The detection and characterization of large populations of pebbles in protoplanetary disks have motivated the study of pebble accretion as a driver of planetary growth. This review covers all aspects of planet formation by pebble accretion, from dust growth over planetesimal formation to the accretion of protoplanets and fully grown planets with gaseous envelopes. Pebbles are accreted at a very high rate—orders of magnitude higher than planetesimal accretion—and the rate decreases only slowly with distance from the central star. This allows planetary cores to start their growth in much more distant positions than their final orbits. The giant planets orbiting our Sun and other stars, including systems of wide-orbit exoplanets, can therefore be formed in complete consistency with planetary migration. We demonstrate how growth tracks of planetary mass versus semimajor axis can be obtained for all the major classes of planets by integrating a relatively simple set of governing equations.

中文翻译：

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通过卵石吸积形成行星

原行星盘中大量卵石的检测和表征激发了对卵石吸积作为行星增长驱动因素的研究。这篇综述涵盖了由卵石吸积形成的行星的所有方面，从微行星形成过程中的尘埃生长到原行星的吸积和具有气态包层的完全生长的行星。鹅卵石以非常高的速度吸积——比星子吸积高出几个数量级——并且随着距离中心恒星的距离增加，这个速度只会缓慢下降。这允许行星核心在比最终轨道更远的位置开始生长。因此，围绕太阳和其他恒星运行的巨行星，包括宽轨道系外行星系统，可以与行星迁移完全一致地形成。