论文标题
GW190814的次要组件，质量$（2.50-2.67）$ m $ _ {\ odot} $作为超级快速的脉冲星
GW190814's secondary component with mass $(2.50-2.67)$ M$_{\odot}$ as a super-fast pulsar
论文作者
论文摘要
使用Stergioulas的RNS代码来调查与高密度EOS参数空间的因果表面（声音的速度等于光的速度）上具有状态方程（EOSS）（EOSS）的快速脉冲，我们表明了G190814 $ Mass $ $（2.50）的所有已知约束，我们显示了一个可能的解释。 m $ _ {\ odot} $是它是一种超快速的脉冲星旋转速度，比971 Hz的旋转速度快于其开普勒频率低约42 \％。如果确认，它将是目前观察到的最快的脉冲星。在因果关系表面以下有一个大且物理上允许的EOS参数空间，其中支持脉冲脉冲比2.50 m $ _ {\ odot} $重，如果它们可以在核对象的高密度行为上以临界频率更快地旋转，它们的旋转速度更快。
Using Stergioulas's RNS code for investigating fast pulsars with Equation of States (EOSs) on the causality surface (where the speed of sound equals that of light) of the high-density EOS parameter space satisfying all known constraints from both nuclear physics and astrophysics, we show that one possible explanation for the GW190814's secondary component of mass $(2.50-2.67)$ M$_{\odot}$ is that it is a super-fast pulsar spinning faster than 971 Hz about 42\% below its Kepler frequency. If confirmed, it would be the fastest pulsar with the highest mass observed presently. There is a large and physically allowed EOS parameter space below the causality surface where pulsars heavier than 2.50 M$_{\odot}$ are supported if they can rotate even faster with critical frequencies depending strongly on the high-density behavior of nuclear symmetry energy.
