Equation of state and strangeness in neutron stars - role of hyperon-nuclear three-body forces -

Weise, W.

doi:10.1051/epjconf/202227106003

Cited by 3 publications

(2 citation statements)

References 35 publications

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“…(2) Y N and Y Y interactions are the most basic elements of the dynamics of hyper-nuclei [3,4]. (3) Strange baryons may play critical roles in dense nuclear matter that can be realized in compact stars in the universe [5].…”

Section: Introductionmentioning

confidence: 99%

“…For such quantum numbers, the totally symmetric [6] orbital state is forbidden and therefore we expect a strong short-range repulsion induced by the Pauli principle. Such channels include BB ′ (S, I) = N ∆(1, 1), N ∆(2, 2), ∆∆(2, 3), ∆∆(3, 2), (∆Σ + ∆Σ * )(2, 5 2 ), ∆Σ * (3, 3 2 ), ∆Σ * (3, 5 2 ), and so on. On the other hand, many combinations of quantum numbers, particularly with lower spins, appear both in the [33] and [51] SU (6) sf representations.…”

Section: Introductionmentioning

confidence: 99%

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Spin-Flavor SU(6) Symmetry for Baryon-Baryon Interactions

Oka¹

2023

Preprint

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Short-range parts of the baryon-baryon (BB) interactions are analyzed from the spin-flavor SU (6) sf ⊃ SU (3) f × SU (2)s symmetry viewpoint. Due to the Pauli principle of quarks, the symmetry structure of the wave functions is restricted at short distances. Consequently, the BB states with the same spin-flavor quantum numbers may be reduced into one or a few spin-flavor states. Such reduction causes repulsion and/or suppression of transitions at short distances. We show that the observed suppression of the ΞN → ΛΛ conversion can be explained following the above argument. It is also applied to the suppression of the ΣN to ΛN conversion in the spin 1 and isospin 1/2 channel. Furthermore, the effects of the color-magnetic interaction (CMI), which prefers flavor antisymmetric states, to the Pauli-allowed states are discussed.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Spin-Flavor SU(6) Symmetry for Baryon-Baryon Interactions

Oka¹

2023

Preprint

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Sound in a bubbly hybrid neutron star

Kerbikov,

Lukashov

2024

Phys. Rev. D

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Increasingly precise astrophysical observations of the last decade in combination with intense theoretical studies allow for drawing a conclusion about potential quark matter presence in neutron stars’ interiors. Quark matter may form the neutron star inner core or be immersed in the form of bubbles, or droplets. We consider the second scenario and demonstrate that even a small fraction of quark matter bubbles can lead to a high nonlinearity of the sound wave. Below the bubble resonant frequency the sound speed is lower than the ambient value. At the resonance it sharply grows. The peak is constrained by viscous dissipation. Above the resonance the speed exceeds the pure neutron star matter value. The dispersion equation for the bubbly neutron star compressibility is derived. Published by the American Physical Society 2024

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Hyperon–nucleon interaction in chiral effective field theory at next-to-next-to-leading order

et al. 2023

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A hyperon–nucleon potential for the strangeness $$S=-1$$ S = - 1 sector ($$\varLambda N$$ Λ N , $$\varSigma N$$ Σ N ) up to third order in the chiral expansion is presented. SU(3) flavor symmetry is imposed for constructing the interaction, however, the explicit SU(3) symmetry breaking by the physical masses of the pseudoscalar mesons and in the leading-order contact terms is taken into account. A novel regularization scheme is employed which has already been successfully used in studies of the nucleon–nucleon interaction within chiral effective field theory up to high orders. An excellent description of the low-energy $$\varLambda p$$ Λ p , $$\varSigma ^- p$$ Σ - p and $$\varSigma ^+ p$$ Σ + p scattering data is achieved. New data from J-PARC on angular distributions for the $$\varSigma N$$ Σ N channels are analyzed. Results for the hypertriton and $$A=4$$ A = 4 hyper-nuclear separation energies are presented. An uncertainty estimate for the chiral expansion is performed for selected hyperon–nucleon observables.

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Equation of state and strangeness in neutron stars - role of hyperon-nuclear three-body forces -

Cited by 3 publications

References 35 publications

Spin-Flavor SU(6) Symmetry for Baryon-Baryon Interactions

Spin-Flavor SU(6) Symmetry for Baryon-Baryon Interactions

Sound in a bubbly hybrid neutron star

Hyperon–nucleon interaction in chiral effective field theory at next-to-next-to-leading order

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