The nonradial oscillations of stars in various regions of the HR diagram provide an alternate window into the processes of stellar evolution. In many cases, the nonradial pulsators play a crucial role in filling out the evolutionary picture. Two examples serve to illustrate this new probe: the rapidly oscillating Ap (ROAp) stars, and the pulsating white dwarfs. Because of the complex light curves that result from multiperiodic pulsations in these stars, global observing campaigns are required to fully decode their pulsation spectra. Such efforts can bear substantial scientific rewards. The observed frequency spacings in some of the ROAp stars allow identification of their evolutionary stage and, possibly, measurement of their rates of evolutionary expansion. For white dwarfs, seismological analysis using the observed g-mode pulsations allows us to determine the compositional structure of their outer layers, measure their masses, and determine their rotation and cooling rates.