Lecture_4_Elements2 - 1 Fusion in stars Small stars fuse H...

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2 Fusion in stars • Small stars fuse H to form He • The fusion reactions in stars produce energy • In centers of large stars, temperatures are higher and He can fuse to form 12 C and successively heavier elements up to 56 Fe • To form nuclides past 56 Fe energy is required • While many nuclides can form by a variety of pathways, 4 He is particularly stable so nuclides made up of whole numbers of 4 He are particularly abundant.
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3 Big Bang Fusion in l a rge stars
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4 Neutron capture (s-process) 56 Fe (26 p + and 30 n 0 ) stable nuclide 56 Fe + n -> 57 Fe (26 p + and 31 n 0 ) stable nuclide 57 Fe + n -> 58 Fe (26 p + and 32 n 0 ) stable nuclide 58 Fe + n -> 59 Fe (26 p + and 33 n 0 ) radionuclide 59 Fe -> 59 Co + e - (27 p + and 32 n 0 ) stable nuclide Beta decay n 0 -> e - + p + 59 Co 59 Fe 27 26 32 33 protons neutrons
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6 S-process • S-process can build elements heavier than iron • Neutrons are byproduct of nuclear reactions in stars • Neutrons are absorbed easily into nucleus
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This note was uploaded on 02/08/2011 for the course EAS 1601 taught by Professor Lynch during the Spring '08 term at Georgia Institute of Technology.

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Lecture_4_Elements2 - 1 Fusion in stars Small stars fuse H...

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