Model of a variable radio period for Saturn
Identifieur interne : 001882 ( Istex/Corpus ); précédent : 001881; suivant : 001883Model of a variable radio period for Saturn
Auteurs : B. Cecconi ; P. ZarkaSource :
- Journal of Geophysical Research: Space Physics [ 0148-0227 ] ; 2005-12.
Abstract
We propose an explanation for the variations at the 1% level of Saturn's radio rotation period measured at kilometer wavelengths. Because Saturn's kilometric radiation (SKR) is strongly controlled by the solar wind, we suggest that nonrandom variations of solar wind characteristics, especially its velocity, at Saturn may result in systematic displacement of the auroral sources in local time and finally in modifications of the apparent radio period. Alternatively, it may result in the superposition of two apparent periods, as also observed in Voyager data. We develop two simple models of local time variations of the SKR sources and analyze the conditions under which the measured radio period may be shifted by up to a few percent from the planet's sidereal period. Our results provide a possible explanation for the 1% variation observed and suggest that the dominant peak in the harmonic analysis of SKR variations seen by Voyager may be different from Saturn's sidereal rotation period. We relate the limitation in the accuracy of planetary rotation period determination to long‐term variations of “control” parameters (like the solar wind velocity). One and a half to three years of continuous SKR observations with Cassini will be required to reliably and accurately derive Saturn's true sidereal period.
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DOI: 10.1029/2005JA011085
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Cecconi</name><affiliation><mods:affiliation>Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa, USA</mods:affiliation></affiliation><affiliation><mods:affiliation>Also at Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Centre National de la Recherche Scientifique, Observatoire de Paris, Meudon, France.</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: baptiste.cecconi@obspm.fr</mods:affiliation></affiliation></author><author><name sortKey="Zarka, P" sort="Zarka, P" uniqKey="Zarka P" first="P." last="Zarka">P. Zarka</name><affiliation><mods:affiliation>Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Centre National de la Recherche Scientifique, Observatoire de Paris, Meudon, France</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j">Journal of Geophysical Research: Space Physics</title><title level="j" type="abbrev">J. Geophys. 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Because Saturn's kilometric radiation (SKR) is strongly controlled by the solar wind, we suggest that nonrandom variations of solar wind characteristics, especially its velocity, at Saturn may result in systematic displacement of the auroral sources in local time and finally in modifications of the apparent radio period. Alternatively, it may result in the superposition of two apparent periods, as also observed in Voyager data. We develop two simple models of local time variations of the SKR sources and analyze the conditions under which the measured radio period may be shifted by up to a few percent from the planet's sidereal period. Our results provide a possible explanation for the 1% variation observed and suggest that the dominant peak in the harmonic analysis of SKR variations seen by Voyager may be different from Saturn's sidereal rotation period. We relate the limitation in the accuracy of planetary rotation period determination to long‐term variations of “control” parameters (like the solar wind velocity). One and a half to three years of continuous SKR observations with Cassini will be required to reliably and accurately derive Saturn's true sidereal period.</div></front></TEI><istex><corpusName>wiley</corpusName><author><json:item><name>B. Cecconi</name><affiliations><json:string>Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa, USA</json:string><json:string>Also at Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Centre National de la Recherche Scientifique, Observatoire de Paris, Meudon, France.</json:string><json:string>E-mail: baptiste.cecconi@obspm.fr</json:string></affiliations></json:item><json:item><name>P. 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Because Saturn's kilometric radiation (SKR) is strongly controlled by the solar wind, we suggest that nonrandom variations of solar wind characteristics, especially its velocity, at Saturn may result in systematic displacement of the auroral sources in local time and finally in modifications of the apparent radio period. Alternatively, it may result in the superposition of two apparent periods, as also observed in Voyager data. We develop two simple models of local time variations of the SKR sources and analyze the conditions under which the measured radio period may be shifted by up to a few percent from the planet's sidereal period. Our results provide a possible explanation for the 1% variation observed and suggest that the dominant peak in the harmonic analysis of SKR variations seen by Voyager may be different from Saturn's sidereal rotation period. We relate the limitation in the accuracy of planetary rotation period determination to long‐term variations of “control” parameters (like the solar wind velocity). One and a half to three years of continuous SKR observations with Cassini will be required to reliably and accurately derive Saturn's true sidereal period.</abstract><qualityIndicators><score>7.448</score><pdfVersion>1.3</pdfVersion><pdfPageSize>592 x 807 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractCharCount>1316</abstractCharCount><pdfWordCount>5796</pdfWordCount><pdfCharCount>30844</pdfCharCount><pdfPageCount>9</pdfPageCount><abstractWordCount>204</abstractWordCount></qualityIndicators><title>Model of a variable radio period for Saturn</title><refBibs><json:item><author><json:item><name>J. K. Alexander</name></json:item><json:item><name>M. D. Desch</name></json:item><json:item><name>M. L. Kaiser</name></json:item><json:item><name>J. R. 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Rev.</title></host><title>Radio wave emission from the outer planets before Cassini</title></json:item></refBibs><genre><json:string>article</json:string></genre><host><volume>110</volume><publisherId><json:string>JGRA</json:string></publisherId><pages><total>9</total><last>n/a</last><first>n/a</first></pages><issn><json:string>0148-0227</json:string></issn><issue>A12</issue><subject><json:item><value>Magnetospheric Physics</value></json:item><json:item><value>GEODESY AND GRAVITY</value></json:item><json:item><value>Lunar and planetary geodesy and gravity</value></json:item><json:item><value>MAGNETOSPHERIC PHYSICS</value></json:item><json:item><value>Solar wind/magnetosphere interactions</value></json:item><json:item><value>ATMOSPHERIC PROCESSES</value></json:item><json:item><value>Planetary meteorology</value></json:item><json:item><value>PLANETARY SCIENCES: FLUID PLANETS</value></json:item><json:item><value>Meteorology</value></json:item><json:item><value>Orbital and rotational dynamics</value></json:item><json:item><value>PLANETARY SCIENCES: SOLAR SYSTEM OBJECTS</value></json:item><json:item><value>Saturn</value></json:item><json:item><value>SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY</value></json:item><json:item><value>Radio emissions</value></json:item><json:item><value>Magnetospheric Physics</value></json:item></subject><genre><json:string>journal</json:string></genre><language><json:string>unknown</json:string></language><eissn><json:string>2156-2202</json:string></eissn><title>Journal of Geophysical Research: Space Physics</title><doi><json:string>10.1002/(ISSN)2156-2202a</json:string></doi></host><categories><wos><json:string>science</json:string><json:string>geosciences, multidisciplinary</json:string></wos><scienceMetrix><json:string>natural sciences</json:string><json:string>earth & environmental sciences</json:string><json:string>meteorology & atmospheric sciences</json:string></scienceMetrix></categories><publicationDate>2005</publicationDate><copyrightDate>2005</copyrightDate><doi><json:string>10.1029/2005JA011085</json:string></doi><id>D06FBD19BCC421BBDFE9BDB7F748A4A4359B70D7</id><score>0.1359517</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/D06FBD19BCC421BBDFE9BDB7F748A4A4359B70D7/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/D06FBD19BCC421BBDFE9BDB7F748A4A4359B70D7/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/D06FBD19BCC421BBDFE9BDB7F748A4A4359B70D7/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main" xml:lang="en">Model of a variable radio period for Saturn</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><availability><p>Copyright 2005 by the American Geophysical Union.</p></availability><date>2005</date></publicationStmt><sourceDesc><biblStruct type="inbook"><analytic><title level="a" type="main" xml:lang="en">Model of a variable radio period for Saturn</title><author xml:id="author-1"><persName><forename type="first">B.</forename><surname>Cecconi</surname></persName><email>baptiste.cecconi@obspm.fr</email><affiliation>Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa, USA</affiliation><affiliation>Also at Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Centre National de la Recherche Scientifique, Observatoire de Paris, Meudon, France.</affiliation></author><author xml:id="author-2"><persName><forename type="first">P.</forename><surname>Zarka</surname></persName><affiliation>Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Centre National de la Recherche Scientifique, Observatoire de Paris, Meudon, France</affiliation></author></analytic><monogr><title level="j">Journal of Geophysical Research: Space Physics</title><title level="j" type="abbrev">J. Geophys. Res.</title><idno type="pISSN">0148-0227</idno><idno type="eISSN">2156-2202</idno><idno type="DOI">10.1002/(ISSN)2156-2202a</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><date type="published" when="2005-12"></date><biblScope unit="volume">110</biblScope><biblScope unit="issue">A12</biblScope><biblScope unit="page" from="/">n/a</biblScope><biblScope unit="page" to="/">n/a</biblScope></imprint></monogr><idno type="istex">D06FBD19BCC421BBDFE9BDB7F748A4A4359B70D7</idno><idno type="DOI">10.1029/2005JA011085</idno><idno type="ArticleID">2005JA011085</idno></biblStruct></sourceDesc></fileDesc><profileDesc><creation><date>2005</date></creation><langUsage><language ident="en">en</language></langUsage><abstract><p>We propose an explanation for the variations at the 1% level of Saturn's radio rotation period measured at kilometer wavelengths. Because Saturn's kilometric radiation (SKR) is strongly controlled by the solar wind, we suggest that nonrandom variations of solar wind characteristics, especially its velocity, at Saturn may result in systematic displacement of the auroral sources in local time and finally in modifications of the apparent radio period. Alternatively, it may result in the superposition of two apparent periods, as also observed in Voyager data. We develop two simple models of local time variations of the SKR sources and analyze the conditions under which the measured radio period may be shifted by up to a few percent from the planet's sidereal period. Our results provide a possible explanation for the 1% variation observed and suggest that the dominant peak in the harmonic analysis of SKR variations seen by Voyager may be different from Saturn's sidereal rotation period. We relate the limitation in the accuracy of planetary rotation period determination to long‐term variations of “control” parameters (like the solar wind velocity). One and a half to three years of continuous SKR observations with Cassini will be required to reliably and accurately derive Saturn's true sidereal period.</p></abstract><textClass><keywords scheme="keyword"><list><head>keywords</head><item><term>Saturn</term></item><item><term>sidereal period</term></item><item><term>auroral radio emission</term></item></list></keywords></textClass><textClass><keywords scheme="Journal Subject"><list><head>index-terms</head><item><term>Magnetospheric Physics</term></item><item><term>GEODESY AND GRAVITY</term></item><item><term>Lunar and planetary geodesy and gravity</term></item><item><term>MAGNETOSPHERIC PHYSICS</term></item><item><term>Solar wind/magnetosphere interactions</term></item><item><term>ATMOSPHERIC PROCESSES</term></item><item><term>Planetary meteorology</term></item><item><term>PLANETARY SCIENCES: FLUID PLANETS</term></item><item><term>Meteorology</term></item><item><term>Orbital and rotational dynamics</term></item><item><term>PLANETARY SCIENCES: SOLAR SYSTEM OBJECTS</term></item><item><term>Saturn</term></item><item><term>SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY</term></item><item><term>Radio emissions</term></item></list></keywords></textClass><textClass><keywords scheme="Journal Subject"><list><head>article-category</head><item><term>Magnetospheric Physics</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="2005-02-16">Received</change><change when="2005-09-12">Registration</change><change when="2005-12">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/D06FBD19BCC421BBDFE9BDB7F748A4A4359B70D7/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration><istex:document><component type="serialArticle" version="2.0" xml:lang="en" xml:id="jgra17926"><header><publicationMeta level="product"><doi>10.1002/(ISSN)2156-2202a</doi><issn type="print">0148-0227</issn><issn type="electronic">2156-2202</issn><idGroup><id type="product" value="JGRA"></id><id type="coden" value="JGREA2"></id></idGroup><titleGroup><title type="main" xml:lang="en" sort="JOURNAL OF GEOPHYSICAL RESEARCH: SPACE PHYSICS">Journal of Geophysical Research: Space Physics</title><title type="short">J. 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Geophys. Res.</journalTitle>, <vol>110</vol>, A12203, doi:<accessionId ref="info:doi/10.1029/2005JA011085">10.1029/2005JA011085</accessionId>.</citation></selfCitationGroup><linkGroup><link type="toTypesetVersion" href="file:JGRA.JGRA17926.pdf"></link></linkGroup></publicationMeta><contentMeta><countGroup><count type="figureTotal" number="8"></count></countGroup><titleGroup><title type="main">Model of a variable radio period for Saturn</title><title type="short">MODEL OF A VARIABLE RADIO PERIOD FOR SATURN</title><title type="shortAuthors">Cecconi and Zarka</title></titleGroup><creators><creator creatorRole="author" xml:id="jgra17926-cr-0001" affiliationRef="#jgra17926-aff-0001 #jgra17926-aff-0003"><personName><givenNames>B.</givenNames> <familyName>Cecconi</familyName></personName><contactDetails><email normalForm="baptiste.cecconi@obspm.fr">baptiste.cecconi@obspm.fr</email></contactDetails></creator><creator creatorRole="author" xml:id="jgra17926-cr-0002" affiliationRef="#jgra17926-aff-0002"><personName><givenNames>P.</givenNames> <familyName>Zarka</familyName></personName></creator></creators><affiliationGroup><affiliation countryCode="US" type="organization" xml:id="jgra17926-aff-0001"><orgDiv>Department of Physics and Astronomy</orgDiv><orgName>University of Iowa</orgName><address><city>Iowa City</city><countryPart>Iowa</countryPart><country>USA</country></address></affiliation><affiliation countryCode="FR" type="organization" xml:id="jgra17926-aff-0002"><orgDiv>Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Centre National de la Recherche Scientifique</orgDiv><orgName>Observatoire de Paris</orgName><address><city>Meudon</city><country>France</country></address></affiliation><affiliation type="organization" xml:id="jgra17926-aff-0003"><unparsedAffiliation>Also at Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Centre National de la Recherche Scientifique, Observatoire de Paris, Meudon, France.</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup type="author"><keyword xml:id="jgra17926-kwd-0001">Saturn</keyword><keyword xml:id="jgra17926-kwd-0002">sidereal period</keyword><keyword xml:id="jgra17926-kwd-0003">auroral radio emission</keyword></keywordGroup><abstractGroup><abstract type="main"><p xml:id="jgra17926-para-0001" label="1">We propose an explanation for the variations at the 1% level of Saturn's radio rotation period measured at kilometer wavelengths. Because Saturn's kilometric radiation (SKR) is strongly controlled by the solar wind, we suggest that nonrandom variations of solar wind characteristics, especially its velocity, at Saturn may result in systematic displacement of the auroral sources in local time and finally in modifications of the apparent radio period. Alternatively, it may result in the superposition of two apparent periods, as also observed in Voyager data. We develop two simple models of local time variations of the SKR sources and analyze the conditions under which the measured radio period may be shifted by up to a few percent from the planet's sidereal period. Our results provide a possible explanation for the 1% variation observed and suggest that the dominant peak in the harmonic analysis of SKR variations seen by Voyager may be different from Saturn's sidereal rotation period. We relate the limitation in the accuracy of planetary rotation period determination to long‐term variations of “control” parameters (like the solar wind velocity). One and a half to three years of continuous SKR observations with Cassini will be required to reliably and accurately derive Saturn's true sidereal period.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Model of a variable radio period for Saturn</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>MODEL OF A VARIABLE RADIO PERIOD FOR SATURN</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Model of a variable radio period for Saturn</title></titleInfo><name type="personal"><namePart type="given">B.</namePart><namePart type="family">Cecconi</namePart><affiliation>Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa, USA</affiliation><affiliation>Also at Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Centre National de la Recherche Scientifique, Observatoire de Paris, Meudon, France.</affiliation><affiliation>E-mail: baptiste.cecconi@obspm.fr</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">P.</namePart><namePart type="family">Zarka</namePart><affiliation>Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Centre National de la Recherche Scientifique, Observatoire de Paris, Meudon, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article"></genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><dateIssued encoding="w3cdtf">2005-12</dateIssued><dateCaptured encoding="w3cdtf">2005-02-16</dateCaptured><dateValid encoding="w3cdtf">2005-09-12</dateValid><edition>Cecconi, B., and P. Zarka (2005), Model of a variable radio period for Saturn, J. Geophys. Res., 110, A12203, doi:10.1029/2005JA011085.</edition><copyrightDate encoding="w3cdtf">2005</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType><extent unit="figures">8</extent></physicalDescription><abstract>We propose an explanation for the variations at the 1% level of Saturn's radio rotation period measured at kilometer wavelengths. Because Saturn's kilometric radiation (SKR) is strongly controlled by the solar wind, we suggest that nonrandom variations of solar wind characteristics, especially its velocity, at Saturn may result in systematic displacement of the auroral sources in local time and finally in modifications of the apparent radio period. Alternatively, it may result in the superposition of two apparent periods, as also observed in Voyager data. We develop two simple models of local time variations of the SKR sources and analyze the conditions under which the measured radio period may be shifted by up to a few percent from the planet's sidereal period. Our results provide a possible explanation for the 1% variation observed and suggest that the dominant peak in the harmonic analysis of SKR variations seen by Voyager may be different from Saturn's sidereal rotation period. We relate the limitation in the accuracy of planetary rotation period determination to long‐term variations of “control” parameters (like the solar wind velocity). One and a half to three years of continuous SKR observations with Cassini will be required to reliably and accurately derive Saturn's true sidereal period.</abstract><subject><genre>keywords</genre><topic>Saturn</topic><topic>sidereal period</topic><topic>auroral radio emission</topic></subject><relatedItem type="host"><titleInfo><title>Journal of Geophysical Research: Space Physics</title></titleInfo><titleInfo type="abbreviated"><title>J. Geophys. Res.</title></titleInfo><genre type="journal">journal</genre><subject><genre>index-terms</genre><topic authorityURI="http://psi.agu.org/subset/SMP">Magnetospheric Physics</topic><topic authorityURI="http://psi.agu.org/taxonomy5/1200">GEODESY AND GRAVITY</topic><topic authorityURI="http://psi.agu.org/taxonomy5/1221">Lunar and planetary geodesy and gravity</topic><topic authorityURI="http://psi.agu.org/taxonomy5/2700">MAGNETOSPHERIC PHYSICS</topic><topic authorityURI="http://psi.agu.org/taxonomy5/2784">Solar wind/magnetosphere interactions</topic><topic authorityURI="http://psi.agu.org/taxonomy5/3300">ATMOSPHERIC PROCESSES</topic><topic authorityURI="http://psi.agu.org/taxonomy5/3346">Planetary meteorology</topic><topic authorityURI="http://psi.agu.org/taxonomy5/5700">PLANETARY SCIENCES: FLUID PLANETS</topic><topic authorityURI="http://psi.agu.org/taxonomy5/5739">Meteorology</topic><topic authorityURI="http://psi.agu.org/taxonomy5/5744">Orbital and rotational dynamics</topic><topic authorityURI="http://psi.agu.org/taxonomy5/6200">PLANETARY SCIENCES: SOLAR SYSTEM OBJECTS</topic><topic authorityURI="http://psi.agu.org/taxonomy5/6275">Saturn</topic><topic authorityURI="http://psi.agu.org/taxonomy5/7500">SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY</topic><topic authorityURI="http://psi.agu.org/taxonomy5/7534">Radio emissions</topic></subject><subject><genre>article-category</genre><topic>Magnetospheric Physics</topic></subject><identifier type="ISSN">0148-0227</identifier><identifier type="eISSN">2156-2202</identifier><identifier type="DOI">10.1002/(ISSN)2156-2202a</identifier><identifier type="CODEN">JGREA2</identifier><identifier type="PublisherID">JGRA</identifier><part><date>2005</date><detail type="volume"><caption>vol.</caption><number>110</number></detail><detail type="issue"><caption>no.</caption><number>A12</number></detail><extent unit="pages"><start>n/a</start><end>n/a</end><total>9</total></extent></part></relatedItem><identifier type="istex">D06FBD19BCC421BBDFE9BDB7F748A4A4359B70D7</identifier><identifier type="DOI">10.1029/2005JA011085</identifier><identifier type="ArticleID">2005JA011085</identifier><accessCondition type="use and reproduction" contentType="copyright">Copyright 2005 by the American Geophysical Union.</accessCondition><recordInfo><recordContentSource>WILEY</recordContentSource></recordInfo></mods></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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