CO₂ formation on interstellar dust grains: a detailed study of the barrier of the CO + O channel

¹ LERMA, UMR8112 du CNRS, de l’Observatoire de Paris et de l’Université de Cergy Pontoise, 5 mail Gay Lussac, 95000 Cergy Pontoise Cedex, France
e-mail: marco.minissale@obspm.fr
² Dipartimento di Fisica ed Astronomia, Universitá degli Studi di Catania, via Santa Sofia 64, 95123 Catania, Italy

Received: 12 March 2013
Accepted: 5 September 2013

Abstract

Context. The formation of carbon dioxide in quiescent regions of molecular clouds has not yet been fully understood, even though CO₂ is one of the most abundant species in interstellar ices.

Aims. CO₂ formation is studied via oxidation of CO molecules on cold surfaces under conditions close to those encountered in quiescent molecular clouds.

Methods. Carbon monoxide and oxygen atoms are codeposited using two differentially pumped beam lines on two different surfaces (amorphous water ice or oxydized graphite) held at given temperatures between 10 and 60 K. The products are probed via mass spectroscopy by using the temperature-programmed desorption technique.

Results. We show that the reaction CO + O can form carbon dioxide in solid phase with an efficiency that depends on the temperature of the surface. The activation barrier for the reaction, based on modelling results, is estimated to be in the range of 780−475 K/k_b. Our model also allows us to distinguish the mechanisms (Eley Rideal or Langmuir-Hinshelwood) at play in different temperature regimes. Our results suggest that competition between CO₂ formation via CO + O and other surface reactions of O is a key factor in the yields of CO₂ obtained experimentally.

Conclusions. CO₂ can be formed by the CO + O reaction on cold surfaces via processes that mimic carbon dioxide formation in the interstellar medium. Astrophysically, the presence of CO₂ in quiescent molecular clouds could be explained by the reaction CO + O occurring on interstellar dust grains.