Silicate-mediated interstellar water formation: A theoretical study.

ISM: atoms ISM: molecules astrochemistry molecular processes

Journal

Monthly notices of the Royal Astronomical Society
ISSN: 0035-8711
Titre abrégé: Mon Not R Astron Soc
Pays: England
ID NLM: 100954591

Informations de publication

Date de publication:
14 May 2019
Historique:
entrez: 4 6 2019
pubmed: 4 6 2019
medline: 4 6 2019
Statut: ppublish

Résumé

Water 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 (

Identifiants

pubmed: 31156274
doi: 10.1093/mnras/sty3024
pmc: PMC6544534
mid: EMS82852
doi:

Types de publication

Journal Article

Langues

eng

Pagination

5389-5400

Subventions

Organisme : European Research Council
ID : 610256
Pays : International

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Auteurs

Germán Molpeceres (G)

Instituto de Estructura de la Materia, IEM-CSIC, Serrano 123, E-28006, Madrid, Spain.

Albert Rimola (A)

Departament de Química, Universitat Autònoma de Barcelona, 08193 Bellaterra, Spain.

Cecilia Ceccarelli (C)

Univ. Grenoble Alpes, CNRS, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 38000 Grenoble, France.

Johannes Kästner (J)

Institute for Theoretical Chemistry, University of Stuttgart, Pfaffenwaldring 55, 70569 Stuttgart, Germany.

Piero Ugliengo (P)

Dipartimento di Chimica and Nanostructured Interfaces and Surfaces (NIS), Università degli Studi di Torino, Via P. Giuria 7, 10125 Torino, Italy.

Belén Maté (B)

Instituto de Estructura de la Materia, IEM-CSIC, Serrano 123, E-28006, Madrid, Spain.

Classifications MeSH