  We evaluate the optical/near-infrared (OIR) color variability of 3C 279 in
both gamma-ray flaring and non-flaring states over 7-year timescales using the
Small and Medium Aperture Research Telescope System (SMARTS) in Cerro Tololo,
Chile and gamma-ray fluxes obtained from the Fermi Gamma-ray Space Telescope.
This observing strategy differs from previous blazar color variability studies
in two key ways: 1) the reported color variability is assessed across optical
through near-infrared wavelengths, and 2) the color variability is assessed
over timescales significantly longer than an individual flare or ground-based
observing season. We highlight 3C 279 because of its complex color variability,
which is difficult to reconcile with the simple "redder when brighter" behavior
often associated with Flat Spectrum Radio Quasar (FSRQ) color variability. We
suggest that the observed OIR color changes depend on a combination of the jet
and disk emission. We parameterize this behavior in terms of a single variable,
$\zeta^m_n$, representing a smooth transition from disk-dominated, to a mixed
contribution, to a jet-dominated system, which provides an explanation of the
long-term OIR color variability in the same blazar over time. This suggests a
general scheme that could apply to OIR color variability in other blazars.
