  We present the analysis of KIC 7760680, the rotating Slowly Pulsating B-type
star identified in the Kepler photometry. The oscillation spectrum of the star
exhibits a series of 36 frequencies which are quasi-equally spaced in period.
We confirm that this series can be associated with prograde dipole modes of
consecutive radial orders. In our studies, the effects of rotation were
included in the MESA equilibrium models as well as in the puslational
calculations in the framework of the traditional approximation. We find that
pulsational models computed with the OPLIB opacities best reproduce the
observed frequency range. The modified opacity data with an enhancement of the
opacity at $\log T=5.3$, 5.46 and 5.06 were tested as well. Increasing the
OPLIB opacities by about 50% at $\log T=5.3$ is sufficient to excite modes in
the whole range of 36 frequency peaks of KIC 7760680.
