Kaon condensation in dense stellar matter

Lee, Chang-Hwan

doi:10.1016/0370-1573(96)00005-1

Cited by 136 publications

(120 citation statements)

References 75 publications

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“…The connection to astrophysics problems, supernovae explosions and neutron stars, is also quite evident [6][7][8][9]. The isovector channel has been introduced through a coupling to the charged vector ρ-meson.…”

Section: Introductionmentioning

confidence: 99%

Asymmetric nuclear matter: The role of the isovector scalar channel

et al. 2002

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We try to single out some qualitative new effects of the coupling to the δ-isovector-scalar meson introduced in a minimal way in a phenomenological hadronic field theory. Results for the equation of state (EOS) and the phase diagram of asymmetric nuclear matter (AN M ) are discussed. We stress the consistency of the δ-coupling introduction in a relativistic approach.New contributions to the slope and curvature of the symmetry energy and the neutron-proton effective mass splitting appear particularly interesting.A more repulsive EOS for neutron matter at high baryon densities is expected.Effects on new critical properties of warm AN M , mixing of mechanical and chemical instabilities and isospin distillation, are also presented. The δ influence is mostly on the isovectorlike collective response.The results are largely analytical and this makes the physical meaning quite transparent. Implications for nuclear structure properties of drip-line nuclei and for reaction dynamics with Radioactive Beams are finally pointed out.

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Section: Introductionmentioning

confidence: 99%

Asymmetric nuclear matter: The role of the isovector scalar channel

et al. 2002

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“…Ever since the pioneering work of Kaplan and Nelson [1,2] on the possibility of kaon condensation in nuclear matter, a huge amount of theoretical effort has been devoted to the study of kaon properties in dense matter, based mostly on the SU(3) chiral perturbation theory [3][4][5][6][7][8][9][10][11][12][13][14][15][16]. Kaons, as Goldstone bosons with strangeness, play a special role in the development of hadron models.…”

Section: Introductionmentioning

confidence: 99%

Kaons in dense matter, kaon production in heavy-ion collisions, and kaon condensation in neutron stars

1997

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The recent past witnesses the growing interdependence between the physics of hadrons, the physics of relativistic heavy-ion collisions, and the physics of compact objects in astrophysics. A notable example is the kaon which plays special roles in all the three fields. In this paper, we first review the various theoretical investigations of kaon properties in nuclear medium, focusing on possible uncertainties in each model. We then present a detailed transport model study of kaon production in heavy-ion collisions at SIS energies. We shall discuss especially the elementary kaon and antikaon production cross sections in hadron-hadron interactions, that represent one of the most serious uncertainties in the transport model study of particle production in heavy-ion collisions. The main purpose of such a study is to constrain kaon in-medium properties from the heavy-ion data. This can provide useful guidances for the development of theoretical models of the kaon in medium. In the last part of the paper, we apply the kaon in-medium properties extracted from heavy-ion data to the study of neutron star properties. Based on a conventional equation of state of nuclear matter that can be considered as one of the best constrained by available experimental data on finite nuclei, we find that the maximum mass of neutron stars is about 2M⊙, which is reduced to about 1.5M⊙ once kaon condensation as constrained by heavy-ion data is introduced.pacs: 25.75. Dw, 97.60.Jd, 26.60.+c, 24.10.Lx

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“…In particular, an increasing E sym (ρ) leads to a relatively more proton-rich neutron star whereas a decreasing one would make the neutron star a pure neutron matter at high densities. Consequently, the chemical composition and cooling mechanisms of protoneutron stars [8,9], critical densities for Kaon condensations in dense stellar matter [10,11], mass-radius correlations [12,13] as well as the possibility of a mixed quark-hadron phase [14] in neutron stars will all be rather different. The fundamental cause of the extremely uncertain HD behaviour of E sym (ρ) is the complete lack of terrestrial laboratory data to constrain directly the model predictions.…”

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confidence: 99%

High density behaviour of nuclear symmetry energy and high energy heavy-ion collisions

2002

Nuclear Physics A

131

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High energy heavy-ion collisions are proposed as a novel means to constrain stringently the high density (HD) behaviour of nuclear symmetry energy. Within an isospin-dependent hadronic transport model, it is shown for the first time that the isospin asymmetry of the HD nuclear matter formed in high energy heavyion collisions is uniquely determined by the HD behaviour of nuclear symmetry energy. Experimental signatures in two sensitive probes, i.e., π − to π + ratio and neutron-proton differential collective flow, are also investigated.

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Kaon condensation in dense stellar matter

Cited by 136 publications

References 75 publications

Asymmetric nuclear matter: The role of the isovector scalar channel

Asymmetric nuclear matter: The role of the isovector scalar channel

Kaons in dense matter, kaon production in heavy-ion collisions, and kaon condensation in neutron stars

High density behaviour of nuclear symmetry energy and high energy heavy-ion collisions

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