  We give a brief overview of where we stand with respect to some old and new
questions bearing on how massive stars evolve and end their lifetime. We focus
on the following key points that are further discussed by other contributions
during this conference: convection, mass losses, rotation, magnetic field and
multiplicity. For purpose of clarity, each of these processes are discussed on
its own but we have to keep in mind that they are all interacting between them
offering a large variety of outputs, some of them still to be discovered.
