  We report the evidence for the anti-correlation between pulsed fraction (PF)
and luminosity of the X-ray pulsar SXP 1323, found for the first time in a
luminosity range $10^{35}$--$10^{37}$ erg s$^{-1}$ from observations spanning
15 years. The phenomenon of a decrease in X-ray PF when the source flux
increases has been observed in our pipeline analysis of other X-ray pulsars in
the Small Magellanic Cloud (SMC). It is expected that the luminosity under a
certain value decreases as the PF decreases due to the propeller effect. Above
the propeller region, an anti-correlation between the PF and flux might occur
either as a result of an increase in the un-pulsed component of the total
emission or a decrease of the pulsed component. Additional modes of accretion
may also be possible, such as spherical accretion and a change in emission
geometry. At higher mass accretion rates, the accretion disk could also extend
closer to the neutron star (NS) surface, where a reduced inner radius leads to
hotter inner disk emission. These modes of plasma accretion may affect the
change in the beam configuration to fan-beam dominant emission.
