- Ex 5A, p. 151-155, Models of the Atom
- Ex 5B, p. 160-171, Radioactivity
- Ex 5C, p. 175-182, 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
Mass Energy Equivalence
Nuclear Reactions
Fission Fusion and Radioactive Decay
Fission & Fusion
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