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<ri:Resource created="2010-10-11T08:16:25Z" status="active" updated="2025-06-13T15:25:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>Li abundances in solar-analog stars. II.</title><shortName>J/A+A/515/A93</shortName><identifier>ivo://CDS.VizieR/J/A+A/515/A93</identifier><altIdentifier>doi:10.26093/cds/vizier.35150093</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Takeda Y.</name></creator><creator><name>Honda S.</name></creator><creator><name>Kawanomoto S.</name></creator><creator><name>Ando H.</name></creator><creator><name>Sakurai T.</name></creator><date role="Updated">2017-12-15T10:55:01Z</date><date role="Created">2010-10-11T08:16:25Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>late-type-stars</subject><subject>g-stars</subject><subject>chemical-abundances</subject><subject>effective-temperature</subject><description>We previously attempted to ascertain why the LiI 6708 line-strengths of Sun-like stars differ so significantly despite the superficial similarities of stellar parameters. We carried out a comprehensive analysis of 118 solar analogs and reported that a close connection exists between the Li abundance (A_Li_) and the line-broadening width (v_r+m_) mainly contributed by rotational effect), which led us to conclude that stellar rotation may be the primary control of the surface Li content. To examine our claim in more detail, we study whether the degree of stellar activity exhibits a similar correlation with the Li abundance, which is expected because of the widely believed close connection between rotation and activity.</description><source format="bibcode">2010A&amp;A...515A..93T</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/515/A93</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/I/239">I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/105/2299">J/AJ/105/2299 : Li abundance of solar-type stars. II. (Soderblom+, 1993)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/371/943">J/A+A/371/943 : Lithium abundances for 185 main-sequence stars (Chen+, 2001)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/409/251">J/A+A/409/251 : Li abundances and velocities in F and G stars (Mallik+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/349/757">J/MNRAS/349/757 : Masses, ages and metallicities of F-G dwarfs (Lambert+, 2004)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/PASJ/57/45">J/PASJ/57/45 : Lithium abundances of F-K stars (Takeda+, 2005)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/468/663">J/A+A/468/663 : Li abundances in solar-analog stars (Takeda+, 2007)</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL use="full">https://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/515/A93</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/515/A93</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/515/A93</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/515/A93</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/515/A93</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/515/A93</mirrorURL><queryType>GET</queryType><resultType>text/xml+votable</resultType></interface></capability><capability standardID="ivo://ivoa.net/std/TAP#aux"><interface xsi:type="vs:ParamHTTP" role="std"><accessURL use="base">https://tapvizier.cds.unistra.fr/TAPVizieR/tap</accessURL></interface></capability><capability xsi:type="cs:ConeSearch" standardID="ivo://ivoa.net/std/ConeSearch"><description>Cone search capability for table J/A+A/515/A93/table1 (Activity index, rotation, Li abundance, age, and the atmospheric parameters)</description><interface xsi:type="vs:ParamHTTP" role="std"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/515/A93/table1?</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/515/A93/table1?</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/515/A93/table1?</mirrorURL><queryType>GET</queryType><resultType>text/xml+votable</resultType></interface><maxSR>180.0</maxSR><maxRecords>50000</maxRecords><verbosity>true</verbosity><testQuery><ra>4.6744469</ra><dec>-8.0530006</dec><sr>0.005555555555555556</sr></testQuery></capability><coverage><spatial>6/222 313 414 417 634 742 1058 2032 2072 2366 2456 2476 2697 3307 3398 3691 3919 4128 4241 4313 4437 4665 5073 5263 5522 5699 5726 5858 6087 6269 6325 6409 6522-6523 6612 6705 7052 7217 7326 7978 8103 8286 8993 9492 9883 10400 10424 10473 10878 11212 11709 12343 12922 13766 13778 14349 14411 14650 15014 15030 15174 15221 15727 16930 17083 17219 17266 17419 17486 17888 18366 18373 18623 19424 19796 19923 21114 21211 21484 21516 21594 21940 22313 22355 22746 22779 23123 23150 23177 23429 23511 23545-23546 23583 24178 25966 26496 27254 27750 27757 28282 28362 28961 29513 30123 30127 30878 31029 31287 32575 32585 32617 36057 36590 40317 40892 40932</spatial><footprint ivo-id="ivo://ivoa.net/std/moc">https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/515/A93?format=ascii</footprint><waveband>Optical</waveband></coverage><tableset><schema><name>default</name><table><name>J/A+A/515/A93/table1</name><description>Activity index, rotation, Li abundance, age, and the atmospheric parameters</description><column><name>Rem</name><description>Remarks</description><ucd>meta.note</ucd><dataType xsi:type="vs:VOTableType" arraysize="22*">char</dataType></column><column><name>recno</name><description>Record number assigned by the VizieR team. Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>HIP</name><description>HIP number (0 for Sun/Moon)</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>r0(8542)</name><description>Residual flux at the line center of the CaII 8542 line</description><ucd>phot.flux</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>vsini</name><description>Projected rotational velocity calibrated in this study (cf. 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