Thermal flavor-composition fluctuations lower the activation energy for three-flavor quark matter nucleation, and color-superconducting CFL pairing reduces the critical droplet radius at low baryon density and temperature.
Quark Matter Droplet Formation in Neutron Stars
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abstract
The formation rate of quark matter droplets in neutron stars is calculated from a combination of bubble formation rates in cold degenerate and high temperature matter. Nuclear matter calculations of the viscosity and thermal conductivity are applied. Results show that droplets form only in the core of neutron stars shortly after supernova collapse, where pressures and temperatures are high, and for sufficiently small interface tension between nuclear and quark matter. Coulomb energies hinder formation of large droplets whereas the presence of strange hadrons in nuclear matter increase the droplet formation rate.
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Role of thermal fluctuations in nucleation of three-flavor quark matter
Thermal flavor-composition fluctuations lower the activation energy for three-flavor quark matter nucleation, and color-superconducting CFL pairing reduces the critical droplet radius at low baryon density and temperature.