English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/208814
logo share SHARE logo core CORE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL | DATACITE
Exportar a otros formatos:


Silicate-mediated interstellar water formation: a theoretical study

AuthorsMolpeceres, Germán ; Rimola, Albert; Ceccarelli, C.; Kästner, Johannes; Ugliengo, Piero; Maté, Belén
Molecular processes
ISM: molecules
ISM: atoms
Issue Date10-Nov-2019
PublisherRoyal Astronomical Society
CitationMonthly Notices of the Royal Astronomical Society 482: 5389-5400 (2019)
AbstractWater is one of the most abundant molecules in the form of solid ice phase in the different regions of the interstellar medium (ISM). This large abundance cannot be properly explained by using only traditional low-temperature gas-phase reactions. Thus, surface chemical reactions are believed to be major synthetic channels for the formation of interstellar water ice. Among the different proposals, hydrogenation of atomic O (i.e. 2H + O ¿ H2O) is a chemically `simple¿ and plausible reaction toward water formation occurring on the surfaces of interstellar grains. Here, novel theoretical results concerning the formation of water adopting this mechanism on the crystalline (010) Mg2SiO4 surface (a unequivocally identified interstellar silicate) are presented. The investigated reaction aims to simulate the formation of the first water ice layer covering the silicate core of dust grains. Adsorption of the atomic O as a first step of the reaction has been computed, results indicating that a peroxo (O2¿2¿) group is formed. The following steps involve the adsorption, diffusion, and reaction of two successive H atoms with the adsorbed O atom. Results indicate that H diffusion on the surface has barriers of 4¿6 kcal mol¿1, while actual formation of OH and H2O present energy barriers of 22¿23 kcal mol¿1. Kinetic study results show that tunneling is crucial for the occurrence of the reactions and that formation of OH and H2O are the bottlenecks of the overall process. Several astrophysical implications derived from the theoretical results are provided as concluding remarks.
Description12 pags. 6 figs., 2 tabs.
Publisher version (URL)http://dx.doi.org/10.1093/mnras/sty3024
Identifiersdoi: 10.1093/mnras/sty3024
issn: 00358711
Appears in Collections:(CFMAC-IEM) Artículos
Files in This Item:
File Description SizeFormat 
Silicate-mediated.pdf2,79 MBAdobe PDFThumbnail
Show full item record
Review this work

WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.