论文标题
GW190814的次要组件的$ r $ - 模式稳定性为超大型和超快的脉冲星
$R$-mode Stability of GW190814's Secondary Component as a Supermassive and Superfast Pulsar
论文作者
论文摘要
GW190814的次要组件$ M_2 $的质量$（2.50-2.67）\，\ text {m} _ {\ odot} $在当前已知的最大质量中子星与当前的最大质量质量之间的质量差距和黑洞的最小质量之间存在热门辩论。在文献中提出的许多可能性中，$ M_2 $被建议用作超快速脉冲星，而其R模式稳定性通过Chandrasekhar-Friedman-Schutz机制对逃跑的重力辐射的稳定性仍然未知。在33个统一的状态方程（EOSS）样本中，使用那些实现当前已知的天体物理和核物理的约束，这是由Fortin {\ it等人}（2016）构建的，使用从外壳到核心的相同的核互作用始终如一地比较$ M_2 $所需的最小频率，从而比较$ M_2 $ $ 2.50 \，\ text {m} _ {\ odot} $，其临界频率在该临界频率上发生。假设外壳是完全刚性的，我们使用两个极端阻尼模型。使用19个观察到的低质量X射线二进制的稳定性，这表明R模式的刚性硬皮阻尼在所研究的模型中占主导GW190814的次要组件的提议是超级质量和超快的脉冲星。
The nature of GW190814's secondary component $m_2$ of mass $(2.50-2.67)\,\text{M}_{\odot}$ in the mass gap between the currently known maximum mass of neutron stars and the minimum mass of black holes is currently under hot debate. Among the many possibilities proposed in the literature, the $m_2$ was suggested as a superfast pulsar while its r-mode stability against the run-away gravitational radiation through the Chandrasekhar-Friedman-Schutz mechanism is still unknown. Using those fulfilling all currently known astrophysical and nuclear physics constraints among a sample of 33 unified equation of states (EOSs) constructed previously by Fortin {\it et al.} (2016) using the same nuclear interactions from the crust to the core consistently, we compare the minimum frequency required for the $m_2$ to rotationally sustain a mass higher than $2.50\,\text{M}_{\odot}$ with the critical frequency above which the r-mode instability occurs. We use two extreme damping models assuming the crust is either perfectly rigid or elastic. Using the stability of 19 observed low-mass x-ray binaries as an indication that the rigid crust damping of the r-mode dominates within the models studied, we find that the $m_2$ is r-mode stable while rotating with a frequency higher than 870.2 Hz (0.744 times its Kepler frequency of 1169.6 Hz) as long as its temperate is lower than about $3.9\times 10^7 K$, further supporting the proposal that GW190814's secondary component is a supermassive and superfast pulsar.
