  Interpretation of the oscillation spectrum of the slowly pulsating B-type
star HD21071 is presented. We show that non-rotating models cannot account for
the two highest amplitude frequencies and taking into account the effects of
rotation is necessary. Rotating seismic models are constructed using various
chemical compositions, opacity data, core overshooting parameters and
rotational velocities. There are prospects for seismic modelling of SPB stars,
even if no asymptotic pattern is observed in their oscillation spectra,
provided an unambiguous mode identification is doable and the effects of
rotation are properly included.
