8752 may have a companion. Measurements of the ultraviolet spectral distribution show an excess that corresponds to the output of a B1 main-sequence star. The absolute magnitude was estimated at -4.5, approximately 40 times fainter than the primary at visual wavelengths. Although the stars must be fairly close (< 1400AU), no radial velocity variations have been detected in the spectral lines of the primary, and no lines are observed which can be attributed directly to the secondary. The observed spectrum may be mostly from a shell surrounding both stars. It has been suggested that some variations in spectral line profiles are caused by variations in colliding winds or disturbances of previously ejected material, caused during a periastron passage of the companion. References External links James Kaler's page on HR 8752 Juergen Kummer's page on V509 Cassiopeiae Cassiopeia (constellation) G-type hypergiants A-type hypergiants K-type hypergiants Semiregular variable stars Cassiopeiae, V509 217476 8752 ? 113561 Durchmusterung objects