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<ri:Resource created="2013-09-30T08:09:02Z" 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>Photometric rotation periods of stars in {alpha} Per</title><shortName>V/140</shortName><identifier>ivo://CDS.VizieR/V/140</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Prosser C.F.</name></creator><creator><name>Grankin K.N.</name></creator><date role="Updated">2017-10-16T14:57:22Z</date><date role="Created">2013-09-30T08:09:02Z</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>open-star-clusters</subject><subject>apparent-magnitude</subject><description>We present the results from a photometric monitoring program of primarily solar-type open cluster stars obtained during 1994 and 1995. Several members of the {alpha} Persei cluster have been monitored and the corresponding relation between coronal x-ray activity and rotation period derived. The relation among mid-G/K type members illustrates both the previously noticed downturn in L_X_/L_bol_ at high rotation rates and the sharp decrease in coronal activity at long rotation periods as seen among Pleiades stars. Intensive observation of one slowly rotating G-type member of IC 4665 has enabled a period determination of 8-10 days to be made and illustrates the need for (and limitations of) high quality observations.</description><source format="bibcode">1997cfa..rept.....P</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/V/140</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/V/80">V/80 : Alpha Per Cluster Low-Mass Stars' Membership (Prosser 1992)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/426/3403">J/MNRAS/426/3403 : UKIDSS GCS alpha Persei members (Lodieu+, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/488/409">J/A+A/488/409 : Radial velocities of {alpha} Per stars (Mermilliod+, 2008)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/131/2967">J/AJ/131/2967 : {alpha} Persei open cluster members (Makarov+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/395/813">J/A+A/395/813 : Alpha Per faint stars photometry (Barrado y Navascues+ 2002)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AN/319/215">J/AN/319/215 : Alpha Per cluster low-mass members. II. (Prosser+, 1998)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AN/319/201">J/AN/319/201 : Alpha Per cluster low-mass members. I. 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B-V color index from literature</description><unit>mag</unit><ucd>phot.color;em.opt.B;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>l_Vsini</name><description>Limit flag on Vsini</description><ucd>meta.code.error;phys.veloc.rotat</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>Vsini</name><description>? Projected rotational velocity from literature, or lower limit of Vsini interval</description><unit>km/s</unit><ucd>phys.veloc.rotat</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>f_Vsini</name><description>[-] If -, Vsini and B_Vsini are Vsini interval</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>B_Vsini</name><description>? 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