Equation of state for dense nucleonic matter from metamodeling. I. Foundational aspects

Margueron, J.; Casali, Rudiney Hoffmann; Gulminelli, F.

doi:10.1103/physrevc.97.025805

Cited by 238 publications

(397 citation statements)

References 169 publications

(195 reference statements)

Supporting

Mentioning

371

Contrasting

Order By: Relevance

“…Concerning the range for K 0 sym , for instance, it is worth to mention that it is similar to the one suggested in Ref. [57], in which the authors proposed a metamodeling approach to treat the EoS for dense nuclear mat- Figure 4: Results from Gogny and MDI models for the dimensionless moment of inertiaĪ as a function of (a) dimensionless tidal deformability, and (b) neutron star mass. Dashed blue curve: fitting curve obtained in Ref.…”

Section: Still Regarding the Values Shown Inmentioning

confidence: 68%

See 1 more Smart Citation

GW170817 constraints analyzed with Gogny forces and momentum-dependent interactions

et al. 2020

View full text Add to dashboard Cite

A set of equations of state obtained from finite-range Gogny forces and momentum-dependent interactions is used to investigate the recent observation of gravitational waves from the binary neutron star merger GW170817 event. For this set of interactions, we have calculated the neutron star tidal deformabilities (related to the second Love number), the mass-radius diagram, and the moment of inertia (I). The I-Love relation has been verified. We also have found strong correlations among the tidal deformability of the canonical neutron star, its radius, and the derivatives of the nuclear symmetry energy at the saturation density. Most of the obtained results are located within the constraints of the tidal deformabilities extracted from the GW170817 detection.

show abstract

Section: Still Regarding the Values Shown Inmentioning

confidence: 68%

“…[18] (L 0 = 58.7 ± 28.1 MeV), and in Ref. [57] (L 0 = 60 ± 15 MeV). We note, however, that some of the considered MDI forces have a slope parameter L 0 above the upper boundary suggested in these references.…”

Section: Gogny Forces and MDI Interactions For Stellar Mattermentioning

confidence: 81%

GW170817 constraints analyzed with Gogny forces and momentum-dependent interactions

et al. 2020

View full text Add to dashboard Cite

show abstract

“…In general, K sym <0 for realistic relativistic mean-field (RMF) and Skyrme forces, i.e., those that have been fit to properties of laboratory nuclei. Realistic microscopic interactions also suggest K sym <0: e.g., N 3 LO chiral EFT calculations (Tews et al 2013) yield K n =119± 101 MeV (Margueron et al 2017). The neutron matter calculations of Drischler et al (2016b) yield −70 MeV>K sym > −240 MeV and 10 MeV<K n <100 MeV.…”

Section: The Minimal Constraint On the Symmetry Energymentioning

confidence: 99%

Symmetry Parameter Constraints from a Lower Bound on Neutron-matter Energy

Tews¹,

Lattimer²,

Ohnishi³

et al. 2017

ApJ

282

211

View full text Add to dashboard Cite

We propose the existence of a lower bound on the energy of pure neutron matter (PNM) on the basis of unitary-gas considerations. We discuss its justification from experimental studies of cold atoms as well as from theoretical studies of neutron matter. We demonstrate that this bound results in limits to the density-dependent symmetry energy, which is the difference between the energies of symmetric nuclear matter and PNM. In particular, this bound leads to a lower limit to the volume symmetry energy parameter S 0 . In addition, for assumed values of S 0 above this minimum, this bound implies both upper and lower limits to the symmetry energy slope parameter L, which describes the lowest-order density dependence of the symmetry energy. A lower bound on neutron-matter incompressibility is also obtained. These bounds are found to be consistent with both recent calculations of the energies of PNM and constraints from nuclear experiments. Our results are significant because several equations of state that are currently used in astrophysical simulations of supernovae and neutron star mergers, as well as in nuclear physics simulations of heavy-ion collisions, have symmetry energy parameters that violate these bounds. Furthermore, below the nuclear saturation density, the bound on neutron-matter energies leads to a lower limit to the density-dependent symmetry energy, which leads to upper limits to the nuclear surface symmetry parameter and the neutron-star crust-core boundary. We also obtain a lower limit to the neutron-skin thicknesses of neutronrich nuclei. Above the nuclear saturation density, the bound on neutron-matter energies also leads to an upper limit to the symmetry energy, with implications for neutron-star cooling via the direct Urca process.

show abstract

“…In the present approach, as discussed in [34], no a-priori correlations exist between the different parameters of the EoS. However, as we will see, imposing experimental and observational constraints will give rise to correlations.…”

Section: Eos Parametrizationmentioning

confidence: 83%

“…The coefficients of low orders are already quite well constrained experimentally [38][39][40][41][42][43], however Q sat , Z sat and K sym , Q sym , Z sym are only poorly known [30,32,36,[44][45][46][47]. The saturation energy E sat and saturation density n sat being rather well constrained, we fix their values throughout this work: E sat = −15.8 MeV (the current estimated value is −15.8 ± 0.3 MeV [34]), and n sat = 0.155 fm −3 .…”

Section: Eos Parametrizationmentioning

confidence: 99%

Empirical constraints on the high-density equation of state from multimessenger observables

et al. 2020

View full text Add to dashboard Cite

We search for possible correlations between neutron star observables and thermodynamic quantities that characterize high density nuclear matter. We generate a set of model-independent equations of state describing stellar matter from a Taylor expansion around saturation density. Each equation of state which is a functional of the nuclear matter parameters is thermodynamically consistent, causal and compatible with astrophysical observations. We find that the neutron star tidal deformability and radius are strongly correlated with the pressure, the energy density and the sound velocity at different densities. Similar correlations are also exhibited by a large set of mean-field models based on non-relativistic and relativistic nuclear energy density functionals. These model independent correlations can be employed to constrain the equation of state at different densities above saturation from measurements of NS properties with multi-messenger observations. In particular, precise constraints on the radius of PSR J0030+0451 thanks to NICER observations would allow to better infer the properties of matter around two times the nuclear saturation density.

show abstract

Equation of state for dense nucleonic matter from metamodeling. I. Foundational aspects

Cited by 238 publications

References 169 publications

GW170817 constraints analyzed with Gogny forces and momentum-dependent interactions

GW170817 constraints analyzed with Gogny forces and momentum-dependent interactions

Symmetry Parameter Constraints from a Lower Bound on Neutron-matter Energy

Empirical constraints on the high-density equation of state from multimessenger observables

Contact Info

Product

Resources

About