Quantum Stars (Lecture - 10) by Professor G Srinivasan

Summer course 2018 - A Random walk in astro-physics
Lecture - 10 : Quantum Stars (Lecture - 10) by G Srinivasan
10.00 to 12.00 Friday, 15 June 2018
Madhava Lecture Hall, ICTS Bangalore
The range of densities, temperatures, magnetic fields, etc. that obtain in the Universe are staggering: from 10-27 g cm-3 to 1015 g cm-3, from 3K to 1010 K, from 10-6 G to 1015 G. Not surprisingly, the variety of physical phenomena one encounters during the study of celestial objects is truly impressive. This set of lectures is intended to illustrate the richness of Astrophysics. It will be a random walk in basic physics, with numerous illustrations from astronomy. The topics in physics that will be reviewed have been chosen on the basis of their importance in contemporary astronomy.
Topics:
Absorption and emission of radiation
Radiation from relativistic electrons
Compton scattering of radiation
Spontaneous and stimulated emission
Hyperfine splitting of energy levels
Molecular spectra
Astrophysical plasma.
Quantum tunnelling.
Nuclear matter
Neutrino Oscillation
Phase transitions and the early Universe
During this random walk in physics, one will encounter a range of astronomical objects and phenomena, such as, Solar wind, gaseous nebulae, interstellar hydrogen clouds, giant molecular clouds, neutron stars and pulsars, supernova remnants, radio galaxies and quasars, active galactic nuclei, the cosmic microwave background, etc.
www.icts.res.in/summercourse2018
Table of Contents (powered by videoken.com)
0:00:00 Summer course 2018 - A Random walk in astro-physics
0:00:10 Quantum Stars (Lecture - 10)
0:01:11 The strange companion of Sirius!
0:05:01 Are such super-dense stars doomed?
0:05:29 What will happen to the star when the nuclear reactor at its center fails?
0:06:40 Sir Ralph Howard Fowler 1889-1944
0:10:36 Quantum Physics
0:11:54 Energy levels of a particle in a one-dimensional box
0:13:15 Heisenberg's Uncertainty Principle
0:18:35 White Dwarfs are Quantum Stars
0:19:26 White Dwarfs are for ever!
0:22:02 Enter Chandra: 1928
0:24:49 Radiation Pressure
0:24:58 Hydrostatic Equilibrium
0:25:26 Gaseous Star & Quantum Star
0:26:03 Classical Physics: All momentum values are allowed.
0:28:06 Quantum Physics
0:29:55 Pauli's exclusion principle allows us to put two fermions in a cell in phase space.
0:30:17 Fermi Momentum
0:32:59 Fermi Energy
0:34:20 Pressure of an ideal classical gas
0:35:26 Pressure of a Fermi gas at T=0 K
0:37:26 Chandrasekhar's Theory of White Dwarfs
0:37:57 Chandrasekhar's Theory of White Dwarfs (1930)
0:38:28 Mass - Radius Relation for White Dwarfs S. Chandrasekhar, 1930
0:39:52 Stars of all mass will find their ultimate peace as Quantum Stars supported by the pressure of electrons.
0:41:04 Diamonds in the sky!
0:44:22 History is made
0:44:52 Gravitational Collapse of massive white dwarfs
0:47:30 Relativistic Fermi Gas
0:52:19 Relativistic White Dwarfs
0:52:49 A fully relativistic WD has no radius! But it has a unique mass!
0:57:46 Mass - Radius Relation for White Dwarfs S. Chandrasekhar, 1934
0:58:34 Chandrasekhar Limit
1:00:11 Supernovae and Neutron Stars
1:00:43 Guest Stars
1:04:06 Supernovae and Cosmic Rays by W. Baade and F. Zwicky
1:07:38 Supernova Explosion
1:09:03 Between 1932 and 1937:
1:09:20 Lev Landau
1:09:29 Landau invents neutron stars in 1938
1:13:49 Neutronization of matter at high density
1:16:34 Dynamical instability
1:19:37 The maximum mass of neutron stars
1:21:44 Tolman, Oppenheimer, Volkoff equation
1:25:08 OV: Oppenheimer - Volkoff Equation of State
1:26:09 Oppenheimer and Volkoff, 1938
1:27:48 Limiting Mass for Neutron Stars
1:35:28 The fate of massive stars
1:37:23 If radiation pressure exceeds 9.2 percent of the total pressure then matter will never become degenerate no matter what the density is.
1:38:18 Condition for degeneracy
1:43:40 Radiation pressure and Degeneracy
1:43:56 Ideal gas versus relativistic degeneracy
1:51:27 Why are there only two classes of 'cold stars'?
1:51:34 Stability of Matter
1:58:03 HW: Harrison - Wheeler Equation of State OV: Oppenheimer - Volkoff Equation of State
1:58:50 There are only two types of cold stars in nature!
2:01:28 Sir Arthur Eddington, at the meeting of the Royal Astronomical Society in London in 1935.
2:04:37 Chandrasekhar Limit
2:07:34 Next Lecture: A Journey to the center of a Neutron Star
2:07:46 Q&A

[@pcalculas]

Professor ... When I see yu , I memorise "What a piece of work is a man, how noble in reason, how infinite in faculties, in form and moving, how express and admirable in action, how like an angel in apprehension, how like a god......."

[@Only1INDRAJIT]

I absolutely love every single second of his lectures... I think he should make one episode on GRB and Blazars also. It would be beyond awesome

[@naimulhaq9626]

Very interesting lectures, very well explained.

[@yonggao3349]

so awesome

[@santyclause8034]

I never realised my flashlight had kick... Q. if the expansion of the Universe is accelerating can the Observer instead be shrinking/receding? Are we not spiraling inward towards galactic central point? Is this receding Universe a locally distributed quantum field gradient phenomenon acting under the gravitic tidal influence of attraction to Sagittarius A* instead?

[@wdlang06]

nice lecture!!!!!