Fluctuations in the pasta phase
arXiv:2105.03318 · doi:10.1103/PhysRevC.104.L022801
Abstract
Baryonic matter close to the saturation density is very likely to present complex inhomogeneous structures collectively known under the name of pasta phase. At finite temperature, the different geometric structures are expected to coexist, with potential consequences on the neutron star crust conductivity and neutrino transport in supernova matter. In the framework of a statistical multi-component approach, we calculate the composition of matter in the pasta phase considering density, proton fraction, and geometry fluctuations. Using a realistic energy functional from relativistic mean field theory and a temperature and isospin dependent surface tension fitted from Thomas-Fermi calculations, we show that different geometries can coexist in a large fraction of the pasta phase, down to temperatures of the order of the crystallization temperature of the neutron star crust. Quantitative estimates of the charge fluctuations are given.
arXiv comment6 pages, 3 figures, 1 table
References in corpus (25)
- Relativistic Mean-Field Hadronic Models under Nuclear Matter Constraints
- Relativistic effective interaction for nuclei, giant resonances, and neutron stars
- Disordered nuclear pasta, magnetic field decay, and crust cooling in neutron stars
- Nuclear pasta structures and the charge screening effect
- A highly resistive layer within the crust of X-ray pulsars limits their spin periods
- Nonuniform Neutron-Rich Matter and Coherent Neutrino Scattering
- Unified treatment of sub-saturation stellar matter at zero and finite temperature
- A New Open-Source Nuclear Equation of State Framework based on the Liquid-Drop Model with Skyrme Interaction
- Upper limits on the observational effects of nuclear pasta in neutron stars
- The pasta phase within density dependent hadronic models
- A new baryonic equation of state at sub-nuclear densities for core-collapse simulations
- Stellar properties and nuclear matter constraints
- Consistent relativistic mean field models constrained by GW170817
- Light clusters, pasta phases and phase transitions in core-collapse supernova matter
- Crystallization of the inner crust of a neutron star and the influence of shell effects
- Light clusters and the pasta phase
- Effect of topological defects on "nuclear pasta" observables
- particles and the pasta phase
- Electron transport through nuclear pasta in magnetized neutron stars
- Transport properties of nuclear pasta phase with quantum molecular dynamics
- Light Clusters and Pasta Phases in Warm and Dense Nuclear Matter
- Domains and defects in nuclear "pasta"
- Nuclear pasta and supernova neutrinos at late times
- Pasta fluctuations in symmetric matter at finite temperature
- Nuclear pasta in hot and dense matter and its influence on the equation of state for astrophysical simulations