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Stratospheric aftermath of the 2010 Storm on Saturn as observed by the TEXES instrument. I. Temperature structure.

hal.structure.identifierLaboratoire d'études spatiales et d'instrumentation en astrophysique [LESIA]
dc.contributor.authorFOUCHET, Thierry
dc.contributor.authorGREATHOUSE, Thomas K.
hal.structure.identifierLaboratoire de Météorologie Dynamique (UMR 8539) [LMD]
dc.contributor.authorSPIGA, Aymeric
hal.structure.identifierLaboratoire d'études spatiales et d'instrumentation en astrophysique [LESIA]
dc.contributor.authorFLETCHER, Leigh N.
hal.structure.identifierLaboratoire de Météorologie Dynamique (UMR 8539) [LMD]
dc.contributor.authorGUERLET, Sandrine
hal.structure.identifierECLIPSE 2016
dc.contributor.authorLECONTE, J.
dc.contributor.authorORTON, Glenn S.
dc.date.issued2016-05
dc.identifier.issn0019-1035
dc.description.abstractEnWe report on spectroscopic observations of Saturn’s stratosphere in July 2011 with the Texas Echelon Cross Echelle Spectrograph (TEXES) mounted on the NASA InfraRed Telescope Facility (IRTF). The observations, targeting several lines of the CH4ν4 band and the H2 S(1) quadrupolar line, were designed to determine how Saturn’s stratospheric thermal structure was disturbed by the 2010 Great White Spot. A study of Cassini Composite Infrared Spectrometer (CIRS) spectra had already shown the presence of a large stratospheric disturbance centered at a pressure of 2 hPa, nicknamed the beacon B0, and a tail of warm air at lower pressures (Fletcher et al. 2012. Icarus 221, 560–586). Our observations confirm that the beacon B0 vertical structure determined by CIRS, with a maximum temperature of 180 ± 1K at 2 hPa, is overlain by a temperature decrease up to the 0.2-hPa pressure level. Our retrieved maximum temperature of 180 ± 1K is colder than that derived by CIRS (200 ± 1K), a difference that may be quantitatively explained by terrestrial atmospheric smearing. We propose a scenario for the formation of the beacon based on the saturation of gravity waves emitted by the GWS. Our observations also reveal that the tail is a planet-encircling disturbance in Saturn’s upper stratosphere, oscillating between 0.2 and 0.02 hPa, showing a distinct wavenumber-2 pattern. We propose that this pattern in the upper stratosphere is either the signature of thermal tides generated by the presence of the warm beacon in the mid-stratosphere, or the signature of Rossby wave activity.
dc.language.isoen
dc.publisherElsevier
dc.subject.enAtmospheres
dc.subject.endynamics
dc.subject.enSaturn
dc.subject.enstructure
dc.subject.enInfrared observations
dc.subject.enatmosphere
dc.title.enStratospheric aftermath of the 2010 Storm on Saturn as observed by the TEXES instrument. I. Temperature structure.
dc.typeArticle de revue
dc.identifier.doi10.1016/j.icarus.2016.04.030
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv1604.06479
bordeaux.journalIcarus
bordeaux.page196-214
bordeaux.volume277
bordeaux.peerReviewedoui
hal.identifierhal-01316490
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01316490v1
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