How do stars generate energy in their cores, and once made, how is

that energy transported to the surface where it can be radiated away

as Luminosity? This lecture revisits nuclear fusion and the Kelvin-Helmholz

Mechanism, and discusses the 3 ways energy can be transported in stars:

Radiation, Convection, and Conduction. This will lead us to the

concept of Thermal Equilibrium in stars, which is the last main piece

of stellar physics we need before we can address the question of how

stars are formed and evolve in the rest of this Unit.

Recorded 2006 January 23 in 1008 Evans Laboratory on the Columbus campus

of The Ohio State University.