Mass - Luminosity relation calculated by Eddington
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Luminosity of a star depends only on its mass!
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Why are the stars as they are?
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To Eddington this 'agreement' was most annoying! "What business have they on a curve reserved for a perfect gas?", he exclaimed.
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"Our mistake was that in estimating the congestion in the stellar ball-room we had forgotten that crinolines are no longer infashion" - Eddington
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Eddington was obscure about two things:
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The Bohr radius
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Lifetime of stars
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Element & Relative Masspercent
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Why does the Sun shine?
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Virial Theorem applied to the Sun
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How long will the heat last?
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Sir Arthur Eddington 24 August, 1920
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Mass Deficit
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Proton - proton collision
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Maxwell-Boltzmann Distribution
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Alpha decay of radioactive nuclei
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Quantum Tunnelling
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Energy production in the Sun
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Why doesn't the Sun blow up?
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The Safety Valve
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Nuclear cycles
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To burn or not to burn? That is the question
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Fusion reactions
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The composition of the core when nuclear reactions finally stop
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Q&A
Description:
Explore the fascinating world of stars in this comprehensive lecture by Professor G Srinivasan, part of a summer course on gravity, astrophysics, and cosmology. Delve into topics such as the structure of stars, hydrostatic equilibrium, Eddington's theory, mass-luminosity relationships, and nuclear fusion processes. Learn about the Sun's interior, energy production mechanisms, and the factors that determine stellar lifetimes. Discover the intricacies of quantum tunneling, nuclear cycles, and fusion reactions that power stars. Gain insights into the historical development of stellar physics, including Eddington's contributions and the resolution of early puzzles in the field. Suitable for advanced undergraduates and graduate students in physics and astronomy, this lecture offers a deep dive into the nature of stars and their place in the universe.