  In recent years, there has been a push to understand how chemical composition
affects the magnetic activity levels of main sequence low-mass stars. Results
indicate that more metal-rich stars are more magnetically active for a given
stellar mass and rotation period. This metallicity dependence has implications
for how the rotation periods and activity levels of low-mass stars evolve over
their lifetimes. Numerical modelling suggests that at late ages more metal-rich
stars should be rotating more slowly and be more magnetically active. In this
work, we study the rotation and activity evolution of low-mass stars using a
sample of Kepler field stars. We use the gyro-kinematic age dating technique to
estimate ages for our sample and use the photometric activity index as our
proxy for magnetic activity. We find clear evidence that, at late ages, more
metal-rich stars have spun down to slower rotation in agreement with the
theoretical modeling. However, further investigation is required to
definitively determine whether the magnetic activity evolution occurs in a
metallicity dependent way.
