arXiv 2002.065712020-02-16nucl-thnucl-ex

含$d^*$ -六夸克自由度的中子星物质状态方程

Neutron star matter equation of state including $d^*$-hexaquark degrees of freedom

A. Mantziris, A. Pastore, I. Vidaña, D. P. Watts, M. Bashkanov, A. M. Romero

DOI：: 10.1051/0004-6361/202037749

摘要：

我们提出了以前的工作的扩展，假设一个简单的自由玻色子气体补充相对论meand场模型来描述EoS的纯核子部分，我们研究的后果，第一个非平凡的六夸克$d^*$（2380）可能对中子星的属性。相比，探索性的工作，我们采用了一个标准的非线性Walecka模型，包括额外的条款，描述了通过交换$σ$ -和$ω$ -介子场的$d^*(2380)$与系统的其他粒子的双重子的相互作用。我们的研究结果表明，如果$d^*(2380)$的相互作用是轻微的排斥或$d^*(2380)$不相互作用，$d^*(2380)$的存在导致最大的质量与最近的$\sim 2$ M $_\odot$毫秒双星的观察兼容。一个吸引的相互作用使状态方程太软，不能支持一个$2$ M $_\odot$中子星，而一个极端排斥的诱导中子星坍缩成一个黑洞，只要$d^*(2380)$出现。

英文摘要：

We present an extension of a previous work where, assuming a simple free bosonic gas supplemented with a relativistic meand field model to describe the pure nucleonic part of the EoS, we studied the consequences that the first non-trivial hexaquark $d^*$(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 the $d^*(2380)$ di-baryon with the other particles of the system through the exchange of $σ$- and $ω$-meson fields. Our results have show that the presence of the $d^*(2380)$ leads to maximum masses compatible with the recent observations of $\sim 2$M$_\odot$ millisecond pulsars if the interaction of the $d^*(2380)$ is slightly repulsive or the $d^*(2380)$ does not interacts at all. An attractive interaction makes the equation of state too soft to be able to support a $2$M$_\odot$ neutron star whereas an extremely repulsive one induces the collapse of the neutron star into a black hole as soon as the $d^*(2380)$ appears.

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