  Spectroscopic observations have shown for decades that the Wolf-Rayet (WR)
phenomenon is ubiquitous among stars with different initial masses. Although
much effort to understand the winds from massive WR stars has been presented in
the literature, not much has been done for such type of stars in the low-mass
range. Here we present an attempt to understand the winds from [WR]-type stars
using results from spectral analyses with the full non-LTE stellar atmosphere
code PoWR. These results are put into context with the properties of massive WR
stars. We found that WC+[WC] stars and WO+[WO] stars create independent
sequences in the mass-loss rate ($\dot{M}$) and modified wind momentum
($D_\mathrm{mom}$) versus luminosity ($L$) diagrams. Our analysis indicates
that even when the winds of WR and [WR] stars become optically thin, there is
no breakdown of the general mass-loss trend, contrary to the observed ``weak
wind phenomenon'' in OB stars. We report that all WR-type stars studied here
broadly define single sequences in the wind efficiency ($\eta$) versus
transformed mass-loss rate ($\dot{M}_\mathrm{t}$), the
$\dot{M}_\mathrm{t}$-$T_\mathrm{eff}$ diagram, and the $(L, T_\mathrm{eff},
\dot{M})$ space, which suggest these to be fundamental properties of the WR
phenomenon (regardless of the mass range), at least for WR-type stars of the O
and C sequences. Our analytical estimations could drive computations of future
stellar evolution models for WR-type stars.
