  We briefly review the main problems related to the computation of the
evolution of intermediate-mass stars: the treatment of turbulent convection and
the occurrence of blue loops during the core He-burning phase. It is shown
that, in order to obtain more accurate and reliable stellar models for this
class of stars, one has to consider all possible theoretical and observational
constraints. This includes observations of low-mass stars to constrain the
treatment of envelope convection, and the analysis of the pulsational behaviour
of Cepheid stars.
