Results. The resulting masses for components Aa of 14.0 +/- 2.2 M-circle dot and Ab of 7.4 +/- 1.1 M-circle dot are low compared to theoretical expectations, with a distance of 294 +/- 21 pc which is smaller than a photometric distance estimate of 387 +/- 54 pc based on the spectral type B0III of the B component. If the latter (because it is also consistent with the distance to the Orion OB1 association) is adopted, the mass of the secondary component Ab of 14 +/- 3 M-circle dot would agree with classifying a star of type B0.5IV. It is fainter than the primary by about 2.2 +/- 0.1 magnitudes in the visual. The primary mass is then determined to be 33 +/- 10 M-circle dot. The possible reasons for the distance discrepancy are most likely related to physical effects, such as small systematic errors in the radial velocities due to stellar winds.