  Over half of all observed hot subdwarf B (sdB) stars are found in binaries,
and over half of these are found in close configurations with orbital periods
of 10$ \,\rm{d}$ or less. In order to estimate the companion masses in these
predominantly single-lined systems, tidal locking has frequently been assumed
for sdB binaries with periods less than half a day. Observed non-synchronicity
of a number of close sdB binaries challenges that assumption and hence provides
an ideal testbed for tidal theory. We solve the second-order differential
equations for detailed 1D stellar models of sdB stars to obtain the tidal
dissipation strength and hence to estimate the tidal synchronization time-scale
owing to Zahn's dynamical tide. The results indicate synchronization
time-scales longer than the sdB lifetime in all observed cases. Further, we
examine the roles of convective overshooting and convective dissipation in the
core of sdB stars and find no theoretical framework in which tidally-induced
synchronization should occur.
