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The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry

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dc.contributor.authorBazot, M.en_AU
dc.contributor.authorHuber, Den_AU
dc.contributor.authorBedding, Timothy Russellen_AU
dc.contributor.authorBroomhall, A.-M.en_AU
dc.contributor.authorCampante, T. L.en_AU
dc.contributor.authorCarfantan, Hen_AU
dc.contributor.authorChaplin, W Jen_AU
dc.contributor.authorElsworth, Yen_AU
dc.contributor.authorAsplund, Martinen_AU
dc.contributor.authorCastro, M.en_AU
dc.contributor.authorDo Nascimento, J. D.en_AU
dc.contributor.authorIreland, Michaelen_AU
dc.date.accessioned2015-12-13T22:45:11Z
dc.date.issued2011
dc.date.updated2016-02-24T09:39:15Z
dc.description.abstractThe growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation 134.4 ± 0.3 μHz and angular and linear radiuses of 0.6759 ± 0.0062 mas and 1.010 ± 0.009 R⊙ were estimated. We used these values to derive the mass of the star, 1.02 ± 0.03 M⊙.
dc.identifier.issn0004-6361
dc.identifier.urihttp://hdl.handle.net/1885/79635
dc.publisherSpringer
dc.rightsAuthor/s retain copyrighten_AU
dc.sourceAstronomy and Astrophysics
dc.subjectKeywords: Methods:data analysis; stars: individual: 18 Sco; stars: oscillations; Techniques: interferometric; Techniques: radial velocities; Interferometry; Stars; Data handling methods: data analysis; stars: individual: 18 Sco; stars: oscillations; techniques: interferometric; techniques: radial velocities
dc.titleThe radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry
dc.typeJournal article
dcterms.accessRightsOpen Accessen_AU
local.bibliographicCitation.issue1
local.bibliographicCitation.startpageL4
local.contributor.affiliationBazot, M., Centro de Astrofisica da Universidade do Porto
local.contributor.affiliationIreland, Michael, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationHuber, D, University of Sydney
local.contributor.affiliationBedding, Timothy Russell , University of Sydney
local.contributor.affiliationBroomhall, A.-M., University of Birmingham
local.contributor.affiliationCampante, T. L., Universidade do Porto
local.contributor.affiliationCarfantan, H, Universite de Toulouse
local.contributor.affiliationChaplin, W J, University of Birmingham
local.contributor.affiliationElsworth, Y, University of Birmingham
local.contributor.affiliationAsplund, Martin, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationCastro, M., Universidade Federal do Rio Grande do Norte
local.contributor.affiliationDo Nascimento, J. D., Universidade Federal do Rio Grande do Norte
local.contributor.affiliationAsplund, Martin, Max Planck Institute for Astrophysics
local.contributor.authoruidIreland, Michael, u5544212
local.contributor.authoruidAsplund, Martin, u4042723
local.description.notesImported from ARIES
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systems
local.identifier.ariespublicationf5625xPUB8031
local.identifier.citationvolume526
local.identifier.doi10.1051/0004-6361/201015679
local.identifier.scopusID2-s2.0-78650131000
local.type.statusPublished Version

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