Chemistry in Protoplanetary Disks

TL;DR

This paper reviews the current understanding of chemical processes in protoplanetary disks, highlighting observational and theoretical advances, and discusses future research prospects with upcoming telescopic facilities.

Contribution

It provides a comprehensive summary of modern observational methods, theoretical models, and key findings related to disk chemistry and evolution.

Findings

Chemical diversity in disks due to physical condition variations

Detection of complex organic molecules in disks

Predictions for future observations with ALMA

Abstract

Protoplanetary disks (PPDs) surrounding young stars are short-lived (~0.3-10 Myr), compact (~10-1000 AU) rotating reservoirs of gas and dust. PPDs are believed to be birthplaces of planetary systems, where tiny grains are assembled into pebbles, then rocks, planetesimals, and eventually planets, asteroids, and comets. Strong variations of physical conditions (temperature, density, ionization rate, UV/X-rays intensities) make a variety of chemical processes active in disks, producing simple molecules in the gas phase and complex polyatomic (organic) species on the surfaces of dust particles. In this entry, we summarize the major modern observational methods and theoretical paradigms used to investigate disk chemical composition and evolution, and present the most important results. Future research directions that will become possible with the advent of the Atacama Large Millimeter Array (ALMA) and other forthcoming observational facilities are also discussed.