Bulletin of the American Physical Society
6th Joint Meeting of the APS Division of Nuclear Physics and the Physical Society of Japan
Sunday–Friday, November 26–December 1 2023; Hawaii, the Big Island
Session E08: Minisymposium: Equation of State Information from Astrophysics and Nuclear Physics Experiments |
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Chair: Mizuki Kurata-NIshimura Room: Hilton Waikoloa Village Kohala 1 |
Wednesday, November 29, 2023 7:00PM - 7:30PM |
E08.00001: Status of experimental constraints for the nuclear equation of state Invited Speaker: Zbigniew Chajecki The equation of state (EOS) is a fundamental property of nuclear matter, important for studying the structure of systems as diverse as the atomic nucleus and neutron stars. Understanding the physics of neutron stars is becoming even more important recently because of the observation of gravitational waves from the neutron star merger. Nuclear reactions involving heavy-ion collisions in the laboratories can produce the nuclear matter similar to those contained in neutron stars and allow the exploration of the equation of state of nuclear matters over a wide range of densities and temperatures. The current status of the experimental constraints and future prospects from the experiments in the existing facilities in US and Japan will be presented. |
Wednesday, November 29, 2023 7:30PM - 7:45PM |
E08.00002: The Nuclear Equation of State from Experiments and Astronomical Observations Charles J Horowitz, Chun Y Tsang, Betty Tsang, William G Lynch, Rohit Kumar With recent advances in astronomical observations, major progress has been made in determining the pressure of neutron star matter at high density. This pressure is constrained by the neutron star deformability, determined from gravitational waves emitted in a neutron-star merger, and measurements of radii for two neutron stars using a new X-ray observatory on the International Space Station. Previous studies have relied on nuclear theory calculations to constrain the equation of state at low density. Here we use a combination of 15 constraints composed of three astronomical observations and twelve nuclear experimental constraints that extend over a wide range of densities. A Bayesian inference framework is then used to obtain a comprehensive nuclear equation of state. This data-centric result provides benchmarks for theoretical calculations and modeling of nuclear matter and neutron stars. Furthermore, it provides insights on the composition of neutron stars and their cooling via neutrino radiation. |
Wednesday, November 29, 2023 7:45PM - 8:00PM |
E08.00003: Studying neutron star matter with gravitational wave observations Katerina Chatziioannou Gravitational wave observations of merging neutron stars can be used to study the properties of dense nuclear matter. In this talk I will describe what the latest information about neutron star masses and tidal deformabilities have revealed about the properties of supranuclear matter and the possibility of phase transitions to exotic degrees of freedom in neutron stars. I will also discuss future prospects as gravitational wave detectors increase in sensitivity. |
Wednesday, November 29, 2023 8:00PM - 8:15PM |
E08.00004: The speed of sound in the zero temperature QCD phase diagram Dake Zhou Information from both nuclear theories and astrophysical observations are combined to shed light on the speed of sound across the zero-temperature QCD phase diagram. While calculations based on chiral effective field theory at low densities and measurements of neutron star masses, radii, and tidal deformabilities already provided valuable insights into the neutron star equations of state, predictions of perturbative QCD at ultra-high densities can impose additional constraints orthogonal to those previously reported. Furthermore, information about the phase of matter in the intermediate region that lies beyond the most massive neutron stars and below where perturbative QCD applies may be extracted, opening the possibility of a holistic view of the zero-temperature QCD phase diagram. Prospects of placing bounds on the maximum and minimum speed of sound within and beyond neutron star densities is forecasted based on anticipated astrophysical observations. |
Wednesday, November 29, 2023 8:15PM - 8:30PM |
E08.00005: Consistent inference of neutron star bulk and crust properties and nuclear observables using an Energy-Density Functional approach. William G Newton, Rebecca Preston, Lauren E Balliet, Brianna T Douglas, Thomas B Head We have entered the era of multi-messenger nuclear astrophysics; bringing a host of astrophysical observations and nuclear experimental data to collectively measure the properties of neutron star matter and the nuclear force in neutron-rich systems. In order to combine disparate data sets with meaningful uncertainty quantification, over the past decade statistical inference techniques employing ensembles of models have been increasingly employed. In order to minimize systematic model uncertainty, where possible the same underlying model should be used to construct both neutron star and nuclear models. We present an example of such an approach, using an Energy-Density Functional to model bulk properties of neutron stars such as the maximum mass, radii, tidal deformabilities and moments of inertia, crust properties of neutron stars, and nuclear properties including nuclear masses, neutron skins and dipole polarizabilities. We demonstrate how different observables constrain nuclear matter in different density ranges, and discuss some of the remaining model uncertainties. |
Wednesday, November 29, 2023 8:30PM - 8:45PM |
E08.00006: Nuclear equation of state in relativistic mean-field models with isoscalar- and isovector-meson mixing Tsuyoshi Miyatsu, Myung-Ki Cheoun, Kyungsik Kyungsik Kim, Koichi Saito We construct nuclear equation of state (EoS) of dense matter using the relativistic mean-field (RMF) model with nonlinear couplings. Taking into account the results of neutron skin thickness of 208Pb and 48Ca by the PREX-2 and CREX experiments as well as the particle flow data in heavy-ion collisions, the observed mass of PSR J0740+6620, and the tidal deformability of a neutron star from GW170817, we build new effective interactions in the RMF model with the isovector, Lorentz-scalar (δ) meson. In addition, we study the effect of isoscalar- and isovector-meson mixing, σ2δ2 and ωμωμρν·ρν, on the properties of finite nuclei, nuclear matter, and neutron stars. It is found that the σ-δ mixing is very useful to understand the recent nuclear experiments and astrophysical observations of neutron stars simultaneously. Especially, the EoS of neutron stars exhibits the rapid stiffening around twice the nuclear saturation density, which is caused by the unique behavior of nuclear symmetry energy due to the σ-δ mixing. It is also interesting that the small dimensionless tidal deformability of a canonical neutron star observed from GW170817 can be satisfied within the RMF models with isoscalar- and isovector-meson mixing. |
Wednesday, November 29, 2023 8:45PM - 9:00PM |
E08.00007: Collision dynamics using neutron rich and deficient Sn + Sn collisions with 270MeV/u Mizuki Kurata-NIshimura, Tadaaki Isobe, Tetsuya Murakami, Akira Ono, Natsumi Ikeno, Chun Yuen Tsang, Manyee B Tsang, William G Lynch, Hideaki Otsu, Hiroyoshi Sakurai Heavy-ion collisions are utilized to investigate nuclear EOS worldwide because it is a unique tool to analyze nuclear EOS under supra-saturation density in laboratories. Various observables are proposed and measured as sensitive probes to investigate the symmetry energy in the dense matter produced by heavy-ion collisions. We have performed experiments using Sn isotope beams. nucleus+nucleus collisions for 132Sn+124Sn and 108Sn+112Sn, and 124Sn+112Sn at 270 MeV/u was carried out to study system dependence with different isospin asymmetries and a common total charge. |
Wednesday, November 29, 2023 9:00PM - 9:15PM |
E08.00008: Constraints from the SπRIT experiment and their implications on nuclear matter equation of state Chun Yuen Tsang, Manyee B Tsang, William G Lynch, YingXun Zhang Properties of the nuclear equation of state (EoS) can be probed by measuring the dynamical properties of nucleus-nucleus collision. With appropriate transformation, nuclear EoS also describes the properties of neutron stars. Therefore, it is possible to combine results from terrestrial experiments with astronomical observations to constrain EoS comprehensively. |
Wednesday, November 29, 2023 9:15PM - 9:30PM |
E08.00009: Contraining the momentum dependence of the symmetry energy with heavy-ion collisons Kyle W Brown, Betty Tsang, William G Lynch, Chi-En Teh, Zbigniew Chajecki, Jeonghyeok Park Nucleons in dense nuclear matter appear to have reduced inertial masses due to momentum-dependent interactions they experience with other nucleons. This reduction of their masses is often referred to as their effective mass, and at saturation density the effective masses are about 70% of their vacuum mass. In asymmetric matter the effective masses of neutrons and protons can be different, leading to an effective-mass splitting. The sign and magnitude of this splitting is poorly constrained at densities away from saturation density. |
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