Onset of hyperon formation in neutron star matter from Brueckner theory

Baldo, M.; Burgio, G. F.; Schulze, H.-J.

doi:10.1103/physrevc.58.3688

Cited by 169 publications

(224 citation statements)

References 52 publications

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“…[ 8]. We have extended the BHF approach in a fully microscopic and self-consistent way, in order to describe nuclear matter containing also hyperons [ 9]. We have found rather low hyperon onset densities of about 2 to 3 times normal nuclear matter density for the appearance of the Σ − and Λ hyperons.…”

Section: Eos Of Nuclear Mattermentioning

confidence: 99%

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The hadron-quark phase transition in neutron stars

Burgio¹

2005

Nuclear Physics A

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We study the hadron-quark phase transition in the interior of neutron stars (NS). For the hadronic sector, we use a microscopic equation of state (EOS) involving nucleons and hyperons derived within the Brueckner-Hartree-Fock approach. For the quark sector, we employ the MIT bag model, as well as the Nambu-Jona-Lasinio (NJL) and the Color Dielectric (CD) models, and find that the NS maximum masses lie in the interval between 1.5 and 1.8 solar masses.

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Section: Eos Of Nuclear Mattermentioning

confidence: 99%

“…The inclusion of hyperons produces an EOS which is much softer than the purely nucleonic case. As a consequence, the maximum mass for neutron stars turns out to be less than 1.3 solar masses [ 9], which is below the observational limit of 1.44 solar masses [ 11].…”

Section: Eos Of Nuclear Mattermentioning

confidence: 99%

The hadron-quark phase transition in neutron stars

Burgio¹

2005

Nuclear Physics A

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“…Thus momentum dependence of the potential is neglected, which is reasonable for the Σ − and Λ potentials because of their weak momentum dependence, as suggested from recent microscopic calculations [50,51]. It should be reminded, however, that it is not a good approximation for the nuclear potentials where the potential depths at zero momentum are deeper than the value at the Fermi momentum.…”

Section: Potential Contributionmentioning

confidence: 99%

“…However, hyperons (Λ, Ξ − , Σ − · · ·) may appear in neutron-star matter. Since the early suggestion of hyperon-mixing in neutron stars [40,41], the possible existence of hyperonic matter, where hyperons are mixed as well as neutrons, protons, and leptons in the ground state of neutron-star matter, has been discussed by several authors [42][43][44][45][46][47][48][49][50][51][52][53][54][55][56].…”

Section: Introductionmentioning

confidence: 99%

“…It has been shown that hyperons appear at a baryon number density ρ B = 2 ∼ 3ρ 0 based on the relativistic meanfield (RMF) models [45][46][47][48], relativistic Hartree-Fock methods [49], the nonrelativistic reaction matrix theory [50,51], the nonrelativistic effective baryon-baryon potential models [52][53][54], etc. [55,56] The hyperonic matter is also relevant to static and dynamic properties of neutron stars [57,58] and thermal evolution of neutron stars via rapid cooling [59].…”

Section: Introductionmentioning

confidence: 99%

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Kaonic modes in hyperonic matter and p-wave kaon condensation

Muto

2002

Nuclear Physics A

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Kaon excitations (kaonic modes) are investigated in hyperonic matter, where hyperons (Λ, Σ − , Ξ − ) are mixed in the ground state of neutron-star matter. P -wave kaon-baryon interactions as well as the s-wave interactions are taken into account within chiral effective Lagrangian, and the nonrelativistic effective baryon-baryon interactions are incorporated. When the hyperon Λ is more abundant than the proton at high baryon density, a proton-particle-Λ-hole mode, which has the K + quantum number, appears in addition to other particle-hole modes with the K − quantum number. It is shown that the system becomes unstable with respect to a spontaneous creation of a pair of the particle-hole modes with K + and K − quantum numbers, stemming from the p-wave kaon-baryon interaction. The onset density of this p-wave kaon condensation may be lower than that of the s-wave K − condensation.

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Strangeness content of neutron stars with strong Σ^–‐hyperon repulsion

et al. 2014

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A new constraint on the equation of state and composition of the matter on neutron stars has been provided by the measurement of the mass 2.01 ± 0.04 M for PSR J0348 +0432. In this contribution we investigate the role of many-body correlations in the maximum mass of neutron stars using the effective relativistic QHD-model with parameterized couplings. The complete expression of our QHD interaction Lagrangian exhausts the whole fundamental baryon octet (n, p, Σ − , Σ 0 , Σ + , Λ, Ξ − , Ξ 0 ) and includes many-body forces simulated by nonlinear self-couplings and meson-meson interaction terms involving scalar-isoscalar (σ, σ * ), vector-isoscalar (ω, φ), vector-isovector ( ), and scalar-isovector (δ). We study the behavior of the asymmetry parameter, which describes the relative neutron excess in the system as well as the behavior of the strangeness asymmetry parameter, which specifies the strangeness content in the system and is strictly connected with the appearance of a particular hyperon species in the extreme case where the Σ − experiences such a strong repulsion that it does not appear at all in nuclear matter.

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Onset of hyperon formation in neutron star matter from Brueckner theory

Cited by 169 publications

References 52 publications

The hadron-quark phase transition in neutron stars

The hadron-quark phase transition in neutron stars

Kaonic modes in hyperonic matter and p-wave kaon condensation

Strangeness content of neutron stars with strong Σ^–‐hyperon repulsion

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Onset of hyperon formation in neutron star matter from Brueckner theory

Cited by 169 publications

References 52 publications

The hadron-quark phase transition in neutron stars

The hadron-quark phase transition in neutron stars

Kaonic modes in hyperonic matter and p-wave kaon condensation

Strangeness content of neutron stars with strong Σ–‐hyperon repulsion

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Product

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Strangeness content of neutron stars with strong Σ^–‐hyperon repulsion