We present our analysis of HD 35502 based on high- and medium-resolution spectropolarimetric observations. Our results indicate that the magnetic B5IVsnp star is the primary component of a spectroscopic triple system and that it has an effective temperature of 18.4 ± 0.6 kK, a mass of 5.7 ± 0.6 M⊙, and a polar radius of |3.0+1.1-0.5\, R|. The two secondary components are found to be essentially identical A-type stars for which we derive effective temperatures (8.9 ± 0.3 kK), masses (2.1 ± 0.2 M⊙), and radii (2.1 ± 0.4 R⊙). We infer a hierarchical orbital configuration for the system in which the secondary components form a tight binary with an orbital period of 5.668 66(6) d that orbits the primary component with a period of over 40 yr. Least-Squares Deconvolution profiles reveal Zeeman signatures in Stokes V indicative of a longitudinal magnetic field produced by the B star ranging from approximately −4 to 0 kG with a median uncertainty of 0.4 kG. These measurements, along with the line variability produced by strong emission in Hα, are used to derive a rotational period of 0.853 807(3) d. We find that the measured v sin i = 75 ± 5 km s−1 of the B star then implies an inclination angle of the star's rotation axis to the line of sight of |24⁺⁶₋₁₀^∘|. Assuming the Oblique Rotator Model, we derive the magnetic field strength of the B star's dipolar component (|14⁺⁹₋₃\, kG|) and its obliquity (|63± 13|). Furthermore, we demonstrate that the calculated Alfvén radius (|41⁺¹⁷₋₆R_|) and Kepler radius (|2.1+0.4-0.7R_|) place HD 35502's central B star well within the regime of centrifugal magnetosphere-hosting stars.
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