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 \pm 0.6 { kK } , a mass of 5.7 \pm 0.6 M _ { \odot } , and a polar radius of 3.0 ^ { +1.1 } _ { -0.5 } R _ { \odot } .
The two secondary components are found to be essentially identical A-type stars for which we derive effective temperatures ( 8.9 \pm 0.3 { kK } ) , masses ( 2.1 \pm 0.2 M _ { \odot } ) , and radii ( 2.1 \pm 0.4 R _ { \odot } ) .
We infer a hierarchical orbital configuration for the system in which the secondary components form a tight binary with an orbital period of 5.66866 ( 6 ) { d } that orbits the primary component with a period of over 40 { yrs } .
Least-Squares Deconvolution ( LSD ) 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 H \alpha , are used to derive a rotational period of 0.853807 ( 3 ) { d } .
We find that the measured v \sin { i } = 75 \pm 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 } \degree .
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 \pm 13 \degree ) .
Furthermore , we demonstrate that the calculated Alfvén radius ( 41 ^ { +17 } _ { -6 } R _ { \ast } ) and Kepler radius ( 2.1 ^ { +0.4 } _ { -0.7 } R _ { \ast } ) place HD 35502 ’ s central B star well within the regime of centrifugal magnetosphere-hosting stars .