A redefinition of the symmetry energy expansion that incorporates finite strangeness consistent with SU(3) flavor symmetry and remains valid beyond typical neutron-star central densities.
Interplay between the symmetry energy and the strangeness content of neutron stars
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
abstract
The effect of the density dependence of the nucleonic equation of state and the hyperon meson couplings on the star properties, including strangeness content, mass and radius, are studied within a relativistic mean field formalism. It is shown that there is still lacking information on the nucleonic equation of state at supra-saturation densities and on the hyperon interactions in nuclear matter that will allow a clear answer to the question whether the mass of the pulsar J1614-2230 could rule out exotic degrees of freedom from the interior of compact stars. We show that some star properties are affected in a similar way by the density dependence of the symmetry energy and the hyperon content of the star. To disentangle these two effects it is essential to have a good knowledge of the equation of state at supra-saturation densities. A linear correlation between the radius and the strangeness content of a star with a fixed mass is obtained.
verdicts
UNVERDICTED 3representative citing papers
Bayesian modeling with informed priors reduces uncertainties in neutron-star crust shear properties, predicting torsional mode frequencies of 20-50 Hz compatible with observations.
In baryon- and neutron-rich matter the isospin symmetry energy drops substantially once a small fraction of antinucleons is included, with intrinsically larger isospin splitting for antinucleon potentials than for nucleon potentials.
citing papers explorer
-
Symmetry Energy Expansion with Strange Dense Matter
A redefinition of the symmetry energy expansion that incorporates finite strangeness consistent with SU(3) flavor symmetry and remains valid beyond typical neutron-star central densities.
-
Bayesian analysis of the shear modulus in the neutron-star crust
Bayesian modeling with informed priors reduces uncertainties in neutron-star crust shear properties, predicting torsional mode frequencies of 20-50 Hz compatible with observations.
-
Symmetry energy of baryon- and neutron-rich nuclear matter
In baryon- and neutron-rich matter the isospin symmetry energy drops substantially once a small fraction of antinucleons is included, with intrinsically larger isospin splitting for antinucleon potentials than for nucleon potentials.