  We present high spatial resolution mid-infrared images of the nebula around
the late-type carbon-rich Wolf-Rayet (WC)-OB binary system WR~112 taken by the
recently upgraded VLT spectrometer and imager for the mid-infrared (VISIR) with
the PAH1, NeII\_2, and Q3 filters. The observations reveal a morphology
resembling a series of arc-like filaments and broken shells. Dust temperatures
and masses are derived for each of the identified filamentary structures, which
exhibit temperatures ranging from $179_{-6}^{+8}$ K at the exterior W2 filament
to $355_{-25}^{+37}$ K in the central 3". The total dust mass summed over the
features is $2.6\pm0.4\times10^{-5}$ $\mathrm{M}_\odot$. A multi-epoch analysis
of mid-IR photometry of WR~112 over the past $\sim20$ yr reveals no significant
variability in the observed dust temperature and mass. The morphology of the
mid-IR dust emission from WR~112 also exhibits no significant expansion from
imaging data taken in 2001, 2007, and 2016, which disputes the current
interpretation of the nebula as a high expansion velocity ($\sim1200$ km
s$^{-1}$) "pinwheel"-shaped outflow driven by the central WC-OB colliding-wind
binary. An upper limit of $\lesssim120$ km s$^{-1}$ is derived for the
expansion velocity assuming a distance of $4.15$ kpc. The upper limit on the
average total mass-loss rate from the central 3" of WR~112 is estimated to be
$\lesssim8\times10^{-6}$ $\mathrm{M}_\odot$ yr$^{-1}$. We leave its true nature
as an open question, but propose that the WR~112 nebula may have formed in the
outflow during a previous red or yellow supergiant phase of the central
Wolf-Rayet star.
