  The variability of young stellar objects is mostly driven by star-disk
interactions. In long-term photometric monitoring of the accreting T Tauri star
GI Tau, we detect extinction events with typical depths of $\Delta V \sim 2.5$
mag that last for days-to-months and often appear to occur stochastically. In
2014 - 2015, extinctions that repeated with a quasi-period of 21 days over
several months is the first empirical evidence of slow warps predicted from MHD
simulations to form at a few stellar radii away from the central star. The
reddening is consistent with $R_V=3.85\pm0.5$ and, along with an absence of
diffuse interstellar bands, indicates that some dust processing has occurred in
the disk. The 2015 -- 2016 multi-band lightcurve includes variations in spot
coverage, extinction, and accretion, each of which results in different traces
in color-magnitude diagrams. This lightcurve is initially dominated by a
month-long extinction event and return to the unocculted brightness. The
subsequent light-curve then features spot modulation with a 7.03 day period,
punctuated by brief, randomly-spaced extinction events. The accretion rate
measured from $U$-band photometry ranges from $1.3\times10^{-8}$ to
$1.1\times10^{-10}$ M$_\odot$ yr$^{-1}$ (excluding the highest and lowest 5% of
high- and low- accretion rate outliers), with an average of $4.7 \times
10^{-9}$ M$_\odot$ yr$^{-1}$. A total of 50% of the mass is accreted during
bursts of $>12.8\times10^{-9}$ M$_\odot$ yr${^{-1}}$, which indicates
limitations on analyses of disk evolution using single-epoch accretion rates.
