  It has been observed that Cepheids in the Magellanic Clouds have lower masses
for the same luminosity than those in the Milky Way. The model, from Neilson &
Lester (2008), of pulsation-driven mass loss for Cepheids is applied to
theoretical models of Cepheids with metallicity consistent with the Milky Way
and Large and Small Magellanic Clouds. The mass-loss model is analyzed using
the metallicity correction of the Period-Luminosity relation to compare the
ratio of mass loss of Cepheids with lower metallicity to that of Cepheids with
solar metallicity. It is determined that mass loss may be larger for the lower
metallicity Cepheids, counterintuitive to radiative driving estimates. Also the
mass-loss rates of theoretical Cepheid models are found to be up to $5\times
10^{-9}$ for Galactic Cepheids, $5\times 10^{-8}$ for Large Magellanic Cloud
Cepheids, and $2\times 10^{-7}M_\odot /yr$ for Small Magellanic Cloud Cepheids.
It is argued that mass loss increases as metallicity decreases for Cepheids
with periods less than 20 days and that mass loss decreases for longer periods.
Assuming dust forms in the wind of a Cepheid at some distance, the infrared
excess of the models is computed, finding the infrared brightness is
approximately a magnitude larger due to mass loss. The infrared magnitudes are
compared to recently published Period-Luminosity relations as a test of our
predictions.
