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<ri:Resource created="2014-12-04T15:44:23Z" 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>GALEX observations of exoplanet host stars</title><shortName>J/ApJ/766/9</shortName><identifier>ivo://CDS.VizieR/J/ApJ/766/9</identifier><altIdentifier>doi:10.26093/cds/vizier.17660009</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Shkolnik E.L.</name></creator><date role="Updated">2018-01-04T08:21:52Z</date><date role="Created">2014-12-04T15:44:23Z</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>ultraviolet-photometry</subject><subject>solar-system-planets</subject><subject>multiple-stars</subject><description>Using the far-UV (FUV) and near-UV (NUV) photometry from the NASA Galaxy Evolution Explorer (GALEX), we searched for evidence of increased stellar activity due to tidal and/or magnetic star-planet interactions (SPI) in the 272 known FGK planetary hosts observed by GALEX. With the increased sensitivity of GALEX, we are able probe systems with lower activity levels and at larger distances than what has been done to date with X-ray satellites. We compared samples of stars with close-in planets (a&lt;0.1AU) to those with far-out planets (a&gt;0.5AU) and looked for correlations of excess activity with other system parameters. This statistical investigation found no clear correlations with a, M_p_, or M_p_/a, in contrast to some X-ray and CaII studies. However, there is tentative evidence (at a level of 1.8{sigma}) that stars with radial-velocity-(RV)-detected close-in planets are more FUV-active than stars with far-out planets, in agreement with several published X-ray and Ca II results. The case is strengthened to a level of significance to 2.3{sigma} when transit-detected close-in planets are included. This is most likely because the RV-selected sample of stars is significantly less active than the field population of comparable stars, while the transit-selected sample is similarly active. Given the factor of 2-3 scatter in fractional FUV luminosity for a given stellar effective temperature, it is necessary to conduct a time-resolved study of the planet hosts in order to better characterize their UV variability and generate a firmer statistical result.</description><source format="bibcode">2013ApJ...766....9S</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/766/9</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/II/312">II/312 : GALEX-DR5 (GR5) sources from AIS and MIS (Bianchi+ 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/130">V/130 : Geneva-Copenhagen Survey of Solar neighbourhood III (Holmberg+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/211/9">J/ApJS/211/9 : Variability in UV line emission of F-M stars (Loyd+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/204/24">J/ApJS/204/24 : Kepler planetary candidates. 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