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We present the results of our analysis on V1481 Ori (JW 239), a young SB2 inthe Orion Nebula Cluster with a circumbinary disc accreting on the lower-masscomponent. The analysis is based on high-resolution spectroscopic data andhigh-quality photometric time series about 20-yr long. Thanks to thespectroscopy, we confirm the binary nature of this system consisting of M3 + M4components and derive the mass ratio M_B/M_A = 0.54, a variable luminosityratio L_B/L_A = 0.68--0.94, and an orbital period P_orb = 4.433d. Thephotometric data allowed us to measure the rotation periods of the twocomponents P_phot = 4.4351d and they are found to be synchronized with theorbital period. The simultaneous modeling of V-, I-band, and radial velocitycurves in the 2005 season suggests that the variability is dominated by one hotspot on the secondary component covering at least about 3.5% of the stellarsurface and about 420K hotter than the unperturbed photosphere. Such a spot mayoriginate from the material of the circumbinary disc accreting onto thesecondary component. We also detect an apparent 6-yr periodic variation in theposition of this hot spot, which is inferred from the phase migration of thelight curve maximum, which we interpret as due to either the presence ofsurface differential rotation as large as 0.065%, a value compatible with thefully convective components, or to a periodic exchange of angular momentumbetween the disc and the star, which implies a minimum magnetic field strengthof 650G at the stellar surface.

Physical parameters and long-term photometric variability of V1481 Ori, a SB2 member of Orion Nebula Cluster with an accreting component