Neutron Stars and Black Holes (Lecture - 01: Diffuse Stars) by G Srinivasan
SUMMER COURSES NEUTRON STARS AND BLACK HOLES SPEAKER: G Srinivasan (Raman Research Institute - Retired) DATE: 15 May 2019 to 28 June 2019 VENUE: Emmy Noether Seminar Room, ICTS Bangalore The theme of the course will be neutron stars and black holes, with emphasis on neutron stars in binaries (their formation and rotational history); their mergers; gamma ray bursts; formation of intermediate mass and super massive black holes. Lectures: 1) Diffuse Stars 2) Life History of the stars 3) Quantum Stars 4) Neutron Stars and Supernovae 5) Interior of neutron stars 6) Superfluidity and superconductivity inside neutron stars. 7) Neutron Stars as Pulsars 8) Gravitation - From Newton to Einstein 9) Maximum mass of neutron stars 10) Evolution of neutron stars in close binaries 11) Recycled pulsars 12) Tests General Relativity using Double Neutron Stars 13) Gravitational radiation from neutron star mergers 14) Black Holes of General Relativity 15) Super massive Black Holes 16) Universe versus Multiverse Schedule: May – 15, 17, 22, 24, 29 and 31 June – 5, 7, 12, 14, 19, 21, 24, 26 and 28 Time: 10:00 AM • Summer Course 2019: Neutron Stars and Blac... Table of Contents (powered by https://videoken.com) 0:00:00 Neutron Stars and Black Holes (Lecture - 01) 0:02:44 Momentous discoveries during last three years 0:03:46 What are neutron stars? How are they formed? 0:05:34 Topics 0:09:48 What are the stars? Why are they as they are? 0:10:35 Gaseous Stars 0:12:17 Stars as globes of perfect gas 0:13:18 Gravitational Pressure 0:14:03 Gravitational Pressure = P Gravity approximate GM2/R4 0:16:07 Hydrostatic Equilibrium 0:18:29 Boyle's Law 0:20:27 Equation of Hydrostatic Equilibrium 0:21:05 What are the stars? 0:22:14 Eddington's theory of stars 0:24:08 Radiation Pressure 0:24:45 How hot is the Sun? 0:25:46 Virial Theorem 0:27:39 Virial Theorem applied to the Sun 0:30:56 The interior of the Sun 0:33:50 Mean-free-path is approximate 0.5 cm. Radius approximate 1 million km. 0:35:09 In the Sun, photons take ~ 30,000 years to escape! In massive stars, it will take a million years or more! 0:45:45 Mass - Luminosity relation 0:47:28 Mass - Luminosity relation calculated by Eddington L proportional M3 0:49:23 Why are the stars as they are? 0:53:58 "Our mistake was that in estimating the congestion in the stellar ball-room we had forgotten that crinolines are no longer in fashion" - Eddington 0:54:58 Why are the masses of stars in an incredibly narrow range between (0.5-30) M sun? 0:57:48 Eddington was obscure about two things: 0:59:02 Why are the atoms as they are? 1:00:08 Atoms are as they are because they obey the rules of atomic physics. 1:04:25 Lifetime of stars 1:08:01 Why does the Sun shine? 1:09:31 How long will the heat last? 1:11:09 Sir Arthur Eddington 1:15:02 Mass Deficit 1:17:03 Proton - proton collision 1:20:35 Maxwell-Boltzmann Distribution 1:22:05 Alpha decay of radioactive nuclei 1:24:58 Quantum Tunnelling 1:26:11 Energy production in the Sun 1:26:38 Proton - proton reaction 1:29:23 Why doesn't the Sun blow up? 1:31:18 Nuclear cycles 1:32:32 To burn or not to burn? That is the question 1:34:19 Fusion reactions 1:35:20 The composition of the core when nuclear reactions finally stop 1:35:49 Q&A
