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Energy production in the Sun
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Classroom Contents
What Are the Stars? - by G Srinivasan
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- 1 Time: AM
- 2 A Journey through the Universe
- 3 What are the stars? Lecture-03
- 4 Stars as globes of perfect gas
- 5 Gravitational Force
- 6 Hydrostatic Equilibrium
- 7 Boyle's Law
- 8 Equation of Hydrostatic Equilibrium
- 9 What are the stars?
- 10 Eddington's theory of stars
- 11 Radiation Pressure
- 12 Hydrostatic Equilibrium
- 13 The interior of the Sun
- 14 Mass - Luminosity relation
- 15 Mass - Luminosity relation calculated by Eddington
- 16 Luminosity of a star depends only on its mass!
- 17 Why are the stars as they are?
- 18 To Eddington this 'agreement' was most annoying! "What business have they on a curve reserved for a perfect gas?", he exclaimed.
- 19 "Our mistake was that in estimating the congestion in the stellar ball-room we had forgotten that crinolines are no longer infashion" - Eddington
- 20 Eddington was obscure about two things:
- 21 The Bohr radius
- 22 Lifetime of stars
- 23 Element & Relative Masspercent
- 24 Why does the Sun shine?
- 25 Virial Theorem applied to the Sun
- 26 How long will the heat last?
- 27 Sir Arthur Eddington 24 August, 1920
- 28 Mass Deficit
- 29 Proton - proton collision
- 30 Maxwell-Boltzmann Distribution
- 31 Alpha decay of radioactive nuclei
- 32 Quantum Tunnelling
- 33 Energy production in the Sun
- 34 Why doesn't the Sun blow up?
- 35 The Safety Valve
- 36 Nuclear cycles
- 37 To burn or not to burn? That is the question
- 38 Fusion reactions
- 39 The composition of the core when nuclear reactions finally stop
- 40 Q&A
