Constraints on the nuclear equation of state from nuclear masses and radii in a Thomas-Fermi meta-modeling approach

Chatterjee, Debarati; Gulminelli, F.; Raduta, Ad. R.; Margueron, J.

doi:10.1103/physrevc.96.065805

Cited by 32 publications

(55 citation statements)

References 56 publications

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“…Table I of Ref. [143]). So, as expected, this strategy is equivalent to a direct fit of the parameters of the nuclear effective interaction as it is commonly done in EDFs.…”

Section: Edfsmentioning

confidence: 99%

Nuclear equation of state from ground and collective excited state properties of nuclei

Roca-Maza

Paar

2018

Progress in Particle and Nuclear Physics

195

110

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This contribution reviews the present status on the available constraints to the nuclear equation of state (EoS) around saturation density from nuclear structure calculations on ground and collective excited state properties of atomic nuclei. It concentrates on predictions based on self-consistent mean-field calculations, which can be considered as an approximate realization of an exact energy density functional (EDF). EDFs are derived from effective interactions commonly fitted to nuclear masses, charge radii and, in many cases, also to pseudo-data such as nuclear matter properties. Although in a model dependent way, EDFs constitute nowadays a unique tool to reliably and consistently access bulk ground state and collective excited state properties of atomic nuclei along the nuclear chart as well as the EoS. For comparison, some emphasis is also given to the results obtained with the so called ab initio approaches that aim at describing the nuclear EoS based on interactions fitted to few-body data only. Bridging the existent gap between these two frameworks will be essential since it may allow to improve our understanding on the diverse phenomenology observed in nuclei. Examples on observations from astrophysical objects and processes sensitive to the nuclear EoS are also briefly discussed. As the main conclusion, the isospin dependence of the nuclear EoS around saturation density and, to a lesser extent, the nuclear matter incompressibility remain to be accurately determined. Experimental and theoretical efforts in finding and measuring observables specially sensitive to the EoS properties are of paramount importance, not only for low-energy nuclear physics but also for nuclear astrophysics applications. 7 The expression introduced by Migdal in Ref. [43] neglected the term in a AS . 8 From a macroscopic picture it would correspond to an isotropic compression. 9 From a macroscopic picture it would correspond to a non-isotropic compression. 15

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“…Table I of Ref. [143]). So, as expected, this strategy is equivalent to a direct fit of the parameters of the nuclear effective interaction as it is commonly done in EDFs.…”

Section: Edfsmentioning

confidence: 99%

Nuclear equation of state from ground and collective excited state properties of nuclei

Roca-Maza

Paar

2018

Progress in Particle and Nuclear Physics

195

110

View full text Add to dashboard Cite

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“…e average values of the empirical parameters and their uncertainties are estimated based on experimental and theoretical nuclear physics constraints. In follow-up studies meta-modeling was used to study the e ects of uncertainties in the empirical parameters on NS properties [9], nite size e ects in the description of nuclear masses and radii of ground state nuclei [10], and to compute correlations between empirical parameters from known constraints [11].…”

Section: Introductionmentioning

confidence: 99%

Equation of state effects in the core collapse of a 20−M⊙ star

Schneider

Roberts

Ott³

et al. 2019

Phys. Rev. C

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Uncertainties in our knowledge of the properties of dense ma er near and above nuclear saturation density are among the main sources of variations in multi-messenger signatures predicted for core-collapse supernovae (CCSNe) and the properties of neutron stars (NSs). We construct 97 new nite-temperature equations of state (EOSs) of dense ma er that obey current experimental, observational, and theoretical constraints and discuss how systematic variations in the EOS parameters a ect the properties of cold nonrotating NSs and the core collapse of a 20-M progenitor star. e core collapse of the 20-M progenitor star is simulated in spherical symmetry using the general-relativistic radiation-hydrodynamics code GR1D where neutrino interactions are computed for each EOS using the NuLib library. We conclude that the e ective mass of nucleons at densities above nuclear saturation density is the largest source of uncertainty in the CCSN neutrino signal and dynamics even though it plays a subdominant role in most properties of cold NS ma er. Meanwhile, changes in other observables a ect the properties of cold NSs, while having li le e ect in CCSNe. To strengthen our conclusions, we perform six octant three-dimensional CCSN simulations varying the e ective mass of nucleons at nuclear saturation density. We conclude that neutrino heating and, thus, the likelihood of explosion is signi cantly increased for EOSs where the e ective mass of nucleons at nuclear saturation density is large.PACS numbers: 21.65. Mn,26.50.+x,26.60.Kp

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“…With increasing magnetic fields, it departs strongly from the TOV solution. As was already pointed out in [57,96], this is mainly due to the pure magnetic field contribution and not that of the effect of the magnetised EoS. The other main difference is that for the isotropic TOV calculations, the pure field contribution is a constant, whereas that of the full numerical computation is a profile, generated via a current function.…”

Section: Effect On Radius and Crust-core Propertiesmentioning

confidence: 90%

“…Employing this method, mass-radius relations of magnetised neutron stars were calculated for full numerical solutions. The unified EoSs for describing both the crust and the core were constructed within the same "Meta-Model" scheme [94,96,97,98]. The magnetic field dependence is only included within the core EoS, assuming a non-magnetised crust.…”

Section: Effect On Radius and Crust-core Propertiesmentioning

confidence: 99%

Structure of ultra-magnetised neutron stars

Chatterjee,

Novak,

Oertel

2021

Preprint

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In this review we discuss self-consistent methods to calculate the global structure of strongly magnetised neutron stars within the general-relativistic framework. We outline why solutions in spherical symmetry cannot be applied to strongly magnetised compact stars, and elaborate on a consistent formalism to compute rotating magnetised neutron star models. We also discuss an application of the above full numerical solution for studying the influence of strong magnetic fields on the radius and crust thickness of magnetars. The above technique is also applied to construct a "universal" magnetic field profile inside the neutron star, that may be useful for studies in nuclear physics. The methodology developed here is particularly useful to interpret multi-messenger astrophysical data of strongly magnetised neutron stars.

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Constraints on the nuclear equation of state from nuclear masses and radii in a Thomas-Fermi meta-modeling approach

Cited by 32 publications

References 56 publications

Nuclear equation of state from ground and collective excited state properties of nuclei

Nuclear equation of state from ground and collective excited state properties of nuclei

Equation of state effects in the core collapse of a 20−M⊙ star

Structure of ultra-magnetised neutron stars

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