Afficher la notice abrégée

Observations of CO on Saturn and Uranus at millimeter wavelengths: New upper limit determinations

hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorCAVALIÉ, T.
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorBILLEBAUD, F.
hal.structure.identifierLaboratoire d'études spatiales et d'instrumentation en astrophysique [LESIA]
dc.contributor.authorFOUCHET, T.
hal.structure.identifierLaboratoire d'études spatiales et d'instrumentation en astrophysique [LESIA]
dc.contributor.authorLELLOUCH, E.
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorBRILLET, J.
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorDOBRIJEVIC, M.
dc.date.issued2008
dc.identifier.issn0004-6361
dc.description.abstractEnWe tried to detect CO lines at millimeter wavelength on Saturn and Uranus in order to better constrain the origin of this compound in the atmospheres of these planets. CO sources can be either of internal or of external origin. Methods. We recorded broad multi-band spectra of Saturn and Uranus at the frequencies of the J=1"0 and J=2"1 CO lines, at the IRAM 30m-telescope, Spain, using Lellouch et al. (2005) and Hesman et al. (2007) observing technique. Results. As we do not detect any CO line in the spectra, we derive new upper limits of the abundance of CO in the atmospheres of Saturn and Uranus. The value we obtain for Saturn (6.3×10−8, restricted to the stratosphere) is larger than the value of the CO mixing ratio in the external origin model of Noll & Larson (1991). New observations with better sensitivity and/or more observing time should enable us to state on the CO external source strength. The upper limit we derive on Uranus is slightly lower (2.7 × 10−8, restricted to the stratosphere) than the value derived from the first observation of CO on Uranus, at infrared wavelength, by Encrenaz et al. (2004). As their fluorescence model did not take scattering effects into account, we suggest that their value could be overestimated.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enPlanets and satellites: individual: Saturn
dc.subject.enUranus
dc.subject.enRadio lines: solar system
dc.title.enObservations of CO on Saturn and Uranus at millimeter wavelengths: New upper limit determinations
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361:20079170
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.page555-561
bordeaux.volume484
bordeaux.peerReviewedoui
hal.identifierhal-00261897
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00261897v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Astronomy%20and%20Astrophysics%20-%20A&A&rft.date=2008&rft.volume=484&rft.spage=555-561&rft.epage=555-561&rft.eissn=0004-6361&rft.issn=0004-6361&rft.au=CAVALI%C3%89,%20T.&BILLEBAUD,%20F.&FOUCHET,%20T.&LELLOUCH,%20E.&BRILLET,%20J.&rft.genre=article


Fichier(s) constituant ce document

FichiersTailleFormatVue

Il n'y a pas de fichiers associés à ce document.

Ce document figure dans la(les) collection(s) suivante(s)

Afficher la notice abrégée