Nuclear Astrophysics

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Solar abundances, density = 100 g cm -3 : Full Reaction Rates Rate p + p reaction 14 N + p 12 C + a 10
Reaction Rate: Temperature Dependence p + p reaction 14 N + p 12 C + a 11
Page 1 and 2: Nuclear Astrophysics Lecture 9 &10
Page 3 and 4: We have (again) Set the argument of
Page 5 and 6: Let’s pull out the physics of thi
Page 7 and 8: Finally, recall 7
Page 9: Examples: The core of our Sun has a
Page 13 and 14: Using the equations on previous sli
Page 15 and 16: Finally, then, we have that the mas
Page 17 and 18: The power series expansion of , for
Page 19 and 20: Structure of Polytrope Sun Let us d
Page 21 and 22: Derivative of Luminosity 21
Page 23 and 24: Arbitrary Units Standard Solar Mode
Page 25 and 26: Proton-Proton-Chain p + p d + e +
Page 27 and 28: The nuclear energy production in Ma
Page 29 and 30: PP-Chain Nuclear Energy Rate vs Cor
Page 31 and 32: The power per unit mass produced in
Page 33 and 34: From page 15, Lecture 6, the Main S
Page 35 and 36: Main Sequence: Core Temperature vs
Page 37 and 38: Luminosity vs Effective Temperature
Page 39 and 40: We have a first “hint” here of
Page 41 and 42: Main Sequence: Luminosity vs Effect
Page 43 and 44: Hertzprung-Russel Diagram CNO Cycle
Page 45 and 46: Integrated Luminosity Let us take 9
Page 47 and 48: Mass Interior to Radius Mass contai
Page 49: Nuclear Generation Rate Using the p

Nuclear Astrophysics

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