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dc.contributor.authorBertaux, J.-L.
dc.contributor.authorVandaele, A.-C.
dc.contributor.authorKorablev, O.
dc.contributor.authorVillard, E.
dc.contributor.authorFedorova, A.
dc.contributor.authorFussen, D.
dc.contributor.authorQuémerais, E.
dc.contributor.authorBelyaev, D.
dc.contributor.authorMahieux, A.
dc.contributor.authorMontmessin, F.
dc.contributor.authorMuller, C.
dc.contributor.authorNeefs, E.
dc.contributor.authorNevejans, D.
dc.contributor.authorWilquet, V.
dc.contributor.authorDubois, J.P.
dc.contributor.authorHauchecorne, A.
dc.contributor.authorStepanov, A.
dc.contributor.authorVinogradov, I.
dc.contributor.authorRodin, A.
dc.contributor.authorNevejans, D.
dc.contributor.authorFedorova, A.
dc.contributor.authorCabane, M.
dc.contributor.authorChassefière, E.
dc.contributor.authorChaufray, J.Y.
dc.contributor.authorDimarellis, E.
dc.contributor.authorDubois, J.P.
dc.contributor.authorHauchecorne, A.
dc.contributor.authorLeblanc, F.
dc.contributor.authorLefèvre, F.
dc.contributor.authorRannou, P.
dc.contributor.authorQuémerais, E.
dc.contributor.authorVillard, E.
dc.contributor.authorFussen, D.
dc.contributor.authorMuller, C.
dc.contributor.authorNeefs, E.
dc.contributor.authorVan Ransbeeck, E.
dc.contributor.authorWilquet, V.
dc.contributor.authorRodin, A.
dc.contributor.authorStepanov, A.
dc.contributor.authorVinogradov, I.
dc.contributor.authorZasova, L.
dc.contributor.authorForget, F.
dc.contributor.authorLebonnois, S.
dc.contributor.authorTitov, D.
dc.contributor.authorRafkin, S.
dc.contributor.authorDurry, G.
dc.contributor.authorGérard, J.C.
dc.contributor.authorSandel, B.
dc.date2007
dc.date.accessioned2016-09-26T13:13:22Z
dc.date.available2016-09-26T13:13:22Z
dc.identifier.urihttps://orfeo.belnet.be/handle/internal/4383
dc.descriptionVenus has thick clouds of H2SO4 aerosol particles extending from altitudes of 40 to 60 km. The 60-100 km region (the mesosphere) is a transition region between the 4 day retrograde superrotation at the top of the thick clouds and the solar-antisolar circulation in the thermosphere (above 100 km), which has upwelling over the subsolar point and transport to the nightside. The mesosphere has a light haze of variable optical thickness, with CO, SO2, HCl, HF, H2O and HDO as the most important minor gaseous constituents, but the vertical distribution of the haze and molecules is poorly known because previous descent probes began their measurements at or below 60 km. Here we report the detection of an extensive layer of warm air at altitudes 90-120 km on the night side that we interpret as the result of adiabatic heating during air subsidence. Such a strong temperature inversion was not expected, because the night side of Venus was otherwise so cold that it was named the 'cryosphere' above 100 km. We also measured the mesospheric distributions of HF, HCl, H2O and HDO. HCl is less abundant than reported 40 years ago. HDO/H2O is enhanced by a factor of ∼2.5 with respect to the lower atmosphere, and there is a general depletion of H 2O around 80-90 km for which we have no explanation.
dc.languageeng
dc.relation.ispartofseries
dc.titleA warm layer in Venus' cryosphere and high-altitude measurements of HF, HCl, H2O and HDO
dc.typeArticle
dc.subject.frascatiPhysical sciences
dc.audienceScientific
dc.subject.freehydrochloric acid
dc.subject.freehydrofluoric acid
dc.subject.freewater
dc.subject.freeaerosol
dc.subject.freecloud
dc.subject.freecryosphere
dc.subject.freemeasurement method
dc.subject.freeVenus
dc.subject.freevertical distribution
dc.subject.freewater
dc.subject.freeair
dc.subject.freealtitude
dc.subject.freearticle
dc.subject.freeastronomy
dc.subject.freeatmosphere
dc.subject.freeheating
dc.subject.freenight
dc.subject.freepriority journal
dc.subject.freetemperature
dc.source.titleNature
dc.source.volume450
dc.source.issue7170
dc.source.page646-649
Orfeo.peerreviewedYes
dc.identifier.doi10.1038/nature05974
dc.identifier.scopus2-s2.0-36749073905


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