{"@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/1360011142931023232.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/ja085ia13p08129"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2FJA085iA13p08129"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/JA085iA13p08129"}}],"dc:title":[{"@value":"Cloud and haze properties from Pioneer Venus polarimetry"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>Analysis of linear polarization data obtained by the Pioneer Venus Orbiter Cloud Photopolarimeter experiment indicates that the visible clouds at low and mid‐latitudes are composed predominantly of 1 µm radius H<jats:sub>2</jats:sub>SO<jats:sub>4</jats:sub> droplets, an identification made previously by using earth‐based observations. Mixed within and extending above this main visible cloud is an extensive haze of submicron‐sized particles. These haze particles have a refractive index of 1.45±0.04 at λ ≃550 nm, an effective radius of 0.23±0.04 µm, and a size distribution with an effective variance of 0.18±0.1. The polarization of the bright regions poleward of about 55° latitude is produced almost entirely by this submicron haze. The submicron haze has been found to exhibit large spatial and temporal variations. In January 1979 the haze vertical optical thickness in the polar region at λ=365 nm was τ<jats:sub><jats:italic>h</jats:italic></jats:sub> ∼0.8 above the main cloud of l‐µm particles. By comparison, the optical thickness of the haze above the main cloud at low latitudes was typically 1 order of magnitude smaller, τ<jats:sub><jats:italic>h</jats:italic></jats:sub> ∼0.06, however haze mixed within the cloud contributed ∼18% of the total scattering cross section per unit volume at λ=365 nm. More recent observations indicate that there are major changes of the haze on time scales of hundreds of days (e.g., the optical thickness of the polar cap haze is smaller by a factor of 2–3 in October 1979 than in January 1979). Substantial diurnal variations exist at low latitudes, with a greater amount of haze near the morning terminator than near the noon meridian. The global distribution of haze will be monitored during the extended Pioneer Venus mission to permit analysis of long time scale variations as well as correlation with characteristics of the atmospheric dynamics deduced from ultraviolet images of the cloud tops.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380011142931023233","@type":"Researcher","foaf:name":[{"@value":"K. Kawabata"}]},{"@id":"https://cir.nii.ac.jp/crid/1380011142931023235","@type":"Researcher","foaf:name":[{"@value":"D. L. Coffeen"}]},{"@id":"https://cir.nii.ac.jp/crid/1380011142931023232","@type":"Researcher","foaf:name":[{"@value":"J. E. Hansen"}]},{"@id":"https://cir.nii.ac.jp/crid/1380011142931023237","@type":"Researcher","foaf:name":[{"@value":"W. A. Lane"}]},{"@id":"https://cir.nii.ac.jp/crid/1380011142931023236","@type":"Researcher","foaf:name":[{"@value":"Makoto Sato"}]},{"@id":"https://cir.nii.ac.jp/crid/1380011142931023234","@type":"Researcher","foaf:name":[{"@value":"L. D. Travis"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"01480227"}],"prism:publicationName":[{"@value":"Journal of Geophysical Research: Space Physics"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"1980-12-30","prism:volume":"85","prism:number":"A13","prism:startingPage":"8129","prism:endingPage":"8140"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2FJA085iA13p08129"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/JA085iA13p08129"}],"createdAt":"2008-02-06","modifiedAt":"2023-09-23","relatedProduct":[{"@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/1360016861574264320","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"In situ biochemical characterization of Venus cloud particles using a life-signature detection microscope"}]},{"@id":"https://cir.nii.ac.jp/crid/1360285707161058816","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Venus’ clouds as inferred from the phase curves acquired by IR1 and IR2 on board Akatsuki"}]},{"@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/1360567179754737408","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"The Venus nighttime atmosphere as observed by the VIRTIS‐M instrument. 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