{"@context":{"@vocab":"https://cir.nii.ac.jp/schema/1.0/","rdfs":"http://www.w3.org/2000/01/rdf-schema#","dc":"http://purl.org/dc/elements/1.1/","dcterms":"http://purl.org/dc/terms/","foaf":"http://xmlns.com/foaf/0.1/","prism":"http://prismstandard.org/namespaces/basic/2.0/","cinii":"http://ci.nii.ac.jp/ns/1.0/","datacite":"https://schema.datacite.org/meta/kernel-4/","ndl":"http://ndl.go.jp/dcndl/terms/","jpcoar":"https://github.com/JPCOAR/schema/blob/master/2.0/"},"@id":"https://cir.nii.ac.jp/crid/1360011142931994496.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/2008je003186"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2008JE003186"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2008JE003186"}}],"dc:title":[{"@value":"Preliminary characterization of the upper haze by SPICAV/SOIR solar occultation in UV to mid‐IR onboard Venus Express"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>The Spectroscopy for Investigation of Characteristics of the Atmosphere of Venus/Solar Occultation at Infrared (SPICAV/SOIR) suite of instruments onboard the Venus Express spacecraft comprises three spectrometers covering a wavelength range from ultraviolet to midinfrared and an altitude range from 70 to >100 km. However, it is only recently (more than 1 year after the beginning of the mission) that the three spectrometers can operate simultaneously in the solar occultation mode. These observations have enabled the study of the properties of the Venusian mesosphere over a broad spectral range. In this manuscript, we briefly describe the instrument characteristics and the method used to infer haze microphysical properties from a data set of three selected orbits. Discussion focuses on the wavelength dependence of the continuum, which is primarily shaped by the extinction caused by the aerosol particles of the upper haze. This wavelength dependence is directly related to the effective particle radius (cross section weighted mean radius) of the particles. Through independent analyses for the three channels, we demonstrate the potential to characterize the aerosols in the mesosphere of Venus. The classical assumption that the upper haze is only composed of submicron particles is not sufficient to explain the observations. We find that at high northern latitudes, two types of particles coexist in the upper haze of Venus: mode 1 of mean radius 0.1 ≤ <jats:italic>r</jats:italic><jats:sub><jats:italic>g</jats:italic></jats:sub> ≤ 0.3 <jats:italic>μ</jats:italic>m and mode 2 of 0.4 ≤ <jats:italic>r</jats:italic><jats:sub><jats:italic>g</jats:italic></jats:sub> ≤ 1.0 <jats:italic>μ</jats:italic>m. An additional population of micron‐sized aerosols seems, therefore, needed to reconcile the data of the three spectrometers. Moreover, we observe substantial temporal variations of aerosol extinction over a time scale of 24 h.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380011142931994496","@type":"Researcher","foaf:name":[{"@value":"V. Wilquet"}],"jpcoar:affiliationName":[{"@value":"Belgian Institute for Space Aeronomy  Brussels Belgium"}]},{"@id":"https://cir.nii.ac.jp/crid/1380011142931994504","@type":"Researcher","foaf:name":[{"@value":"A. Fedorova"}],"jpcoar:affiliationName":[{"@value":"Space Research Institute  Moscow Russia"}]},{"@id":"https://cir.nii.ac.jp/crid/1380011142931994498","@type":"Researcher","foaf:name":[{"@value":"F. Montmessin"}],"jpcoar:affiliationName":[{"@value":"Service d'Aéronomie du CNRS  Verrières‐le‐Buisson France"},{"@value":"Institut Pierre Simon Laplace Université de Versailles Saint Quentin  Guyancourt France"}]},{"@id":"https://cir.nii.ac.jp/crid/1380011142931994500","@type":"Researcher","foaf:name":[{"@value":"R. Drummond"}],"jpcoar:affiliationName":[{"@value":"Belgian Institute for Space Aeronomy  Brussels Belgium"}]},{"@id":"https://cir.nii.ac.jp/crid/1380011142931994501","@type":"Researcher","foaf:name":[{"@value":"A. Mahieux"}],"jpcoar:affiliationName":[{"@value":"Belgian Institute for Space Aeronomy  Brussels Belgium"}]},{"@id":"https://cir.nii.ac.jp/crid/1380011142931994499","@type":"Researcher","foaf:name":[{"@value":"A. C. Vandaele"}],"jpcoar:affiliationName":[{"@value":"Belgian Institute for Space Aeronomy  Brussels Belgium"}]},{"@id":"https://cir.nii.ac.jp/crid/1380011142931994502","@type":"Researcher","foaf:name":[{"@value":"E. Villard"}],"jpcoar:affiliationName":[{"@value":"Service d'Aéronomie du CNRS  Verrières‐le‐Buisson France"},{"@value":"Institut Pierre Simon Laplace Université de Versailles Saint Quentin  Guyancourt France"}]},{"@id":"https://cir.nii.ac.jp/crid/1380011142931994497","@type":"Researcher","foaf:name":[{"@value":"O. Korablev"}],"jpcoar:affiliationName":[{"@value":"Space Research Institute  Moscow Russia"}]},{"@id":"https://cir.nii.ac.jp/crid/1380298344859828864","@type":"Researcher","foaf:name":[{"@value":"J.‐L. Bertaux"}],"jpcoar:affiliationName":[{"@value":"Service d'Aéronomie du CNRS  Verrières‐le‐Buisson France"},{"@value":"Institut Pierre Simon Laplace Université de Versailles Saint Quentin  Guyancourt France"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"01480227"}],"prism:publicationName":[{"@value":"Journal of Geophysical Research: Planets"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"2009-07-10","prism:volume":"114","prism:number":"E9","prism:startingPage":"E00B42"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2008JE003186"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2008JE003186"}],"createdAt":"2009-07-09","modifiedAt":"2023-10-13","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050856995323890688","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Ultraviolet imager on Venus orbiter Akatsuki and its initial results"},{"@value":"Mean winds at the cloud top of Venus obtained from two-wavelength UV imaging by Akatsuki"}]},{"@id":"https://cir.nii.ac.jp/crid/1360005516901121408","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Dayside cloud top structure of Venus retrieved from Akatsuki IR2 observations"}]},{"@id":"https://cir.nii.ac.jp/crid/1360302864806108160","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"One-dimensional Microphysics Model of Venusian Clouds from 40 to 100 km: Impact of the Middle-atmosphere Eddy Transport and SOIR Temperature Profile on the Cloud Structure"}]},{"@id":"https://cir.nii.ac.jp/crid/1360567181389174528","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance"}]},{"@id":"https://cir.nii.ac.jp/crid/1360571647804901120","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Brightness modulations of our nearest terrestrial planet Venus reveal atmospheric super-rotation rather than surface features"}]},{"@id":"https://cir.nii.ac.jp/crid/1360861704764051968","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Vertical‐Wind‐Induced Cloud Opacity Variation in Low Latitudes Simulated by a Venus GCM"}]},{"@id":"https://cir.nii.ac.jp/crid/1362539019285093888","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Long-term Variations of Venus’s 365 nm Albedo Observed by Venus Express, Akatsuki, MESSENGER, and the Hubble Space Telescope"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1029/2008je003186"},{"@type":"CROSSREF","@value":"10.3847/psj/ad25f3_references_DOI_AaVVtZDAOl5nO7JnblDI1L11XAG"},{"@type":"CROSSREF","@value":"10.1007/s11214-018-0517-2_references_DOI_AaVVtZDAOl5nO7JnblDI1L11XAG"},{"@type":"CROSSREF","@value":"10.1186/s40623-017-0775-3_references_DOI_AaVVtZDAOl5nO7JnblDI1L11XAG"},{"@type":"CROSSREF","@value":"10.1038/s41467-020-19385-6_references_DOI_AaVVtZDAOl5nO7JnblDI1L11XAG"},{"@type":"CROSSREF","@value":"10.1016/j.icarus.2020.113682_references_DOI_AaVVtZDAOl5nO7JnblDI1L11XAG"},{"@type":"CROSSREF","@value":"10.1029/2022je007595_references_DOI_AaVVtZDAOl5nO7JnblDI1L11XAG"},{"@type":"CROSSREF","@value":"10.3847/1538-3881/ab3120_references_DOI_AaVVtZDAOl5nO7JnblDI1L11XAG"}]}