NuSym23, XIth International Symposium on Nuclear Symmetry Energy

Our knowledge about dense matter explored in the cores of neutron stars remains limited. Fortunately, the detections of gravitational waves emitted from the merger of neutron stars and the corresponding electromagnetic signals provide a new way of studying supranuclear-dense material. Making use of the strength of multi-messenger astronomy, one can combine the information obtained from...

Interpreting high-energy, astrophysical phenomena, such as supernova explosions or neutron-star collisions, requires a robust understanding of matter at supranuclear densities. However, our knowledge about dense matter explored in the cores of neutron stars remains limited. Fortunately, dense matter is not only probed in astrophysical observations, but also in terrestrial heavy-ion collision...

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 with measured masses, using a new X-ray observatory on the...

The impacts of various symmetry energy parameters on the properties of neutron stars have been recently investigated, and the outcomes are at variance. Results obtained from systematic analysis of the correlations of slope and curvature parameters of symmetry energy at the saturation density with the tidal deformability and stellar radius of non-spinning neutron stars in the mass range of...

The last few years have seen tremendous progress in multi-messenger observations of neutron stars (NS) that have constrained their global properties such as their masses, radii and tidal deformabilities. These constraints could be used to obtain valuable information on the nuclear symmetry energy. However, in order to do so, we require rigorous theoretical nuclear physics inputs to interpret...

This contribution concerns the characterization of the nuclear equation of state (EOS) evaluated from ground state properties of nuclei, i.e. from nuclear masses, charge radii and neutron thickness. By using a Thomas-Fermi framework combined with a specific Seyler-Blanchard nucleon-nucleon interaction containing both non-local and density terms, I will show that quantitative information about...

In the last years Bayesian techniques are employed more and more frequently to build equations of state of dense neutron rich matter by imposing various sets of constraints on functional relations derived within models with different degrees of sophistication and physical underpinning. In this talk I shall confront the results obtained when the same constraints are imposed to models of...

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 the statistical inference techniques...