Lecture 17: The Evolution of High-Mass Stars
Update: 2006-01-27
Description
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.
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.
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