  In previous attempts to perform seismic modelling of pulsating subdwarf-B
stars, various mode identification techniques are used with uncertain results.
We investigated a method so far neglected in sdB stars, but very successful for
Main Sequence pulsators, that is, mode identification from the line-profile
variations caused by stellar pulsation. We report the calculation of
time-resolved synthetic spectra for sdB stars pulsating with various
combinations of pulsation modes; these calculations were carried out over
appropriate ranges of effective temperature, surface gravity and helium
abundances. Preliminary tests using these synthetic line-profile variations
demonstrated their potential for mode identification by comparison with
observation.
