Critical properties of calibrated relativistic mean-field models for the transition to warm, nonhomogeneous nuclear and stellar matter

@inproceedings{Boukari2021CriticalPO,
  title={Critical properties of calibrated relativistic mean-field models for the transition to warm, nonhomogeneous nuclear and stellar matter},
  author={O. Boukari and Helena Pais and Sofija Anti'c and Constancca Providencia},
  year={2021}
}
The critical properties for the transition to warm, asymmetric, non-homogeneous nuclear matter are analysed within a thermodynamical spinodal approach for a set of well calibrated equations of state. It is shown that even though different equations of state are constrained by the same experimental, theoretical and observational data, and the properties of symmetric nuclear matter are similar within the models, the properties of very asymmetric nuclear matter, such as the one found inside of… Expand

References

SHOWING 1-10 OF 26 REFERENCES
Neutron star equations of state with optical potential constraint
Abstract Nuclear matter and neutron stars are studied in the framework of an extended relativistic mean-field (RMF) model with higher-order derivative and density dependent couplings of nucleons toExpand
The Equation of State for the Nucleonic and Hyperonic Core of Neutron Stars
Abstract We re-examine the equation of state for the nucleonic and hyperonic inner core of neutron stars that satisfies the 2M⊙ observations as well as the recent determinations of stellar radiiExpand
Cooling of Small and Massive Hyperonic Stars
We perform cooling simulations for isolated neutron stars using recently developed equations of state for their core. The equations of state are obtained from new parametrizations of the FSU2Expand
Relativistic mean-field theory for unstable nuclei with non-linear σ and ω terms
Abstract We search for a new parameter set for the description of stable as well as unstable nuclei in the wide mass range within the relativistic mean-field theory. We include a non-linear ωExpand
A statistical model for a complete supernova equation of state
Abstract A statistical model for the equation of state and the composition of supernova matter is presented. It consists of an ensemble of nuclei and interacting nucleons in nuclear statisticalExpand
The State of Matter in Simulations of Core-Collapse supernovae—Reflections and Recent Developments
Abstract In this review article, we discuss selected developments regarding the role of the equation of state in simulations of core-collapse supernovae. There are no first-principle calculations ofExpand
Equation of State for Nucleonic and Hyperonic Neutron Stars with Mass and Radius Constraints
We obtain a new equation of state for the nucleonic and hyperonic inner core of neutron stars that fulfills the 2$M_{\odot}$ observations as well as the recent determinations of stellar radii belowExpand
Influence of density dependence of symmetry energy in hot and dense matter for supernova simulations
We study the influence of density-dependent symmetry energy at high densities in simulations of core-collapse supernovae, black hole formation and proto-neutron star cooling by extending theExpand
A two-solar-mass neutron star measured using Shapiro delay
TLDR
Radio timing observations of the binary millisecond pulsar J1614-2230 that show a strong Shapiro delay signature are presented and the pulsar mass is calculated to be (1.97 ± 0.04)M⊙, which rules out almost all currently proposed hyperon or boson condensate equations of state. Expand
Effects of Symmetry Energy on the Equation of State for Simulations of Core-collapse Supernovae and Neutron-star Mergers
We construct a new equation of state (EOS) for numerical simulations of core-collapse supernovae and neutron-star mergers based on an extended relativistic mean-field model with a small symmetryExpand
...
1
2
3
...