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V746 Cas is known to be a triple system composed of a close binary with analternatively reported period of either 25.4d or 27.8d and a third component ina 62000d orbit. The object was also reported to exhibit multiperiodic lightvariations with periods from 0.83d to 2.50d, on the basis of which it wasclassified as a slowly pulsating B star. Interest in further investigation ofthis system was raised by the detection of a variable magnetic field. Analysingspectra from four instruments, earlier published radial velocities, and severalsets of photometric observations, we arrived at the following conclusions: (1)The optical spectrum is dominated by the lines of the B-type primary(Teff1~16500(100) K), contributing 70% of the light in the optical region, anda slightly cooler B tertiary (Teff3~13620(150) K). The lines of the low-masssecondary are below our detection threshold; we estimate that it could be anormal A or F star. (2) We resolved the ambiguity in the value of the innerbinary period and arrived at a linear ephemeris of T_super.conj.=HJD2443838.78(81)+25.41569(42)xE. (3) The intensity of the magnetic fieldundergoes a~sinusoidal variation in phase with one of the known photometricperiods, namely 2.503867(19)d, which we identify with the rotational period ofthe tertiary. (4) The second photometric 1.0649524(40)d period is identifiedwith the rotational period of the B-type primary, but this interpretation ismuch less certain and needs further verification. (5) If our interpretation ofphotometric periods is confirmed, the classification of the object as a slowlypulsating B star should be revised. (6) Applying an N-body model to differenttypes of available observational data, we constrain the orbital inclination ofthe inner orbit to ~60 deg to 85 deg even in the absence of eclipses, andestimate the probable properties of the triple system and its components.

Improved model of the triple system V746 Cas that has a bipolar magnetic field associated with the tertiary