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<ri:Resource created="2015-01-09T08:28:04Z" 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>W UMa-type contact binaries ages and masses</title><shortName>J/MNRAS/437/185</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/437/185</identifier><altIdentifier>doi:10.26093/cds/vizier.74370185</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Yildiz M.</name></creator><date role="Updated">2024-08-07T20:12:26Z</date><date role="Created">2015-01-09T08:28:04Z</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>eclipsing-binary-stars</subject><subject>stellar-masses</subject><subject>stellar-ages</subject><description>Recently, our understanding of the origin of W UMa-type contact binaries has become clearer. Initial masses of their components were successfully estimated by Yildiz and Dogan using a new method mainly based on observational properties of overluminous secondary components. In this paper, we continue to discuss the results and make computations for age and orbital evolution of these binaries. It is shown that the secondary mass, according to its luminosity, also successfully predicts the observed radius. While the current mass of the primary component is determined by initial masses, the current secondary mass is also a function of initial angular momentum. We develop methods to compute the age of A- and W-subtype W UMa-type contact binaries in terms of initial masses and mass according to the luminosity of the secondaries. Comparisons of our results with the mean ages from kinematic properties of these binaries and data pertaining to contact binaries in open and globular clusters have increased our confidence on this method. The mean ages of both A- and W-subtype contact binaries are found as 4.4 and 4.6Gyr, respectively. From kinematic studies, these ages are given as 4.5 and 4.4Gyr, respectively. We also compute orbital properties of A-subtype contact binaries at the time of the first overflow. Initial angular momentum of these binaries is computed by comparing them with the well-known detached binaries. The angular momentum loss rate derived in the present study for the detached phase is in very good agreement with the semi-empirical rates available in the literature. In addition to the limitations on the initial masses of W UMa-type contact binaries, it is shown that the initial period of these binaries is less than about 4.45d.</description><source format="bibcode">2014MNRAS.437..185Y</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/437/185</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/119">V/119 : Catalogue of field contact binary stars (Pribulla+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/120">V/120 : Catalog of early-type contact binaries (Bondarenko+, 1996)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/PASP/108/332">J/PASP/108/332 : Photometric analysis of contact binaries (Lapasset+ 1996)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AcA/51/259">J/AcA/51/259 : Contact binaries in OGLE-I database (Szymanski+, 2001)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/426/1001">J/A+A/426/1001 : Catalog of contact binary stars (Csizmadia+, 2004)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/131/621">J/AJ/131/621 : Catalog of 1022 bright contact binary stars (Gettel+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/131/633">J/AJ/131/633 : A ROSAT survey of contact binary stars (Geske+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/131/2986">J/AJ/131/2986 : Multiplicity of contact binaries (Pribulla+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AcA/56/253">J/AcA/56/253 : Period changes of OGLE contact binaries (Kubiak+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/373/1483">J/MNRAS/373/1483 : W UMa type and CAB stars dynamical evolution (Eker+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/430/2029">J/MNRAS/430/2029 : W UMa type contact binaries initial masses (Yildiz+, 2013)</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/MNRAS/437/185</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/437/185</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/437/185</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL 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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>PapI</name><description>Display data of previous paper, Yildiz and Dogan 2013, J/MNRAS/430/2029</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType" arraysize="*">char</dataType></column><column><name>Type</name><description>[A/W] Contact binary subtype</description><ucd>src.class</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>a</name><description>[1.4/5.4] Orbital semimajor axis</description><unit>solRad</unit><ucd>phys.angSize.smajAxis</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Per</name><description>[0.2/0.9] Orbital period</description><unit>d</unit><ucd>time.period</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>M1</name><description>[0.5/2.8] Mass of primary</description><unit>solMass</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_M1</name><description>rms uncertainty on M1</description><unit>solMass</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>M2</name><description>[0.1/1.0] Mass of secondary</description><unit>solMass</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_M2</name><description>rms uncertainty on M2</description><unit>solMass</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>M1i</name><description>Initial mass of primary before the mass transfer</description><unit>solMass</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_M1i</name><description>rms uncertainty on M1i</description><unit>solMass</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>M2i</name><description>Initial mass of secondary before the mass transfer</description><unit>solMass</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_M2i</name><description>rms uncertainty on M2i</description><unit>solMass</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>M2L</name><description>Mass of secondary according to luminosity</description><unit>solMass</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_M2L</name><description>rms uncertainty on M2L</description><unit>solMass</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>t</name><description>[1.2/11.1] Age (see Section 3)</description><unit>Gyr</unit><ucd>time.age</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_t</name><description>rms uncertainty on age</description><unit>Gyr</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>tB</name><description>Age from Bukowiecki et al. 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