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<ri:Resource created="2022-10-28T07:15:27Z" 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>Light minimum times for 4 contact binaries</title><shortName>J/AJ/163/250</shortName><identifier>ivo://CDS.VizieR/J/AJ/163/250</identifier><altIdentifier>doi:10.26093/cds/vizier.51630250</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Yang Y.</name></creator><creator><name>Yuan H.</name></creator><creator><name>Wang S.</name></creator><creator><name>Dai H.</name></creator><date role="Updated">2022-11-25T13:33:25Z</date><date role="Created">2022-10-28T07:15:27Z</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>multiple-stars</subject><subject>eclipsing-binary-stars</subject><subject>infrared-photometry</subject><subject>visible-astronomy</subject><subject>broad-band-photometry</subject><description>We presented new photometry for four short-period late-type binaries, observed by three small telescopes in China from 2020 September to 2021 December. Seven sets of light curves (including the TESS data for FY Boo) were analyzed by using the W-D method. Three binaries (V0576 Peg, V0873 Per, and FY Boo) are W-type binaries with q~2.5, while KW Psc is an A-type binary with q~0.43. Max.I-Max.II is up to 10% of variable light amplitude for the asymmetric light curves, which are modeled by a dark spot on the surface of the more massive component. Photometric results imply the existence of movement and evolution of the cool spot. From the temperature-luminosity and mass-luminosity diagrams, the more massive components are a bit evolved main-sequence stars, while the less massive ones are oversized and overluminous owing to energy exchange. Orbital period analyses indicate that the cyclic oscillations occur in the (O-C) curves. Their modulated periods approach 11yr, which may preferably result from the magnetic activity cycle for four late-type contact binaries. With angular momentum loss through magnetic braking, these short-period contact binaries may evolve into deep-contact configurations.</description><source format="bibcode">2022AJ....163..250Y</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/163/250</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/B/gcvs">B/gcvs : General Catalogue of Variable Stars (Samus+, 2007-2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/II/287">II/287 : Northern Sky Variability Survey (NSVS) (Wozniak+, 2004)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/345">I/345 : Gaia DR2 (Gaia Collaboration, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/146">V/146 : LAMOST DR1 catalogs (Luo+, 2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/106/2096">J/AJ/106/2096 : Limb-darkening coefficients in binaries (Van Hamme 1993)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/311/523">J/A+A/311/523 : Photometry of W UMa (Maceroni+, 1996)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AcA/48/35">J/AcA/48/35 : All Sky Automated Survey variable stars (Pojmamski 1998)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/119/1901">J/AJ/119/1901 : ROTSE all-sky surveys for variable stars (Akerlof+, 2000)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/406/535">J/A+A/406/535 : Hamburg/RASS Cat. of optical ident. 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Final residual</description><unit>d</unit><ucd>stat.fit.residual</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Ref</name><description>References used</description><ucd>meta.ref;instr.setup</ucd><dataType xsi:type="vs:VOTableType" arraysize="5*">char</dataType></column><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>HJD</name><description>Heliocentric Julian Date</description><unit>d</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>e_HJD</name><description>? Error on HJD</description><unit>d</unit><ucd>stat.error;time.epoch</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Epoch</name><description>Epoch time</description><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>Met</name><description>Method used</description><ucd>meta.note</ucd><dataType xsi:type="vs:VOTableType" arraysize="3*">char</dataType></column><column><name>Min</name><description>Minimum eclipse-depth (I or II)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType" arraysize="2*">char</dataType></column></table><table><name>J/AJ/163/250/refs</name><description>References used in this work</description><column><name>recno</name><description>Record number assigned by the VizieR team. 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