Importance of the H2abundance in protoplanetary disk ices for the molecular layer chemical composition

2016/09/06 by V. Wakelam, M. Ruaud, F. Hersant +4 · 1 citation
Chemistry · Physics and Astronomy · #Advanced Physical and Chemical Molecular Interactions #Astrochemistry #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Chemical composition #Chemical evolution #Chemical process #Chemical species #Protoplanetary disk #astro-ph.GA

paper · pdf · doi:10.1051/0004-6361/201628748

published as A&A 594, A35 (2016) · Accepted for publication as a Research Note in A&A

arxiv created 2016/09/06 · openalex publication_date 2016/09/07 · openalex created_date 2016/09/16 · arxiv updated 2016/10/07 · openalex updated_date 2026/08/05

Abstract

Context. Protoplanetary disks are the target of many chemical studies (both observational and theoretical) as they contain the building material for planets. Their large vertical and radial gradients in density and temperature make them challenging objects for chemical models. In the outer part of these disks, the large densities and low temperatures provide a particular environment where the binding of species onto the dust grains can be very efficient and can affect the gas-phase chemical composition.

Citations

• A dual-frequency sub-arcsecond study of proto-planetary disks at mm wavelengths: first evidence for radial variations of the dust properties
• Non-thermal desorption from interstellar dust grains via exothermic surface reactions

Cited by

• Sulfur Chemistry in Protoplanetary Disks: CS and H2CS