Kaon condensation and lambda–nucleon loop in the relativistic mean-field approach

Maruyama, Tomoyuki; Muto, Takumi; Tatsumi, Toshitaka; Tsushima, K.; Thomas, A. W.

doi:10.1016/j.nuclphysa.2005.06.008

Cited by 19 publications

(15 citation statements)

References 123 publications

(161 reference statements)

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“…Here we follow a simple and conventional treatment of this term used in the kaon condensate studies and write it as (see Ref. [5,18] and also the last term in Eq. (2)):…”

Section: Free Space Amplitudes In Cut-off Methodsmentioning

confidence: 99%

Dmesons in nuclear matter: ADNcoupled-channel equations approach

2006

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A set of coupled two-body scattering equations is solved for the DN system embedded in an isosymmetric nuclear matter. The in-medium behavior of charmed D mesons, (D + , D 0 ), is investigated from the self-consistent solution within this scheme. The effective meson-baryon Lagrangian in charm quantum number one sector, the key ingredient in the present study, is adopted from a recent model by Hofmann and Lutz that has aimed at combining the charmed meson degree of freedom in a consistent manner with chiral unitary models. After a critical examination, the original model is modified in several important aspects, such as the method of regularization, to be more consistent and practical for our objective. The resultant interaction is used to reproduce the position and width of the s-wave c (2593) resonance in the isospin zero DN channel. In the isospin one channel, it generates a rather wide resonance at ∼2770 MeV. The corresponding in-medium solution is then sought by incorporating Pauli blocking and the D-and π -meson dressing self-consistently. At normal nuclear matter density, the resultant c (2593) is found to stay narrow and shifted at a lower energy, whereas the I = 1 resonance is lowered in position as well and broadened considerably.

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“…Here we follow a simple and conventional treatment of this term used in the kaon condensate studies and write it as (see Ref. [5,18] and also the last term in Eq. (2)):…”

Section: Free Space Amplitudes In Cut-off Methodsmentioning

confidence: 99%

Dmesons in nuclear matter: ADNcoupled-channel equations approach

2006

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“…The T-W vector interaction is supplemented by a scalar-isoscalar attraction, which turns out to be important in kaon condensate studies (see Ref. [16,29]). The s-wave projection of this interaction is equal to…”

Section: A Coupled Meson-baryon Channels In Free Spacementioning

confidence: 99%

Open charm in nuclear matter at finite temperature

2008

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We study the properties of open-charm mesons (D andD) in nuclear matter at finite temperature within a self-consistent coupled-channel approach. The meson-baryon interactions are adopted from a type of broken SU(4) s-wave Tomozawa-Weinberg term supplemented by an attractive scalar-isoscalar interaction. The inmedium solution at finite temperature incorporates Pauli blocking effects, mean-field binding on all the baryons involved, and π and open-charm meson self-energies in a self-consistent manner. In the DN sector, the c and c resonances, generated dynamically at 2593 and 2770 MeV in free space, remain close to their free-space position while acquiring a remarkable width due to the thermal smearing of Pauli blocking as well as from the nuclear matter density effects. As a result, the D meson spectral density shows a single pronounced peak for energies close to the D meson free-space mass that broadens with increasing matter density with an extended tail particularly toward lower energies. TheD potential shows a moderate repulsive behavior coming from the dominant I = 1 contribution of theDN interaction. The low-density theorem is, however, not a good approximation for theD self-energy in spite of the absence of resonance-hole contributions close to threshold in this case. We speculate the possibility of D-mesic nuclei as well as discuss some consequences for the J / suppression in heavy-ion collisions, in particular for the future CBM experiment at FAIR.

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“…(9)(10)(11)(12) to compute the energy density of nuclear matter in the Hartree-Fock approximation. The ground state of the system is specified by a set of Fermi levels, {k F (f ), f = p, n...}, and their corresponding baryonic densities {n f } with n B = f n f .…”

Section: Energy Density In the Hartree Fock Approximationmentioning

confidence: 99%

“…At sufficiently high density, nuclear matter will most likely be composed not just of nucleons and leptons but also strange baryons and boson condensates [9,10,11,12]. More importantly, it is unlikely that these particles will maintain their identity as confined entities of quarks, but the interaction between overlapping quark bags will result in partial or full deconfinement [13,14].…”

Section: Introductionmentioning

confidence: 99%

Cold uniform matter and neutron stars in the quark–meson-coupling model

et al. 2007

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A new density dependent effective baryon-baryon interaction has been recently derived from the quark-meson-coupling (QMC) model, offering impressive results in application to finite nuclei and dense baryon matter. This self-consistent, relativistic quark-level approach is used to construct the Equation of State (EoS) and to calculate key properties of high density matter and cold, slowly rotating neutron stars. The results include predictions for the maximum mass of neutron star models, together with the corresponding radius and central density, as well the properties of neutron stars with mass of order 1.4 M ⊙ . The cooling mechanism allowed by the QMC EoS is explored and the parameters relevant to slow rotation, namely the moment of inertia and the period of rotation investigated. The results of the calculation, which are found to be in good agreement with available observational data, are compared with the predictions of more traditional EoS, based on the A18+δv+UIX * and modified Reid soft core potentials, the Skyrme SkM * interaction and a relativistic mean field (RMF) models for a hybrid stars including quark matter. The QMC EoS provides cold neutron star models with maximum mass 1.9-2.1 M ⊙ , with central density less than 6 times nuclear saturation density (n 0 = 0.16 fm −3 ) and offers Preprint submitted to Elsevier Science 17 February 2017a consistent description of the stellar mass up to this density limit. In contrast with other models, QMC predicts no hyperon contribution at densities lower than 3n 0 , for matter in β-equilibrium. At higher densities, Ξ −,0 and Λ hyperons are present. The absence of lighter Σ ±,0 hyperons is understood as a consequence of antisymmetrisation, together with the implementation of the color hyperfine interaction in the response of the quark bag to the nuclear scalar field.

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Kaon condensation and lambda–nucleon loop in the relativistic mean-field approach

Cited by 19 publications

References 123 publications

Dmesons in nuclear matter: ADNcoupled-channel equations approach

Dmesons in nuclear matter: ADNcoupled-channel equations approach

Open charm in nuclear matter at finite temperature

Cold uniform matter and neutron stars in the quark–meson-coupling model

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