论文标题
中子星的夸克物质状态
Quarkyonic matter state of neutron stars
论文作者
论文摘要
这项工作将我们先前对同胞对称性夸克物质的研究扩展到可能与中子恒星的内核有关的夸克中子物质。向量分散器$ρ$介子被引入模型主要是为了解释isospin密度相互作用，就像$ω$介子用于BARYON密度相互作用一样。修改后的Lagrangian仍然保留了近似的手性对称性，在较低的密度下可能会明显破坏。通过对对称能量的实验约束及其在饱和密度下的斜率来固定新的自由参数。最终，夸克中性星星预先探索了压力，大摩托比亚关系和潮汐变形。尽管压力和潮汐变形性与实验和观察性限制非常一致，但质量 - 拉迪乌斯关系无法再现观察到的两个PSR J0740+6620的两个太阳能质量。
This work extends our previous study of isospin symmetric quarkyonic matter to quarkyonic neutron matter which might be relevant to the inner cores of neutron stars. The vector-isovector $ρ$ mesons are introduced to the model mainly to account for isospin density interactions, just like $ω$ meson for baryon density interactions. The modified Lagrangian still preserves approximate chiral symmetry which could be significantly broken at lower density. And new free parameters are fixed by adopting the experimental constraints on the symmetry energy and its slope at saturation density. Eventually, the pressure, mass-radius relation, and tidal deformability are explored in advance for the quarkyonic neutron stars. While the pressure and tidal deformability are well consistent with experimental and observational restrictions, the mass-radius relation is unable to reproduce the observed two solar mass of PSR J0740+6620.
