  Photometric observations of accreting, low-mass, pre-main-sequence stars
(i.e., Classical T Tauri stars; CTTS) have revealed different categories of
variability. Several of these classifications have been linked to changes in
$\dot{M}$. To test how accretion variability conditions lead to different
light-curve morphologies, we used 1D hydrodynamic simulations of accretion
along a magnetic field line coupled with radiative transfer models and a simple
treatment of rotation to generate synthetic light curves. We adopted previously
developed metrics in order to classify observations to facilitate comparisons
between observations and our models. We found that stellar mass, magnetic field
geometry, corotation radius, inclination, and turbulence all play roles in
producing the observed light curves and that no single parameter is entirely
dominant in controlling the observed variability. While the periodic behavior
of the light curve is most strongly affected by the inclination, it is also a
function of the magnetic field geometry and inner disk turbulence. Objects with
either pure dipole fields, strong aligned octupole components, or high
turbulence in the inner disk all tend to display accretion bursts. Objects with
anti-aligned octupole components or aligned, weaker octupole components tend to
show light curves with slightly fewer bursts. We did not find clear monotonic
trends between the stellar mass and empirical classification. This work
establishes the groundwork for more detailed characterization of well-studied
targets as more light curves of CTTS become available through missions such as
the Transiting Exoplanet Survey Satellite (TESS).
