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Massive Binary
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Classroom Contents
Neutron Stars and Black Holes - Recycled Pulsars - Lecture 10
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- 1 Time: AM
- 2 Neutron Stars and Black Holes Lecture - 10: Recycled Pulsars
- 3 Recycled Pulsars
- 4 The HULSE-TAYLOR Pulsar
- 5 Hulse-Taylor Binary Pulsar
- 6 Massive Binary
- 7 Spinning up a neutron star
- 8 What will be the period of rotation of the first-born neutron star after the spin up phase is over?
- 9 The Equilibrium Period
- 10 Alfven Radius
- 11 Accretion disk
- 12 Question: For a given magnetic field, can we spin up a neutron star to arbitrarily small period?
- 13 Eddington Luminosity Limit
- 14 Eddington Limit for the Accretion Rate
- 15 The Minimum Equilibrium Period
- 16 The Hulse-Taylor Binary Pulsar
- 17 Any viable theory of field evolution must explain the following questions
- 18 Origin of magnetic field of neutron stars
- 19 Field decay in Neutron Stars
- 20 Superfluid core
- 21 Type II superconductivity in the core
- 22 Type II proton superconductivity in the core
- 23 Feynman "Vortices" to the rescue!
- 24 The inter-pinning of the fluxoids and vortices
- 25 An important prediction
- 26 Recycled Pulsars
- 27 What determines the degree of field decay?
- 28 A Possible scenario
- 29 The population of Recycled Pulsars
- 30 Next Lecture - Millisecond Pulsars
- 31 Q&A
