  Classical Cepheids are powerful probes of both stellar evolution and
near-field cosmology thanks to their high luminosities, pulsations, and that
they follow the Leavitt (Period-Luminosity) Law. However, there still exist a
number of questions regarding their evolution, such as the role of rotation,
convective core overshooting and winds. ln particular, how do these processes
impact Cepheid evolution and the predicted fundamental properties such as
stellar mass. In this work, we compare a sample of period change that are
real-time observations of stellar evolution with new evolution models to test
the impact of these first two processes. In our previous study we found that
enhanced mass loss is crucial for describing the sample, and here we continue
that analysis but for rotational mixing and core overshooting. We show that,
while rotation is important for stellar evolution studies, rotation, itself, is
insufficient to model the distribution of period change rates from the observed
sample. On the other hand, convective core overshooting is needed to explain
the magnitude of the rates of period change, but does not explain the number of
stars with positive and negative period change rates. In conclusion, we
determine that convective core overshooting and stellar rotation alone are not
enough to account for the observed distribution of Cepheid rates of period
change and another mechanism, such as pulsation-driven mass-loss, may be
required.
