α Centauri binary system: calibration and oscillations

Details α Centauri binary system: calibration and oscillations α Centauri binary system: calibration and oscillations

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001esasp.464..439p&link_type=abstract

In: Proceedings of the SOHO 10/GONG 2000 Workshop: Helio- and asteroseismology at the dawn of the millennium, 2-6 October 2000,

Mathematics

Logic

2

Stellar Oscillations, Binaries

Scientific paper

The two members of the visual binary α Centauri A & B provide a great potentiality of testing stellar physics in conditions slightly different from the solar ones and then deserve undivided attention for internal structure modeling and oscillation frequencies calculations. Detailed evolutionary models, including pre main-sequence evolution have been performed using the recently determined masses of Pourbaix et al. (1999). Models have been constructed with updated physics including microscopic diffusion, different convection theories and possible convective core overshoot. A χ2 minimization is empolyed to derive the age of the system, the initial helium content, the initial mass ratio of heavy elements to hydrogen and the convection parameters of each star model. A seismological analysis of our calibrated models has been performed.

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