论文标题
中子和夸克之星：使用GW170817约束简单EOS的参数
Neutron and quark stars: constraining the parameters for simple EoS using the GW170817
论文作者
论文摘要
众所周知，尽管有几种复杂的模型可以描述它，但并未确定诸如中子和夸克之星这样的紧凑型物体的状态方程（EOS）。从\ cite {lattimer01}中总结的电磁观察，以及最近对二元中子星的引力波的观察结果，二进制的引力波GW170817 \ cite {abbott2017_etal} {abbott2017_etal}和gw190425在中子和夸克恒星中，不仅确定了EOS的最佳近似值，还确定了我们会观察到哪种恒星。在本文中，我们使用没有外壳的单层模型，探索了中子星的几种配置，假设状态的简单多潮流方程。特别是，当EOS取决于质量静止密度时，$ p =kρ_{0}^γ$，当它取决于能量密度$ p = kρ^γ$时，发现质量拉迪乌斯关系的差异很大。另一方面，我们还使用MIT袋EOS探索夸克星型号，以实现真空能量密度$ b $的不同值。
It is well known that the equation of state (EoS) of compact objects like neutron and quark stars is not determined despite there are several sophisticated models to describe it. From the electromagnetic observations, summarized in \cite{Lattimer01}, and the recent observation of gravitational waves from binary neutron star inspiral GW170817 \cite{Abbott2017_etal} and GW190425 \cite{Abbott2019}, it is possible to make an estimation of the range of masses and so constraint the mass of the neutron and quark stars, determining not only the best approximation for the EoS, but which kind of stars we would be observing. In this paper we explore several configurations of neutron stars assuming a simple polytropic equation of state, using a single layer model without crust. In particular, when the EoS depends on the mass rest density, $p=K ρ_{0}^Γ$, and when it depends on the energy density $p=K ρ^Γ$, considerable differences in the mass-radius relationships are found. On the other hand, we also explore quark stars models using the MIT bag EoS for different values of the vacuum energy density $B$.
