Star_stuf_5 - Multiple shell burning Advanced nuclear...

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Star stuff Core of a high mass star is hot enough to fuse C (and heavier elements ) Begins at ~600 million K…but lasts only a few hundred yrs. High-mass stars make the elements necessary for life CNO cycle can change C into N and O Helium capture High core temperature allows helium to fuse with heavier elements. Evidence for helium capture Higher abundances of elements with even number’s of protons. High mass stars make heavier elements (like C, Ne, O. .) Advanced nuclear burning Core temperature in stars with >8 Msun allow fusion of elements as heavy as iron Makes elements like Si, S, Ca, F
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Unformatted text preview: Multiple shell burning Advanced nuclear burning proceeds in a series of nested shells Depletion of fuels continues to cause core to shrink and heat up. Fusion ends at iron because reactions with it do not release energy. (Fe has lowest mass per nuclear particles) High mass star ends in a supernova explosion Evolution of a high mass star Beginning is similar to low mass stars, but quicker. End is very different. Core is hot enough to fuse C and other heavy elements. Confirmed by observations of very old stars, which have less heavy elements....
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Star_stuf_5 - Multiple shell burning Advanced nuclear...

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