The End of Massive Stars

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.

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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.

Location

TBC London EC1N 2HH

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