  We present a reanalysis of five transit and eight eclipse observations of the
ultra-short period super-Earth 55 Cancri e observed using the Spitzer Space
Telescope during 2011-2013. We use pixel-level decorrelation to derive accurate
transit and eclipse depths from the Spitzer data, and we perform an extensive
error analysis. We focus on determining possible variability in the eclipse
data, as was reported in Demory et al. 2016a. From the transit data, we
determine updated orbital parameters, yielding T0 = 2455733.0037 $\pm$ 0.0002,
P = 0.7365454 $\pm$ 0.0000003 days, i = 83.5 $\pm$ 1.3 degrees, and $R_p$ =
1.89 $\pm$ 0.05 $R_\oplus$. Our transit results are consistent with a constant
depth, and we conclude that they are not variable. We find a significant amount
of variability between the eight eclipse observations, and confirm agreement
with Demory et al. 2016a through a correlation analysis. We convert the eclipse
measurements to brightness temperatures, and generate and discuss several
heuristic models that explain the evolution of the planet's eclipse depth
versus time. The eclipses are best modeled by a year-to-year variability model,
but variability on shorter timescales cannot be ruled out. The derived range of
brightness temperatures can be achieved by a dark planet with inefficient heat
redistribution intermittently covered over a large fraction of the sub-stellar
hemisphere by reflective grains, possibly indicating volcanic activity or cloud
variability. This time-variable system should be observable with future space
missions, both planned (JWST) and proposed (i.e. ARIEL).
