Hyperon-hyperon interactions with the Nijmegen ESC08 model

Rijken, Th. A.; Schulze, H.‐J.

doi:10.1140/epja/i2016-16021-6

Cited by 45 publications

(38 citation statements)

References 64 publications

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“…Such a higher order quark interaction can be motivated by the existence of vector boson couplings of fourth order. Such boson self-coupling terms occur in the nonlinear Walecka model, but they are also important for explaining a sufficient repulsion in the high-energy nucleon-nucleon scattering by multi-pomeron exchange [231].…”

Section: Stiffnessmentioning

confidence: 99%

Phases of Dense Matter in Compact Stars

Blaschke

Chamel

2018

The Physics and Astrophysics of Neutron Stars

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Formed in the aftermath of gravitational core-collapse supernova explosions, neutron stars are unique cosmic laboratories for probing the properties of matter under extreme conditions that cannot be reproduced in terrestrial laboratories. The interior of a neutron star, endowed with the highest magnetic fields known and with densities spanning about ten orders of magnitude from the surface to the centre, is predicted to exhibit various phases of dense strongly interacting matter, whose physics is reviewed in this chapter. The outer layers of a neutron star consist of a solid nuclear crust, permeated by a neutron ocean in its densest region, possibly on top of a nuclear "pasta" mantle. The properties of these layers and of the homogeneous isospin asymmetric nuclear matter beneath constituting the outer core may still be constrained by terrestrial experiments. The inner core of highly degenerate, strongly interacting matter poses a few puzzles and questions which are reviewed here together with perspectives for their resolution. Consequences of the dense-matter phases for observables such the neutron-star mass-radius relationship and the prospects to uncover their structure with modern observational programmes are touched upon.

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Section: Stiffnessmentioning

confidence: 99%

Phases of Dense Matter in Compact Stars

Blaschke

Chamel

2018

The Physics and Astrophysics of Neutron Stars

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“…In many microscopic calculations [23,24,25,26,27,28], this decrease is so large that the maximum mass obtained is not compatible with the current largest measured neutron star masses of ∼ 2M ⊙ [29,30,31,32]. Most of these microscopic calculations have been performed using NN, NNN and NY interactions and, in some cases, also the YY one [23,28]. Just a few full consistent calculations including YTBF are present in literature.…”

Section: Introductionmentioning

confidence: 99%

Impact of chiral hyperonic three-body forces on neutron stars

Logoteta¹,

Vidaña²,

Bombaci³

2019

Eur. Phys. J. A

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We study the effect of the nucleon-nucleon-lambda (NNΛ) three-body force on neutron stars. In particular, we consider the NNΛ force recently derived by the Jülich-Bonn-Munich group within the framework of chiral effective field theory at next-to-next-to-leading order. This force, together with realistic nucleon-nucleon, nucleon-nucleon-nucleon and nucleon-hyperon interactions, is used to calculate the equation of state and the structure of neutron stars within the many-body non-relativistic Brueckner-Hartree-Fock approach. Our results show that the inclusion of the NNΛ force leads to an equation of state stiff enough such that the resulting neutron star maximum mass is compatible with the largest currently measured (∼ 2 M ⊙ ) neutron star masses. Using a perturbative many-body approach we calculate also the separation energy of the Λ in some hypernuclei finding that the agreement with the experimental data improves for the heavier ones when the effect of the NNΛ force is taken into account.

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“…We mention that the BHF theory was also extended in order to include hyperons, which might appear in the core of a NS, but the corresponding EOSs turn out to be very soft, with too low NS maximum masses, M < 1.7 M (M ≈ 2 × 10 33 g) [40,41,42], well below the current observational limit. Nevertheless, such EOSs could be realized in the so-called two-families scenario in which the heaviest stars are interpreted as quark stars, whereas the lighter and smaller stars are hadronic stars [43,44,45,46].…”

Section: Equations Of Statementioning

confidence: 92%

Constraints from the GW170817 merger event on thenuclear matter equation of state

Burgio¹,

Figura²,

Schulze³

et al. 2019

Proceedings of XIII Quark Confinement and the Hadron Spectrum — PoS(Confinement2018)

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The detection of the GW170817 neutron star merger event has incited an intense research activity towards the understanding of the nuclear matter equation of state. In this paper we compare in particular the pressure-density relation obtained from heavy-ion collisions with the analysis of the NS merger event. Moreover, we present recent calculations of neutron star's moment of inertia and tidal deformability using various microscopic equations of state for nuclear and hybrid star configurations, and confirm several universal relations. We also discuss the recent constraints for the NS radii determined by GW170817, and find compatible radii between 12 and 13 kilometers, thus identifying the suitable equations of state.

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Hyperon-hyperon interactions with the Nijmegen ESC08 model

Cited by 45 publications

References 64 publications

Phases of Dense Matter in Compact Stars

Phases of Dense Matter in Compact Stars

Impact of chiral hyperonic three-body forces on neutron stars

Constraints from the GW170817 merger event on thenuclear matter equation of state

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