Towards understanding astrophysical effects of nuclear symmetry energy
Determining the Equation of State (EOS) of dense neutron-rich nuclear matter is a shared
goal of both nuclear physics and astrophysics. Except possible phase transitions, the density …
goal of both nuclear physics and astrophysics. Except possible phase transitions, the density …
Implications of PREX-2 on the equation of state of neutron-rich matter
Laboratory experiments sensitive to the equation of state of neutron rich matter in the vicinity
of nuclear saturation density provide the first rung in a “density ladder” that connects …
of nuclear saturation density provide the first rung in a “density ladder” that connects …
Equation of state for dense nucleonic matter from metamodeling. I. Foundational aspects
J Margueron, R Hoffmann Casali, F Gulminelli - Physical Review C, 2018 - APS
Metamodeling for the nucleonic equation of state (EOS), inspired from a Taylor expansion
around the saturation density of symmetric nuclear matter, is proposed and parameterized in …
around the saturation density of symmetric nuclear matter, is proposed and parameterized in …
A short walk through the physics of neutron stars
I Vidana - The European Physical Journal Plus, 2018 - epjplus.epj.org
In this work we shortly review several aspects of the physics of neutron stars. After the
introduction we present a brief historical overview of the idea of neutron stars as well as of …
introduction we present a brief historical overview of the idea of neutron stars as well as of …
Exploring robust correlations between fermionic dark matter model parameters and neutron star properties: A two-fluid perspective
We investigate the probable existence of dark matter in the interior of neutron stars. Despite
the current state of knowledge, the observational properties of neutron stars have not …
the current state of knowledge, the observational properties of neutron stars have not …
Constraining the symmetry energy at subsaturation densities using isotope binding energy difference and neutron skin thickness
Z Zhang, LW Chen - Physics Letters B, 2013 - Elsevier
We show that the neutron skin thickness Δ rnp of heavy nuclei is uniquely fixed by the
symmetry energy density slope L (ρ) at a subsaturation cross density ρ c≈ 0.11 fm− 3 rather …
symmetry energy density slope L (ρ) at a subsaturation cross density ρ c≈ 0.11 fm− 3 rather …
Bayesian inference of the symmetry energy and the neutron skin in and from CREX and PREX-2
Z Zhang, LW Chen - Physical Review C, 2023 - APS
Using the recent model-independent determination of the charge-weak form factor
difference Δ F CW in Ca 48 and Pb 208 by the CREX and PREX-2 collaborations together …
difference Δ F CW in Ca 48 and Pb 208 by the CREX and PREX-2 collaborations together …
Core-crust transition in neutron stars: Predictivity of density developments
The possibility to draw links between the isospin properties of nuclei and the structure of
compact stars is a stimulating perspective. In order to pursue this objective on a sound basis …
compact stars is a stimulating perspective. In order to pursue this objective on a sound basis …
Symmetry energy, its density slope, and neutron-proton effective mass splitting at normal density extracted from global nucleon optical potentials
Based on the Hugenholtz–Van Hove theorem, it is shown that both the symmetry energy E
sym (ρ) and its density slope L (ρ) at normal density ρ 0 are completely determined by the …
sym (ρ) and its density slope L (ρ) at normal density ρ 0 are completely determined by the …
Pulsar glitches: The crust may be enough
Background: Pulsar glitches—the sudden spin-up in the rotational frequency of a neutron
star—suggest the existence of an angular-momentum reservoir confined to the inner crust of …
star—suggest the existence of an angular-momentum reservoir confined to the inner crust of …