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The Chemical Evolution of Protoplanetary Disks
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In this review we re-evaluate our observational and theoretical understanding of the chemical evolution of protoplanetary disks. We discuss how improved observational capabilities have enabled the detection of numerous molecules exposing an active disk chemistry that appears to be in disequilibrium. We outline the primary facets of static and dynamical theoretical chemical models. Such models have demonstrated that the observed disk chemistry arises from warm surface layers that are irradiated by X-ray and FUV emission from the central accreting star. Key emphasis is placed on reviewing areas where disk chemistry and physics are linked: including the deuterium chemistry, gas temperature structure, disk viscous evolution (mixing), ionization fraction, and the beginnings of planet formation.
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Cited by 4 Pith papers
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Chemical Divergence and Water Depletion: Gas Properties of Evolved Upper Scorpius Disks Revealed by JWST/MIRI
JWST/MIRI survey of 2-6 Myr Upper Scorpius disks finds diverse chemotypes, 10-1000x lower water luminosities, and evidence that outer dust traps control inner-disk chemistry.
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Gas Phase Ion Species Released During Grain Collisions: Implications For Protoplanetary Disks
Colliding glass beads release water-related molecules detected by mass spectrometry, giving the first species-level evidence that grain collisions can contribute water to protoplanetary disk gas.
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Formation and Early Evolution of Protoplanetary Disks under Nonuniform Cosmic-Ray Ionization
Cosmic-ray absorption inside forming disks lowers the ionization rate there, weakens magnetic angular momentum transport, and produces larger, more gravitationally unstable disks with stronger spiral arms than uniform...
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Tracking the Chemical Evolution of Hydrocarbons Through Carbon Grain Supply in Protoplanetary Disks
In chemical models of inner protoplanetary disk gas, X-ray-driven chemistry stores carbon in long-chain hydrocarbons and CO, while UV-driven chemistry stores it in atomic carbon and CO, and water strongly enhances C2H2.
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