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Comparative seismology of pre- and main sequence stars in the instability strip
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Astronomy Astrophysics manuscript no.
(will be inserted by hand later)
Comparative seismology of pre- and main sequence stars in the
instability strip
Marian Suran1, MarieJo Goupil2, Annie Baglin3,
Yveline Lebreton2, Claude Catala4
1 Astronomical Institute of Romanian Academy,
2 DASGAL, UMR CNRS 8633, Observatoire de Paris-Meudon,
3 DESPA, UMR CNRS 8632, Observatoire de Paris-Meudon,
4LAT, UMR CNRS 5572, Observatoire de Midi-Pyre?ne?es
Abstract. Pulsational properties of 1.8 M⊙ stellar models covering the latest stages of contraction toward the
main sequence up to early hydrogen burning phases are investigated by means of linear nonadiabatic analyses.
Results confirm that pre-main sequence stars (pms) which cross the classical instability strip on their way toward
the main sequence are pulsationally unstable with respect to the classical opacity mechanisms. For both pms and
main sequence types of models in the lower part of the instability strip, the unstable frequency range is found
to be roughly the same. Some non-radial unstable modes are very sensitive to the deep internal structure of the
star. It is shown that discrimination between pms and main sequence stages is possible using differences in their
oscillation frequency distributions in the low frequency range.
Key words. stars: oscillations, stars: pre-main sequence
1. Introduction
In the vicinity of the main sequence, the HR diagram is
confusing as stars of similar global properties but different
stages of evolution lie at the same position. In some cases
the young pre-main sequence stars are recognized through
specific characteristics, for instance the presence of nebu-
losity or high degree of activity. But, this is not always the
case. An alternative is to take advantage of seismological
pieces of information whenever it is possible. We therefore
carry out a comparative study of the pulsational behavior
of pre-main sequence (hereafte
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