Production of a twin single hypernuclei and the Ξ−-nuclear interaction

Aoki, Shigeki; Bahk, S. Y.; Chung, K.S.; Chung, S. H.; Funahashi, H.; Hahn, C.; Hara, T.; Hirata, Shuichi; Hoshino, K.; Ieiri, M.; Ijima, T.; Imai, K.; Itow, Y.; Jin-ya, T.; Kazuno, M.; Kikuchi, Keiji; Kim, C.O.; Kim, D.C.; Kim, J.Y.; Kodama, K.; Maeda, Y.; Masaike, A.; Masuoka, A.; Matsuda, Y.; Nagoshi, C.; Nakamura, Mitsuhiro; Nakanishi, S.; Nakano, Takashi; Nakazawa, Kimitaka; Niwa, K.; Oda, Hirotaka; Ogawa, S.; Oh, S. H.; Okabe, H.; Ozaki, Ryosuke; Park, I.G.; Park, M.S.; Sato, Yoshihiro; Shibuya, H.; Shimizu, Hirohiko M.; Sim, Young-Jae; Song, J.; Sugimoto, M.; Tajima, H.; Takashima, R.; Takéutchi, F.; Tanaka, Kenichi; Tanaka, Ryotaro; Teranaka, M.; Tezuka, I.; Togawa, H.; Ushida, N.; Watanabe, Toru; Yasuda, N.; Yokota, J.; Yoon, C. S.

doi:10.1016/0370-2693(95)00688-h

Cited by 62 publications

(17 citation statements)

References 18 publications

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“…These models describe the normal nuclear properties very well [49,50], while the hypernuclear properties in these models are not satisfactory from a phenomenological point of view. Especially and hyperons are considered to feel repulsive [62] and weakly attractive [63] potentials, but these features are not explained yet. This may be suggesting the importance of other types of meson-hyperon couplings other than the Yukawa coupling or the SU f (3) breaking effects.…”

Section: B Hypernucleimentioning

confidence: 95%

Λhypernuclei and neutron star matter in a chiral SU(3) relativistic mean field model with a logarithmic potential

et al. 2010

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We develop a chiral SU(3) symmetric relativistic mean field model with a logarithmic potential of scalar condensates. Experimental and empirical data of symmetric nuclear matter saturation properties, bulk properties of normal nuclei, and separation energies of single-and double-hypernuclei are well explained. The nuclear matter equation of state (EOS) is found to be softened by σ ζ mixing which comes from determinant interaction. The neutron star matter EOS is further softened by hyperons.

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Section: B Hypernucleimentioning

confidence: 95%

Λhypernuclei and neutron star matter in a chiral SU(3) relativistic mean field model with a logarithmic potential

et al. 2010

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“…Recent developments in hypernuclear physics suggest that hyperon potentials in nuclear matter are repulsive for Σ [20,21,22,23], and weakly attractive for Ξ [24,25,26,27], respectively.…”

Section: Relativistic Mean Field Model With Hyperonsmentioning

confidence: 99%

Tables of hyperonic matter equation of state for core-collapse supernovae

Ishizuka

Ohnishi

Tsubakihara

et al. 2008

J. Phys. G: Nucl. Part. Phys.

155

226

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Abstract. We present sets of equation of state (EOS) of nuclear matter including hyperons using an SU f (3) extended relativistic mean field (RMF) model with a wide coverage of density, temperature, and charge fraction for numerical simulations of core collapse supernovae. Coupling constants of Σ and Ξ hyperons with the σ meson are determined to fit the hyperon potential depths in nuclear matter, U Σ (ρ 0 ) ≃ +30MeV and U Ξ (ρ 0 ) ≃ −15MeV, which are suggested from recent analyses of hyperon production reactions. At low densities, the EOS of uniform matter is connected with the EOS by Shen et al., in which formation of finite nuclei is included in the Thomas-Fermi approximation. In the present EOS, the maximum mass of neutron stars decreases from 2.17M ⊙ (N eµ) to 1.63M ⊙ (N Y eµ) when hyperons are included. In a spherical, adiabatic collapse of a 15M ⊙ star by the hydrodynamics without neutrino transfer, hyperon effects are found to be small, since the temperature and density do not reach the region of hyperon mixture, where the hyperon fraction is above 1 % (T > 40MeV or ρ B > 0.4 fm −3 ).

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“…These are mainly single-Λ hypernuclei; see, e.g., the reviews by Hashimoto and Tamura (2006) and Gal, Hungerford, and Millener (2016). Some events with double-Λ hypernuclei have been detected; see Aoki et al (1991) and Nakazawa (2010). The absence of Σ-bound states, except for an s-wave Σ bound state in 4 Σ He (Nagae et al, 1998), indicates a repulsive ΣN interaction (Bart et al, 1999;Saha et al, 2004;Kohno et al, 2006).…”

Section: Experimental Datamentioning

confidence: 99%

“…The absence of Σ-bound states, except for an s-wave Σ bound state in 4 Σ He (Nagae et al, 1998), indicates a repulsive ΣN interaction (Bart et al, 1999;Saha et al, 2004;Kohno et al, 2006). Only a few events for Ξ hypernuclei have been observed up to now (Aoki et al, 1995;Fukuda et al, 1998;Khaustov et al, 2000). Considerable experimental efforts are underway to improve hypernuclear data; see, e.g., Agnello et al (2012) and Sugimura et al (2014).…”

Section: Experimental Datamentioning

confidence: 99%

Equations of state for supernovae and compact stars

et al. 2017

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A review is given of various theoretical approaches for the equation of state (EoS) of dense matter, relevant for the description of core-collapse supernovae, compact stars, and compact star mergers. The emphasis is put on models that are applicable to all of these scenarios. Such EoS models have to cover large ranges in baryon number density, temperature, and isospin asymmetry. The characteristics of matter change dramatically within these ranges, from a mixture of nucleons, nuclei, and electrons to uniform, strongly interacting matter containing nucleons, and possibly other particles such as hyperons or quarks. As the development of an EoS requires joint efforts from many directions, different theoretical approaches are considered and relevant experimental and observational constraints which provide insights for future research are discussed. Finally, results from applications of the discussed EoS models are summarized.

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Production of a twin single hypernuclei and the Ξ−-nuclear interaction

Cited by 62 publications

References 18 publications

Λhypernuclei and neutron star matter in a chiral SU(3) relativistic mean field model with a logarithmic potential

Λhypernuclei and neutron star matter in a chiral SU(3) relativistic mean field model with a logarithmic potential

Tables of hyperonic matter equation of state for core-collapse supernovae

Equations of state for supernovae and compact stars

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