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Prog. Theor. Phys. Vol. 108 No. 4 (2002) pp. 703-718

[ Full Text PDF : FREE ACCESS (309K) ]

Hyperon-Mixed Neutron Star Matter and Neutron Stars*

Shigeru Nishizaki,1 Yasuo Yamamoto2 and Tatsuyuki Takatsuka1

1Faculty of Humanities and Social Sciences, Iwate University, Morioka 020-8550, Japan
2Physics Section, Tsuru University, Tsuru 402-8555, Japan

(Received December 23, 2001)

Abstract:

Effective Σ- n and Σ-Σ- interactions are derived from the G-matrix calculations for {n+Σ-} matter and employed in the investigation of hyperon mixing in neutron star matter. The threshold densities ρt(Y) at which hyperons start to appear are between 2ρ0 and 3ρ0 (where ρ0 is the normal nuclear density) for both Λ and Σ-, and their fractions increase rapidly with baryon density, reaching 10% already for ρ≃ρt+ρ0. The mechanism of hyperon mixing and single-particle properties, such as the effective mass and the potential depth, are analyzed taking into account the roles of YN and NN interactions. The resulting equation of state is found to be too soft to sustain the observed neutron star mass M obs=1.44M⊙. We discuss the reason for this and stress the necessity of the “extra repulsion” for YN and YY interactions to resolve this crucial problem. It is remarked that ρt(Y) would be as large as 4ρ0 for neutron stars compatible with M obs. A comment is given regarding the effects on the Y-mixing problem from a less attractive ΛΛ interaction, newly suggested by the NAGARA event.


URL : http://ptp.ipap.jp/link?PTP/108/703/
DOI : 10.1143/PTP.108.703


*A part of this work was reported in Refs. 1) and 2).

[ Full Text PDF : FREE ACCESS (309K) ] Citation:

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  13. Progress of Theoretical Physics Supplement No. 185 (2010) pp. 14-71 :
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