  We applied the ATON code to the computation of detailed grids of standard
(non--rotating) and rotating Pre--Main Sequence (PMS) models and computed their
adiabatic oscillation spectra,with the aim of exploring the seismic properties
of young stars. We adopt a method similar to the matching mode method by
Guenther and Brown making use, when necessary, also of our rotating
evolutionary code to compute the models for PMS stars. The method is described
by a preliminary application to the frequency spectrum of two PMS stars (85 and
278) in the young open cluster NGC 6530. For the Star 85 we confirm, with
self--consistent rotating models, previous interpretation of the data,
attributing three close frequencies to the mode n=4, l=1 and m=0,+1,--1. For
the Star 278 we find a different fit for the frequencies, corresponding to a
model within the original error box of the star, and dispute the possibility
thatthis star has an effective temperature much cooler that the red boundary of
the radial instability strip.
