  Strongly magnetic, rapidly rotating B-type stars with relatively weak winds
form centrifugal magnetospheres (CMs), as the stellar wind becomes magnetically
confined above the Kepler co-rotation radius. Approximating the magnetic field
as a dipole tilted by an angle $\beta$ with respect to the rotation axis, the
CM plasma is concentrated in clouds at and above the Kepler radius along the
intersection of the rotational and magnetic equatorial planes. Stellar rotation
can bring such clouds in front of the stellar disk, leading to absorption of
order 0.1 magnitude ($\sim 10 \%$ of continuum flux). However some stars with
prominent CMs, such as $\sigma$ Ori E, show an emission bump in addition to
absorption dips, which has been so far unexplained. We show that emission can
occur from electron scattering toward the observer when CM clouds are projected
off the stellar limb. Using the Rigidly Rotating Magnetosphere model, modified
with a centrifugal breakout density scaling, we present a model grid of
photometric light curves spanning parameter space in observer inclination angle
$i$, magnetic obliquity angle $\beta$, critical rotation fraction $W$, and
optical depth at the Kepler radius $\tau_{\text{K}}$. We show that
$\tau_{\text{K}}$ of order unity can produce emission bumps of the magnitude
$\sim 0.05$ seen in $\sigma$ Ori E. We discuss the implications for modeling
the light curves of CM stars, as well as future work for applying the radiative
transfer model developed here to 3D MHD simulations of CMs.
