Mean winds at the cloud top of Venus obtained from two-wavelength UV imaging by Akatsuki
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DOI[10.1186/s40623-017-0775-3]のデータに遷移します
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- 資料種別
- 記事
- 著者・編者
- Takeshi HorinouchiToru KouyamaYeon Joo Lee
- 出版年月日等
- 2018-01-15
- 出版年（W3CDTF）
- 2018-01-15
- タイトル（掲載誌）
- EPS : Earth, Planets and Space
- 巻号年月日等（掲載誌）
- 70(10)
- 掲載巻
- 70(10)
- ISSN（掲載誌）
- 1880-5981
- ISSN-L（掲載誌）
- 1343-8832
- 本文の言語コード
- eng
- DOI
- 10.1186/s40623-017-0775-3
- 国立国会図書館永続的識別子
- info:ndljp/pid/11067466
- コレクション（共通）
- コレクション（障害者向け資料：レベル1）
- コレクション（個別）
- 国立国会図書館デジタルコレクション > 電子書籍・電子雑誌 > その他
- 収集根拠
- オンライン資料収集制度
- 受理日（W3CDTF）
- 2018-04-12T16:47:48+09:00
- 保存日（W3CDTF）
- 2018-04-12
- 記録形式（IMT）
- application/pdf
- オンライン閲覧公開範囲
- 国立国会図書館内限定公開
- デジタル化資料送信
- 図書館・個人送信対象外
- 遠隔複写可否（NDL）
- 可
- 掲載誌（国立国会図書館永続的識別子）
- info:ndljp/pid/11067456
- 連携機関・データベース
- 国立国会図書館 : 国立国会図書館デジタルコレクション
- 要約等
- The ultraviolet imager (UVI) has been developed for the Akatsuki spacecraft (Venus Climate Orbiter mission). The UVI takes ultraviolet (UV) images of the solar radiation reflected by the Venusian clouds with narrow bandpass filters centered at the 283 and 365 nm wavelengths. There are absorption bands of SO2 and unknown absorbers in these wavelength regions. The UV images provide the spatial distribution of SO2 and the unknown absorber around cloud top altitudes. The images also allow us to understand the cloud top morphologies and haze properties. Nominal sequential images with 2-h intervals are used to understand the dynamics of the Venusian atmosphere by estimating the wind vectors at the cloud top altitude, as well as the mass transportation of UV absorbers. The UVI is equipped with off-axial catadioptric optics, two bandpass filters, a diffuser installed in a filter wheel moving with a step motor, and a high sensitivity charge-coupled device with UV coating. The UVI images have spatial resolutions ranging from 200 m to 86 km at sub-spacecraft points. The UVI has been kept in good condition during the extended interplanetary cruise by carefully designed operations that have maintained its temperature maintenance and avoided solar radiation damage. The images have signal-to-noise ratios of over 100 after onboard desmear processing.
- DOI
- 10.1186/s40623-017-0775-3
- オンライン閲覧公開範囲
- インターネット公開
- 著作権情報
- © The Author(s) 2018.This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made.
- 関連情報（URI）
- 参照
- Rotational/divergent flow and energy conversion of thermal tides in a Venus general circulation modelEvaluation of new radio occultation observations among small satellites at Venus by data assimilationFormation and Quasi‐Periodic Variation of Equatorial Jet Caused by Planetary‐Scale Waves in the Venusian Lower Cloud LayerPeriodic Variation of Mesoscale Ultraviolet Contrast at the Cloud Top of VenusCold Collar Reproduced by a Venus GCM With the Akatsuki Horizontal Wind AssimilationLong‐Term Variation of the Quasi‐Five‐Day Wave in the Top Layer of Venus CloudsVenus cloud discontinuity in 2022Twelve-Year Cycle in the Cloud Top Winds Derived from VMC/Venus Express and UVI/Akatsuki ImagingReflectivity of Venus’s Dayside Disk During the 2020 Observation Campaign: Outcomes and Future PerspectivesThe first assimilation of Akatsuki single-layer winds and its validation with Venusian atmospheric waves excited by solar heatingCorrelation of Venusian Mesoscale Cloud Morphology Between Images Acquired at Various WavelengthsA Sensitivity Study of the Thermal Tides in the Venusian Atmosphere: Structures and Dynamical Effects on the SuperrotationHorizontal structures of bow-shaped mountain wave trains seen in thermal infrared images of venusian clouds taken by Akatsuki LIRA GCM Study on the 4‐Day and 5‐Day Waves in the Venus AtmosphereAmateur Observers Witness the Return of Venus’ Cloud DiscontinuityPlanetary‐Scale Waves Seen in Thermal Infrared Images of Venusian Cloud TopThermal Tides in the Upper Cloud Layer of Venus as Deduced From the Emission Angle Dependence of the Brightness Temperature by Akatsuki/LIRGravity Wave Packets in the Venusian Atmosphere Observed by Radio Occultation Experiments: Comparison With Saturation TheoryThe nightside cloud-top circulation of the atmosphere of VenusInstrumental requirements for the study of Venus’ cloud top using the UV imaging spectrometer VeSUVAtmospheric response to high-resolution topographical and radiative forcings in a general circulation model of Venus: Time-mean structures of waves and variancesBrightness modulations of our nearest terrestrial planet Venus reveal atmospheric super-rotation rather than surface featuresSuperrotation in Planetary AtmospheresSpatial and Temporal Variability of the 365‐nm Albedo of Venus Observed by the Camera on Board Venus ExpressEvaluation of a method to retrieve temperature and wind velocity profiles of the Venusian nightside mesosphere from mid-infrared CO2 absorption line observed by heterodyne spectroscopyHow waves and turbulence maintain the super-rotation of Venus' atmosphereInfluence of the cloud-level neutral layer on the vertical propagation of topographically generated gravity waves on VenusPlanetary‐Scale Variations in Winds and UV Brightness at the Venusian Cloud Top: Periodicity and Temporal EvolutionLong-term Variations of Venus’s 365 nm Albedo Observed by Venus Express, Akatsuki, MESSENGER, and the Hubble Space TelescopePrincipal components of short-term variability in the ultraviolet albedo of VenusStationary Features at the Cloud Top of Venus Observed by Ultraviolet Imager Onboard AkatsukiMorphology and Dynamics of Venus's Middle Clouds With Akatsuki/IR1Solar-locked and geographical atmospheric structures inferred from a Venus general circulation model with radiative transferNightside Winds at the Lower Clouds of Venus with Akatsuki/IR2: Longitudinal, Local Time, and Decadal Variations from Comparison with Previous MeasurementsSpecial issue “Akatsuki at Venus : the first year of scientific operation”Local Time Dependence of the Thermal Structure in the Venusian Equatorial Upper Atmosphere: Comparison of Akatsuki Radio Occultation Measurements and GCM ResultsUltraviolet imager on Venus orbiter Akatsuki and its initial results
- 参照
- Inst. of Space and Astronautical Science, Japan Aerospace Exploration AgencyUltraviolet imager on Venus orbiter Akatsuki and its initial resultsOverview of Akatsuki data products: definition of data levels, method and accuracy of geometric correctionSulfur dioxide in the Venus atmosphere: I. Vertical distribution and variabilityEquatorial jet in the lower to middle cloud layer of Venus revealed by AkatsukiImage velocimetry for clouds with relaxation labeling based on deformation consistencyScattering Properties of the Venusian Clouds Observed by the UV Imager on board AkatsukiVenus's winds and temperatures during the MESSENGER's flyby: An approximation to a three‐dimensional instantaneous state of the atmosphereVENUS CLOUD MORPHOLOGY AND MOTIONS FROM GROUND-BASED IMAGES AT THE TIME OF THE AKATSUKI ORBIT INSERTION<sup>∗</sup>Aerosol properties in the upper haze of Venus from SPICAV IR dataInfluence of Venus topography on the zonal wind and UV albedo at cloud top level: The role of stationary gravity wavesImproved automatic estimation of winds at the cloud top of Venus using superposition of cross-correlation surfacesAKATSUKI returns to VenusOptical properties of the Venus upper clouds from the data obtained by Venus Monitoring Camera on-board the Venus ExpressSix years of Venus winds at the upper cloud level from UV, visible and near infrared observations from VIRTIS on Venus ExpressVenus mesospheric sulfur dioxide measurement retrieved from SOIR on board Venus ExpressThe relationship between mesoscale circulation and cloud morphology at the upper cloud level of Venus from VMC/Venus ExpressGlory on Venus cloud tops and the unknown UV absorberCloud level winds from the Venus Express Monitoring Camera imagingLong‐term variation in the cloud‐tracked zonal velocities at the cloud top of Venus deduced from Venus Express VMC imagesThe abundance and vertical distribution of the unknown ultraviolet absorber in the venusian atmosphere from analysis of Venus Monitoring Camera imagesVertical profiling of SO2 and SO above Venus’ clouds by SPICAV/SOIR solar occultationsDynamical properties of the Venus mesosphere from the radio-occultation experiment VeRa onboard Venus ExpressAutomated cloud tracking system for the Akatsuki Venus Climate Orbiter dataOptical extinction due to aerosols in the upper haze of Venus: Four years of SOIR/VEX observations from 2006 to 2010Morphology of the cloud tops as observed by the Venus Express Monitoring CameraVertical structure of the Venus cloud top from the VeRa and VIRTIS observations onboard Venus ExpressHorizontal structure of planetary-scale waves at the cloud top of Venus deduced from Galileo SSI images with an improved cloud-tracking techniqueThe Roles of Equatorial Trapped Waves and Internal Inertia–Gravity Waves in Driving the Quasi-Biennial Oscillation. Part II: Three-Dimensional Distribution of Wave ForcingPreliminary characterization of the upper haze by SPICAV/SOIR solar occultation in UV to mid‐IR onboard Venus ExpressVenus cloud top winds from tracking UV features in Venus Monitoring Camera imagesVariable winds on Venus mapped in three dimensionsA reanalysis of Venus winds at two cloud levels from Galileo SSI imagesZonally non‐uniform distribution of equatorial gravity waves in an atmospheric general circulation modelThe quasi‐biennial oscillationHigh Resolution Cloud Feature Tracking on Venus by GalileoCloud-Tracked Winds from<i>Pioneer Venus</i>OCPP ImagesPlanetary-Scale Waves and the Cyclic Nature of Cloud Top Dynamics on VenusVenus: Cloud level circulation during 1982 as determined from Pioneer cloud photopolarimeter imagesVenus: Cloud level circulation during 1982 as determined from pioneer cloud photopolarimeter imagesVenus atmospheric circulation: Observations and implications of the thermal structureCirculation of the atmosphere from the surface to 100 kmMorphology and movements of polarizations features on Venus as seen in the pioneer Orbiter Cloud Photopolarimeter dataZonal mean circulation at the cloud level on Venus: Spring and fall 1979 OCPP observationsCloud Motions on Venus: Global Structure and OrganizationDistribution and source of the UV absorption in Venus' atmosphereCloud morphology and motions from Pioneer Venus imagesStructure and circulation of the Venus atmosphere
- 連携機関・データベース
- 国立情報学研究所 : CiNii Research
- 提供元機関・データベース
- 学術機関リポジトリデータベース国立国会図書館デジタルコレクションCrossrefCiNii Articles科学研究費助成事業データベース科学研究費助成事業データベース科学研究費助成事業データベースJapan Link CenterCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossrefCrossref
- NII論文ID
- 120006489890