  We employ a Monte Carlo radiation transfer code to investigate the multi-
wavelength photopolarimetric variability arising from a spotted T Tauri star
surrounded by a dusty circumstellar disk. Our aim is to assess the ability of
the magnetic accretion model to explain the observed photopolarimetric
variability of classical T Tauri stars, and to identify potentially useful
observational diagnostics of T Tauri star/disk/spot parameters. We model a
range of spot sizes, spot latitudes, inner disk truncation radii, and system
inclination angles, as well as multiple disk and spot geometries. We find that
the amplitude, morphology, and wavelength dependence of the photopolarimetric
variability predicted by our models are generally consistent with existing
observations; a flared disk geometry is required to reproduce the largest
observed polarization levels and variations. Our models can further explain
stochastic polarimetric variability if unsteady accretion is invoked, in which
case irregular -- but correlated -- photometric variability is predicted, in
agreement with observations.
  Potentially useful observational diagnostics of system parameters of interest
are discussed. We also investigate the reliability of modeling spot parameters
via analytic fits to multi-band photometric variations.
