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<ri:Resource created="2018-06-19T08:30:33Z" 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>C/O vs Mg/Si ratios in solar type stars</title><shortName>J/A+A/614/A84</shortName><identifier>ivo://CDS.VizieR/J/A+A/614/A84</identifier><altIdentifier>doi:10.26093/cds/vizier.36140084</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Suarez-Andres L.</name></creator><creator><name>Israelian G.</name></creator><creator><name>Gonzalez Hernandez J.I.</name></creator><creator><name>Adibekyan V.Zh.,Delgado Mena E.</name></creator><creator><name>Santos N.C.</name></creator><creator><name>Sousa S.G.</name></creator><date role="Updated">2018-09-18T15:03:38Z</date><date role="Created">2018-06-19T08:30:33Z</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>g-stars</subject><subject>chemical-abundances</subject><description>We aim to present a detailed study of the magnesium-to-silicon and carbon-to-oxygen ratios (Mg/Si and C/O) and their importance in determining the mineralogy of planetary companions. Using 499 solar-like stars from the HARPS sample, we determined C/O and Mg/Si elemental abundance ratios to study the nature of the possible planets formed. We separated the planetary population in low-mass planets (&lt;30M_{sun}_) and high-mass planets (&gt;30M_{sun}_) to test for a possible relation with the mass. We find a diversity of mineralogical ratios that reveal the different kinds of planetary systems that can be formed, most of them dissimilar to our solar system. The different values of the Mg/Si and C/O can determine different composition of planets formed. {We found that 100% of our planetary sample present C/O&lt;0.8. 86% of stars with high-mass companions present 0.8&gt;C/O&gt;0.4, while 14% present C/O values lower than 0.4. Regarding Mg/Si, all stars with low-mass planetary companion showed values between one and two, while 85% of the high-mass companion sample does. The other 15% showed Mg/Si values below one. No stars with planets were found with Mg/Si&gt;2. Planet hosts with low-mass companions present C/O and Mg/Si similar to those found in the Sun, whereas stars with high-mass companions have lower C/O.</description><source format="bibcode">2018A&amp;A...614A..84S</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/614/A84</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/J/AJ/105/2299">J/AJ/105/2299 : Li abundance of solar-type stars. II. (Soderblom+, 1993)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/327/587">J/A+A/327/587 : Abundances of 9 solar-type stars (Tomkin+ 1997)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AZh/81/541">J/AZh/81/541 : Abundances of 15 solar analogues (Galeev+, 2004)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/636/1098">J/ApJ/636/1098 : Debris disks around solar-type stars (Bryden+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/468/663">J/A+A/468/663 : Li abundances in solar-analog stars (Takeda+, 2007)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/508/L17">J/A+A/508/L17 : Abundances in solar analogs (Ramirez+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/515/A93">J/A+A/515/A93 : Li abundances in solar-analog stars. II. (Takeda+, 2010)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/720/1592">J/ApJ/720/1592 : Abundances of solar analogs with planets (Hernandez+, 2010)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/601/A67">J/A+A/601/A67 : Kepler solar-type stars modeling (Creevey+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/839/94">J/ApJ/839/94 : Abundances of solar twins from Keck/HIRES (Bedell+, 2017)</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/A+A/614/A84</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/614/A84</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South 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