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Energy, Opacity, and Stellar Evolution: Nuclear Reactions in Stars

This lecture covers essential concepts of stellar energy generation, focusing on nuclear reactions like fission and fusion. Key topics include binding energy per nucleon, the temperature dependence of proton-proton (p-p) and CNO chains, and bound-free opacity (κbf(ν)). It also explores the homology of stellar structures and relationships including the Mass-Luminosity relation (L ∝ M^3.9) and the Mass-Radius relation (R ∝ M^0.75). The lecture concludes with insights on stellar age and the main sequence turn-off point, critical for understanding stellar evolution.

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Energy, Opacity, and Stellar Evolution: Nuclear Reactions in Stars

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Presentation Transcript

  1. Ay 123 Lecture 4 - Energy & Opacity Energy from Nuclear Reactions Fission Binding energy per nucleon Fusion Atomic # A

  2. Temperature Dependence of p-p & CNO chains

  3. Bound-free Opacity bf()

  4. Ay 123 Lecture 5 - Homology & Main Sequence Mass-Luminosity Relation L  M3.9

  5. Mass-Radius Relation R  M0.75

  6. Age and Main Sequence Turn-off

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