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<ri:Resource created="2000-10-29T21:13:19Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" 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/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>1984-1998 BV photometry of V815 Her</title><shortName>J/A+A/362/223</shortName><identifier>ivo://CDS.VizieR/J/A+A/362/223</identifier><altIdentifier>doi:10.26093/cds/vizier.33620223</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Jetsu L.</name></creator><creator><name>Hackman T.</name></creator><creator><name>Hall D.S.</name></creator><creator><name>Henry G.W.</name></creator><creator><name>Kokko M.</name></creator><creator><name>You J.</name></creator><date role="Updated">2000-10-29T20:13:25Z</date><date role="Created">2000-10-29T21:13:19Z</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>variable-stars</subject><subject>visible-astronomy</subject><subject>broad-band-photometry</subject><description>As a case study of the solar-stellar connection, we have analysed a prolonged time series of BV photometry of the chromospherically active binary V815 Her. The surface differential rotation in the rapidly rotating G5V primary caused changes of 4.6% in the seasonal photometric rotation periods. This would imply a differential rotation coefficient of k=0.184, if the rotation of the starspots follow the solar law of differential rotation and the activity is confined within the same latitudinal range as in the Sun, having k=0.189 and the spectral type G2V. Our analysis of the primary and secondary minima of the seasonal light curves indicated that the regions of stronger activity have concentrated on one active longitude, which has maintained a constant rotation period of 1.79244d for about 14 years. No regular activity cycle was detected in the mean brightness changes of V815 Her.</description><source format="bibcode">2000A&amp;A...362..223J</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/362/223</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>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/350/513">J/A+A/350/513 : V368 Cep UBVRI time series (Kahanpaa+, 1999)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+AS/139/513">J/A+AS/139/513 : 1975-1995 V1794 Cyg UBVRI photometry (Jetsu+, 1999)</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/362/223</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/362/223</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/362/223</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/362/223</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/362/223</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/362/223</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><coverage><footprint ivo-id="ivo://ivoa.net/std/moc"/><waveband>Optical</waveband></coverage><tableset><schema><name>default</name><table><name>J/A+A/362/223/table1</name><description>V and B V815 Her differential magnitudes</description><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>SET</name><description>Subset number ( a total of 98 subsets)</description><ucd>meta.id</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>HJD</name><description>Heliocentric Julian date</description><unit>d</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>Bmag</name><description>? V815 Her minus HD 166093 magnitude difference in the standard Johnson B system</description><unit>mag</unit><ucd>phot.mag;arith.diff</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Vmag</name><description>? V815 Her minus HD 166093 magnitude difference in the standard Johnson V system</description><unit>mag</unit><ucd>phot.mag;arith.diff</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column></table></schema></tableset></ri:Resource>