Abstract
The first orbital solution for the spectroscopic pair in the multiple star system σ Scorpii, determined from measurements with the Sydney University Stellar Interferometer, is presented. The primary component is of β Cephei variable type and has been one of the most intensively studied examples of its class. The orbital solution, when combined with radial velocity results found in the literature, yields a distance of 174 +23 -18 pc, which is consistent with, but more accurate than the Hipparcos value. For the primary component we determine 18.4 ± 5.4 M ⊙ , -4.12 ± 0.34 mag and 12.7 ± 1.8 R ⊙ for the mass, absolute visual magnitude and radius, respectively. A B 1 dwarf spectral type and luminosity class for the secondary is proposed from the mass determination of 11.9 ± 3.1 M ⊙ and the estimated system age of 10Myr.
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