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<ri:Resource created="2020-11-30T09:15:43Z" 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>68 Gaia DR2 ultra-short-period planet host stars</title><shortName>J/AJ/160/138</shortName><identifier>ivo://CDS.VizieR/J/AJ/160/138</identifier><altIdentifier>doi:10.26093/cds/vizier.51600138</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Hamer J.H.</name></creator><creator><name>Schlaufman K.C.</name></creator><date role="Updated">2021-09-22T07:34:42Z</date><date role="Created">2020-11-30T09:15:43Z</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>exoplanets</subject><subject>variable-stars</subject><subject>radial-velocity</subject><subject>visible-astronomy</subject><description>It has been unambiguously shown both in individual systems and at the population level that hot Jupiters experience tidal inspiral before the end of their host stars main-sequence lifetimes. Ultra-short-period (USP) planets have orbital periods P&lt;1 day, rocky compositions, and are expected to experience tidal decay on similar timescales to hot Jupiters if the efficiency of tidal dissipation inside their host stars parameterized as Q_*_' is independent of P and/or secondary mass M_p_. Any difference between the two classes of systems would reveal that a model with constant Q_*_' is insufficient. If USP planets experience tidal inspiral, then USP planet systems will be relatively young compared to similar stars without USP planets. Because it is a proxy for relative age, we calculate the Galactic velocity dispersions of USP planet candidate host and non-host stars using data from Gaia Data Release 2 supplemented with ground-based radial velocities. We find that main-sequence USP planet candidate host stars have kinematics consistent with similar stars in the Kepler field without observed USP planets. This indicates that USP planet hosts have similar ages to field stars and that USP planets do not experience tidal inspiral during the main-sequence lifetimes of their host stars. The survival of USP planets requires that Q_*_'&gt;~10^7^ at P~0.7day and M_p_~2.6M{Earth}. This result demands that Q_*_' depend on the orbital period and/or mass of the secondary in the range 0.5day&lt;~P&lt;~5days and 1M{Earth}&lt;~M_p_&lt;~1000M{sun}.</description><source format="bibcode">2020AJ....160..138H</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/160/138</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/V/164">V/164 : LAMOST DR5 catalogs (Luo+, 2019)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/345">I/345 : Gaia DR2 (Gaia Collaboration, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/141/11">J/AJ/141/11 : Spitzer observations planet-host stars (Dodson-Robinson+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/142/176">J/AJ/142/176 : Exoplanet host stars. II. Speckle interferometry (Mason+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/566/A103">J/A+A/566/A103 : Kepler planet host candidates imaging (Lillo-Box+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/787/47">J/ApJ/787/47 : 106 Kepler ultra-short-period planets (Sanchis-Ojeda+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/788/L9">J/ApJ/788/L9 : Stellar parameters of KIC planet-host stars (Bastien+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/791/35">J/ApJ/791/35 : Detection of 715 Kepler planet candidates host stars (Law+,2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/576/A94">J/A+A/576/A94 : Northern bright planet host stars parameters (Sousa+, 2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/153/136">J/AJ/153/136 : Planets &amp; their host stars with Gaia parallaxes (Stassun+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/154/94">J/AJ/154/94 : APOGEE-2 data from DR16 (Majewski+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/154/107">J/AJ/154/107 : California-Kepler Survey (CKS). I. 1305 stars (Petigura+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/154/228">J/AJ/154/228 : Properties of transiting planet's host stars (Sandford+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/155/89">J/AJ/155/89 : California-Kepler Survey (CKS). IV. 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