Exact versus Taylor-expanded energy density in the study of the neutron star crust–core transition

Routray, T. R.; Viñas, X.; Basu, Debabrata; Pattnaik, Subhaswaraj; Centelles, M.; Robledo, L. M.; Behera, Banarji

doi:10.1088/0954-3899/43/10/105101

Cited by 25 publications

(64 citation statements)

References 73 publications

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“…The extracted value of the crustal fraction of total moment of inertia, ∆I I > 1.4%, from the observed glitches in vela-pulsar allows us to limit the radius of vela pulsar to R ≥3.69+3.44M/M ⊙ . The calculation also suggest, as can be seen from table 2, that the crustal fraction of total moment of inertia can be as large as 3.6% due to crustal entrainment which is in agreement with Simple Effective Interaction [20] and Density Dependent M3Y interaction [33].…”

Section: Discussionsupporting

confidence: 80%

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Crustal moment of inertia of glitching pulsars with the KDE0v1 Skyrme interaction

et al. 2017

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Abstract. The mass, radius and crustal fraction of moment of inertia in neutron stars are calculated using β-equilibrated nuclear matter obtained from Skyrme effective interaction. The transition density, pressure and proton fraction at the inner edge separating the liquid core from the solid crust of the neutron stars are determined from the thermodynamic stability conditions using the KDE0v1 set. The neutron star masses obtained by solving the Tolman-Oppenheimer-Volkoff equations using neutron star matter obtained from this set is able to describe highly massive compact stars ∼2M ⊙ . The crustal fraction of the moment of inertia can be extracted from studying pulsar glitches. This fraction is highly dependent on the core-crust transition pressure and corresponding density. These results for pressure and density at core-crust transition together with the observed minimum crustal fraction of the total moment of inertia provide a limit for the radius of the Vela pulsar: R ≥ 3.69+3.44 M/M ⊙ . Present calculations suggest that the crustal fraction of the total moment of inertia can be at most 3.6% due to crustal entrainment caused by Bragg reflection of unbound neutrons by lattice ions.

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Section: Discussionsupporting

confidence: 80%

“…(3) [19,9,20] by setting V thermal = 0, plays an important role in crustal fraction of moment of inertia. The crustal fraction of moment of inertia is important for the explanation of the observed glitches in the pulsars [20].…”

Section: Formalismmentioning

confidence: 99%

Crustal moment of inertia of glitching pulsars with the KDE0v1 Skyrme interaction

et al. 2017

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“…The main features discussed above are in general agreement with those found in other recent studies, see, e.g., refs. [201,202,203,204,205,206,208,209,214,215,216,217,218,219,220,221,223], while quantitatively, the predicted core-crust transition densities and pressures are still model and interactions dependent for the reasons we mentioned above. Among all the available studies in the literature, it is very instructive to mention the rather systematic work in refs.…”

Section: Effects Of High-order Isospin and Density Dependences Of Thementioning

confidence: 95%

Towards understanding astrophysical effects of nuclear symmetry energy

et al. 2019

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Determining the Equation of State (EOS) of dense neutron-rich nuclear matter is a shared goal of both nuclear physics and astrophysics. Except possible phase transitions, the density dependence of nuclear symmetry Esym(ρ) is the most uncertain part of the EOS of neutron-rich nucleonic matter especially at supra-saturation densities. Much progresses have been made in recent years in predicting the symmetry energy and understanding why it is still very uncertain using various microscopic nuclear many-body theories and phenomenological models. Simultaneously, significant progresses have also been made in probing the symmetry energy in both terrestrial nuclear laboratories and astrophysical observatories. In light of the GW170817 event as well as ongoing or planned nuclear experiments and astrophysical observations probing the EOS of dense neutron-rich matter, we review recent progresses and identify new challenges to the best knowledge we have on several selected topics critical for understanding astrophysical effects of the nuclear symmetry energy.PACS. 2 6.60.Kp Contents B.A Li, P.G. Krastev, D.H. Wen and N.B. Zhang: Astrophysical Effects of Nuclear Symmetry Energy 5.2.2 Predicted correlation strength between the radii of neutron stars and the symmetry energy from low to high densities 32 5.2.3 Predicted effects of the symmetry energy on the tidal deformability of neutron stars 33 5.3 Post-GW170817 analyses of tidal deformability and radii of neutron stars as well as constraints on the nuclear EOS and symmetry energy . . . 34 5.3.

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“…To avoid this problem, the crust-core phase transition has been also studied from the core side. There are mainly three well-established methods, namely the thermodynamical method [17], the dynamical method [18,19] and the random phase approximation (for more details, see [12,13] and references therein). These methods are based on the onset of violation of the stability conditions of the homogeneous core against small-amplitude density fluctuations, which indicates the formation of inhomogeneous nuclear structures, i.e.…”

Section: The Crust-core Phase Transitionmentioning

confidence: 99%

“…Although large scale calculations of the inner crust could provide such densities, there are not many calculations of this type available in the literature. Therefore, it is easier to go in the opposite direction and examine the stability conditions of the core against small-amplitude density fluctuations using the so-called thermodynamical and dynamical methods (see [12,13] for references and more details). The paper is organized as follows.…”

Section: Introductionmentioning

confidence: 99%

Pasta-phase Transitions in the Inner Crust of Neutron Stars

Viñas¹,

Gonzalez-Boquera²,

Sharma³

et al. 2017

Acta Phys. Pol. B Proc. Suppl.

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We perform calculations of nuclear pasta phases in the inner crust of neutron stars with the Thomas-Fermi method and the Compressible Liquid Drop Model using the Barcelona-Catania-Paris-Madrid (BCPM) energy density functional and several Skyrme forces. We compare the crust-core transition density estimated from the crust side with the predictions obtained from the core by using the thermodynamical and dynamical methods. Finally, the correlation between the crust-core transition density and the slope of the symmetry energy at saturation is briefly analyzed.

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Exact versus Taylor-expanded energy density in the study of the neutron star crust–core transition

Cited by 25 publications

References 73 publications

Crustal moment of inertia of glitching pulsars with the KDE0v1 Skyrme interaction

Crustal moment of inertia of glitching pulsars with the KDE0v1 Skyrme interaction

Towards understanding astrophysical effects of nuclear symmetry energy

Pasta-phase Transitions in the Inner Crust of Neutron Stars

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