Chemistry in Protoplanetary Disks

Details Chemistry in Protoplanetary Disks Chemistry in Protoplanetary Disks

2010-11-22

arxiv.org/abs/1011.4770v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

14 pages, 2 figures, 2 tables, pre-final chapter to be published in Encyclopedia of Astrobiology by Gargaud, M.; Cernicharo, J

Scientific paper

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.

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