Bárbara M. T. B. Soares
FCUP/IA

Abstract
Nearly all the physical processes that determine the structure and evolution of stars occur in their interiors. However, the extent of chemically mixed regions associated to stellar convective cores is notoriously uncertain. Asteroseismology has revolutionized the study of solar-type stars through the measurement and modelling of their resonant modes of oscillation. The precise characterization of these oscillations in main-sequence stars makes the measurement of the extent of convective cores possible.
We compute ratios of combinations of mode frequencies built with l = 0 and l = 1 modes, which in turn can be used to calculate stellar parameters. We will compare the uncertainties associated with the parameters of the polynomial ?t of the ratios obtained through Monte Carlo simulations and using the covariance matrix, since they will limit the precision with which stellar parameters can be estimated. It was used the Kepler data for stars KIC8379927 and KIC 12069424 (16 Cyg A).

2019 September 27, 13:30

IA/U.Porto
Centro de Astrofísica da Universidade do Porto (Classroom)
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