Poster abstract details

Mixing processes such as convection and overshooting have paramount importance in the evolutionary properties of stars. The treatment of convectively unstable zones affects the outcoming luminosity, temperature, and main-sequence lifetime of stars. Since the presence of a convective region creates a discontinuity in the chemical profile of a star, by locating the position where this discontinuity is we can learn about the mixing process taking place in the stellar interior. A sharp feature in the density profile translates into a rapid variation of the adiabatic sound speed, which produces an oscillatory signal in the p-mode spectra whose period is related to the position of the discontinuity. Thus, we study the possibility if discriminating between different mixing processes in the core such as convection, semiconvection and overshooting by determining the size of the convective core using different low-degree p-modes frequency combination. We study the applicability of these tools in the light of the data being obtained by the Kepler mission.