The evolution of our Sun from ordinary star into red giant is radically different from the evolution of much more massive stars towards their end-points: supernova explosions followed by black holes.
This lecture will contrast the relevant nuclear physics and thermodynamics that determine these very different outcomes.
Speakers
The evolution of our Sun from ordinary star into red giant is radically different from the evolution of much more massive stars towards their end-points: supernova explosions followed by black holes.
This lecture will contrast the relevant nuclear physics and thermodynamics that determine these very different outcomes.