We present models of the inner region of the circumstellar disk of RY Tau which aim to explain our near-infrared ($K$-band: $2.1,mu$m) interferometric observations while remaining consistent with the optical to near-infrared portions of the spectral energy distribution. Our sub-milliarcsecond resolution CHARA Array observations are supplemented with shorter baseline, archival data from PTI, KI and VLTI/GRAVITY and modeled using an axisymmetric Monte Carlo radiative transfer code. The $K$-band visibilities are well-fit by models incorporating a central star illuminating a disk with an inner edge shaped by dust sublimation at $0.210pm0.005,$au, assuming a viewing geometry adopted from millimeter interferometry ($65^{circ}$ inclined with a disk major axis position angle of $23^{circ}$). This sublimation radius is consistent with that expected of Silicate grains with a maximum size of $0.36-0.40,mu$m contributing to the opacity and is an order of magnitude further from the star than the theoretical magnetospheric truncation radius. The visibilities on the longest baselines probed by CHARA indicate that we lack a clear line-of-sight to the stellar photosphere. Instead, our analysis shows that the central star is occulted by the disk surface layers close to the sublimation rim. While we do not see direct evidence of temporal variability in our multi-epoch CHARA observations, we suggest the aperiodic photometric variability of RY~Tau is likely related temporal and/or azimuthal variations in the structure of the disk surface layers.
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