Light clusters and the pasta phase

Abstract

The effects of including light clusters in nuclear matter at low densities are investigated within four different parametrizations of relativistic models at finite temperature. Both homogeneous and inhomogeneous matter (pasta phase) are described for neutral nuclear matter with fixed proton fractions. We discuss the effect of the density dependence of the symmetry energy, the temperature and the proton fraction on the non-homogeneous matter forming the inner crust of proto-neutron stars. It is shown that the number of nucleons in the clusters, the cluster proton fraction and the sizes of the Wigner Seitz cell and of the cluster are very sensitive to the density dependence of the symmetry energy.

14 pages, 14 figures; Accepted for publication in Phys. Rev. C

References in corpus (7)

• Neutron-Rich Nuclei in Heaven and Earth
• Relativistic effective interaction for nuclei, giant resonances, and neutron stars
• Locating the inner edge of neutron star crust using terrestrial nuclear laboratory data
• Appearance of Light Clusters in Post-bounce Evolution of Core-Collapse Supernovae
• The pasta phase within density dependent hadronic models
• Statistical description of complex nuclear phases in supernovae and proto-neutron stars
• Light clusters in nuclear matter: Excluded volume versus quantum many-body approaches

Cited by in corpus (29)

• Equations of state for supernovae and compact stars
• Unified treatment of sub-saturation stellar matter at zero and finite temperature
• Equation of state and thickness of the inner crust of neutron stars
• Thermodynamics of isospin-asymmetric nuclear matter from chiral effective field theory
• Non-congruence of the nuclear liquid-gas and deconfinement phase transitions
• Nuclear Equation of state for Compact Stars and Supernovae
• Nuclear matter equation of state including few-nucleon correlations $(A\le 4)$
• Light clusters, pasta phases and phase transitions in core-collapse supernova matter
• Imprint of the symmetry energy on the inner crust and strangeness content of neutron stars
• Constraining supernova equations of state with equilibrium constants from heavy-ion collisions
• Nuclear Statistical Equilibrium Equation of State for Core Collapse
• Full distribution of clusters with universal couplings and in-medium effects
• Description of light clusters in relativistic nuclear models
• Magnetic susceptibility and magnetization properties of asymmetric nuclear matter under a strong magnetic field
• Neutron stars: from the inner crust to the core with the (Extended) Nambu-Jona-Lasinio model
• Low density nuclear matter with light clusters in a generalized nonlinear relativistic mean-field model
• Pasta phases within the QMC model
• Pasta phases in neutron star studied with extended relativistic mean field models
• Hyperons in the pasta phase
• Pasta fluctuations in symmetric matter at finite temperature
• Warm unstable asymmetric nuclear matter: critical properties and the density dependence of the symmetry energy
• Light clusters in warm stellar matter: calibrating the cluster couplings
• Anisotropic electron transport in the nuclear pasta phase
• Strong magnetic fields and pasta phases revisited
• Nuclear pasta in hot and dense matter and its influence on the equation of state for astrophysical simulations
• Fluctuations in the pasta phase
• Cold dilute nuclear matter with $\alpha$-particle condensation in a generalized nonlinear relativistic mean-field model
• Neutron star properties: Constraining the nuclear matter EoS
• Light clusters as a possible source of crustal impurities: a quasi-particle approach