  Horizontal branch stars should show significant differential rotation with
depth. Models that assume systematic angular momentum exchange in the
convective envelope and local conservation of angular momentum in the core
produce HB models that preserve a rapidly rotating core. A direct probe of core
rotation is available. The nonradial pulsations of the EC14026 stars frequently
show rich pulsation spectra. Thus their pulsations probe the internal rotation
of these stars, and should show the effects of rapid rotation in their cores.
Using models of sdB stars that include angular momentum evolution, we explore
this possibility and show that some of the sdB pulsators may indeed have
rapidly rotating cores.
