  Seismic modeling of the Slowly Pulsating B-type star HD182255 yields strong
constraints on the radial orders of the two dominant modes. For these
frequencies, we derive also the empirical values of the complex nonadiabatic
parameter $f$. These two seismic tools, i.e., pulsational frequencies and the
associated values of $f$, allow to test available opacity data, chemical
composition and overshooting efficiency.
