Massive stars play a key role in many aspects of the evolution of the Universe, 
therefore the understanding of their evolution is of paramount importance in astrophysics.
In this seminar I will present an overview of the evolution of massive stars during all 
their hydrostatic burning stages, i.e., from the pre main sequence phase up to the onset 
of the iron core collapse, their hydrostatic and explosive nucleosynthesis and their final 
fate. The models extend in mass between 13 and 80 Msun, have initial metallicities 
corresponding to [Fe/H]=0,-1,-2,-3 and have initial rotation velocities corresponding to 
v=0, 150 and 300 km/s.