  We acquired H$\alpha$ spectroscopic observations from 2005 to 2019 showing
Pleione has transitioned from a Be phase to a Be-shell phase during this
period. Using the radiative transfer code \hdust\ we created a grid of
$\sim100,000$ disk models for Pleione. We successfully reproduced the observed
transition with a disk model that varies in inclination while maintaining an
equatorial density of $\rho_0(r) = 3\times 10^{-11}
(r/R_{eq})^{-2.7}~\rm{g~cm^{-3}}$, and an H$\alpha$ emitting region extending
to $15~\rm{R_{eq}}$. We use a precessing disk model to extrapolate the changing
disk inclination over $120$ years and follow the variability in archival
observations. The best-fit disk model precesses over a line of sight
inclination between $\sim25\rm{^{\circ}}$ and $\sim144\rm{^{\circ}}$ with a
precessional period of $\sim80.5$ years. Our precessing models match some of
the observed variability but fail to reproduce all of the historical data
available. Therefore, we propose an ad-hoc model based on our precessing disk
model inspired by recent SPH simulations of similar systems, where the disk
tears due to the tidal influence of a companion star. In this model, a single
disk is slowly tilted to an angle of $30^{\circ}$ from the stellar equator over
$34$ years. Then, the disk is torn by the companion's tidal torque, with the
outer region separating from the innermost disk. The small inner disk returns
to the stellar equator as mass injection remains constant. The outer disk
precesses for $\sim15$ years before gradually dissipating. The process repeats
every $34$ years and reproduces all trends in Pleione's variability.
