γ Cas analogs constitute a small group of Be stars characterized by unusual X-ray spectra and high X-ray luminosities, LX ∼ 1031 –1033 erg s−1. This is 2–3 orders of magnitude higher than for typical Be stars, yet lower than that observed in massive X-ray binaries with Be components. Compared to classical Be stars, these objects exhibit unusually hard X-ray spectra. In the present paper, we present results from the analysis of the spectral and photometric variability of binary γ Cas analogs in both optical and X-ray bands. Notably, the periods of regular optical and X-ray variability appear to be similar. This suggests that at least part of the X-ray emission arises from interactions between local magnetic fields of the Be stars and the magnetic fields of their decretion disks. X-ray flares are expected to result from the reconnection of magnetic field lines. For the stars BZ Cru and π Aqr, several thousand flare events were identified in the X-ray light curves obtained with the XMM-Newton satellite. Moreover, regular variations in X-ray brightness with periods of 50–90 seconds have been detected for the γ Cas analogs HD 45314, HD 45995, NGC 6649 9, and V558 Lyr. These periods may correspond to the rotation periods of white dwarfs in binary Be+WD systems. We propose that the hard component of X-ray emission from γ Cas stars is generated via the accretion of disk material onto a rapidly rotating white dwarf. © 2025, Azerbaijan National Academy of Sciences. All rights reserved.