Superfluidity and Superconductivity in nucleonic Neutron Stars - - PowerPoint PPT Presentation

superfluidity and superconductivity in nucleonic neutron
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Superfluidity and Superconductivity in nucleonic Neutron Stars - - PowerPoint PPT Presentation

Superfluidity and Superconductivity in nucleonic Neutron Stars matter 1. Outline of neutron star structure 2. Origin of Superfluidity and basic properties 3. Elementary excitations : phonon and vortices 3. More microscopic approach


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Superfluidity and Superconductivity in nucleonic Neutron Stars matter

  • 1. Outline of neutron star structure
  • 2. Origin of Superfluidity and basic properties
  • 3. Elementary excitations : phonon and vortices
  • 3. More microscopic approach
  • 4. Superfluidity in Fermi systems : basic principes
  • 5. Nuclear matter
  • 6. Superconductivity . The proton component
  • 7. Magnetic field and flux tubes
  • 8. Microscopic theory
  • 9. Basic open questions
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Schematic view

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A section (schematic)

  • f a neutron star
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Vortex ring from the vulcan Etna Natural vortex ring

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Calculations in Neutron Matter ( Matsuo 2006 )

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Nygaard et al., PRL 90 (2003) Bogoliubov-De Gennes equations (BCS) Yu & Bulgac, PRL 90 (2003) Energy functional Bulgac and Yu, PRL 91 (2003)

  • En. funct. inspired by Monte-Carlo

calculations. Very low density, maybe not relevant for NS (rather for trapped atomic gas) The structure of a single vortex line

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A section (schematic)

  • f a neutron star
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Negele & Vautherin classical paper (no pairing) The structure of nuclei and Z/N ratio are dictated by beta equilibrium

e p n

µ µ µ + =

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No drip region Drip region Outer Crust Inner Crust Position of the neutron chemical potential

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Possible positions of a vortex in the crust Top view Side view

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Neutron and proton density profiles Neutron and proton pairing profiles Density = 1/10 saturation density , Wigner-Seitz cell

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A close view at a glitch The “regular” increase of the period is mainly due to dipolar radiation

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A set of glitches in the Vela pulsar (Period time derivative)

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Many-body effects on the proton gap

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Pairing gap for the s-wave in neutron matter

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Including many-body effects

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The intrinsic uncertainity on the 3P2 pairing gap due to the uncertainity on the bare NN interaction PRC 58, 1921 (1998)

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OPEN PROBLEMS

  • 1. Strength of the 3P2 pairing
  • 2. Density dependence of pairing
  • 3. Proton superfluidity
  • 4. Pinning energy
  • 5. Effects of superfluidity on transport

processes , neutrino emission and transport, ………

  • 6. Vortices dynamics
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  • 7. Many-body effects on the gap
  • 8. Neutron-proton excitations in the core

3P2 , “angulons”

  • 9. Excitations in the crust (role of the

lattice)

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2 3P

The pairing gap as a function of density calculated within the Renormalization Group method. (Schwenk & Friman, PRL 2004 )