NuSym23, XIth International Symposium on Nuclear Symmetry Energy

In this contribution we consider hybrid compact stars located in the third branch of the corresponding mass-radius diagram. We introduce a set of equations of state whose symmetry energy parameters vary. These are described by multi-polytropes and by a RMF model with several isovector mesons, fulfilling laboratory constraints. We find correlations between tidal deformabilities, stellar radii...

Neutrinos play a crucial role in neutron star physics, from their birth in a core-collapse supernovae where neutrinos dictate the dynamics of the explosion, to the merger by determining the matter composition in the ejecta for heavy element nucleosynthesis. They are also key actors of cooling in (proto-)neutron stars and of the thermal relaxation of accreting neutron stars. Identifying...

The understanding of neutron star properties from fundamental physics is still far from being completed. One of the reasons is that the theory for strong force, QCD, does not apply simply to neutron star matter at a few times the nuclear saturation density. At low density, chiral effective field theory is fixing a limit which can be incorporated in the description of the crust of neutron...

Core-collapse supernovae are one of the most fascinating phenomena in astrophysics but the explosion mechanism is not clearly understood yet because of their intricacies. I will give an overview about the role of nuclear equation-of-state (EOS) and nuclei in supernovae. I will also discuss key nuclei and their key information to be investigated for further supernova study, and introduce recent...

Using a meta model for nuclear Equation of State (EOS) with its parameters constrained by astrophysical observations and terrestrial nuclear experiments, we examine effects of nuclear EOS especially its symmetry energy \esym term on the speed of sound squared $C^2_s(\rho)$ and the critical density $\rho_t$ where $C^2_s(\rho_t)$ vanishes (indicating the onset of spinodal decomposition) in both...

I will discuss the equation of state and composition of dense matter with heavy baryons within covariant density functional (CDF) theory. The sensitivity of the results on the structure of compact stars to variation of the slope of symmetry energy and the skewness is demonstrated. The finite temperature equation of state and its implications for multimessenger astrophysics is also discussed

Observed for the first time in 1967 as pulsars, neutron
stars represent the most extreme bodies known in our universe. Relict
of the gravitational collapse and subsequent supernova explosion of a
massive star at the end of his life, they gather a mass of up to twice
that of our sun in a sphere with a radius of about 10 km. Their
phenomenology is very rich and complex. Modelling requires...