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

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 mu Hz and angular and linear radiuses of 0.6759 +/- 0.0062 mas and 1.010 +/- 0.009 R(circle dot) were estimated. We used these values to derive the mass of the star, 1.02 +/- 0.03 M(circle dot).

FCT/MCTES[SFRH/BPD/47994/2008]

FCT/MCTES[PTDC/CTE-AST/098754/2008]

FCT/MCTES[PTDC/CTE-AST/66181/2006]

FEDER, Portugal

Australian Research Council[DP0878674]

AMRFP[09/10-O-02]

Commonwealth of Australia

National Science Foundation (NSF) [AST09-08253]

W. M. Keck Foundation

NASA Exoplanet Science Center