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<ri:Resource created="2022-11-28T09:16:57Z" 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>Kepler eclipsing binaries with Gaia data</title><shortName>J/ApJS/262/10</shortName><identifier>ivo://CDS.VizieR/J/ApJS/262/10</identifier><altIdentifier>doi:10.26093/cds/vizier.22620010</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Knote M.F.</name></creator><creator><name>Caballero-Nieves S.M.</name></creator><creator><name>Gokhale V.</name></creator><creator><name>Johnston K.B.</name></creator><creator><name>Perlman E.S.</name></creator><date role="Updated">2023-07-03T14:20:44Z</date><date role="Created">2022-11-28T09:16:57Z</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>photometry</subject><subject>visible-astronomy</subject><subject>stellar-spectral-types</subject><description>The O'Connell effect --the presence of unequal maxima in eclipsing binaries-- remains an unsolved riddle in the study of close binary systems. The Kepler space telescope produced high-precision photometry of nearly 3000 eclipsing binary systems, providing a unique opportunity to study the O'Connell effect in a large sample and in greater detail than in previous studies. We have characterized the observational properties-including temperature, luminosity, and eclipse depth-of a set of 212 systems (7.3% of Kepler eclipsing binaries) that display a maxima flux difference of at least 1%, representing the largest sample of O'Connell effect systems yet studied. We explored how these characteristics correlate with each other to help understand the O'Connell effect's underlying causes. We also describe some system classes with peculiar light-curve features aside from the O'Connell effect (~24% of our sample), including temporal variation and asymmetric minima. We found that the O'Connell effect size's correlations with period and temperature are inconsistent with Kouzuma's starspot study. Up to 20% of systems display the parabolic eclipse timing variation signal expected for binaries undergoing mass transfer. Most systems displaying the O'Connell effect have the brighter maximum following the primary eclipse, suggesting a fundamental link between which maximum is brighter and the O'Connell effect's physical causes. Most importantly, we find that the O'Connell effect occurs exclusively in systems where the components are close enough to significantly affect each other, suggesting that the interaction between the components is ultimately responsible for causing the O'Connell effect.</description><source format="bibcode">2022ApJS..262...10K</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/262/10</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/133">V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/350">I/350 : Gaia EDR3 (Gaia Collaboration, 2020)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/352">I/352 : Distances to 1.47 billion stars in Gaia EDR3 (Bailer-Jones+, 2021)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/395/587">J/A+A/395/587 : GR Tau BV light curves (Zhang+, 2002)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/128/1761">J/AJ/128/1761 : HATNET variability survey (Hartman+, 2004)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/454/855">J/A+A/454/855 : Geneva photometry of W Cru (Pavlovski+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/135/850">J/AJ/135/850 : Eclipsing binaries found in TrES (Devor+, 2008)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/136/1067">J/AJ/136/1067 : New beta Lyrae and Algol candidates in NSVS (Hoffman+, 2008)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/138/466">J/AJ/138/466 : NSVS variables automated classification (Hoffman+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AcA/59/33">J/AcA/59/33 : ASAS. 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