Planets form in disks of gas and dust around young stars. The disk molecular reservoirs and their chemical evolution affect all aspects of planet formation, from the coagulation of dust grains into pebbles to the elemental and molecular compositions of the mature planet. Disk chemistry also enables unique probes of disk structures and dynamics, including those directly linked to ongoing planet formation. We review the protoplanetary disk chemistry of the volatile elements H, O, C, N, S, and P; the associated observational and theoretical methods; and the links between disk and planet chemical compositions. Three takeaways from this review are: ▪The disk chemical composition, including the organic reservoirs, is set by both inheritance and in situ chemistry.▪Disk gas and solid O/C/N/H elemental ratios often deviate from stellar values due to a combination of condensation of molecular carriers, chemistry, and dynamics.▪Chemical, physical, and dynamical processes in disks are closely linked, which complicates disk chemistry modeling, but these links also present an opportunity to develop chemical probes of different aspects of disk evolution and planet formation.

中文翻译：

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原行星盘化学


行星在年轻恒星周围形成气体和尘埃盘。盘状分子储层及其化学演化影响着行星形成的方方面面，从尘埃颗粒凝结成鹅卵石到成熟行星的元素和分子组成。盘化学还可以对盘结构和动力学进行独特的探测，包括与正在进行的行星形成直接相关的结构和动力学。我们回顾了挥发性元素 H、O、C、N、S 和 P 的原行星盘化学;相关的观察和理论方法;以及圆盘和行星化学成分之间的联系。这篇综述的三个要点是：▪盘的化学成分，包括有机储层，是由遗传和原位化学决定的。▪由于分子载体的凝结、化学和动力学的结合，盘状气体和固体 O/C/N/H 元素比经常偏离恒星值。 ▪ 这使得盘化学建模复杂化，但这些链接也为开发盘演化和行星形成不同方面的化学探针提供了机会。