Stellar Nucleosynthesis

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The Coloumb BarrierFor 12 C and α1 fm = 10 -15 mhttp://nu.phys.laurentian.ca/~fleurot/fusionrate/
Occurrence of fusion reactionsNow will discuss the conditions under which fusion can occur – and whether suchconditions exist in stellar interiors• Nuclei interact through four forces of physics – only electromagnetic and strong nuclearimportant here• Two positively charged nuclei must overcome coulomb barrier (long range force ∝1/r 2 ), toreach separation distances where strong force dominates (10 -15 m, typical size ofnucleus)Schematic plots• V (potential energy) vs nuclei separation distance• Wave function representing penetration of a potentialbarrier by nucleus with kinetic energy of approach E kin(below barrier height).Slide: Stephen Smartt9
Page 1 and 2: Stellar NucleosynthesisThey Might b
Page 3 and 4: Abundances of nuclei3Slide: Stephen
Page 5 and 6: Review: Binding Energy of Nuclei
Page 7: Rate of Reactions
Page 11 and 12: The Gamow peakSchematically this is
Page 13 and 14: ResonancesResonanceC 12 + P => N 13
Page 15 and 16: Relative importance of PPIand PPII
Page 17 and 18: When does a given P-P chain dominat
Page 19 and 20: The CNO CycleAt birth stars contain
Page 21 and 22: Temperature dependence of PP chain
Page 23 and 24: Changes in Elemental Abundances Dur
Page 25 and 26: Helium Burning: the triple-α react
Page 27 and 28: Carbon and oxygen burningCarbon bur
Page 29 and 30: Major nuclear burning processesComm
Page 31 and 32: In the process two types of reactio
Page 33: 1.We described the basic accounting

Stellar Nucleosynthesis

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