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Models of SAR Backscattering for Bright Flows and Dark Spots on Titan

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.authorPAILLOU, Philippe
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.authorCRAPEAU, M.
hal.structure.identifierJet Propulsion Laboratory [JPL]
dc.contributor.authorELACHI, M.
hal.structure.identifierJet Propulsion Laboratory [JPL]
dc.contributor.authorWALL, Ch.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorENCRENAZ, S.
dc.date.issued2006
dc.identifier.issn2169-9097
dc.description.abstractEnThe SAR imaging mode of the Cassini RADAR instrument enables us to map the surface of Titan through its thick atmosphere. The first Cassini close flyby Ta, acquired on 26 October 2004, revealed a complex surface, with areas of low relief and dome-like volcanic constructs, flows and sinuous channels. In particular, fan-like features with strong radar backscattering were observed. Such structures, extending from tens of kilometers to more than 200 km in length, could be the result of cryovolcanism. Several radar-dark spots, up to 30 km across, were also observed: they may correspond to smooth hydrocarbon deposits. We present here a first modeling of these radar-bright and radar-dark features, based on classical radar backscattering models. We considered two main materials which could constitute the surface of Titan, tholins and water-ammonia ice, and modeled both single and two- layer cases, taking into account volume and sub-surface scattering. Our results show that SAR-bright regions could better be explained by the effect of a thin layer of water-ammonia ice covering a tholin substratum. Radar-dark spots can be modeled two-ways: a rough tholin surface or a smooth one with some volume scattering. We show that multi-incidence SAR data could help discriminate between the various scenarios proposed.
dc.language.isoen
dc.publisherWiley-Blackwell
dc.title.enModels of SAR Backscattering for Bright Flows and Dark Spots on Titan
dc.typeArticle de revue
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.journalJournal of Geophysical Research. Planets
bordeaux.page1-18
bordeaux.volume111
bordeaux.issueE11
bordeaux.peerReviewedoui
hal.identifierhal-00095885
hal.version1
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00095885v1
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