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

Fattoyev, F. J.; Carvajal, J.; Newton, William; Li, Bao-An

doi:10.1103/physrevc.87.015806

Cited by 119 publications

(123 citation statements)

References 93 publications

(133 reference statements)

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“…However such a large error is not enough to constrain the various nuclear models. In addition the large determined neutron skin (compared to previous experimental measurements) creates a new open problem concerning the correlation between the nuclear equation of state of nuclear matter and the density functional theory in finite nuclei (see for a pertinent discussion in [34,57]). …”

Section: Resultsmentioning

confidence: 99%

“…Actually there is a variety of neutron star properties which are sensitive to SE, that is the maximum mass value and the corresponding radius, the onset of the direct Urca process, the crust-core transition density and pressure e.t.c. [2,9] Recently, there is an extended theoretical [10,11,12,13,14,15,16,17,18,19,20,21,22,23,24,25,26,27,28,29,30,31,32,33,34,57,36,37,38,39,40,41,42,43,44,45,46,47,48,49,50,51,52,53,54,55,56,…”

Section: Introductionmentioning

confidence: 99%

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Effects of the symmetry energy on the isovector properties of neutron-rich nuclei within a Thomas-Fermi approach

Papazoglou

Moustakidis

2014

Phys. Rev. C

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We employ a variational method, in the framework of the Thomas-Fermi approximation, to study the effect of the symmetry energy on the neutron skin thickness and the symmetry energy coefficients of various neutron rich nuclei. We concentrate our interest on 208 Pb, 124 Sn, 90 Zr, and 48 Ca, although the method can be applied in the totality of medium and heavy neutron rich nuclei. Our approach has the advantage that the isospin asymmetry function α(r), which is the key quantity to calculate isovector properties of various nuclei, is directly related with the symmetry energy as a consequence of the variational principle. Moreover, the Coulomb interaction is included in a self-consistent way and its effects can be separated easily from the nucleon-nucleon interaction. We confirm, both qualitatively and quantitatively, the strong dependence of the symmetry energy on the various isovector properties for the relevant nuclei, using possible constraints between the slope and the value of the symmetry energy at the saturation density. PACS number(s): 21.65. Ef, 21.65.Mn, 21.65.Cd, 21.10.Gv

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Effects of the symmetry energy on the isovector properties of neutron-rich nuclei within a Thomas-Fermi approach

Papazoglou

Moustakidis

2014

Phys. Rev. C

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“…We calculate the crust and core EOSs and the transition density consistently using the widely used Skyrme nuclear matter model. As the baseline Skyrme parameterization, we choose the SkIUFSU model used in previous work (Fattoyev et al 2012(Fattoyev et al , 2013, which shares the same saturation symmetric nuclear matter (SNM) properties as the relativistic mean field (RMF) IUFSU model , has isovector nuclear matter parameters obtained from a fit to state-of-the-art PNM calculations, and describes well the binding energies and charge radii of doubly magic nuclei (Fattoyev et al 2012). Two parameters in the Skyrme model are purely isovector -they can be systematically adjusted to vary the symmetry energy J and its density slope L at saturation density while leaving SNM properties unchanged (Chen et al 2009).…”

Section: Nuclear Matter Parameters and Crust And Core Equations Of Statementioning

confidence: 99%

Efficacy of crustal superfluid neutrons in pulsar glitch models

Hooker¹,

Newton²,

Li³

2015

Monthly Notices of the Royal Astronomical Society

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In order to assess the ability of purely crust-driven glitch models to match the observed glitch activity in the Vela pulsar, we conduct a systematic analysis of the dependence of the fractional moment of inertia of the inner crustal neutrons on the stiffness of the nuclear symmetry energy at saturation density L. We take into account both crustal entrainment and the fact that only a fraction Y g of the core neutrons may couple to the crust on the glitch-rise timescale. We use a set of consistently-generated crust and core compositions and equations-of-state which are fit to results of lowdensity pure neutron matter calculations. When entrainment is included at the level suggested by recent microscopic calculations and the core is fully coupled to the crust, the model is only able to account for the Vela glitch activity for a 1.4M star if the equation of state is particularly stiff L > 100 MeV. However, an uncertainty of about 10% in the crust-core transition density and pressure allows for the Vela glitch activity to be marginally accounted for in the range L ≈ 30 − 60MeV consistent with a range of experimental results. Alternatively, only a small amount of core neutrons need be involved. If less than 50% of the core neutrons are coupled to the crust during the glitch, we can also account for the Vela glitch activity using crustal neutrons alone for EOSs consistent with the inferred range of L. We also explore the possibility of Vela being a high-mass neutron star, and of crustal entrainment being reduced or enhanced relative to its currently predicted values.

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“…For our base models we use two recently established EOSs for neutron-rich nucleonic matter within the IU-FSU Relativistic Mean Field (RMF) and the SkIU-FSU Skyrme-Hartree-Fork (SHF) models [20][21][22]. The slope of the symmetry energy at saturation for these models is L = 47.2 MeV.…”

Section: The Equation Of State Of Nuclear Mattermentioning

confidence: 99%

Shedding Light on the EOS-Gravity Degeneracy and Constraining the Nuclear Symmetry Energy from the Gravitational Binding Energy of Neutron Stars

Fattoyev

et al. 2016

EPJ Web of Conferences

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Abstract. A thorough understanding of properties of neutron stars requires both a reliable knowledge of the equation of state (EOS) of super-dense nuclear matter and the strong-field gravity theories simultaneously. To provide information that may help break this EOS-gravity degeneracy, we investigate effects of nuclear symmetry energy on the gravitational binding energy of neutron stars within GR and the scalar-tensor subset of alternative gravity models. We focus on effects of the slope L of nuclear symmetry energy at saturation density and the high-density behavior of nuclear symmetry energy. We find that the variation of either the density slope L or the high-density behavior of nuclear symmetry energy leads to large changes in the binding energy of neutron stars. The difference in predictions using the GR and the scalar-tensor theory appears only for massive neutron stars, and even then is significantly smaller than the difference resulting from variations in the symmetry energy.

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

Cited by 119 publications

References 93 publications

Effects of the symmetry energy on the isovector properties of neutron-rich nuclei within a Thomas-Fermi approach

Effects of the symmetry energy on the isovector properties of neutron-rich nuclei within a Thomas-Fermi approach

Efficacy of crustal superfluid neutrons in pulsar glitch models

Shedding Light on the EOS-Gravity Degeneracy and Constraining the Nuclear Symmetry Energy from the Gravitational Binding Energy of Neutron Stars

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