论文标题
中子星号国家方程，包括$ d^*$ - 六夸克自由度
Neutron star matter equation of state including $d^*$-hexaquark degrees of freedom
论文作者
论文摘要
我们提出了以前的工作的扩展，假设一个简单的游离骨气气体补充了相对论的螺旋场模型来描述EOS的纯核电，我们研究了后果，即第一个非平凡的Hexaquark $ d^*$（2380）可能具有中子星的特性。与探索性工作相比，我们采用了标准的非线性Walecka模型，其中包括其他术语，这些术语描述了$ d^*（2380）$ di-baryon与系统其他粒子的相互作用，通过交换$σ$ - 和$ω$ - $ -Meson Fields。我们的结果表明，$ d^*（2380）$的存在导致最大质量与$ \ sim 2 $ \ sim 2 $ m $ _ \ odot $ millisecond Pulsars兼容，如果$ d^*（2380）$的相互作用略有抑制或$ d^*（2380）$不相互作用。一种有吸引力的互动使状态方程式太软，无法支撑$ 2 $ m $ _ \ odot $中子星星，而极具反击的人会在出现$ d^*（2380）$后立即引起中子星的崩溃。
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.
