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

M. Bazot*, M. J. Ireland, D. Huber, T. R. Bedding, A. M. Broomhall, T. L. Campante, H. Carfantan, W. J. Chaplin, Y. Elsworth, J. Meléndez, P. Petit, S. Théado, V. Van Grootel, T. Arentoft, M. Asplund, M. Castro, J. Christensen-Dalsgaard, J. D. Do Nascimento, B. Dintrans, X. Dumusque & 11 others H. Kjeldsen, H. A. McAlister, T. S. Metcalfe, M. J P F G Monteiro, N. C. Santos, S. Sousa, J. Sturmann, L. Sturmann, T. A. Ten Brummelaar, N. Turner, S. Vauclair

*Corresponding author for this work

Research output: Contribution to journalArticle

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Abstract

The 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⊙.

Original languageEnglish
Article numberL4
Pages (from-to)1-4
Number of pages4
JournalAstronomy and Astrophysics
Volume526
Issue number1
DOIs
Publication statusPublished - 13 Dec 2010
Externally publishedYes

Bibliographical note

Copyright 2010 ESO. First published in Astronomy and Astrophysics, Vol. 526, No. 1, published by EDP Sciences. The original publication is available at http://dx.doi.org/10.1051/0004-6361/201015679

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