Seismic study of stellar convective regions: the base of the convective envelope in low-mass stars

The possibility of observing solar-type oscillations on other stars is of g reat relevance to investigating the uncertain aspects of the internal struc ture of stars. One of these aspects is the convective overshoot that takes place at the borders of the envelopes of stars of mass similar to, or lower than, the Sun. It affects the temperature stratification, mixing, rotation and magnetic-field generation. Asteroseismology can provide an observation al test for the studies of the structure of such overshoot regions. The seismic study of the transition in the Sun, located at the base of the convection zone, has been successful in determining the characteristics of this layer in the Sun. In this work we consider the extension of the analys is to other solar-type stars (of mass between 0.85 and 1.2 M.) in order to establish a method for determining the characteristics of their convective envelopes. In particular, we hope to be able to establish seismologically t hat a star does indeed possess a convective envelope, to measure the size o f the convective region and also to constrain the properties of an overshoo t layer at the bottom of the envelope. The limitations in terms of observat ional uncertainties and stellar characteristics, and the detectability of a n overshoot layer, are discussed.