What can we learn from global acoustic modes about the structure
of the Sun and  Centauri A ? J. Ballot, S. Turck-Chièze and P.A.P. Nghiem
Service d'Astrophysique, CEA/DSM/DAPNIA, CE Saclay,
91191 Gif-sur-Yvette CEDEX, France
In asteroseismology, only global acoustic modes are available to constrain
the internal structure of stars.
In this poster, we examine the existing seismic observations of the Sun and
of Centauri A to show how the duration of the observations
influence the obtained results.
Since the structure of the Sun is well known, we can take it as a very
interesting first case to see the determination accuracy of the
convective zone depth or of the photospheric helium abundance,
using only the low degree modes (l=0,1,2).
Then we present different modellings of Cen A and illustrate how
the different seismic indicators vary with age
and mass. We derive for this star the minimal observation duration to determine
the convective zone depth and which accuracy we reach,
simulating different frequency ranges and observation lengths.
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Last changed: 2002/Jun/19
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