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On the origin of O2 and other volatile species in comets

Published online by Cambridge University Press:  04 September 2018

Vianney Taquet ,
Kenji Furuya ,
Catherine Walsh Open the ORCID record for Catherine Walsh [Opens in a new window]  and
Ewine F. van Dishoeck
Vianney Taquet
Affiliation:
Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy
Kenji Furuya
Affiliation:
Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands Center for Computational Sciences, University of Tsukuba, 1-1-1 Tennoudai, 305-8577, Tsukuba, Japan
Catherine Walsh
Affiliation:
Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT, UK
Ewine F. van Dishoeck
Affiliation:
Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands Max-Planck-Institut fur Extraterrestrische Physik, Giessenbachstrasse, 85741, Garching, Germany
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Abstract

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Molecular oxygen, O2, was recently detected in comet 67P by the ROSINA instrument on board the Rosetta spacecraft with a surprisingly high abundance of 4% relative to H2O, making O2 the fourth most abundant in comet 67P. Other volatile species with similar volatility, such as molecular nitrogen N2, were also detected by Rosetta, but with much lower abundances and much weaker correlations with water. Here, we investigate the chemical and physical origin of O2 and other volatile species using the new constraints provided by Rosetta. We follow the chemical evolution during star formation with state-of-the-art astrochemical models applied to dynamical physical models by considering three origins: i) in dark clouds, ii) during forming protostellar disks, and iii) during luminosity outbursts in disks. The models presented here favour a dark cloud (or “primordial”) grain surface chemistry origin for volatile species in comets, albeit for dark clouds which are slightly warmer and denser than those usually considered as solar system progenitors.

Keywords

astrochemistrycomets: individual: 67P/C-GISM: abundancesISM: moleculesprotoplanetary discsstars: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S332: Astrochemistry VII: Through the Cosmos from Galaxies to Planets , March 2017 , pp. 187 - 195
Copyright
Copyright © International Astronomical Union 2018 

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