AI 中文总结
本研究对比凌日多行星与共振行星系统轨道半长轴和原行星盘关键半径，明确盘驱动迁移决定行星系统内边缘，动力学迁移塑造半长轴分布，为解释行星系统结构提供了关键观测与理论依据。
AI 中文摘要
本研究旨在增进对原行星盘内≤1.5天文单位区域中，盘驱动迁移与行星-行星动力学迁移在塑造行星系统结构方面的竞争作用的理解。在一系列主恒星质量范围内，我们将凌日多行星系统与共振系统的轨道半长轴数值，与观测得到的原行星盘内截断半径Ri、共转半径Rco及尘埃升华半径Rdust的估计值进行比较。研究发现，盘驱动迁移是决定行星系统内边缘位置的主要因素，该内边缘靠近Rco；后续动力学迁移则塑造了行星半长轴在≈20-300R★范围内的分布。若多行星系统的形成方式与共振链系统相似，则要么意味着在≥100R★处存在一个高效行星形成区，随后发生盘驱动迁移；要么需要一个修正的原位机制，该机制在≈15-100R★的区域内运行并结合盘驱动迁移。有迹象表明，原行星盘消散后，动力学迁移会导致部分行星迁移至Rco以内的位置。
英文摘要
In this study, we seek to improve our understanding of the competing roles of disk-driven and planet-planet dynamical migration in sculpting planetary system architecture in the inner $\lesssim 1.5$ au of protoplanetary disks. Over a range of host star masses, we compare the orbit semimajor axis values of transiting multi-planet and resonant systems to observationally-derived estimates of protoplanetary disk inner truncation radius $R_{i}$, corotation radius $R_{co}$, and dust sublimation radius $R_{dust}$. We find that disk-driven migration is primarily responsible for setting the inner edge of planetary systems near $R_{co}$ and that subsequent dynamical migration shapes the distribution of planetary semimajor axis values over the range $\approx 20-300$ $R_{\star}$. If multi-planet systems form in a way similar to the resonant chain systems, either a zone of highly efficient planet formation at $\gtrsim 100 R_{\star}$, followed by subsequent disk-driven migration, is implied, or a modified in-situ mechanism operating over a region from $\simeq 15-100 R_{\star}$ and incorporating disk-driven migration is needed. There are indications that after disk dispersal, dynamical migration causes a subset of planets to migrate to locations inside $R_{co}$.
Commentssubmitted to AAS Journals
