Issue |
A&A
Volume 423, Number 2, August IV 2004
|
|
---|---|---|
Page(s) | 643 - 650 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20047105 | |
Published online | 06 August 2004 |
Magellanic Cloud Cepheids: Pulsational and evolutionary modelling vs. observations
1
Physics Department, University of Florida, Gainesville, FL 32611, USA e-mail: buchler@phys.ufl.edu
2
Konkoly Observatory, Budapest, Hungary e-mail: kollath@konkoly.hu
3
Institut d'Astrophysique de Paris, France e-mail: beaulieu@iap.fr
Received:
20
January
2004
Accepted:
7
May
2004
The pulsational properties of the Cepheid models along the
evolutionary tracks from the Padova group (Girardi et al.), as calculated with
our turbulent convective pulsation code, are in good agreement with the
resonance constraints imposed by the observational OGLE-2 data of the Small and
Large Magellanic Clouds. Our study suggests that the resonance
for the overtone Cepheids occurs for periods clustering around 4.2 d, in
disagreement with the suggestion of Antonello & Poretti based on the
observations of light curves, but in agreement with Kienzle et al. and
Feuchtinger et al. For the fundamental Cepheids the lowest order Fourier
decomposition coefficients from the light curves, viz. R21 and
can be used to locate the resonance region, but not so for the first overtone
Cepheids. Here, the radial velocity curves can be used to locate the overtone
resonance region, or in their absence, one needs to resort to numerical
hydrodynamic modelling.
Key words: stars: oscillations / stars: variables: Cepheids / galaxies: Magellanic Clouds / stars: distances / stars: evolution
© ESO, 2004
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