  The shape of light cures of fundamental-mode and of first-overtone pulsators,
as observed in RR~Lyrae variables and Cepheids, differ characteristically. The
stellar physical origin of the morphological differences is not well documented
and the topic seems not to be part of the elementary curriculum of students of
stellar variability. To ameliorate the situation, this exposition analyzes
hydrodynamical simulations of radial pulsations computed with the newly
available numerical instrument RSP in MESA. The stellar physical processes that
affect the light curves are identified and contrasted to the explanation based
on experiments with one-zone models. The encounter of first-overtone pulsators
sporting light curves that mimic those of fundamental-mode variables serves as
a warning that light-curve morphology alone is not a reliable path to correctly
classify pulsating variables; the exposition closes with a short discussion of
constraints these modes might impose on understanding the origin of anomalous
Cepheids.
