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Neutron Stars and Black Holes - Lecture 1: Diffuse Stars
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- 1 Time: AM
- 2 Neutron Stars and Black Holes Lecture - 01
- 3 Momentous discoveries during last three years
- 4 What are neutron stars? How are they formed?
- 5 Topics
- 6 What are the stars? Why are they as they are?
- 7 Gaseous Stars
- 8 Stars as globes of perfect gas
- 9 Gravitational Pressure
- 10 Gravitational Pressure = P Gravity approximate GM2/R4
- 11 Hydrostatic Equilibrium
- 12 Boyle's Law
- 13 Equation of Hydrostatic Equilibrium
- 14 What are the stars?
- 15 Eddington's theory of stars
- 16 Radiation Pressure
- 17 How hot is the Sun?
- 18 Virial Theorem
- 19 Virial Theorem applied to the Sun
- 20 The interior of the Sun
- 21 Mean-free-path is approximate 0.5 cm. Radius approximate 1 million km.
- 22 In the Sun, photons take ~ 30,000 years to escape! In massive stars, it will take a million years or more!
- 23 Mass - Luminosity relation
- 24 Mass - Luminosity relation calculated by Eddington L proportional M3
- 25 Why are the stars as they are?
- 26 "Our mistake was that in estimating the congestion in the stellar ball-room we had forgotten that crinolines are no longer in fashion" - Eddington
- 27 Why are the masses of stars in an incredibly narrow range between 0.5-30 M sun?
- 28 Eddington was obscure about two things:
- 29 Why are the atoms as they are?
- 30 Atoms are as they are because they obey the rules of atomic physics.
- 31 Lifetime of stars
- 32 Why does the Sun shine?
- 33 How long will the heat last?
- 34 Sir Arthur Eddington
- 35 Mass Deficit
- 36 Proton - proton collision
- 37 Maxwell-Boltzmann Distribution
- 38 Alpha decay of radioactive nuclei
- 39 Quantum Tunnelling
- 40 Energy production in the Sun
- 41 Proton - proton reaction
- 42 Why doesn't the Sun blow up?
- 43 Nuclear cycles
- 44 To burn or not to burn? That is the question
- 45 Fusion reactions
- 46 The composition of the core when nuclear reactions finally stop
- 47 Q&A
