Convective mixing in intermediate mass stars

Stellar evolution can nowadays be modelled with a high degree of accuracy and completeness up to the most advanced stages. However in spite of the progresses, complex physical processes exist that still suffer of large uncertainties even in the most placid evolutionary phases. The straightforward drawback is that models lose their predictive power and this is particularly critical for stellar population synthesis. Here I will focus on one of such processes, convective mixing, and briefly review potentially helpful observational tests to decipher its efficiency during the main nuclear burning phases of intermediate mass stars.