| DOI | Trouver le DOI : https://doi.org/10.1016/j.icarus.2009.05.024 |
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| Auteur | Rechercher : Cavalié, T.; Rechercher : Billebaud, F.; Rechercher : Dobrijevic, M.; Rechercher : Fouchet, T.; Rechercher : Lellouch, E.; Rechercher : Encrenaz, T.; Rechercher : Brillet, J.; Rechercher : Moriarty-Schieven, G. H.1; Rechercher : Wouterloot, J. G. A.; Rechercher : Hartogh, P. |
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| Affiliation | - Conseil national de recherches Canada. Institut Herzberg d'astrophysique du CNRC
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| Format | Texte, Article |
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| Sujet | Saturn; atmosphere; spectroscopy |
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| Résumé | We have performed the first observation of the CO(3-2) spectral line in the atmosphere of Saturn with the James Clerk Maxwell Telescope. We have used a transport model of the atmosphere of Saturn to constrain the origin of the observed CO. The CO line is best-fit when the CO is located at pressures less than (15 +- 2) mbar with a mixing ratio of (2.5 +- 0.6) x 10(-8)implying an external origin. By modeling the transport in Saturn’s atmosphere, we find that a cometary impact origin with an impact 200–350 years ago is more likely than continuous deposition by interplanetary dust particles (IDP) or local sources (rings/satellites). This result would confirm that comet impacts are relatively frequent and efficient providers of CO to the atmospheres of the outer planets. However, a diffuse and/or local source cannot be rejected, because we did not account for photochemistry of oxygen compounds. Finally, we have derived an upper limit of ∼1 x 10(-9) on the tropospheric CO mixing ratio. |
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| Date de publication | 2009-06-09 |
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| Maison d’édition | Elsevier |
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| Dans | |
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| Langue | anglais |
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| Publications évaluées par des pairs | Oui |
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| Numéro NPARC | 23004904 |
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| Exporter la notice | Exporter en format RIS |
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| Signaler une correction | Signaler une correction (s'ouvre dans un nouvel onglet) |
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| Identificateur de l’enregistrement | c7d7ddd6-bea4-417b-a04b-5f0e75193d6c |
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| Enregistrement créé | 2019-01-18 |
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| Enregistrement modifié | 2020-04-16 |
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