Ângela R. G. Santos
CAUP

Abstract
The solar magnetic cycle leads to periodic changes in the overall magnetic field, as well in the number of emerging sunspots. These magnetic-related variations can lead to changes on the internal structure of the star, on which the wave propagation depends. Therefore, cyclic variations on the oscillation properties related with magnetic activity are also expected, as found for the Sun and, later, for a solar-pulsator observed by CoRoT. With this recent discovery, the understanding of the different contributions to the activity-related variations on the oscillation properties becomes even more important. With this in mind, we built an empirical model to simulate the properties of the sun/stellar spots over a cycle. The simulations can then be used to estimate the frequency shifts induced by spots. We started by using a simple toy model and gradually increase its complexity in order to improve the agreement between the simulations and the observational data. To apply the model to other solar-like pulsators from which less information is available, we will apply a simplified version of the model.

2014 July 01, 13:30

IA/U.Porto
Centro de Astrofísica da Universidade do Porto (Classroom)
Rua das Estrelas, 4150-762 Porto