Hyperon-nucleon single-particle potentials with low-momentum interactions

Đapo, Haris; Schaefer, B.; Wambach, J.

doi:10.1140/epja/i2008-10542-5

Cited by 15 publications

(18 citation statements)

References 35 publications

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“…The results are in reasonable agreement between the different approaches, but large uncertainties remain owing to the not very well known fundamental interaction (see, e.g., the discussion in Ref. [54]). It has been shown, too, that the inclusion of hyperonic three-body forces (Y NN) do not strongly change the results [55].…”

Section: A Hyperonic Datasupporting

confidence: 68%

“…Nevertheless, differences have to be noticed, especially for T = 1 MeV. This could be explained by the fact that in their four-species EOS, the authors assume 54 Mn to be the representative heavy nucleus, while in LS EOS the mean nucleus varies as a function of density to satisfy the energy minimization condition. This affects the relative abundances and the macroscopic properties of the system.…”

Section: A Characteristics Of the Lattimer And Swesty Equation Of Statementioning

confidence: 99%

“…4 of Ref. [32], where the authors plot the results obtained by the original LS EOS and by their four-species (neutrons, protons, α-particles, and 54 Mn as representative heavy nucleus) EOS derived assuming nuclear statistical equilibrium (NSE). The results obtained by our tables and by the NSE EOS introduced in Ref.…”

Section: A Characteristics Of the Lattimer And Swesty Equation Of Statementioning

confidence: 99%

“…In addition to the traditional G-matrix calculations [51][52][53], a Hartree-Fock calculation based on a V lowk potential has recently been presented in Ref. [54]. The results are in reasonable agreement between the different approaches, but large uncertainties remain owing to the not very well known fundamental interaction (see, e.g., the discussion in Ref.…”

Section: A Hyperonic Datamentioning

confidence: 99%

“…The observation of a 4 He bound state [57] requires an attractive potential, whereas the analysis of the (π − , K + ) inclusive spectra [56,58] indicate a repulsive potential, possibly up to a value of V N = 100 MeV at saturation density. Theoretical many-body calculations show a large variety of results, too (see, e.g., [54]), ranging from slightly less attractive values as the N case to strongly repulsive values of up to several tens of MeV. Balberg and Gal [47] adopt two different versions: one with an attractive potential of the same form as for the and another local potential form giving rise to a repulsive potential.…”

Section: A Hyperonic Datamentioning

confidence: 99%

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Extended equation of state for core-collapse simulations

2012

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In stellar core-collapse events matter is heated and compressed to densities above nuclear matter saturation density. For progenitor stars with masses above roughly 25M , which eventually form black holes, the temperatures and densities reached during the collapse are so high that a traditional description in terms of electrons, nuclei, and nucleons is no longer adequate. We present here an improved equation of state containing, in addition, pions and hyperons. They become abundant in the high-temperature-and-density regime. We study the different constraints on such an equation of state, coming from both hyperonic data and observations of neutron-star properties. To test the zero-temperature versions of our new equations of state, we perform numerical simulations of the collapse of a neutron star to a black hole. We discuss the influence of the additional particles on the thermodynamic properties within the hot versions of the equation of state and we show that, in regimes relevant to core-collapse and black-hole formation, the effects of pions and hyperons on pressure, internal energy, and sound speed are not negligible.

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Section: A Hyperonic Datasupporting

confidence: 68%

Section: A Characteristics Of the Lattimer And Swesty Equation Of Statementioning

confidence: 99%

Section: A Characteristics Of the Lattimer And Swesty Equation Of Statementioning

confidence: 99%

Section: A Hyperonic Datamentioning

confidence: 99%

Section: A Hyperonic Datamentioning

confidence: 99%

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Extended equation of state for core-collapse simulations

2012

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Nuclear Data Sheets for A = 60

Browne

Tuli

2013

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116

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Strangeness in Compact Stars

Schaffner-Bielich

2010

Nuclear Physics A

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We discuss the impact of strange hadrons, in particular hyperons, on the gross features of compact stars and on core-collapse supernovae. Hyperons are likely to be the first exotic species which appears around twice normal nuclear matter density in the core of neutron stars. Their presence largely influences the mass-radius relation of compact stars, the maximum mass, the cooling of neutron stars, the stability with regard to the emission of gravitational waves from rotationpowered neutron stars and the possible early onset of the QCD phase transition in core-collapse supernovae. We outline also the constraints from subthreshold kaon production in heavy-ion collisions for the maximum possible mass of neutron stars.

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Hyperon-nucleon single-particle potentials with low-momentum interactions

Cited by 15 publications

References 35 publications

Extended equation of state for core-collapse simulations

Extended equation of state for core-collapse simulations

Nuclear Data Sheets for A = 60

Strangeness in Compact Stars

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