1 Summer course 2018 - A Random walk in astro-physics 0:09
2 Quantum Stars Lecture - 10 1:00
3 The strange companion of Sirius! 3:49
4 Are such super-dense stars doomed? 0:27
5 What will happen to the star when the nuclear reactor at its center fails? 1:10
6 Sir Ralph Howard Fowler 1889-1944 3:55
7 Quantum Physics 1:17
8 Energy levels of a particle in a one-dimensional box 1:20
9 Heisenberg's Uncertainty Principle 5:19
10 White Dwarfs are Quantum Stars 0:50
11 White Dwarfs are for ever! 2:35
12 Enter Chandra: 1928 2:46
13 Radiation Pressure 0:08
14 Hydrostatic Equilibrium 0:27
15 Gaseous Star & Quantum Star 0:36
16 Classical Physics: All momentum values are allowed. 2:02
17 Quantum Physics 1:48
18 Pauli's exclusion principle allows us to put two fermions in a cell in phase space. 0:21
19 Fermi Momentum 2:41
20 Fermi Energy 1:20
21 Pressure of an ideal classical gas 1:05
22 Pressure of a Fermi gas at T=0 K 1:59
23 Chandrasekhar's Theory of White Dwarfs 0:30
24 Chandrasekhar's Theory of White Dwarfs 1930 0:30
25 Mass - Radius Relation for White Dwarfs S. Chandrasekhar, 1930 1:23
26 Stars of all mass will find their ultimate peace as Quantum Stars supported by the pressure of electrons. 1:11
27 Diamonds in the sky! 3:17
28 History is made 0:29
29 Gravitational Collapse of massive white dwarfs 2:37
30 Relativistic Fermi Gas 4:48
31 Relativistic White Dwarfs 0:29
32 A fully relativistic WD has no radius! But it has a unique mass! 4:56
33 Mass - Radius Relation for White Dwarfs S. Chandrasekhar, 1934 0:47
34 Chandrasekhar Limit 1:36
35 Supernovae and Neutron Stars 0:31
36 Guest Stars 3:22
37 Supernovae and Cosmic Rays by W. Baade and F. Zwicky 3:31
38 Supernova Explosion 1:24
39 Between 1932 and 1937: 0:16
40 Lev Landau 0:08
41 Landau invents neutron stars in 1938 4:19
42 Neutronization of matter at high density 2:44
43 Dynamical instability 3:02
44 The maximum mass of neutron stars 2:06
45 Tolman, Oppenheimer, Volkoff equation 3:23
46 OV: Oppenheimer - Volkoff Equation of State 1:00
47 Oppenheimer and Volkoff, 1938 1:38
48 Limiting Mass for Neutron Stars 7:39
49 The fate of massive stars 1:54
50 If radiation pressure exceeds 9.2 percent of the total pressure then matter will never become degenerate no matter what the density is. 0:54
51 Condition for degeneracy 5:21
52 Radiation pressure and Degeneracy 0:15
53 Ideal gas versus relativistic degeneracy 7:30
54 Why are there only two classes of 'cold stars'? 0:06
55 Stability of Matter 6:28
56 HW: Harrison - Wheeler Equation of State OV: Oppenheimer - Volkoff Equation of State 0:46
57 There are only two types of cold stars in nature! 2:37
58 Sir Arthur Eddington, at the meeting of the Royal Astronomical Society in London in 1935. 3:08
59 Chandrasekhar Limit 2:56
60 Next Lecture: A Journey to the center of a Neutron Star 0:11
61 Q&A