Published in
EDP Sciences, Astronomy & Astrophysics, (526), p. L4, 2010
DOI: 10.1051/0004-6361/201015679
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The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry
,
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
and other authors.
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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 $134.4±0.3$ $μ$Hz 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$_{⊙}$. ; Comment: 5 pages, 5 figures