  Over much of the initial mass function, stars are destined to become luminous
and cool red giants. They may then be able to produce dust in an atmosphere
which has been elevated by strong radial pulsations, and hence drive a wind.
The amount of mass that is lost in this way can be a very significant fraction
of the stellar mass, and especially in the case of intermediate-mass stars it
is highly enriched. The delay between a star's birth and its feedback into the
environment varies from several million years for massive stars to almost the
age of the Universe for the least massive red giants we see today. I here
present a review on the metallicity dependence of red giant winds. I show that
recent measurements not only confirm theoretical expectations, but also
admonish of common misconceptions with implications for feedback at low initial
metallicity.
