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<ri:Resource created="2013-08-12T13:46:20Z" 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>Spectroscopic Binarity of O and B type stars</title><shortName>J/MNRAS/424/1925</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/424/1925</identifier><altIdentifier>doi:10.26093/cds/vizier.74241925</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Chini R.</name></creator><creator><name>Hoffmeister V.H.</name></creator><creator><name>Nasseri A.</name></creator><creator><name>Stahl O.</name></creator><creator><name>Zinnecker H.</name></creator><date role="Updated">2024-07-18T20:18:46Z</date><date role="Created">2013-08-12T13:46:20Z</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>spectroscopic-binary-stars</subject><subject>o-stars</subject><subject>morgan-keenan-classification</subject><description>The formation of stars above about 20M_{sun}_ and their apparently high multiplicity remain heavily debated subjects in astrophysics. We have performed a vast high-resolution radial velocity spectroscopic survey of about 250 O- and 540 B-type stars in the southern Milky Way which indicates that the majority of stars (&gt;82%) with masses above 16M_{sun}_ form close binary systems while this fraction rapidly drops to 20% for stars of 3M_{sun}_. The binary fractions of O-type stars among different environment classes are: clusters (72+/-13%), associations (73+/-8%), field (43+/-13%) and runaways (69+/-11%). The high frequency of close pairs with components of similar mass argues in favour of a multiplicity originating from the formation process rather than from a tidal capture in a dense cluster. The high binary frequency of runaway O stars that we found in our survey (69% compared to 19-26% in previous surveys) points to the importance of ejection from young star clusters and thus supports the competitive accretion scenario.</description><source format="bibcode">2012MNRAS.424.1925C</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/424/1925</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/I/239">I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/116">V/116 : Galactic O star 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