Neutron star matter equation of state including d * -hexaquark degrees of freedom
Neutron star matter equation of state including d * -hexaquark degrees of freedom
复制标题
中子星物质状态方程，包括 d * -六夸克自由度
DOI：
10.1051/0004-6361/202037749
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发表时间：
2020
影响因子：
6.5
通讯作者：
Mantziris A
中科院分区：
文献类型：
--
作者：
Mantziris A
我们提出了以前的研究的延伸，假设一个简单的自由玻色子气体补充相对论平均场模型来描述状态方程的纯核子部分，我们研究了第一个非平凡的六夸克d *（2380）可能对中子星的性质的后果。与探索性工作相比，我们采用了一个标准的非线性Walecka模型，该模型包含了描述 *（2380）重子通过σ-和ω-介子场交换与系统中其他粒子相互作用的附加项。我们的结果表明，如果the *（2380）的相互作用是轻微排斥的或the *（2380）根本不相互作用，那么the *（2380）的存在会导致与最近观测到的102 M毫秒双星相一致的最大质量。吸引力的相互作用使状态方程太软，不能支持一个2 M的中子星星，而一个极端排斥的相互作用导致中子星星在the *（2380）出现时立即坍缩成黑洞。
We present the extension of a previous study where, assuming a simple free bosonic gas supplemented with a relativistic mean-field model to describe the pure nucleonic part of the equation of state, we studied the consequences that the first non-trivial hexaquarkd*(2380) could have on the properties of neutron stars. Compared to that exploratory work, we employ a standard non-linear Walecka model including additional terms that describe the interaction of thed*(2380) di-baryon with the other particles of the system through the exchange ofσ- andω-meson fields. Our results show that the presence of thed*(2380) leads to maximum masses compatible with recent observations of ∼2M⊙millisecond pulsars if the interaction of thed*(2380) is slightly repulsive or thed*(2380) does not interact at all. An attractive interaction makes the equation of state too soft to be able to support a 2M⊙neutron star whereas an extremely repulsive one induces the collapse of the neutron star into a black hole as soon as thed*(2380) appears.