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Summer course 2018 - A Random walk in astro-physics
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Quantum Stars Lecture - 10
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The strange companion of Sirius!
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Are such super-dense stars doomed?
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What will happen to the star when the nuclear reactor at its center fails?
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Sir Ralph Howard Fowler 1889-1944
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Quantum Physics
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Energy levels of a particle in a one-dimensional box
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Heisenberg's Uncertainty Principle
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White Dwarfs are Quantum Stars
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White Dwarfs are for ever!
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Enter Chandra: 1928
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Radiation Pressure
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Hydrostatic Equilibrium
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Gaseous Star & Quantum Star
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Classical Physics: All momentum values are allowed.
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Quantum Physics
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Pauli's exclusion principle allows us to put two fermions in a cell in phase space.
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Fermi Momentum
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Fermi Energy
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Pressure of an ideal classical gas
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Pressure of a Fermi gas at T=0 K
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Chandrasekhar's Theory of White Dwarfs
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Chandrasekhar's Theory of White Dwarfs 1930
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Mass - Radius Relation for White Dwarfs S. Chandrasekhar, 1930
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Stars of all mass will find their ultimate peace as Quantum Stars supported by the pressure of electrons.
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Diamonds in the sky!
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History is made
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Gravitational Collapse of massive white dwarfs
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Relativistic Fermi Gas
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Relativistic White Dwarfs
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A fully relativistic WD has no radius! But it has a unique mass!
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Mass - Radius Relation for White Dwarfs S. Chandrasekhar, 1934
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Chandrasekhar Limit
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Supernovae and Neutron Stars
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Guest Stars
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Supernovae and Cosmic Rays by W. Baade and F. Zwicky
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Supernova Explosion
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Between 1932 and 1937:
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Lev Landau
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Landau invents neutron stars in 1938
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Neutronization of matter at high density
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Dynamical instability
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The maximum mass of neutron stars
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Tolman, Oppenheimer, Volkoff equation
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OV: Oppenheimer - Volkoff Equation of State
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Oppenheimer and Volkoff, 1938
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Limiting Mass for Neutron Stars
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The fate of massive stars
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If radiation pressure exceeds 9.2 percent of the total pressure then matter will never become degenerate no matter what the density is.
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Condition for degeneracy
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Radiation pressure and Degeneracy
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Ideal gas versus relativistic degeneracy
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Why are there only two classes of 'cold stars'?
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Stability of Matter
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HW: Harrison - Wheeler Equation of State OV: Oppenheimer - Volkoff Equation of State
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There are only two types of cold stars in nature!
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Sir Arthur Eddington, at the meeting of the Royal Astronomical Society in London in 1935.
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Chandrasekhar Limit
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Next Lecture: A Journey to the center of a Neutron Star
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Q&A
Description:
Explore the fascinating world of quantum stars in this comprehensive 2-hour lecture by Professor G Srinivasan. Delve into the physics of white dwarfs, neutron stars, and supernovae, examining concepts like quantum mechanics, degeneracy pressure, and relativistic effects. Learn about groundbreaking work by scientists such as Chandrasekhar, Landau, and Oppenheimer. Discover why there are only two types of cold stars in nature and understand the limits of stellar masses. Gain insights into the fate of massive stars and the conditions for stellar degeneracy. Perfect for those interested in astrophysics and the quantum nature of dense stellar objects.

Quantum Stars by Professor G Srinivasan

International Centre for Theoretical Sciences
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#Science #Physics #Quantum Mechanics #Quantum Physics #Astronomy #Astrophysics #Phase Transitions #Neutron Stars #Pulsars #Particle Physics #Neutrino Oscillations
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Summer course 2018 - A Random walk in astro-physics