<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>Λ</mml:mi><mml:mi>Λ</mml:mi></mml:mrow></mml:math>bond energy from the Nijmegen potentials

Vidaña, Isaac; Ramos, À.; Polls, A.

doi:10.1103/physrevc.70.024306

Cited by 50 publications

(46 citation statements)

References 42 publications

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“…Taking U ( ) (n s ) = −5 MeV [62] (see also the discussion in [61]), the value of g σ * can then be fixed. This is, however, only an indicative effect that should be taken with care, since the hyperon-meson couplings should be constrained by fitting the experimental binding energy of hyperons in hypernuclei [63]. This subject requires further investigation.…”

Section: A Rmf Unified Eosmentioning

confidence: 99%

Neutron star radii and crusts: Uncertainties and unified equations of state

Fortin¹,

Providência²,

Raduta³

et al. 2016

Phys. Rev. C

318

377

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The uncertainties in neutron star radii and crust properties due to our limited knowledge of the equation of state are quantitatively analyzed. We first demonstrate the importance of a unified microscopic description for the different baryonic densities of the star. If the pressure functional is obtained matching a crust and a core equation of state based on models with different properties at nuclear matter saturation, the uncertainties can be as large as ∼30 % for the crust thickness and 4% for the radius. Necessary conditions for causal and thermodynamically consistent matchings between the core and the crust are formulated and their consequences examined. A large set of unified equations of state for purely nucleonic matter is obtained based on twenty-four Skyrme interactions and nine relativistic mean-field nuclear parametrizations. In addition, for relativistic models fifteen equations of state including a transition to hyperonic matter at high density are presented. All these equations of state have in common the property of describing a 2M star and of being causal within stable neutron stars. Spans of ∼3 and ∼4 km are obtained for the radius of, respectively, 1.0M and 2.0M stars. Applying a set of nine further constraints from experiment and ab initio calculations the uncertainty is reduced to ∼1 and 2 km, respectively. These residual uncertainties reflect lack of constraints at large densities and insufficient information on the density dependence of the equation of state near the nuclear matter saturation point. The most important parameter to be constrained is shown to be the symmetry energy slope L. Indeed, this parameter exhibits a linear correlation with the stellar radius, which is particularly clear for small mass stars around 1.0M . The other equation-of-state parameters do not show clear correlations with the radius, within the present uncertainties. Potential constraints on L, the neutron star radius, and the equation of state from observations of thermal states of neutron stars are also discussed. The unified equations of state are made available in the Supplemental Materials and via the CompOSE database.

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Section: A Rmf Unified Eosmentioning

confidence: 99%

Neutron star radii and crusts: Uncertainties and unified equations of state

Fortin¹,

Providência²,

Raduta³

et al. 2016

Phys. Rev. C

318

377

View full text Add to dashboard Cite

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“…All of the EOSs are adjusted to satisfy the following four conditions within their respective uncertain ranges: (1) reproducing the PNM EOS at sub-saturation densities predicted by the latest state-of-the-art microscopic nuclear many-body theories [28,[70][71][72][73][74][75]; (2) [12] and references therein); (4) passing through the terrestrial constraints on the EOS of SNM between 2ρ 0 and 4.5ρ 0 [2] and giving a maximum mass of neutron stars of about 2M ⊙ assuming they are made of only the npeµ matter without considering other degrees of freedom or invoking any exotic mechanism [3,79].…”

Section: Constrained Eos Of Neutron-rich Nuclear Mattermentioning

confidence: 99%

Constraining the high-density behavior of the nuclear symmetry energy with the tidal polarizability of neutron stars

et al. 2013

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Using a set of model equations of state satisfying the latest constraints from both terrestrial nuclear experiments and astrophysical observations as well as state-of-the-art nuclear many-body calculations of the pure neutron matter equation of state, the tidal polarizability of canonical neutron stars in coalescing binaries is found to be a very sensitive probe of the high-density behavior of nuclear symmetry energy which is among the most uncertain properties of dense neutron-rich nucleonic matter. Moreover, it changes less than ±10% by varying various properties of symmetric nuclear matter and symmetry energy around the saturation density within their respective ranges of remaining uncertainty.PACS numbers: 26.60. Kp, 21.65.Mn, 04.40.Dg, 97.60.Jd, 95.85.Sz

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“…This reduction increases with density up to a factor of 0.3 at ρ = 0.8f m −3 . The above result is common to most Bruckner calculations [8,11,9,10]. More pronounced is the queching due to three-body force.…”

Section: Results and Conclusionmentioning

confidence: 61%

“…On the other hand, non-relativistic approaches [7][8][9][10] do not support such a transition except Hartree-Fock calculations with phenomenological Skyrme-like forces (for a review see Ref. [4]).…”

Section: Introductionmentioning

confidence: 99%

Spin-Polarized States of Nuclear Matter

Zuo

Lombardo

Shen

2003

Commun. Theor. Phys.

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The equations of state of spin-polarized nuclear matter and pure neutron matter are studied in the framework of the Brueckner-Hartree-Fock theory including a three-body force. The energy per nucleon E A (δ) calculated in the full range of spin polarization δ = ρ ↑ −ρ ↓ ρ for symmetric nuclear matter and pure neutron matter fulfills a parabolic law. In both cases the spin-symmetry energy is calculated as a function of the baryonic density along with the related quantities such as the magnetic susceptibility and the Landau parameter G 0 . The main effect of the three-body force is to strongly reduce the degenerate Fermi gas magnetic susceptibility even more than the value with only two body force. The EOS is monotonically increasing with the density for all spin-aligned configurations studied here so that no any signature is found for a spontaneous transition to a ferromagnetic state.

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ΛΛbond energy from the Nijmegen potentials

Cited by 50 publications

References 42 publications

Neutron star radii and crusts: Uncertainties and unified equations of state

Neutron star radii and crusts: Uncertainties and unified equations of state

Constraining the high-density behavior of the nuclear symmetry energy with the tidal polarizability of neutron stars

Spin-Polarized States of Nuclear Matter

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