Influence of the tetraneutron on the EoS under core-collapse supernovae and heavy-ion collisions conditions

Abstract

Recently, a resonant state of four neutrons (tetraneutron) with an energy of $E_{4n}=2.37\pm 0.38(\mathrm{stat})\pm 0.44(\mathrm{sys})$ MeV and a width of $\Gamma =1.75\pm 0.22(\mathrm{stat})\pm 0.30(\mathrm{sys})$ MeV was reported. In this work, we analyse the effect of including such an exotic state on the yields of other light clusters, that not only form in astrophysical sites, such as core-collapse supernovae and neutron star mergers, but also in heavy-ion collisions. To this aim, we use a relativistic mean-field formalism, where we consider in-medium effects in a two-fold way, via the couplings of the clusters to the mesons, and via a binding energy shift, to compute the low-density equation of state for nuclear matter at finite temperature and fixed proton fraction. We consider five light clusters, deuterons, tritons, heliums, $\alpha$-particles, and ${}^6$He, immersed in a gas of protons and neutrons, and we calculate their abundances and chemical equilibrium constants with and without the tetraneutron. We also analyse how the associated energy of the tetraneutron would influence such results. We find that the low-temperature, neutron-rich systems, are the ones most affected by the presence of the tetraneutron, making neutron stars excellent environments for their formation. Moreover, its presence in strongly asymmetric matter may increase considerably the proton and the $\alpha$-particle fractions. This may have an influence on the dissolution of the accretion disk of the merger of two neutron stars.

arXiv comment10 pages, 6 figures

References in corpus (28)

• Equations of state for supernovae and compact stars
• Composition and thermodynamics of nuclear matter with light clusters
• Relativistic Equation of State of Nuclear Matter for Supernova and Neutron Star
• Hadron production in central nucleus-nucleus collisions at chemical freeze-out
• Neutron-Rich Nuclei in Heaven and Earth
• Statistical Model for a Complete Supernova Equation of State
• Systematics of dynamical mass ejection, nucleosynthesis, and radioactively powered electromagnetic signals from neutron-star mergers
• Cluster Formation and The Virial Equation of State of Low-Density Nuclear Matter
• Multi-messenger picture of compact binary mergers
• The detection of neutron clusters
• Influence of light nuclei on neutrino-driven supernova outflows
• Laboratory Tests of Low Density Astrophysical Equations of State
• The Virial Equation of State of Low-Density Neutron Matter
• Statistical description of complex nuclear phases in supernovae and proto-neutron stars
• Nuclear matter equation of state including few-nucleon correlations $(A\le 4)$
• Light clusters, pasta phases and phase transitions in core-collapse supernova matter
• Constraining mean-field models of the nuclear matter equation of state at low densities
• Nuclear Statistical Equilibrium Equation of State for Core Collapse
• $\alpha$ particles and the pasta phase
• Light clusters in warm stellar matter: explicit mass shifts and universal cluster-meson couplings
• Full distribution of clusters with universal couplings and in-medium effects
• Description of light clusters in relativistic nuclear models
• Light Clusters and Pasta Phases in Warm and Dense Nuclear Matter
• Equilibrium constants of Hydrogen and Helium isotopes at low nuclear densities
• Composition of nuclear matter with light clusters and Bose-Einstein condensation of $\alpha$ particles
• Hubble constant and nuclear equation of state from kilonova spectro-photometric light curves
• Tetraneutron condensation in neutron rich matter
• Improved method for the experimental determination of in-medium effects from heavy-ion collisions

Cited by in corpus (1)

• Virialized equation of state for warm and dense stellar plasmas in proto-neutron stars and Supernova matter