2018A&A...609A...5H

V746 Cas is known to be a triple system composed of a close binary with an alternatively reported period of either 25.4d or 27.8d and a distant third component in a 170yr (62000d) orbit. The object was also reported to exhibit multiperiodic light variations with periods from 0..83d to 2.50d, on the basis of which it was classified as a slowly pulsating B star. Interest in further investigation of this system was raised by the recent detection of a variable magnetic field. Analysing spectra from four instruments, earlier published radial velocities, and several sets of photometric observations, we arrived at the following conclusions: (1) The optical spectrum is dominated by the lines of the B-type primary (T_eff1∼16500(100)K), contributing 70% of the light in the optical region, and a slightly cooler B tertiary (T_eff3∼13620(150)K). The lines of the low-mass secondary are below our detection threshold; we estimate that it could be a normal A or F star. (2) We resolved the ambiguity in the value of the inner binary period and arrived at a linear ephemeris of T_super.,conj.=HJD∼2,443,838.78(81)+25.41569(42)dxE. (3) The intensity of the magnetic field undergoes a sinusoidal variation in phase with one of the known photometric periods, namely 2.503867(19)d, which we identify with the rotational period of the tertiary. (4) The second dominant photometric 1.0649524(40)d period is tentatively identified with the rotational period of the broad-lined B-type primary, but this interpretation is much less certain and needs further verification. (5) If our interpretation of photometric periods is confirmed, the classification of the object as a slowly pulsating B star should be revised. (6) Applying an N-body model to different types of available observational data, we can constrain the orbital inclination of the inner orbit to ∼60°<i₁< 85° even in the absence of binary eclipses, and we estimate the probable properties of the triple system and its components.