Fine Vertical Structures at the Cloud Heights of Venus Revealed by Radio Holographic Analysis of Venus Express and Akatsuki Radio Occultation Data

Radio occultation (RO) is one of the most efficient techniques for studying fine vertical structures in planetary atmospheres. However, the geometrical optics (GO) method, which has been used for the analysis of RO data, suffers blurring by the finite width (Fresnel scale) of the radio ray and canno...

Ausführliche Beschreibung

Gespeichert in:
Bibliographische Detailangaben
Veröffentlicht in:Journal of geophysical research. Planets 2018-08, Vol.123 (8), p.2151-2161
Hauptverfasser: Imamura, Takeshi, Miyamoto, Mayu, Ando, Hiroki, Häusler, Bernd, Pätzold, Martin, Tellmann, Silvia, Tsuda, Toshitaka, Aoyama, Yuichi, Murata, Yasuhiro, Takeuchi, Hiroshi, Yamazaki, Atsushi, Toda, Tomoaki, Tomiki, Atsushi
Format: Artikel
Sprache:eng
Schlagworte:
Online-Zugang:Volltext
Tags: Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
container_end_page 2161
container_issue 8
container_start_page 2151
container_title Journal of geophysical research. Planets
container_volume 123
creator Imamura, Takeshi
Miyamoto, Mayu
Ando, Hiroki
Häusler, Bernd
Pätzold, Martin
Tellmann, Silvia
Tsuda, Toshitaka
Aoyama, Yuichi
Murata, Yasuhiro
Takeuchi, Hiroshi
Yamazaki, Atsushi
Toda, Tomoaki
Tomiki, Atsushi
description Radio occultation (RO) is one of the most efficient techniques for studying fine vertical structures in planetary atmospheres. However, the geometrical optics (GO) method, which has been used for the analysis of RO data, suffers blurring by the finite width (Fresnel scale) of the radio ray and cannot decipher multipath propagation, which also prevents retrieval of fine structures. Here we apply Full Spectrum Inversion (FSI), which is one of the radio holographic methods, to RO data taken in Venus Express and Akatsuki missions to retrieve fine structures in Venus' cloud‐level atmosphere. The temperature profiles obtained by FSI achieve vertical resolutions of ~150 m, which is much higher than the typical resolution of 400–700 m in GO, and resolve structures in multipath regions. Thin, near‐neutral layers are found to be ubiquitous at cloud heights; we suggest here that those layers are caused by the mixing associated with the breaking of short‐wavelength gravity waves. The wavenumber spectra of small‐scale structures are consistent with the semiempirical spectrum of saturated gravity waves and show larger amplitudes at higher latitudes. Temperature profiles in the high latitudes frequently show a sharp temperature minimum near the cloud top, below which the vertical temperature gradient is near adiabat, implying that the sharp temperature minimum is created by adiabatic cooling associated with convective plumes that impinge on the overlying stable layer. Key Points Full Spectrum Inversion was applied to radio occultation of Venus to disentangle multipath and achieve unprecedented vertical resolution Thin, near‐neutral layers are frequently observed, implying breaking of gravity waves having short vertical wavelengths Temperature profiles in the high latitudes frequently show a sharp temperature minimum near the cloud top
doi_str_mv 10.1029/2018JE005627
format Article
fullrecord <record><control><sourceid>proquest_cross</sourceid><recordid>TN_cdi_proquest_journals_2107813846</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2107813846</sourcerecordid><originalsourceid>FETCH-LOGICAL-a4781-bd7a310c72ce60f2d00c9fa83a2b2f8b667f6038fd255cd7d760bc3012a94f53</originalsourceid><addsrcrecordid>eNp9kdtOAkEMhjdGEwly5wNM4q1oZxb2cEmQg4SEBIm3m-4cYGDdwZlZldfwiR0DJlzZmzbN17_N3yi6pfBAgeWPDGg2GwH0E5ZeRC1Gk7ybU4DLvxry9DrqOLeFEFlo0bgVfY91LcmrtF5zrMiLtw33jZWOoCd-I8mwMo0gU6nXG--IUYGtG0eW8kNiJQUpD2SJQhsyNZVZW9xvNCeDGquD02f86GsfRINqLchgh941O30aXHDeVB69NjV5Qo830ZXCysnOKbej1Xi0Gk6788XkeTiYd7GXZrRbihRjCjxlXCagmADgucIsRlYylZVJkqoE4kwJ1u9zkYo0gZLHQBnmPdWP29HdUXZvzXsjnS-2prHhcFcwCmFDnPWSQN0fKW6Nc1aqYm_1G9pDQaH49b049z3g8RH_1JU8_MsWs8lyxCAPb_gBw52EvA</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2107813846</pqid></control><display><type>article</type><title>Fine Vertical Structures at the Cloud Heights of Venus Revealed by Radio Holographic Analysis of Venus Express and Akatsuki Radio Occultation Data</title><source>Wiley Online Library Journals Frontfile Complete</source><source>Wiley Online Library Free Content</source><source>Alma/SFX Local Collection</source><creator>Imamura, Takeshi ; Miyamoto, Mayu ; Ando, Hiroki ; Häusler, Bernd ; Pätzold, Martin ; Tellmann, Silvia ; Tsuda, Toshitaka ; Aoyama, Yuichi ; Murata, Yasuhiro ; Takeuchi, Hiroshi ; Yamazaki, Atsushi ; Toda, Tomoaki ; Tomiki, Atsushi</creator><creatorcontrib>Imamura, Takeshi ; Miyamoto, Mayu ; Ando, Hiroki ; Häusler, Bernd ; Pätzold, Martin ; Tellmann, Silvia ; Tsuda, Toshitaka ; Aoyama, Yuichi ; Murata, Yasuhiro ; Takeuchi, Hiroshi ; Yamazaki, Atsushi ; Toda, Tomoaki ; Tomiki, Atsushi</creatorcontrib><description>Radio occultation (RO) is one of the most efficient techniques for studying fine vertical structures in planetary atmospheres. However, the geometrical optics (GO) method, which has been used for the analysis of RO data, suffers blurring by the finite width (Fresnel scale) of the radio ray and cannot decipher multipath propagation, which also prevents retrieval of fine structures. Here we apply Full Spectrum Inversion (FSI), which is one of the radio holographic methods, to RO data taken in Venus Express and Akatsuki missions to retrieve fine structures in Venus' cloud‐level atmosphere. The temperature profiles obtained by FSI achieve vertical resolutions of ~150 m, which is much higher than the typical resolution of 400–700 m in GO, and resolve structures in multipath regions. Thin, near‐neutral layers are found to be ubiquitous at cloud heights; we suggest here that those layers are caused by the mixing associated with the breaking of short‐wavelength gravity waves. The wavenumber spectra of small‐scale structures are consistent with the semiempirical spectrum of saturated gravity waves and show larger amplitudes at higher latitudes. Temperature profiles in the high latitudes frequently show a sharp temperature minimum near the cloud top, below which the vertical temperature gradient is near adiabat, implying that the sharp temperature minimum is created by adiabatic cooling associated with convective plumes that impinge on the overlying stable layer. Key Points Full Spectrum Inversion was applied to radio occultation of Venus to disentangle multipath and achieve unprecedented vertical resolution Thin, near‐neutral layers are frequently observed, implying breaking of gravity waves having short vertical wavelengths Temperature profiles in the high latitudes frequently show a sharp temperature minimum near the cloud top</description><identifier>ISSN: 2169-9097</identifier><identifier>EISSN: 2169-9100</identifier><identifier>DOI: 10.1029/2018JE005627</identifier><language>eng</language><publisher>Washington: Blackwell Publishing Ltd</publisher><subject>Akatsuki ; atmosphere ; Blurring ; Clouds ; FSI ; Geometrical optics ; Gravitational waves ; Gravity waves ; Missions ; Optics ; Planetary atmospheres ; Radio ; Radio occultation ; Temperature gradients ; Temperature profiles ; Thin films ; Venus ; Venus atmosphere ; Venus clouds ; Venus Express ; Venus Express (ESA) ; Wavelengths</subject><ispartof>Journal of geophysical research. Planets, 2018-08, Vol.123 (8), p.2151-2161</ispartof><rights>2018. American Geophysical Union. All Rights Reserved.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-a4781-bd7a310c72ce60f2d00c9fa83a2b2f8b667f6038fd255cd7d760bc3012a94f53</citedby><cites>FETCH-LOGICAL-a4781-bd7a310c72ce60f2d00c9fa83a2b2f8b667f6038fd255cd7d760bc3012a94f53</cites><orcidid>0000-0002-0655-4982 ; 0000-0001-5088-6186 ; 0000-0002-8539-922X ; 0000-0002-9470-4492 ; 0000-0001-6468-6812</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://onlinelibrary.wiley.com/doi/pdf/10.1029%2F2018JE005627$$EPDF$$P50$$Gwiley$$H</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1029%2F2018JE005627$$EHTML$$P50$$Gwiley$$H</linktohtml><link.rule.ids>314,776,780,1411,1427,27901,27902,45550,45551,46384,46808</link.rule.ids></links><search><creatorcontrib>Imamura, Takeshi</creatorcontrib><creatorcontrib>Miyamoto, Mayu</creatorcontrib><creatorcontrib>Ando, Hiroki</creatorcontrib><creatorcontrib>Häusler, Bernd</creatorcontrib><creatorcontrib>Pätzold, Martin</creatorcontrib><creatorcontrib>Tellmann, Silvia</creatorcontrib><creatorcontrib>Tsuda, Toshitaka</creatorcontrib><creatorcontrib>Aoyama, Yuichi</creatorcontrib><creatorcontrib>Murata, Yasuhiro</creatorcontrib><creatorcontrib>Takeuchi, Hiroshi</creatorcontrib><creatorcontrib>Yamazaki, Atsushi</creatorcontrib><creatorcontrib>Toda, Tomoaki</creatorcontrib><creatorcontrib>Tomiki, Atsushi</creatorcontrib><title>Fine Vertical Structures at the Cloud Heights of Venus Revealed by Radio Holographic Analysis of Venus Express and Akatsuki Radio Occultation Data</title><title>Journal of geophysical research. Planets</title><description>Radio occultation (RO) is one of the most efficient techniques for studying fine vertical structures in planetary atmospheres. However, the geometrical optics (GO) method, which has been used for the analysis of RO data, suffers blurring by the finite width (Fresnel scale) of the radio ray and cannot decipher multipath propagation, which also prevents retrieval of fine structures. Here we apply Full Spectrum Inversion (FSI), which is one of the radio holographic methods, to RO data taken in Venus Express and Akatsuki missions to retrieve fine structures in Venus' cloud‐level atmosphere. The temperature profiles obtained by FSI achieve vertical resolutions of ~150 m, which is much higher than the typical resolution of 400–700 m in GO, and resolve structures in multipath regions. Thin, near‐neutral layers are found to be ubiquitous at cloud heights; we suggest here that those layers are caused by the mixing associated with the breaking of short‐wavelength gravity waves. The wavenumber spectra of small‐scale structures are consistent with the semiempirical spectrum of saturated gravity waves and show larger amplitudes at higher latitudes. Temperature profiles in the high latitudes frequently show a sharp temperature minimum near the cloud top, below which the vertical temperature gradient is near adiabat, implying that the sharp temperature minimum is created by adiabatic cooling associated with convective plumes that impinge on the overlying stable layer. Key Points Full Spectrum Inversion was applied to radio occultation of Venus to disentangle multipath and achieve unprecedented vertical resolution Thin, near‐neutral layers are frequently observed, implying breaking of gravity waves having short vertical wavelengths Temperature profiles in the high latitudes frequently show a sharp temperature minimum near the cloud top</description><subject>Akatsuki</subject><subject>atmosphere</subject><subject>Blurring</subject><subject>Clouds</subject><subject>FSI</subject><subject>Geometrical optics</subject><subject>Gravitational waves</subject><subject>Gravity waves</subject><subject>Missions</subject><subject>Optics</subject><subject>Planetary atmospheres</subject><subject>Radio</subject><subject>Radio occultation</subject><subject>Temperature gradients</subject><subject>Temperature profiles</subject><subject>Thin films</subject><subject>Venus</subject><subject>Venus atmosphere</subject><subject>Venus clouds</subject><subject>Venus Express</subject><subject>Venus Express (ESA)</subject><subject>Wavelengths</subject><issn>2169-9097</issn><issn>2169-9100</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNp9kdtOAkEMhjdGEwly5wNM4q1oZxb2cEmQg4SEBIm3m-4cYGDdwZlZldfwiR0DJlzZmzbN17_N3yi6pfBAgeWPDGg2GwH0E5ZeRC1Gk7ybU4DLvxry9DrqOLeFEFlo0bgVfY91LcmrtF5zrMiLtw33jZWOoCd-I8mwMo0gU6nXG--IUYGtG0eW8kNiJQUpD2SJQhsyNZVZW9xvNCeDGquD02f86GsfRINqLchgh941O30aXHDeVB69NjV5Qo830ZXCysnOKbej1Xi0Gk6788XkeTiYd7GXZrRbihRjCjxlXCagmADgucIsRlYylZVJkqoE4kwJ1u9zkYo0gZLHQBnmPdWP29HdUXZvzXsjnS-2prHhcFcwCmFDnPWSQN0fKW6Nc1aqYm_1G9pDQaH49b049z3g8RH_1JU8_MsWs8lyxCAPb_gBw52EvA</recordid><startdate>201808</startdate><enddate>201808</enddate><creator>Imamura, Takeshi</creator><creator>Miyamoto, Mayu</creator><creator>Ando, Hiroki</creator><creator>Häusler, Bernd</creator><creator>Pätzold, Martin</creator><creator>Tellmann, Silvia</creator><creator>Tsuda, Toshitaka</creator><creator>Aoyama, Yuichi</creator><creator>Murata, Yasuhiro</creator><creator>Takeuchi, Hiroshi</creator><creator>Yamazaki, Atsushi</creator><creator>Toda, Tomoaki</creator><creator>Tomiki, Atsushi</creator><general>Blackwell Publishing Ltd</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0002-0655-4982</orcidid><orcidid>https://orcid.org/0000-0001-5088-6186</orcidid><orcidid>https://orcid.org/0000-0002-8539-922X</orcidid><orcidid>https://orcid.org/0000-0002-9470-4492</orcidid><orcidid>https://orcid.org/0000-0001-6468-6812</orcidid></search><sort><creationdate>201808</creationdate><title>Fine Vertical Structures at the Cloud Heights of Venus Revealed by Radio Holographic Analysis of Venus Express and Akatsuki Radio Occultation Data</title><author>Imamura, Takeshi ; Miyamoto, Mayu ; Ando, Hiroki ; Häusler, Bernd ; Pätzold, Martin ; Tellmann, Silvia ; Tsuda, Toshitaka ; Aoyama, Yuichi ; Murata, Yasuhiro ; Takeuchi, Hiroshi ; Yamazaki, Atsushi ; Toda, Tomoaki ; Tomiki, Atsushi</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a4781-bd7a310c72ce60f2d00c9fa83a2b2f8b667f6038fd255cd7d760bc3012a94f53</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2018</creationdate><topic>Akatsuki</topic><topic>atmosphere</topic><topic>Blurring</topic><topic>Clouds</topic><topic>FSI</topic><topic>Geometrical optics</topic><topic>Gravitational waves</topic><topic>Gravity waves</topic><topic>Missions</topic><topic>Optics</topic><topic>Planetary atmospheres</topic><topic>Radio</topic><topic>Radio occultation</topic><topic>Temperature gradients</topic><topic>Temperature profiles</topic><topic>Thin films</topic><topic>Venus</topic><topic>Venus atmosphere</topic><topic>Venus clouds</topic><topic>Venus Express</topic><topic>Venus Express (ESA)</topic><topic>Wavelengths</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Imamura, Takeshi</creatorcontrib><creatorcontrib>Miyamoto, Mayu</creatorcontrib><creatorcontrib>Ando, Hiroki</creatorcontrib><creatorcontrib>Häusler, Bernd</creatorcontrib><creatorcontrib>Pätzold, Martin</creatorcontrib><creatorcontrib>Tellmann, Silvia</creatorcontrib><creatorcontrib>Tsuda, Toshitaka</creatorcontrib><creatorcontrib>Aoyama, Yuichi</creatorcontrib><creatorcontrib>Murata, Yasuhiro</creatorcontrib><creatorcontrib>Takeuchi, Hiroshi</creatorcontrib><creatorcontrib>Yamazaki, Atsushi</creatorcontrib><creatorcontrib>Toda, Tomoaki</creatorcontrib><creatorcontrib>Tomiki, Atsushi</creatorcontrib><collection>CrossRef</collection><collection>Meteorological &amp; Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological &amp; Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Journal of geophysical research. Planets</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Imamura, Takeshi</au><au>Miyamoto, Mayu</au><au>Ando, Hiroki</au><au>Häusler, Bernd</au><au>Pätzold, Martin</au><au>Tellmann, Silvia</au><au>Tsuda, Toshitaka</au><au>Aoyama, Yuichi</au><au>Murata, Yasuhiro</au><au>Takeuchi, Hiroshi</au><au>Yamazaki, Atsushi</au><au>Toda, Tomoaki</au><au>Tomiki, Atsushi</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Fine Vertical Structures at the Cloud Heights of Venus Revealed by Radio Holographic Analysis of Venus Express and Akatsuki Radio Occultation Data</atitle><jtitle>Journal of geophysical research. Planets</jtitle><date>2018-08</date><risdate>2018</risdate><volume>123</volume><issue>8</issue><spage>2151</spage><epage>2161</epage><pages>2151-2161</pages><issn>2169-9097</issn><eissn>2169-9100</eissn><abstract>Radio occultation (RO) is one of the most efficient techniques for studying fine vertical structures in planetary atmospheres. However, the geometrical optics (GO) method, which has been used for the analysis of RO data, suffers blurring by the finite width (Fresnel scale) of the radio ray and cannot decipher multipath propagation, which also prevents retrieval of fine structures. Here we apply Full Spectrum Inversion (FSI), which is one of the radio holographic methods, to RO data taken in Venus Express and Akatsuki missions to retrieve fine structures in Venus' cloud‐level atmosphere. The temperature profiles obtained by FSI achieve vertical resolutions of ~150 m, which is much higher than the typical resolution of 400–700 m in GO, and resolve structures in multipath regions. Thin, near‐neutral layers are found to be ubiquitous at cloud heights; we suggest here that those layers are caused by the mixing associated with the breaking of short‐wavelength gravity waves. The wavenumber spectra of small‐scale structures are consistent with the semiempirical spectrum of saturated gravity waves and show larger amplitudes at higher latitudes. Temperature profiles in the high latitudes frequently show a sharp temperature minimum near the cloud top, below which the vertical temperature gradient is near adiabat, implying that the sharp temperature minimum is created by adiabatic cooling associated with convective plumes that impinge on the overlying stable layer. Key Points Full Spectrum Inversion was applied to radio occultation of Venus to disentangle multipath and achieve unprecedented vertical resolution Thin, near‐neutral layers are frequently observed, implying breaking of gravity waves having short vertical wavelengths Temperature profiles in the high latitudes frequently show a sharp temperature minimum near the cloud top</abstract><cop>Washington</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1029/2018JE005627</doi><tpages>11</tpages><orcidid>https://orcid.org/0000-0002-0655-4982</orcidid><orcidid>https://orcid.org/0000-0001-5088-6186</orcidid><orcidid>https://orcid.org/0000-0002-8539-922X</orcidid><orcidid>https://orcid.org/0000-0002-9470-4492</orcidid><orcidid>https://orcid.org/0000-0001-6468-6812</orcidid><oa>free_for_read</oa></addata></record>
fulltext fulltext
identifier ISSN: 2169-9097
ispartof Journal of geophysical research. Planets, 2018-08, Vol.123 (8), p.2151-2161
issn 2169-9097
2169-9100
language eng
recordid cdi_proquest_journals_2107813846
source Wiley Online Library Journals Frontfile Complete; Wiley Online Library Free Content; Alma/SFX Local Collection
subjects Akatsuki
atmosphere
Blurring
Clouds
FSI
Geometrical optics
Gravitational waves
Gravity waves
Missions
Optics
Planetary atmospheres
Radio
Radio occultation
Temperature gradients
Temperature profiles
Thin films
Venus
Venus atmosphere
Venus clouds
Venus Express
Venus Express (ESA)
Wavelengths
title Fine Vertical Structures at the Cloud Heights of Venus Revealed by Radio Holographic Analysis of Venus Express and Akatsuki Radio Occultation Data
url https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-30T06%3A24%3A01IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_cross&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Fine%20Vertical%20Structures%20at%20the%20Cloud%20Heights%20of%20Venus%20Revealed%20by%20Radio%20Holographic%20Analysis%20of%20Venus%20Express%20and%20Akatsuki%20Radio%20Occultation%20Data&rft.jtitle=Journal%20of%20geophysical%20research.%20Planets&rft.au=Imamura,%20Takeshi&rft.date=2018-08&rft.volume=123&rft.issue=8&rft.spage=2151&rft.epage=2161&rft.pages=2151-2161&rft.issn=2169-9097&rft.eissn=2169-9100&rft_id=info:doi/10.1029/2018JE005627&rft_dat=%3Cproquest_cross%3E2107813846%3C/proquest_cross%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2107813846&rft_id=info:pmid/&rfr_iscdi=true