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<ri:Resource created="2005-06-16T13:31:16Z" status="active" updated="2025-05-19T09:50:00Z" 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>Chromospheric activity-age relation</title><shortName>J/MNRAS/298/332</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/298/332</identifier><altIdentifier>doi:10.26093/cds/vizier.72980332</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Rocha-Pinto H.J.</name></creator><creator><name>Maciel W.J.</name></creator><date role="Updated">2024-06-25T20:18:02Z</date><date role="Created">2005-06-16T13:31:16Z</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>stellar-ages</subject><subject>metallicity</subject><description>We show that there is a relationship between the age excess, defined as the difference between the stellar isochrone and chromospheric ages, and the metallicity as measured by the index [Fe/H] for late-type dwarfs. The chromospheric age tends to be lower than the isochrone age for metal-poor stars, and the opposite occurs for metal-rich objects. We suggest that this could be an effect of neglecting the metallicity dependence of the calibrated chromospheric emission-age relation. We propose a correction to account for this dependence. We also investigate the metallicity distributions of these stars, and show that there are distinct trends according to the chromospheric activity level. Inactive stars have a metallicity distribution which resembles the metallicity distribution of solar neighbourhood stars, while active stars appear to be concentrated in an activity strip on the log(R'_HK_)*[Fe/H] diagram. 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>HD</name><description>HD (Cat. &lt;III/135&gt;) number</description><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>m_HD</name><description>[ABC] Multiplicity index on HD</description><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>logR'HK</name><description>logR'_HK_ index (measurement of the chromospheric emission)</description><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>[Fe/H]</name><description>Metallicity</description><unit>log(Sun)</unit><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>logTeff</name><description>Effective temperature</description><unit>log(K)</unit><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>DVMAG</name><description>Differential absolute V magnitude</description><unit>mag</unit><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>logtiso</name><description>? 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