  We measure the rotation periods of 19 stars in the {\it Kepler} transiting
planetary systems, $P_{\rm rot, astero}$ from asteroseismology and $P_{\rm rot,
phot}$ from photometric variation of their lightcurve. Two stars exhibit two
clear peaks in the Lomb-Scargle periodogram, neither of which agrees with the
seismic rotation period. Other four systems do not show any clear peak, whose
stellar rotation period is impossible to estimate reliably from the photometric
variation; their stellar equators may be significantly inclined with respect to
the planetary orbital plane. For the remaining 13 systems, $P_{\rm rot,
astero}$ and $P_{\rm rot, phot}$ agree within 30\%. Interestingly, three out of
the 13 systems are in the spin-orbit resonant state in which $P_{\rm orb,
b}/P_{\rm rot, astero} \approx 1$ with $P_{\rm orb, b}$ being the orbital
period of the inner-most planet of each system. The corresponding chance
probability is ($0.2$-$4.7$) \% based on the photometric rotation period data
for 464 {\it Kepler} transiting planetary systems. While further analysis of
stars with reliable rotation periods is required to examine the statistical
significance, the spin-orbit resonance between the star and planets, if
confirmed, have important implications for the star-planet tidal interaction,
in addition to the origin of the spin-orbit (mis-)alignment of transiting
planetary systems.
