1 / 30

New State of Matter in White Dwarfs

New State of Matter in White Dwarfs . Gregory Gabadadze (NYU, CCPP). with R. A. Rosen, JCAP, JHEP 08,09 D. Pirtskhalava , JCAP 09. He or C nuclei . Electrons. and . d -- average interparticle separation.

wattan
Download Presentation

New State of Matter in White Dwarfs

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. New State of Matter in White Dwarfs Gregory Gabadadze (NYU, CCPP) with R. A. Rosen, JCAP, JHEP 08,09 D. Pirtskhalava, JCAP 09

  2. He or C nuclei Electrons and d -- average interparticle separation .. 1 Fermi << d << 1 Angstrom ??? 10 eV < T << 10 KeV

  3. Crystallization temperature To crystallize

  4. Critical Temperature Temperature at which thermal de Broglie wavelengths begin to overlap Uncertainties in particle position as large as inter-particle separation Critical T > Crystallization T => Charged Condensation!

  5. Relatively Light Stars End Up As White Dwarfs Heavier Stars End Up Either As Neutron Stars Or As Black Holes Typical density:

  6. What Keeps White Dwarfs Stable? Electrons - Nuclei + Inward Directed Gravitational Pull Outward Directed Electron Pressure versus

  7. Standard Theory: Carbon, Oxygen, …, Containing WD’s Crystallize As they Cool Down (Mestel, Ruderman) Specific heat dominated by the crystal phonon contribution Cooling time: ~10 Gyr

  8. Helium White Dwarfs In Binary Systems 0.2-0.5 solar mass dwarfs with helium core

  9. Some characteristics for helium white dwarfs

  10. Average carbon white dwarf

  11. Building up effective field theory • Order parameter: complex scalar • U(1) symmetries for scalars and fermions • Rotational symmetry • Galilean invariance • Schrodinger equation in the lowest order ..

  12. Effective Order Parameter Lagrangian for Charged Condensation Greiter, Wilczek,Witten in BCS superconductivity Solution

  13. Small perturbations (simplified)

  14. Spectrum of small perturbations Phonon contribution to specific heat:

  15. Impurity Interactions (H, He3,…)

  16. Gap-less Fermion Excitations

  17. Gap-less Fermions and Phonon

  18. White dwarf cooling

  19. Magnetic Vortices in Superconductors and White Dwarfs Rotation and Magnetic Properties of Helium White Dwarfs

  20. Magnetic flux lines

  21. Magnetic Flux Lines

  22. Critical Magnetic Field Disruption of Condensate

  23. London Magnetic Field

  24. Conclusions and Outlook Charge Condensate – new state of matter in the Universe Fast cooling of helium white dwarfs (super-massive carbon dwarfs ?) Magnetic field in flux tubes, high critical field; small London field Other possible applications: neutron star crust,…???

More Related