  Stellar winds from fast-rotating Population III (Pop III) stars have long
been suspected to make important contributions to early metal enrichment, as
features in the nucleosynthesis of such `spinstars' are consistent with the
chemical abundance patterns of some metal-poor stars in the local Universe.
Particularly, stellar winds rich in light elements can provide another pathway
towards explaining the carbon enhancement in carbon-enhanced metal-poor (CEMP)
stars. In this work, we focus on the feedback of Pop III stellar winds combined
with supernovae (SNe), and derive the resulting chemical signatures in the
enriched medium. We explore a large parameter space of Pop III star formation
and feedback with a semi-analytical model. The predicted pattern of carbon and
iron abundances of second-generation stars agrees well with observations of
CEMP-no stars ($[\rm Ba/Fe]<0$) at $[\rm Fe/H]\lesssim -3$ and
$A(\mathrm{C})\lesssim 7$, under the optimistic assumption of significant mass
loss by winds. In this scenario, carbon-rich but iron-free second-generation
stars can form in systems dominated by enrichment from winds, gaining trace
amounts of iron by accretion from the interstellar medium, to become the most
iron-poor and carbon-enhanced stars seen in observations ($[\rm Fe/H]\lesssim
-4$, $[\rm C/Fe]\gtrsim 2$). Wind feedback from Pop III spinstars deserves more
detailed modelling in early cosmic structure formation.
