2024MNRAS.527.6389B

New photometry, including TESS data, have been combined with recent spectroscopic observations of the Orion Ib pulsating triple-star system VV Ori. This yields a revised set of absolute parameters with increased precision. Two different programmes were utilized for the light-curve analysis, with results in predictably close agreement. The agreement promotes confidence in the analysis procedures. The spectra were analysed using the FDBINARY programme. The main parameters are as follows: M₁ = 11.56 ± 0.14 and M₂ = 4.81 ± 0.06 (M_⊙). We estimate an approximate mass of the wide companion as M₃ = 2.0 ± 0.3 M_⊙. Similarly, R₁ = 5.11 ± 0.03, R₂ = 2.51 ± 0.02, R₃ = 1.8 ± 0.1 (R_⊙); T_e1 = 26600 ± 300, T_e2 = 16250 ± 420, and T_e3 = 10000 ± 1000 (K). The close binary's orbital separation is a = 13.91 (R_⊙); its age is 8 ± 2 (Myr) and its photometric distance is 396 ± 7 pc. The primary's β Cep type oscillations support these properties and confirm our understanding of its evolutionary status. Examination of the well-defined λ6678 He I profiles reveals the primary to have a significantly low projected rotation: some 80 per cent of the synchronous value. This can be explained on the basis of the precession of an unaligned spin axis. This proposal can resolve also observed variations of the apparent inclination and address other longer term irregularities of the system reported in the literature. This topic invites further observations and follow-up theoretical study of the dynamics of this intriguing young multiple star.