Quark-quark interaction and quark matter in neutron stars

被引：9

作者：

Yamamoto, Y. ^{[1
]}

Yasutake, N. ^{[2
]}

Rijken, Th. A. ^{[1
,3
]}

机构：

[1] RIKEN Nishina Ctr, 2-1 Hirosawa, Wako, Saitama 3510198, Japan

[2] Chiba Inst Technol, Dept Phys, 2-1-1 Shibazono, Narashino, Chiba 2750023, Japan

[3] Radboud Univ Nijmegen, IMAPP, NL-6500 GL Nijmegen, Netherlands

来源：

PHYSICAL REVIEW C | 2022年 / 105卷 / 01期

基金：

日本学术振兴会;

关键词：

EQUATION-OF-STATE; PHASE;

D O I：

10.1103/PhysRevC.105.015804

中图分类号：

O57 [原子核物理学、高能物理学];

学科分类号：

070202 ;

摘要：

Hyperon (Y) mixing in neutron-star matter brings about a remarkable softening of the equation of state (EoS) and the maximum mass is reduced to a value far less than 2M(circle dot). One idea to avoid this "hyperon puzzle in neutron stars" is to assume that the many-body repulsions work universally for every kind of baryons. The other is to take into account the quark deconfinement phase transitions from a hadronic EoS to a sufficiently stiff quark-matter EoS. In the present approach, both effects are handled in a common framework. As well as the hadronic matter, the quark matter with the two-body quark-quark interactions are treated within the Brueckner-Bethe-Goldstone theory beyond the mean-field frameworks, where interaction parameters are based on the terrestrial data. The derived mass-radius relations of neutron stars show that maximum masses reach over 2M(circle dot) even in the cases of including hadron-quark phase transitions, being consistent with the recent observations for maximum masses and radii of neutron stars by the Neutron Star Interior Composition Explorer (NICER) measurements and the other multimessenger data.

引用

页数：12

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