 pages, 18 figures. Accepted to MNRAS
