Constraints on the equation of state of cold dense matter from nuclear physics and astrophysics

Fantina, Anthea; Chamel, Nicolas; Goriely, Stéphane

doi:10.1051/epjconf/20146607005

Cited by 15 publications

(14 citation statements)

References 23 publications

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“…The first two rows refer to pressure of SNM. They are obtained from analysis of directed and elliptic flow [37] and kaon production [38,39] in heavy ion collisions (HIC). The next four rows correspond to PNM.…”

Section: A Fitting Of Macrodatamentioning

confidence: 99%

Nucleon effective mass and its isovector splitting

et al. 2018

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Using an energy density functional (EDF) based on the thermodynamic Gibbs-Duhem relation, found equivalent to the standard Skyrme EDF for infinite nuclear matter, it is demonstrated that the parameters of this EDF are not uniquely determined from the fit of the empirical and theoretical data related to nuclear matter. This prevents an unambiguous determination of the nucleon effective mass ( m * 0 m ) and its isovector splitting (∆m * 0 ). Complementary information from dipole polarizability of atomic nuclei helps in removing this ambiguity and plausible values of m * 0 m and ∆m * 0 can be arrived at. Presently considered fit data on infinite nuclear matter and dipole polarizability of finite nuclei yield m * 0 m = 0.68 ± 0.04 and ∆m * 0 = (−0.20 ± 0.09)δ. This EDF is consistent with the constraint on the maximum mass of the neutron star.

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Section: A Fitting Of Macrodatamentioning

confidence: 99%

Nucleon effective mass and its isovector splitting

et al. 2018

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“…The violet shades show the calculated uncertainties. The shaded red and orange regions in the upper panel display the 'experimental' EoS for SNM extracted from collective flow data [74] and from data for Kaon production [75,76], respectively. The shaded green region in the EoS of PNM is a theoretically obtained result where the density dependence of symmetry energy is taken to be soft.…”

Section: B Supranormal Density and Neutron Starsmentioning

confidence: 99%

Limiting symmetry energy elements from empirical evidence

Agrawal

Samaddar

et al. 2017

Int. J. Mod. Phys. E

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In the framework of an equation of state (EoS) constructed from a momentum and density-dependent finite-range two-body effective interaction, the quantitative magnitudes of the different symmetry elements of infinite nuclear matter are explored. The parameters of this interaction are determined from well-accepted characteristic constants associated with homogeneous nuclear matter. The symmetry energy coefficient $a_2$, its density slope $L_0$, the symmetry incompressibility $K_\delta $ as well as the density dependent incompressibility $K(\rho )$ evaluated with this EoS are seen to be in good harmony with those obtained from other diverse perspectives. The higher order symmetry energy coefficients $a_4,~a_6$ etc are seen to be not very significant in the domain of densities relevant to finite nuclei, but gradually build up at supra-normal densities. The analysis carried with a Skyrme-inspired energy density functional obtained with the same input values for the empirical bulk data associated with nuclear matter yields nearly the same results.Comment: Accepted in "International journal of Modern Physics E

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“…Recently a couple of massive neutron stars, with masses of 2.01 ± 0.04 M ⊙ and 1.97 ± 0.04 M ⊙ , were discovered by Antoniadis et al [6] and Demorest et al [7], respectively, which triggered multiple papers proposing various models of cold, dense, degenerate nuclear matter that can support stable configurations of self-gravitating fluid with those observed large mass values [8][9][10][11][12]. Specifically, superconductivity and superfluidity have been hypothesized in the past to exist in neutron stars to explain certain observational effects (see, e.g., Ref.…”

Section: Introductionmentioning

confidence: 99%

Observational constraints on spinning, relativistic Bose-Einstein condensate stars

2015

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Bose-Einstein condensates (BECs) have been proposed as candidate states of matter for the interior of neutron stars. Specifically, Chavanis and Harko obtained the mass-radius relation for a BEC star and proposed that the recently discovered neutron stars with masses around 2M⊙ are BEC stars. They employed a barotropic equation of state (EOS), with one free parameter, that was first found by Colpi, Wasserman, and Shapiro (CSW), to describe them and derive stable equilibrium configurations of spinning BEC stars in General Relativity. In this work we show that while it is true that BECs allow for compact object masses as heavy as the heaviest observed ones, such stars cannot simultaneously have radii that are small enough to be consistent with the latest observations, in spite of the flexibility available in the EOS in the form of the free parameter. In fact, our conclusion applies to any spinning relativistic boson star that obeys the CSW EOS.

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Constraints on the equation of state of cold dense matter from nuclear physics and astrophysics

Cited by 15 publications

References 23 publications

Nucleon effective mass and its isovector splitting

Nucleon effective mass and its isovector splitting

Limiting symmetry energy elements from empirical evidence

Observational constraints on spinning, relativistic Bose-Einstein condensate stars

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