  We present a dust spectral energy distribution (SED) and binary stellar
population analysis revisiting the dust production rates (DPRs) in the winds of
carbon-rich Wolf-Rayet (WC) binaries and their impact on galactic dust budgets.
DustEM SED models of 19 Galactic WC ``dustars" reveal DPRs of
$\dot{M}_d\sim10^{-10}-10^{-6}$ M$_\odot$ yr$^{-1}$ and carbon dust
condensation fractions, $\chi_C$, between $0.002 - 40\%$. A large ($0.1 - 1.0$
$\mu$m) dust grain size composition is favored for efficient dustars where
$\chi_C\gtrsim1\%$. Results for dustars with known orbital periods verify a
power-law relation between $\chi_C$, orbital period, WC mass-loss rate, and
wind velocity consistent with predictions from theoretical models of dust
formation in colliding-wind binaries. We incorporated dust production into
Binary Population and Spectral Synthesis (BPASS) models to analyze dust
production rates from WC dustars, asymptotic giant branch stars (AGBs), red
supergiants (RSGs), and core-collapse supernovae (SNe). BPASS models assuming
constant star formation (SF) and a co-eval $10^6$ M$_\odot$ stellar population
were performed at low, Large Magellanic Cloud (LMC)-like, and solar
metallicities (Z = 0.001, 0.008, and 0.020). Both constant SF and co-eval
models show that SNe are net dust destroyers at all metallicities. Constant SF
models at LMC-like metallicities show that AGB stars slightly outproduce WC
binaries and RSGs by factors of $2-3$, whereas at solar metallicites WC
binaries are the dominant source of dust for $\sim60$ Myr until the onset of
AGBs, which match the dust input of WC binaries. Co-eval population models show
that for "bursty" SF, AGB stars dominate dust production at late times
($t\gtrsim 70$ Myr).
