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arXiv 2203.09759astro-ph.EPastro-ph.SR
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ALMA和Kepler时代的行星形成理论：从卵石到系外行星

Planet Formation Theory in the Era of ALMA and Kepler: from Pebbles to Exoplanets

Joanna Drazkowska, Bertram Bitsch, Michiel Lambrechts, Gijs D. Mulders, Daniel Harsono, Allona Vazan, Beibei Liu, Chris W. Ormel, Katherine Kretke, Alessandro Morbidelli

备注：
38 pages, 13 figures, review chapter accepted to Protostars and Planets VII, editors: Shu-ichiro Inutsuka, Yuri Aikawa, Takayuki Muto, Kengo Tomida, and Motohide Tamura, corrected label in Fig. 1
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AI总结：

本文综述了ALMA和Kepler时代行星形成理论的新进展，包括从尘埃到行星核的吸积生长、种群合成模型，并强调盘内行星形成的空间不均匀性及卵石吸积的关键作用。

摘要：

近年来，我们对行星形成的理解在迅速发展。当唯一已知的行星系统还是我们自己的太阳系时，发展出的经典行星形成理论已被修正，以解释观测到的系外行星系统的多样性。同时，对年轻恒星及其周围盘的观测能力的提升，为行星形成过程带来了新的约束。在本章中，我们总结了从系外行星群和环星盘观测中得出的新信息。我们介绍了行星形成理论的新进展，从尘埃演化到通过吸积星子、卵石和气体使行星核生长。我们回顾了用于形成多样行星系统的最先进模型，包括将理论模型结果与系外行星群进行比较所必需的种群合成方法。我们强调，行星形成过程在盘中可能不是空间均匀的，并且存在星子和行星形成的优先位置。在这些位置之外，很大一部分固体不会增长超过卵石大小。卵石储层在卵石吸积过程中的行星核生长中起着重要作用。大质量行星核出现的时间尺度是当前模型的一个重要方面，并且一个盘内的核很可能在不同时间形成。此外，越来越多的证据表明，第一批行星核在环星盘形成过程中很早就开始形成。

英文摘要：

Our understanding of planet formation has been rapidly evolving in recent years. The classical planet formation theory, developed when the only known planetary system was our own Solar System, has been revised to account for the observed diversity of the exoplanetary systems. At the same time, the increasing observational capabilities of the young stars and their surrounding disks bring new constraints on the planet formation process. In this chapter, we summarize the new information derived from the exoplanets population and the circumstellar disks observations. We present the new developments in planet formation theory, from dust evolution to the growth of planetary cores by accretion of planetesimals, pebbles, and gas. We review the state-of-the-art models for the formation of diverse planetary systems, including the population synthesis approach which is necessary to compare theoretical model outcomes to the exoplanet population. We emphasize that the planet formation process may not be spatially uniform in the disk and there are preferential locations for the formation of planetesimals and planets. Outside of these locations, a significant fraction of solids is not growing past the pebble-sizes. The reservoir of pebbles plays an important role in the growth of planetary cores in the pebble accretion process. The timescale of the emergence of massive planetary cores is an important aspect of the present models and it is likely that the cores within one disk form at different times. In addition, there is growing evidence that the first planetary cores start forming early, during the circumstellar disk buildup process.

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