Asymmetric nuclear matter based on chiral two- and three-nucleon interactions

Drischler, C.; Hebeler, K.; Schwenk, A.

doi:10.1103/physrevc.93.054314

Cited by 174 publications

(269 citation statements)

References 58 publications

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“…Cai & Chen (2014) have argued, based on heavy-ion flow data analyzed by Danielewicz et al (2002) and the existence of 2 M e neutron stars, that −494 MeV<Q 0 <−10 MeV. This range is consistent with that suggested by the neutron matter calculations of Drischler et al (2016b), −450 MeV<Q 0 <−50 MeV. Fitting the energies of the giant monopole resonance, Farine et al (1997) argue that −1200 MeV<Q 0 <−200 MeV, which is also consistent with these other results.…”

Section: The Minimal Constraint On the Symmetry Energysupporting

confidence: 71%

“…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. Since both experimental data and theoretical neutron matter calculations indicate that K sym <0, it follows that K 0 >K n >K n,0 .…”

Section: The Minimal Constraint On the Symmetry Energymentioning

confidence: 99%

“…calculations of Drischler et al (2016b) give −750 MeV<Q n < −250 MeV. From these parameter ranges and Equation (22), K n =K 0 is a conservative (least exclusionary) choice for the bound.…”

Section: The Minimal Constraint On the Symmetry Energymentioning

confidence: 99%

“…Most theoretical calculations of the potential contribution to the symmetry energy also find only small corrections beyond the quadratic term (Carbone et al 2014;Wellenhofer et al 2016). Recent calculations of neutron-rich matter (Drischler et al 2016b) have shown that up to densities approaching u∼1.5 the quadratic assumption is accurate to better than 1 MeV in the symmetry energy per particle for all values of x. However, note that the kinetic contributions to quartic and higher-order terms vary as u 2/3 and potential contributions vary with higher powers of u.…”

Section: E U X E U S U X S U Xmentioning

confidence: 99%

“…The values of the saturation parameters are E 0 =−15.9±0.4 MeV, n 0 = 0.164±0.007 fm −3 (Drischler et al 2016b), and K 0 =240± 20 MeV (Shlomo et al 2006;Piekarewicz 2010) or K 0 =230± 40 MeV (Khan et al 2012). 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.…”

Section: The Minimal Constraint On the Symmetry Energymentioning

confidence: 99%

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

Tews¹,

Lattimer²,

Ohnishi³

et al. 2017

ApJ

295

213

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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.

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Section: The Minimal Constraint On the Symmetry Energysupporting

confidence: 71%

Section: The Minimal Constraint On the Symmetry Energymentioning

confidence: 99%

Section: The Minimal Constraint On the Symmetry Energymentioning

confidence: 99%

Section: E U X E U S U X S U Xmentioning

confidence: 99%

Section: The Minimal Constraint On the Symmetry Energymentioning

confidence: 99%

See 3 more Smart Citations

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

Tews¹,

Lattimer²,

Ohnishi³

et al. 2017

ApJ

295

213

View full text Add to dashboard Cite

show abstract

Nuclear Equation of State for Compact Stars and Supernovae

Burgio

Fantina

2018

Astrophysics and Space Science Library

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The equation of state (EoS) of hot and dense matter is a fundamental input to describe static and dynamical properties of neutron stars, core-collapse supernovae and binary compact-star mergers. We review the current status of the EoS for compact objects, that have been studied with both ab-initio many-body approaches and phenomenological models. We limit ourselves to the description of EoSs with purely nucleonic degrees of freedom, disregarding the appearance of strange baryonic matter and/or quark matter. We compare the theoretical predictions with different data coming from both nuclear physics experiments and astrophysical observations. Combining the complementary information thus obtained greatly enriches our insight into the dense nuclear matter properties. Current challenges in the description of the EoS are also discussed, mainly focusing on the model dependence of the constraints extracted from either experimental or observational data, the lack of a consistent and rigorous many-body treatment at zero and finite temperature of the matter encountered in compact stars (e.g. problem of cluster formation and extension of the EoS to very high temperatures), the role of nucleonic three-body forces, and the dependence of the direct URCA processes on the EoS.

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Properties of Neutron Star Crust with Improved Nuclear Physics: Impact of Chiral EFT Interactions and Experimental Nuclear Masses

et al. 2021

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A compressible liquid-drop approach adjusted to uniform matter many-body calculations based on chiral EFT interactions and to the experimental nuclear masses is used to investigate the neutron star crust properties. Eight chiral EFT hamiltonians and a representative phenomenological force (SLy4) are confronted. We show that some properties of the crust, e.g. clusters mass, charge, and asymmetry, are mostly determined by symmetric matter properties close to saturation density and are therefore mainly constrained by experimental nuclear masses, while other properties, e.g., energy per particle, pressure, sound speed, are mostly influenced by low-density predictions in neutron matter, where chiral EFT and phenomenological forces substantially differ.

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Asymmetric nuclear matter based on chiral two- and three-nucleon interactions

Cited by 174 publications

References 58 publications

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

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

Nuclear Equation of State for Compact Stars and Supernovae

Properties of Neutron Star Crust with Improved Nuclear Physics: Impact of Chiral EFT Interactions and Experimental Nuclear Masses

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