What happens when a high-mass (more than 4 solar masses) Main Sequence

stars runs out of Hydrogen in its core. At first the internal evolution

looks like that of a low-mass star, but now we get first a Red Supergiant

then a sucession of blue and red supergiant phases as different nuclear

fuels are tapped by the star for its energy. This lecture describes

the evolution of high-mass stars from the Main Sequence until their

eventual ends.

Recorded 2006 January 27 in 1008 Evans Laboratory on the Columbus campus

of The Ohio State University.