Chemistry In Protoplanetary Disks

Planets are formed inside disks around young stars. The gas, dust, and ice in these natal disks are the building materials of planets, and therefore their compositions fundamentally shape the final chemical compositions of planets.

In this review, we summarize current observations of molecular lines in protoplanetary disks, from near-infrared to millimeter wavelengths. We discuss the basic types of chemical reactions in disks and the current development of chemical modeling.

In particular, we highlight the progress made in understanding snowline locations, abundances of main carriers of carbon, oxygen, and nitrogen, and complex organic molecules in disks.

Finally, we discuss efforts to trace planet formation history by combining the understanding of disk chemistry and planet formation processes.

Ke Zhang

Comments: Chapter 2 accepted for publication in the Reviews in Mineralogy and Geochemistry (RiMG) Volume 90 on “Exoplanets: Compositions, Mineralogy, and Evolution” edited by Natalie Hinkel, Keith Putirka, and Siyi Xu; 24 pages and 4 figures
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR); Geophysics (physics.geo-ph)
Cite as: arXiv:2404.15423 [astro-ph.EP] (or arXiv:2404.15423v1 [astro-ph.EP] for this version)
Submission history
From: Ke Zhang [via Natalie Hinkel as proxy]
[v1] Tue, 23 Apr 2024 18:18:37 UTC (2,282 KB)
https://arxiv.org/abs/2404.15423

astrobiology