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Coulomb barrier
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Classroom Contents
The Origin of Stellar Energy by Professor G Srinivasan
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- 1 Summer course 2018 - A Random walk in astro-physics
- 2 The Origin of Stellar Energy Lecture-08
- 3 What are the stars?
- 4 Stars as globes of perfect gas
- 5 Hydrostatic Equilibrium
- 6 Boyle's Law
- 7 Equation of Hydrostatic Equilibrium
- 8 Stars are globes of gas in which the inward pull of gravity is balanced by the combined effect of the pressure of an ideal gas and the pressure of radiation.
- 9 Eddington's theory of stars
- 10 Radiation Pressure
- 11 Hydrostatic Equilibrium
- 12 Why do the stars shine?
- 13 Why does the Sun shine?
- 14 Virial Theorem applied to the Sun
- 15 How long will the heat last?
- 16 Sir Arthur Eddington
- 17 Mass Deficit
- 18 Proton - proton collision
- 19 Maxwell-Boltzmann Distribution
- 20 Quantum Tunnelling
- 21 Energy production in the Sun
- 22 proton - proton reaction
- 23 Nuclear cycles
- 24 To burn or not to burn? That is the question
- 25 Coulomb barrier
- 26 Fusion reactions
- 27 Onion skin model of a star
- 28 The composition of the core when nuclear reactions finally stop
- 29 Lifetime of stars
- 30 Why doesn't the Sun blow up?
- 31 The Safety Valve
- 32 Q&A
