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 .