Completed
White Dwarfs are for ever!
Class Central Classrooms beta
YouTube videos curated by Class Central.
Classroom Contents
Quantum Stars by Professor G Srinivasan
Automatically move to the next video in the Classroom when playback concludes
- 1 Summer course 2018 - A Random walk in astro-physics
- 2 Quantum Stars Lecture - 10
- 3 The strange companion of Sirius!
- 4 Are such super-dense stars doomed?
- 5 What will happen to the star when the nuclear reactor at its center fails?
- 6 Sir Ralph Howard Fowler 1889-1944
- 7 Quantum Physics
- 8 Energy levels of a particle in a one-dimensional box
- 9 Heisenberg's Uncertainty Principle
- 10 White Dwarfs are Quantum Stars
- 11 White Dwarfs are for ever!
- 12 Enter Chandra: 1928
- 13 Radiation Pressure
- 14 Hydrostatic Equilibrium
- 15 Gaseous Star & Quantum Star
- 16 Classical Physics: All momentum values are allowed.
- 17 Quantum Physics
- 18 Pauli's exclusion principle allows us to put two fermions in a cell in phase space.
- 19 Fermi Momentum
- 20 Fermi Energy
- 21 Pressure of an ideal classical gas
- 22 Pressure of a Fermi gas at T=0 K
- 23 Chandrasekhar's Theory of White Dwarfs
- 24 Chandrasekhar's Theory of White Dwarfs 1930
- 25 Mass - Radius Relation for White Dwarfs S. Chandrasekhar, 1930
- 26 Stars of all mass will find their ultimate peace as Quantum Stars supported by the pressure of electrons.
- 27 Diamonds in the sky!
- 28 History is made
- 29 Gravitational Collapse of massive white dwarfs
- 30 Relativistic Fermi Gas
- 31 Relativistic White Dwarfs
- 32 A fully relativistic WD has no radius! But it has a unique mass!
- 33 Mass - Radius Relation for White Dwarfs S. Chandrasekhar, 1934
- 34 Chandrasekhar Limit
- 35 Supernovae and Neutron Stars
- 36 Guest Stars
- 37 Supernovae and Cosmic Rays by W. Baade and F. Zwicky
- 38 Supernova Explosion
- 39 Between 1932 and 1937:
- 40 Lev Landau
- 41 Landau invents neutron stars in 1938
- 42 Neutronization of matter at high density
- 43 Dynamical instability
- 44 The maximum mass of neutron stars
- 45 Tolman, Oppenheimer, Volkoff equation
- 46 OV: Oppenheimer - Volkoff Equation of State
- 47 Oppenheimer and Volkoff, 1938
- 48 Limiting Mass for Neutron Stars
- 49 The fate of massive stars
- 50 If radiation pressure exceeds 9.2 percent of the total pressure then matter will never become degenerate no matter what the density is.
- 51 Condition for degeneracy
- 52 Radiation pressure and Degeneracy
- 53 Ideal gas versus relativistic degeneracy
- 54 Why are there only two classes of 'cold stars'?
- 55 Stability of Matter
- 56 HW: Harrison - Wheeler Equation of State OV: Oppenheimer - Volkoff Equation of State
- 57 There are only two types of cold stars in nature!
- 58 Sir Arthur Eddington, at the meeting of the Royal Astronomical Society in London in 1935.
- 59 Chandrasekhar Limit
- 60 Next Lecture: A Journey to the center of a Neutron Star
- 61 Q&A
