The seismic study of the base of the convection zone in the Sun
(eg Christensen-Dalsgaard et.al. 1995, MNRAS 276, 283) has been successful
in determining not only the position of the base of the convective
envelope, but also the characteristics of this transition layer.
In this work we extend the analysis to other solar-type stars,
possessing also convective envelopes, in order to investigate
methods for determining characteristics of the envelopes of
these stars.
In particular, we may hope to establish seismologically that a
star does indeed possess a convective envelope and to measure
the size of this convective region.
The method used consists in identifying a signal in the observed
frequencies whose characteristics depend on the location of the
base of the convective region in the star.
The limitations in terms of observational uncertainties and
stellar characteristics are discussed.