Abstract

The binding energy per nucleon for nuclear matter, i.e., equation of state (EOS), within the Brueckner–Hartree–Fock (BHF) approach with the consideration of various three-body forces (3BFs) like the phenomenological 3BF and by adding a contact term to the BHF calculations are considered at variance densities. The 3BF contribution turns out to be nonnegligible contribution and to have a substantial saturation effect. The calculations are done utilizing the CD-Bonn and Argonne V18 nucleon–nucleon (NN) potentials. These NN potentials give great fitting to the deuteron properties and are phase-shift equivalent. The resultant EOS is compatible with the phenomenological analysis on the saturation point. It is demonstrated that the 3BF influences significantly on the nuclear matter EOS at high densities. Moreover, it is necessary for reproducing the empirical saturation properties for symmetric nuclear matter. The pressure has been also calculated and the suggested approaches reproduce fairly well agreement with the empirical data. We also examined the maximum neutron star masses which are close to two solar masses, which is again compatible with recent observational data. Comparison with other microscopic EOS is presented and discussed.

中文翻译：

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各种三体力对核物质和中子星特性的影响

摘要

在布吕克纳-哈特里-福克（BHF）方法中，考虑到诸如现象学3BF之类的各种三体力（3BF）并通过添加接触，每个核子对核物质的结合能，即状态方程（EOS） BHF计算的项以方差密度考虑。事实证明，3BF贡献是不可忽略的，并且具有实质性的饱和效应。计算是利用CD-Bonn和Argonne V18核子-核子（NN）势进行的。这些NN电位非常适合氘核性质，并且是相移等效物。生成的EOS与饱和点的现象学分析兼容。结果表明，3BF对高密度核物质EOS的影响很大。此外，对于对称核物质来说，有必要再现经验饱和特性。还计算了压力，建议的方法与经验数据相当吻合。我们还检查了接近两个太阳质量的最大中子星质量，这也与最近的观测数据兼容。介绍并讨论了与其他微观EOS的比较。