Abstract
The massive OB-type binary σ Ori AB is in the centre of the very young σ Orionis cluster. I have computed the most probable distances and masses of the binary for several ages using a dynamical parallax-like method. It incorporates the BVRIH-band apparent magnitudes of both components, precise orbital parameters, interstellar extinction and a widely used grid of stellar models from the literature, Kepler's third law and a χ 2 minimization. The derived distance is 334 +25 −22 pc for an age of 3 ± 2 Ma; larger ages and distances are unlikely. The masses of the primary and the secondary lie on the approximate intervals 16–20 and 10–12 M ⊙ , respectively. I also discuss the possibility of σ Ori AB being a triple system at ∼ 385 pc. These results will help to constrain the properties of young stars and substellar objects in the σ Orionis cluster.
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