Issue |
A&A
Volume 372, Number 1, June II 2001
|
|
---|---|---|
Page(s) | 233 - 240 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20010485 | |
Published online | 15 June 2001 |
Comparative seismology of pre- and main sequence stars in the instability strip
1
Astronomical Institute of Romanian Academy
2
DASGAL, UMR CNRS 8633, Observatoire de Paris-Meudon, France
3
DESPA, UMR CNRS 8632, Observatoire de Paris-Meudon, France
4
LAT, UMR CNRS 5572, Observatoire de Midi-Pyrénées, France
Corresponding author: M. Goupil, goupil@obspm.fr
Received:
22
January
2001
Accepted:
30
March
2001
Pulsational properties of
1.8 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
© ESO, 2001
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