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A substance that reaches superconductivity, a state in which magnetic fields cannot penetrate, and there is no electrical resistance, is referred to as a superconductor. In 1911, Heike Kamerlingh Onnes of Leiden University, a Dutch physicist, observed a relation between the temperature and the resistance of the element mercury. The mercury sample was then cooled in liquid helium to study the linear dependence of resistance on temperature. It was observed that, as the temperature decreased, the...
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Color Superconductivity under Neutron-Star Conditions at Next-to-Leading Order.

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|December 5, 2025
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Summary
This summary is machine-generated.

The equation of state for quark matter at high densities is explored. Sizable pairing corrections in the color-flavor-locked (CFL) phase constrain the CFL gap to approximately 140 MeV.

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Area of Science:

  • High-energy nuclear physics
  • Quantum chromodynamics (QCD)
  • Astrophysical implications of dense matter

Background:

  • The equation of state for deconfined strongly interacting matter at high densities is not fully understood.
  • Quark pairing in the color-flavor-locked (CFL) ground state may significantly influence this equation of state.
  • Previous research indicated large pairing gaps in the CFL phase might contradict neutron star observations.

Purpose of the Study:

  • To compute next-to-leading-order corrections to the pressure of quark matter in the CFL phase.
  • To incorporate neutron-star equilibrium conditions and advanced perturbative QCD results.
  • To constrain the CFL gap using these calculations and astrophysical observations.

Main Methods:

  • Calculation of next-to-leading-order corrections to quark matter pressure in the CFL phase.
  • Inclusion of pairing gap and strong coupling constant effects.
  • Application of neutron-star equilibrium conditions and perturbative QCD.
  • Analysis of the dependence of the CFL gap on the chemical potential.

Main Results:

  • Corrections to the pressure due to pairing and coupling constant effects were found to be sizable.
  • The CFL gap in the quark energy spectrum is constrained to be less than or equal to 140 MeV at a baryon chemical potential of 2.6 GeV.
  • This constraint holds even when considering a broad range of gap behaviors.

Conclusions:

  • The study provides significant constraints on the CFL gap, reconciling theoretical calculations with astrophysical data.
  • Accurate modeling of quark matter at high densities requires careful consideration of pairing effects and perturbative QCD corrections.
  • The findings advance our understanding of the equation of state for matter within neutron stars.