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Pulsational properties of 1.8 M$_{\odot}$ stellar models covering the lateststages of contraction toward the main sequence up to early hydrogen burningphases are investigated by means of linear nonadiabatic analyses. Resultsconfirm that pre-main sequence stars (pms) which cross the classicalinstability strip on their way toward the main sequence are pulsationallyunstable with respect to the classical opacity mechanisms. For both pms andmain sequence types of models in the lower part of the instability strip, theunstable frequency range is found to be roughly the same. Some non-radialunstable modes are very sensitive to the deep internal structure of the star.It is shown that discrimination between pms and main sequence stages ispossible using differences in their oscillation frequency distributions in thelow frequency range.Comment: 8 pages, 9 figures, accepted for publication in A&

Comparative seismology of pre- and main sequence stars in the instability strip