PHOTOMETRIC VARIABILITY OF THE Be STAR HD 328990

Abstract

We present a photometric analysis of a classical Be-type star HD 328990 using archival data from the ASAS-SN survey covering the period from 2016 to 2025. The long-term light curve in the V and g bands reveals low-amplitude variability, with a peak-to-peak magnitude difference of approximately 0.2 mag. A Lomb-Scargle periodogram analysis identifies a significant periodic signal at P_orb ≈ 176.3 days, which is further supported by the phase-folded light curve. Although the folded light curve exhibits substantial scatter, the presence of weak but recurrent photometric modulations suggests the existence of a quasi-periodic phenomenon. Given the star's classification as a classical Be object, we interpret the observed variability as a result of structural changes within the circumstellar disk or dynamical effects induced by a possible binary companion. Our findings are consistent with typical photometric behavior observed in other Be stars and highlight the complex nature of variability mechanisms in rapidly rotating B-type stars with circumstellar material.