Homework:
- Act 15A, p. 173-176, Particles and Half-Life
- Act 16A, p. 181, Nuclear Reactions
Nuclear Reactions:
- Conservation of Atomic Number
- Conservation of Nucleon Number
- Conservation of Mass-Energy E = Δmc2
E = Δmc2
Nuclear Fusion in the Sun
Binding Energy comes from the change in mass from individual nucleons to being combined into a nucleus. This is energy lost by the nucleons joined together in a nucleus and must be returned in order to separate the nucleons
E = Δmc2
Element formation in Stars Nuclear Fusion
Binding Energy Per Nucleon
Mass Per Nucleon
Nuclear Reactions
Fission Fusion and Radioactive Decay
Fission & Fusion
Natural Nuclear Fission Reactor
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