Effects of the liquid-gas phase transition and cluster formation on the symmetry energy

Abstract

Various definitions of the symmetry energy are introduced for nuclei, dilute nuclear matter below saturation density and stellar matter, which is found in compact stars or core-collapse supernovae. The resulting differences are exemplified by calculations in a theoretical approach based on a generalized relativistic density functional for dense matter. It contains nucleonic clusters as explicit degrees of freedom with medium dependent properties that are derived for light clusters from a quantum statistical approach. With such a model the dissolution of clusters at high densities can be described. The effects of the liquid-gas phase transition in nuclear matter and of cluster formation in stellar matter on the density dependence of the symmetry energy are studied for different temperatures. It is observed that correlations and the formation of inhomogeneous matter at low densities and temperatures causes an increase of the symmetry energy as compared to calculations assuming a uniform uncorrelated spatial distribution of constituent baryons and leptons.

20 pages, 19 figures, version accepted for publication in EPJA special volume on Nuclear Symmetry Energy

References in corpus (19)

• Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
• Symmetry Energy II: Isobaric Analog States
• Symmetry energy of dilute warm nuclear matter
• Constraining the High-Density Behavior of Nuclear Symmetry Energy with the Tidal Polarizability of Neutron Stars
• Light nuclei quasiparticle energy shift in hot and dense nuclear matter
• Experimental determination of the symmetry energy of a low density nuclear gas
• Density dependence of the symmetry energy from neutron skin thickness in finite nuclei
• A comparative study of statistical models for nuclear equation of state of stellar matter
• Neutrino Breakup of A=3 Nuclei in Supernovae
• Density dependence of nuclear symmetry energy constrained by mean-field calculations
• Cluster virial expansion for nuclear matter within a quasiparticle statistical approach
• Nuclear symmetry energy from the Fermi-energy difference in nuclei
• Isospin Distillation with Radial Flow: a Test of the Nuclear Symmetry Energy
• Origin of symmetry energy in finite nuclei and density dependence of nuclear matter symmetry energy from measured alpha-decay energies
• Lifetime measurement of the 6792 keV state in 15O, important for the astrophysical S factor extrapolation in 14N(p,g)15O
• Constraining the density dependence of symmetry energy from nuclear masses
• Liquid-gas phase transition in hot asymmetric nuclear matter with density-dependent relativistic mean-field models
• Thermodynamics of clusterized matter
• Pure Neutron Matter Constraints and Nuclear Symmetry Energy

Cited by in corpus (30)

• Equations of state for supernovae and compact stars
• Towards Understanding Astrophysical Effects of Nuclear Symmetry Energy
• Neutron skin thickness of heavy nuclei with $\alpha$-particle correlations and the slope of the nuclear symmetry energy
• Nuclear Equation of state for Compact Stars and Supernovae
• Symmetry energy of cold nucleonic matter within a relativistic mean field model encapsulating effects of high momentum nucleons induced by short-range correlations
• Nuclear matter equation of state including few-nucleon correlations $(A\le 4)$
• Collision dynamics at medium and relativistic energies
• Delineating Effects of Nuclear Symmetry Energy on the Radii and Tidal Polarizabilities of Neutron Stars
• Equations of state for hot neutron stars -- II. The role of exotic particle degrees of freedom
• Candidates for the 5$\alpha$ condensed state in ${}^{20}$Ne
• Towards a Unified Quark-Hadron Matter Equation of State for Applications in Astrophysics and Heavy-Ion Collisions
• The state of matter in simulations of core-collapse supernovae -- Reflections and recent developments
• EoS for hot neutron stars
• Universal relations for rapidly rotating cold and hot hybrid star
• Nucleon self-energies for supernova equations of state
• Signals of Bose Einstein condensation and Fermi quenching in the decay of hot nuclear systems
• Low density nuclear matter with light clusters in a generalized nonlinear relativistic mean-field model
• Embedding short-range correlations in relativistic density functionals through quasi-deuterons
• Inhomogeneity growth in two-component fermionic systems
• Pairing effects on neutrino transport in low-density stellar matter
• Phenomenological Equation of State of Strongly Interacting Matter with First-Order Phase Transitions and Critical Points
• Cold dilute nuclear matter with $\alpha$-particle condensation in a generalized nonlinear relativistic mean-field model
• Effect of the Coulomb interaction on the liquid-gas phase transition of nuclear matter
• Competition between fermions and bosons in nuclear matter at low densities and finite temperatures
• Modification of the universal relation between mass, radius and nonradial $f$-mode oscillation in proto-neutron stars
• Isospin-Asymmetry Dependence of the Thermodynamic Nuclear Equation of State in Many-Body Perturbation Theory
• Effects of Neutron-Proton Short-Range Correlation on the Equation of State of Dense Neutron-Rich Nucleonic Matter
• Equation of State in a Generalized Relativistic Density Functional Approach
• Violent Nuclear Reactions: Large-Amplitude Nuclear Dynamic Phenomena in Fermionic Systems
• Tracing the Trace Anomaly of Dense Matter inside Neutron Stars