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Lecture 17- Nuclear Reactions in Stellar Interiors

Lecture 17- Nuclear Reactions in Stellar Interiors. H + H. 2 H + e + + nu. H + 2 H. 3 He + gamma. 3 He + 3 He. 4 He + H + H. Net effect: 4H 4 He. Question: why does this occur exclusively in the core of a star?. A small mass difference between Hydrogen and Helium.

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Lecture 17- Nuclear Reactions in Stellar Interiors

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  1. Lecture 17- Nuclear Reactions in Stellar Interiors H + H 2H + e+ + nu H + 2H 3He + gamma 3He + 3He 4He + H + H Net effect: 4H 4He Question: why does this occur exclusively in the core of a star?

  2. A small mass difference between Hydrogen and Helium • 4 Hydrogen atoms: 6.693E-27 kg • 1 Helium atom: 6.645E-27 kg • Difference = 0.048E-27 kg • Difference = 0.7 percent Why is this small difference important?

  3. The Einstein Energy-Mass equivalence relation E=mc2 c=speed of light You get a lot of bang for the buck: 6.3E+14 J/kg

  4. The Power Source of Main Sequence Stars MS stars fuse hydrogen into helium, releasing prodigious amounts of energy in the process. Their fuel source is the matter of which they are made

  5. The Structure of Main Sequence Stars The Powerhouse

  6. How can we tell if this is right? Detect neutrinos emitted from the center of the Sun.

  7. The Neutrino Sun: A View into the Solar Interior

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