2 μm Spectrophotometry of Jovian Stratospheric Aerosols—Scattering Opacities, Vertical Distributions, and Wind Speeds
Identifieur interne : 000744 ( Main/Corpus ); précédent : 000743; suivant : 0007452 μm Spectrophotometry of Jovian Stratospheric Aerosols—Scattering Opacities, Vertical Distributions, and Wind Speeds
Auteurs : Don Banfield ; Peter J. Gierasch ; Steven W. Squyres ; Philip D. Nicholson ; Barney J. Conrath ; Keith MatthewsSource :
- Icarus [ 0019-1035 ] ; 1996.
Abstract
Narrow-band 2.0–2.35 μm spectrophotometric observations of Jupiter at nine wavelengths were taken with the 5-m Hale Telescope at Palomar during the month following the impact of Comet P/Shoemaker–Levy 9. Spectra were obtained for the principal impact sites, and also for regions not affected by the comet impacts (the South Polar Region, North Equatorial Zone, South Equatorial Zone, and the Great Red Spot). A technique by which near-infrared reflection spectra can be inverted to yield vertical profiles of scatterer density is presented. For our wavelengths and bandwidths, the sensitivity of the inversions extends from pressure levels near 1 bar up to about 20 mbar. We find that all comet-induced aerosol clouds lie near or above the vertical limit of our sensitivity, i.e., 20 mbar. The lower limit of the clouds is around 50 mbar. The total scattering opacity of the clouds decreased by a factor of about 1.7 over the 35 days spanned by these observations, while the area covered by them increased by a factor of about 1.5. Westet al.(West, R. A., E. Karkoschka, A. J. Friedson, M. Seymour, K. H. Baines, and H. B. Hammel 1995.Science267, 1296–1301.) suggest particle coagulation during this time which fits with our observations, but particle fallout is also likely. All the aerosols comprise a volume the equivalent ofa∼ 0.6-km radius sphere assuming a particle size of 0.25 μm. We also measured the drift speeds of these clouds using two different techniques. One involved scaling down Voyager-measured cloud-top winds (Limaye, S. S. 1986.Icarus65, 335–352.) and deforming early images to match later images, while the other involved directly cross-correlating longitudinally shifted images of spots from different times. Both techniques indicate wind speeds of order 5 m/sec, or ∼30% of the tropospheric wind speeds measured by Voyager in this region.
Url:
DOI: 10.1006/icar.1996.0095
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<record><TEI wicri:istexFullTextTei="biblStruct"><teiHeader><fileDesc><titleStmt><title xml:lang="en">2 μm Spectrophotometry of Jovian Stratospheric Aerosols—Scattering Opacities, Vertical Distributions, and Wind Speeds</title><author><name sortKey="Banfield, Don" sort="Banfield, Don" uniqKey="Banfield D" first="Don" last="Banfield">Don Banfield</name><affiliation><mods:affiliation>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</mods:affiliation></affiliation></author><author><name sortKey="Gierasch, Peter J" sort="Gierasch, Peter J" uniqKey="Gierasch P" first="Peter J." last="Gierasch">Peter J. Gierasch</name><affiliation><mods:affiliation>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</mods:affiliation></affiliation></author><author><name sortKey="Squyres, Steven W" sort="Squyres, Steven W" uniqKey="Squyres S" first="Steven W." last="Squyres">Steven W. Squyres</name><affiliation><mods:affiliation>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</mods:affiliation></affiliation></author><author><name sortKey="Nicholson, Philip D" sort="Nicholson, Philip D" uniqKey="Nicholson P" first="Philip D." last="Nicholson">Philip D. Nicholson</name><affiliation><mods:affiliation>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</mods:affiliation></affiliation></author><author><name sortKey="Conrath, Barney J" sort="Conrath, Barney J" uniqKey="Conrath B" first="Barney J." last="Conrath">Barney J. 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Gierasch</name><affiliation><mods:affiliation>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</mods:affiliation></affiliation></author><author><name sortKey="Squyres, Steven W" sort="Squyres, Steven W" uniqKey="Squyres S" first="Steven W." last="Squyres">Steven W. Squyres</name><affiliation><mods:affiliation>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</mods:affiliation></affiliation></author><author><name sortKey="Nicholson, Philip D" sort="Nicholson, Philip D" uniqKey="Nicholson P" first="Philip D." last="Nicholson">Philip D. Nicholson</name><affiliation><mods:affiliation>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</mods:affiliation></affiliation></author><author><name sortKey="Conrath, Barney J" sort="Conrath, Barney J" uniqKey="Conrath B" first="Barney J." last="Conrath">Barney J. Conrath</name><affiliation><mods:affiliation>Code 693, Goddard Space Flight Center, Greenbelt, Maryland, 20771</mods:affiliation></affiliation></author><author><name sortKey="Matthews, Keith" sort="Matthews, Keith" uniqKey="Matthews K" first="Keith" last="Matthews">Keith Matthews</name><affiliation><mods:affiliation>Caltech 320–47, Pasadena, California, 91125</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j">Icarus</title><title level="j" type="abbrev">YICAR</title><idno type="ISSN">0019-1035</idno><imprint><publisher>ELSEVIER</publisher><date type="published" when="1996">1996</date><biblScope unit="volume">121</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="389">389</biblScope><biblScope unit="page" to="410">410</biblScope></imprint><idno type="ISSN">0019-1035</idno></series><idno type="istex">E9D70F4740BB744514B753685518C5269CF65389</idno><idno type="DOI">10.1006/icar.1996.0095</idno><idno type="PII">S0019-1035(96)90095-0</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0019-1035</idno></seriesStmt></fileDesc><profileDesc><textClass></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Narrow-band 2.0–2.35 μm spectrophotometric observations of Jupiter at nine wavelengths were taken with the 5-m Hale Telescope at Palomar during the month following the impact of Comet P/Shoemaker–Levy 9. Spectra were obtained for the principal impact sites, and also for regions not affected by the comet impacts (the South Polar Region, North Equatorial Zone, South Equatorial Zone, and the Great Red Spot). A technique by which near-infrared reflection spectra can be inverted to yield vertical profiles of scatterer density is presented. For our wavelengths and bandwidths, the sensitivity of the inversions extends from pressure levels near 1 bar up to about 20 mbar. We find that all comet-induced aerosol clouds lie near or above the vertical limit of our sensitivity, i.e., 20 mbar. The lower limit of the clouds is around 50 mbar. The total scattering opacity of the clouds decreased by a factor of about 1.7 over the 35 days spanned by these observations, while the area covered by them increased by a factor of about 1.5. Westet al.(West, R. A., E. Karkoschka, A. J. Friedson, M. Seymour, K. H. Baines, and H. B. Hammel 1995.Science267, 1296–1301.) suggest particle coagulation during this time which fits with our observations, but particle fallout is also likely. All the aerosols comprise a volume the equivalent ofa∼ 0.6-km radius sphere assuming a particle size of 0.25 μm. We also measured the drift speeds of these clouds using two different techniques. One involved scaling down Voyager-measured cloud-top winds (Limaye, S. S. 1986.Icarus65, 335–352.) and deforming early images to match later images, while the other involved directly cross-correlating longitudinally shifted images of spots from different times. Both techniques indicate wind speeds of order 5 m/sec, or ∼30% of the tropospheric wind speeds measured by Voyager in this region.</div></front></TEI><istex><corpusName>elsevier</corpusName><author><json:item><name>Don Banfield</name><affiliations><json:string>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</json:string></affiliations></json:item><json:item><name>Peter J. Gierasch</name><affiliations><json:string>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</json:string></affiliations></json:item><json:item><name>Steven W. Squyres</name><affiliations><json:string>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</json:string></affiliations></json:item><json:item><name>Philip D. 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Spectra were obtained for the principal impact sites, and also for regions not affected by the comet impacts (the South Polar Region, North Equatorial Zone, South Equatorial Zone, and the Great Red Spot). A technique by which near-infrared reflection spectra can be inverted to yield vertical profiles of scatterer density is presented. For our wavelengths and bandwidths, the sensitivity of the inversions extends from pressure levels near 1 bar up to about 20 mbar. We find that all comet-induced aerosol clouds lie near or above the vertical limit of our sensitivity, i.e., 20 mbar. The lower limit of the clouds is around 50 mbar. The total scattering opacity of the clouds decreased by a factor of about 1.7 over the 35 days spanned by these observations, while the area covered by them increased by a factor of about 1.5. Westet al.(West, R. A., E. Karkoschka, A. J. Friedson, M. Seymour, K. H. Baines, and H. B. Hammel 1995.Science267, 1296–1301.) suggest particle coagulation during this time which fits with our observations, but particle fallout is also likely. All the aerosols comprise a volume the equivalent ofa∼ 0.6-km radius sphere assuming a particle size of 0.25 μm. We also measured the drift speeds of these clouds using two different techniques. One involved scaling down Voyager-measured cloud-top winds (Limaye, S. S. 1986.Icarus65, 335–352.) and deforming early images to match later images, while the other involved directly cross-correlating longitudinally shifted images of spots from different times. Both techniques indicate wind speeds of order 5 m/sec, or ∼30% of the tropospheric wind speeds measured by Voyager in this region.</abstract><qualityIndicators><score>8</score><pdfVersion>1.1</pdfVersion><pdfPageSize>550 x 746 pts</pdfPageSize><refBibsNative>false</refBibsNative><keywordCount>0</keywordCount><abstractCharCount>1863</abstractCharCount><pdfWordCount>9838</pdfWordCount><pdfCharCount>54418</pdfCharCount><pdfPageCount>22</pdfPageCount><abstractWordCount>293</abstractWordCount></qualityIndicators><title>2 μm Spectrophotometry of Jovian Stratospheric Aerosols—Scattering Opacities, Vertical Distributions, and Wind Speeds</title><pii><json:string>S0019-1035(96)90095-0</json:string></pii><genre><json:string>research-article</json:string></genre><host><volume>121</volume><pii><json:string>S0019-1035(00)X0064-4</json:string></pii><pages><last>410</last><first>389</first></pages><issn><json:string>0019-1035</json:string></issn><issue>2</issue><genre><json:string>journal</json:string></genre><language><json:string>unknown</json:string></language><title>Icarus</title><publicationDate>1996</publicationDate></host><categories><wos><json:string>ASTRONOMY & ASTROPHYSICS</json:string></wos></categories><publicationDate>1996</publicationDate><copyrightDate>1996</copyrightDate><doi><json:string>10.1006/icar.1996.0095</json:string></doi><id>E9D70F4740BB744514B753685518C5269CF65389</id><score>1.2149911</score><fulltext><json:item><original>true</original><mimetype>application/pdf</mimetype><extension>pdf</extension><uri>https://api.istex.fr/document/E9D70F4740BB744514B753685518C5269CF65389/fulltext/pdf</uri></json:item><json:item><original>false</original><mimetype>application/zip</mimetype><extension>zip</extension><uri>https://api.istex.fr/document/E9D70F4740BB744514B753685518C5269CF65389/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/E9D70F4740BB744514B753685518C5269CF65389/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main" xml:lang="en">2 μm Spectrophotometry of Jovian Stratospheric Aerosols—Scattering Opacities, Vertical Distributions, and Wind Speeds</title><respStmt><resp>Références bibliographiques récupérées via GROBID</resp><name resp="ISTEX-API">ISTEX-API (INIST-CNRS)</name></respStmt></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>ELSEVIER</publisher><availability><p>©1996 Academic Press</p></availability><date>1996</date></publicationStmt><notesStmt><note type="content">Section title: Regular Article</note></notesStmt><sourceDesc><biblStruct type="inbook"><analytic><title level="a" type="main" xml:lang="en">2 μm Spectrophotometry of Jovian Stratospheric Aerosols—Scattering Opacities, Vertical Distributions, and Wind Speeds</title><author xml:id="author-1"><persName><forename type="first">Don</forename><surname>Banfield</surname></persName><email>banfield@astrosun.tn.cornell.eduf1</email></author><author xml:id="author-2"><persName><forename type="first">Peter J.</forename><surname>Gierasch</surname></persName><email>banfield@astrosun.tn.cornell.eduf1</email></author><author xml:id="author-3"><persName><forename type="first">Steven W.</forename><surname>Squyres</surname></persName><email>banfield@astrosun.tn.cornell.eduf1</email></author><author xml:id="author-4"><persName><forename type="first">Philip D.</forename><surname>Nicholson</surname></persName><email>banfield@astrosun.tn.cornell.eduf1</email></author><author xml:id="author-5"><persName><forename type="first">Barney J.</forename><surname>Conrath</surname></persName><affiliation>Code 693, Goddard Space Flight Center, Greenbelt, Maryland, 20771</affiliation></author><author xml:id="author-6"><persName><forename type="first">Keith</forename><surname>Matthews</surname></persName><affiliation>Caltech 320–47, Pasadena, California, 91125</affiliation></author></analytic><monogr><title level="j">Icarus</title><title level="j" type="abbrev">YICAR</title><idno type="pISSN">0019-1035</idno><idno type="PII">S0019-1035(00)X0064-4</idno><imprint><publisher>ELSEVIER</publisher><date type="published" when="1996"></date><biblScope unit="volume">121</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="389">389</biblScope><biblScope unit="page" to="410">410</biblScope></imprint></monogr><idno type="istex">E9D70F4740BB744514B753685518C5269CF65389</idno><idno type="DOI">10.1006/icar.1996.0095</idno><idno type="PII">S0019-1035(96)90095-0</idno></biblStruct></sourceDesc></fileDesc><profileDesc><creation><date>1996</date></creation><langUsage><language ident="en">en</language></langUsage><abstract xml:lang="en"><p>Narrow-band 2.0–2.35 μm spectrophotometric observations of Jupiter at nine wavelengths were taken with the 5-m Hale Telescope at Palomar during the month following the impact of Comet P/Shoemaker–Levy 9. Spectra were obtained for the principal impact sites, and also for regions not affected by the comet impacts (the South Polar Region, North Equatorial Zone, South Equatorial Zone, and the Great Red Spot). A technique by which near-infrared reflection spectra can be inverted to yield vertical profiles of scatterer density is presented. For our wavelengths and bandwidths, the sensitivity of the inversions extends from pressure levels near 1 bar up to about 20 mbar. We find that all comet-induced aerosol clouds lie near or above the vertical limit of our sensitivity, i.e., 20 mbar. The lower limit of the clouds is around 50 mbar. The total scattering opacity of the clouds decreased by a factor of about 1.7 over the 35 days spanned by these observations, while the area covered by them increased by a factor of about 1.5. Westet al.(West, R. A., E. Karkoschka, A. J. Friedson, M. Seymour, K. H. Baines, and H. B. Hammel 1995.Science267, 1296–1301.) suggest particle coagulation during this time which fits with our observations, but particle fallout is also likely. All the aerosols comprise a volume the equivalent ofa∼ 0.6-km radius sphere assuming a particle size of 0.25 μm. We also measured the drift speeds of these clouds using two different techniques. One involved scaling down Voyager-measured cloud-top winds (Limaye, S. S. 1986.Icarus65, 335–352.) and deforming early images to match later images, while the other involved directly cross-correlating longitudinally shifted images of spots from different times. Both techniques indicate wind speeds of order 5 m/sec, or ∼30% of the tropospheric wind speeds measured by Voyager in this region.</p></abstract></profileDesc><revisionDesc><change when="1996-02-20">Modified</change><change when="1996">Published</change><change xml:id="refBibs-istex" who="#ISTEX-API" when="2016-10-6">References added</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><original>false</original><mimetype>text/plain</mimetype><extension>txt</extension><uri>https://api.istex.fr/document/E9D70F4740BB744514B753685518C5269CF65389/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Elsevier converted-article found"><istex:xmlDeclaration>version="1.0" encoding="utf-8"</istex:xmlDeclaration><istex:docType PUBLIC="-//ES//DTD journal article DTD version 4.5.2//EN//XML" URI="art452.dtd" name="istex:docType"></istex:docType><istex:document><converted-article version="4.5.2" docsubtype="fla" xml:lang="en"><item-info><jid>YICAR</jid><aid>90095</aid><ce:pii>S0019-1035(96)90095-0</ce:pii><ce:doi>10.1006/icar.1996.0095</ce:doi><ce:copyright type="full-transfer" year="1996">Academic Press</ce:copyright></item-info><head><ce:dochead><ce:textfn>Regular Article</ce:textfn></ce:dochead><ce:title>2 μm Spectrophotometry of Jovian Stratospheric Aerosols—Scattering Opacities, Vertical Distributions, and Wind Speeds</ce:title><ce:author-group><ce:author><ce:given-name>Don</ce:given-name><ce:surname>Banfield</ce:surname><ce:cross-ref refid="A0"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Peter J.</ce:given-name><ce:surname>Gierasch</ce:surname><ce:cross-ref refid="A0"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Steven W.</ce:given-name><ce:surname>Squyres</ce:surname><ce:cross-ref refid="A0"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Philip D.</ce:given-name><ce:surname>Nicholson</ce:surname><ce:cross-ref refid="A0"><ce:sup>a</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Barney J.</ce:given-name><ce:surname>Conrath</ce:surname><ce:cross-ref refid="A1"><ce:sup>b</ce:sup></ce:cross-ref></ce:author><ce:author><ce:given-name>Keith</ce:given-name><ce:surname>Matthews</ce:surname><ce:cross-ref refid="A2"><ce:sup>c</ce:sup></ce:cross-ref></ce:author><ce:affiliation id="A0"><ce:label>a</ce:label><ce:textfn>Department of Astronomy, Cornell University, Ithaca, New York, 14853, <ce:footnote id="F1"><ce:label>f1</ce:label><ce:note-para>E-mail: banfield@astrosun.tn.cornell.edu</ce:note-para></ce:footnote><ce:cross-ref refid="F1"><ce:sup>f1</ce:sup></ce:cross-ref></ce:textfn></ce:affiliation><ce:affiliation id="A1"><ce:label>b</ce:label><ce:textfn>Code 693, Goddard Space Flight Center, Greenbelt, Maryland, 20771</ce:textfn></ce:affiliation><ce:affiliation id="A2"><ce:label>c</ce:label><ce:textfn>Caltech 320–47, Pasadena, California, 91125</ce:textfn></ce:affiliation></ce:author-group><ce:date-received day="17" month="7" year="1995"></ce:date-received><ce:date-revised day="20" month="2" year="1996"></ce:date-revised><ce:abstract><ce:section-title>Abstract</ce:section-title><ce:abstract-sec><ce:simple-para>Narrow-band 2.0–2.35 μm spectrophotometric observations of Jupiter at nine wavelengths were taken with the 5-m Hale Telescope at Palomar during the month following the impact of Comet P/Shoemaker–Levy 9. Spectra were obtained for the principal impact sites, and also for regions not affected by the comet impacts (the South Polar Region, North Equatorial Zone, South Equatorial Zone, and the Great Red Spot).</ce:simple-para><ce:simple-para>A technique by which near-infrared reflection spectra can be inverted to yield vertical profiles of scatterer density is presented. For our wavelengths and bandwidths, the sensitivity of the inversions extends from pressure levels near 1 bar up to about 20 mbar. We find that all comet-induced aerosol clouds lie near or above the vertical limit of our sensitivity, i.e., 20 mbar. The lower limit of the clouds is around 50 mbar. The total scattering opacity of the clouds decreased by a factor of about 1.7 over the 35 days spanned by these observations, while the area covered by them increased by a factor of about 1.5. West<ce:italic>et al.</ce:italic>(West, R. A., E. Karkoschka, A. J. Friedson, M. Seymour, K. H. Baines, and H. B. Hammel 1995.<ce:italic>Science</ce:italic>267, 1296–1301.) suggest particle coagulation during this time which fits with our observations, but particle fallout is also likely. All the aerosols comprise a volume the equivalent of<ce:italic>a</ce:italic>∼ 0.6-km radius sphere assuming a particle size of 0.25 μm.</ce:simple-para><ce:simple-para>We also measured the drift speeds of these clouds using two different techniques. One involved scaling down Voyager-measured cloud-top winds (Limaye, S. S. 1986.<ce:italic>Icarus</ce:italic>65, 335–352.) and deforming early images to match later images, while the other involved directly cross-correlating longitudinally shifted images of spots from different times. Both techniques indicate wind speeds of order 5 m/sec, or ∼30% of the tropospheric wind speeds measured by Voyager in this region.</ce:simple-para></ce:abstract-sec></ce:abstract></head></converted-article></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>2 μm Spectrophotometry of Jovian Stratospheric Aerosols—Scattering Opacities, Vertical Distributions, and Wind Speeds</title></titleInfo><titleInfo type="alternative" lang="en" contentType="CDATA"><title>2 μm Spectrophotometry of Jovian Stratospheric Aerosols—Scattering Opacities, Vertical Distributions, and Wind Speeds</title></titleInfo><name type="personal"><namePart type="given">Don</namePart><namePart type="family">Banfield</namePart><affiliation>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Peter J.</namePart><namePart type="family">Gierasch</namePart><affiliation>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Steven W.</namePart><namePart type="family">Squyres</namePart><affiliation>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Philip D.</namePart><namePart type="family">Nicholson</namePart><affiliation>Department of Astronomy, Cornell University, Ithaca, New York, 14853, f1 E-mail: banfield@astrosun.tn.cornell.eduf1</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Barney J.</namePart><namePart type="family">Conrath</namePart><affiliation>Code 693, Goddard Space Flight Center, Greenbelt, Maryland, 20771</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Keith</namePart><namePart type="family">Matthews</namePart><affiliation>Caltech 320–47, Pasadena, California, 91125</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="research-article" displayLabel="Full-length article"></genre><originInfo><publisher>ELSEVIER</publisher><dateIssued encoding="w3cdtf">1996</dateIssued><dateModified encoding="w3cdtf">1996-02-20</dateModified><copyrightDate encoding="w3cdtf">1996</copyrightDate></originInfo><language><languageTerm type="code" authority="iso639-2b">eng</languageTerm><languageTerm type="code" authority="rfc3066">en</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType></physicalDescription><abstract lang="en">Narrow-band 2.0–2.35 μm spectrophotometric observations of Jupiter at nine wavelengths were taken with the 5-m Hale Telescope at Palomar during the month following the impact of Comet P/Shoemaker–Levy 9. Spectra were obtained for the principal impact sites, and also for regions not affected by the comet impacts (the South Polar Region, North Equatorial Zone, South Equatorial Zone, and the Great Red Spot). A technique by which near-infrared reflection spectra can be inverted to yield vertical profiles of scatterer density is presented. For our wavelengths and bandwidths, the sensitivity of the inversions extends from pressure levels near 1 bar up to about 20 mbar. We find that all comet-induced aerosol clouds lie near or above the vertical limit of our sensitivity, i.e., 20 mbar. The lower limit of the clouds is around 50 mbar. The total scattering opacity of the clouds decreased by a factor of about 1.7 over the 35 days spanned by these observations, while the area covered by them increased by a factor of about 1.5. Westet al.(West, R. A., E. Karkoschka, A. J. Friedson, M. Seymour, K. H. Baines, and H. B. Hammel 1995.Science267, 1296–1301.) suggest particle coagulation during this time which fits with our observations, but particle fallout is also likely. All the aerosols comprise a volume the equivalent ofa∼ 0.6-km radius sphere assuming a particle size of 0.25 μm. We also measured the drift speeds of these clouds using two different techniques. One involved scaling down Voyager-measured cloud-top winds (Limaye, S. S. 1986.Icarus65, 335–352.) and deforming early images to match later images, while the other involved directly cross-correlating longitudinally shifted images of spots from different times. Both techniques indicate wind speeds of order 5 m/sec, or ∼30% of the tropospheric wind speeds measured by Voyager in this region.</abstract><note type="content">Section title: Regular Article</note><relatedItem type="host"><titleInfo><title>Icarus</title></titleInfo><titleInfo type="abbreviated"><title>YICAR</title></titleInfo><genre type="journal">journal</genre><originInfo><dateIssued encoding="w3cdtf">199606</dateIssued></originInfo><identifier type="ISSN">0019-1035</identifier><identifier type="PII">S0019-1035(00)X0064-4</identifier><part><date>199606</date><detail type="volume"><number>121</number><caption>vol.</caption></detail><detail type="issue"><number>2</number><caption>no.</caption></detail><extent unit="issue pages"><start>207</start><end>511</end></extent><extent unit="pages"><start>389</start><end>410</end></extent></part></relatedItem><identifier type="istex">E9D70F4740BB744514B753685518C5269CF65389</identifier><identifier type="DOI">10.1006/icar.1996.0095</identifier><identifier type="PII">S0019-1035(96)90095-0</identifier><accessCondition type="use and reproduction" contentType="copyright">©1996 Academic Press</accessCondition><recordInfo><recordContentSource>ELSEVIER</recordContentSource><recordOrigin>Academic Press, ©1996</recordOrigin></recordInfo></mods></metadata><enrichments><istex:catWosTEI uri="https://api.istex.fr/document/E9D70F4740BB744514B753685518C5269CF65389/enrichments/catWos"><teiHeader><profileDesc><textClass><classCode scheme="WOS">ASTRONOMY & ASTROPHYSICS</classCode></textClass></profileDesc></teiHeader></istex:catWosTEI><istex:refBibTEI uri="https://api.istex.fr/document/E9D70F4740BB744514B753685518C5269CF65389/enrichments/refBib"><teiHeader></teiHeader><text><front></front><body></body><back><listBibl><biblStruct><analytic><title level="a" type="main">The average wind speeds throughout the spot region using our second technique were greater for spot Quasi-spot K by a factor of about 4/3. 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