Gregory Gabadadze (NYU, CCPP) with R. A. Rosen, JCAP, JHEP 08,09 D. Pirtskhalava, JCAP 09.

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Presentation transcript:

Gregory Gabadadze (NYU, CCPP) with R. A. Rosen, JCAP, JHEP 08,09 D. Pirtskhalava, JCAP 09

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

Crystallization temperature To crystallize

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

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

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

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

Helium White Dwarfs In Binary Systems solar mass dwarfs with helium core

Some characteristics for helium white dwarfs

Average carbon white dwarf

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..

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

Small perturbations (simplified)

Spectrum of small perturbations Phonon contribution to specific heat:

Impurity Interactions (H, He3,…)

Gap-less Fermion Excitations

Gap-less Fermions and Phonon

White dwarf cooling

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

Magnetic flux lines

Magnetic Flux Lines

Critical Magnetic Field Disruption of Condensate

London Magnetic Field

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,…???

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