Issue |
A&A
Volume 430, Number 2, February I 2005
|
|
---|---|---|
Page(s) | 571 - 583 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20041405 | |
Published online | 20 January 2005 |
Seismic constraints on open clusters
1
Institut d'Astronomie et d'Astrophysique, ULB, CP226, 1050 Brussels, Belgium e-mail: piau@astro.ulb.ac.be
2
CEA/DSM/DAPNIA/Service d'Astrophysique, CE Saclay, 91191 Gif-sur-Yvette Cedex 01, France e-mail: [jballot;cturck]@cea.fr
Received:
3
June
2004
Accepted:
27
August
2004
The aim of this theoretical and modelling
paper is to derive knowledge on the global and structural parameters
of low-mass stars
using asteroseismology and taking advantage
of the stellar collective behavior within open clusters.
We build stellar models and compute the seismic signal expected
from main sequence objects in the range. We first
evaluate apparent magnitudes and oscillations-induced luminosity
fluctuations expected in the Hyades, the Pleiades and the α Persei clusters.
The closest cluster presents a feasible challenge to
observational asteroseismology in the present and near future. The
remainder of the work therefore focuses on the Hyades.
We combine seismological and classical computations to address three questions:
what can be inferred about 1) mass; 2) composition; and 3) extension
of outer convection zones of solar analogs in the Hyades.
The first issue relies on the strong sensitivity of the
large separation to mass. We show that seismic constraints
provide masses to a precision level (
) that is competitive
with the actual mass estimations from binary systems.
Then large separations (
) and second differences
(
) are used to
respectively constrain metal and helium fractions in the
Hyades.
When plotted for several masses, the relation of
effective temperature (
)
vs. large separation (
) is found to be
strongly dependent on the metal content. Besides
this the second difference main
modulation is related to the second ionization of helium.
An accuracy in the helium mass fraction of 0.02 to 0.01
can be achieved provided mass and age
are accurately known, which is the case for a few Hyades binary
systems. The second difference
modulations are also partly due to the
discontinuity in stellar stratification
at the convective envelope/radiative core transition. They
permit direct insight in the stellar structure. We compute
acoustic radii of the convective bases
for different values of the mixing length theory
parameter
in convection modelling, i.e. different
convective efficiency in the
superadiabatic layers. For a given effective
temperature we show that the acoustic radius changes with convection
efficiency. This suggests that seismology can
provide constraints on the extension of outer convection and
also more generally on the direct
approaches of convection and dynamical phenomena
being currently developed.
Key words: Galaxy: open clusters and associations: general / stars: oscillations / stars: late-type / stars: abundances / stars: interiors
© ESO, 2005
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