Unmasking the nuclear matter equation of state

Abstract

Accurately calibrated (or ``best fit'') relativistic mean-field models are used to compute the distribution of isoscalar monopole strength in 90Zr and 208Pb, and the isovector dipole strength in 208Pb using a continuum random-phase-approximation approach. It is shown that the distribution of isoscalar monopole strength in 208Pb--but not in 90Zr--is sensitive to the density dependence of the symmetry energy. This sensitivity hinders the extraction of the compression modulus of symmetric nuclear matter from the isoscalar giant monopole resonance (ISGMR) in 208Pb. Thus, one relies on 90Zr, a nucleus with both a small neutron-proton asymmetry and a well developed ISGMR peak, to constrain the compression modulus of symmetric nuclear matter to the range K=(248 +/- 6) MeV. In turn, the sensitivity of the ISGMR in 208Pb to the density dependence of the symmetry energy is used to constrain its neutron skin to the range Rn-Rp<=0.22 fm. The impact of this result on the enhanced cooling of neutron stars is briefly addressed.

5 pages with 4 figures

References in corpus (6)

• Improved Models of Stellar Core Collapse and Still no Explosions: What is Missing?
• Low Mass Neutron Stars and the Equation of State of Dense Matter
• A microscopic estimate of the nuclear matter compressibility and symmetry energy in relativistic mean-field models
• Nuclear matter incompressibility coefficient in relativistic and nonrelativistic microscopic models
• The long journey from the giant-monopole resonance to the nuclear-matter incompressibility
• Relativistic mean-field study of neutron-rich nuclei

Cited by in corpus (80)

• Recent Progress and New Challenges in Isospin Physics with Heavy-Ion Reactions
• Equations of state for supernovae and compact stars
• Neutron-Rich Nuclei in Heaven and Earth
• Constraints on the density dependence of the symmetry energy
• Statistical Model for a Complete Supernova Equation of State
• Relativistic Mean-Field Hadronic Models under Nuclear Matter Constraints
• Relativistic effective interaction for nuclei, giant resonances, and neutron stars
• Nucleon-nucleon cross sections in neutron-rich matter and isospin transport in heavy-ion reactions at intermediate energies
• New Equations of State in Simulations of Core-Collapse Supernovae
• Microscopic determination of the nuclear incompressibility within the non-relativistic framework
• Building relativistic mean field models for finite nuclei and neutron stars
• Neutron Stars and the Nuclear Equation of State
• Strangeness Production close to Threshold in Proton-Nucleus and Heavy-Ion Collisions
• Neutron skin thickness in droplet model with surface width dependence: indications of softness of the nuclear symmetry energy
• Hadronic Matter is Soft
• Pygmy dipole resonance as a constraint on the neutron skin of heavy nuclei
• Pygmy Resonances and Neutron Skins
• Do we understand the incompressibility of neutron-rich matter?
• Neutron star properties and the symmetry energy
• The Giant Monopole Resonance in the Sn Isotopes: Why is Tin so "Fluffy"?
• Heavy Baryons in Compact Stars
• Sensitivity of the Moment of Inertia of Neutron Stars to the Equation of State of Neutron-Rich Matter
• Why is Tin so soft?
• Double neutron/proton ratio of nucleon emissions in isotopic reaction systems as a robust probe of nuclear symmetry energy
• Has a thick neutron skin in ${}^{208}$Pb been ruled out?
• Nuclear matter symmetry energy and the symmetry energy coefficient in the mass formula
• Gravitational radiation from pulsar glitches
• Nuclear Equation of state for Compact Stars and Supernovae
• Microscopic Study of the Isoscalar Giant Monopole Resonance in Cd, Sn and Pb Isotopes
• Accurate calibration of relativistic mean-field models: correlating observables and providing meaningful theoretical uncertainties
• Progress of Quantum Molecular Dynamics model and its applications in Heavy Ion Collisions
• Single and double pi^{-}/pi^{+} ratios in heavy-ion reactions as probes of the high-density behavior of the nuclear symmetry energy
• Information content of the weak-charge form factor
• Symmetry Energy Constraints from Giant Resonances: A Theoretical Overview
• Imposing multi-physics constraints at different densities on the Neutron Star Equation of State
• Continuous-wave gravitational radiation from pulsar glitch recovery
• Quantum Monte Carlo calculations of symmetric nuclear matter
• Effects of $\omega$ meson self-coupling on the properties of finite nuclei and neutron stars
• Isospin dependence of 6He+p optical potential and the symmetry energy
• Measurement of the nuclear symmetry energy parameters from gravitational wave events
• Correlations between the nuclear breathing mode energy and properties of asymmetric nuclear matter
• The breathing-mode giant monopole resonance and the surface compressibility in the relativistic mean-field theory
• Dense Matter in Neutron Stars with eXTP
• The effect of isoscalar-isovector coupling in infinite nuclear matter
• Isospin observables from fragment energy spectra
• Nuclear matter fourth-order symmetry energy in non-relativistic mean-field models
• Diquark Bose-Einstein Condensation and Nuclear Matter
• Neutron-skin thickness of finite nuclei in relativistic mean-field models with chiral limits
• Relativistic Mean Field Model parameterizations in the light of GW170817, GW190814, and PSR J0740 + 6620
• Symmetry energy effects on the properties of hybrid stars
• Indirect methods in nuclear astrophysics with relativistic radioactive beams
• Finding quark content of neutron stars in light of GW170817
• Finite- to zero-range relativistic mean-field interactions
• Influence of the symmetry energy on the giant monopole resonance of neutron-rich nuclei
• Nuclear Incompressibility in Asymmetric Systems at Finite Temperature and Entropy
• Nuclei in Core-Collapse Supernovae Engine
• Effect of the momentum dependence of nuclear symmetry potential on the transverse and elliptic flows
• Bayesian Inference of dense matter equation of state of neutron star with antikaon condensation
• Parametrization of the Relativistic ($\sigma -\omega$) Model for Nuclear Matter
• Small radii of neutron stars as an indication of novel in-medium effects
• New quantification of symmetry energy from neutron skin thicknesses of ${}^{48}$Ca and ${}^{208}$Pb
• Relativistic Transport Approach to Collective Nuclear Dynamics
• Symmetry coefficients and incompressibility of clusterized supernova matter
• Giant monopole energies from a constrained relativistic mean-field approach
• Nuclear matter properties, phenomenological theory of clustering at the nuclear surface, and symmetry energy
• Nuclear Incompressibility at Finite Temperature and Entropy
• The Auxiliary Field Diffusion Monte Carlo Method for Nuclear Physics and Nuclear Astrophysics
• Effects of the symmetry energy on the kaon condensates in the QMC Model
• The nuclear symmetry energy and the neutron skin thickness in nuclei
• Exploring $\Delta$-resonance in neutron stars: implications from astrophysical and nuclear observations
• Can the nuclear symmetry potential at supra-saturation densities be negative?
• Composition of scalar mesons and their effects on nuclear matter properties in an extended linear sigma model
• Correlation between the charge radii difference in mirror partner nuclei and the symmetry energy slope
• Parity Violation, the Neutron Radius of Lead, and Neutron Stars
• Recent astrophysical and accelerator based results on the Hadronic Equation of State
• Alpha Cluster Model of Atomic Nuclei
• Nuclear equation of state and incompressibility in a model with correlations from giant monopole vibrations
• Symmetry energy from fragment observables in the canonical thermodynamic model
• Dense Hadronic Matter in Neutron Stars
• Effects of Symmetry Energy in the Reaction 40Ca+124Sn at 140 MeV/nucleon