相对论性中子星的剪切不稳定性
On the Shear Instability in Relativistic Neutron Stars
摘要：
我们提出了新的结果，在快速和差分旋转中子星的不稳定性。我们在完全的广义相对论中对恒星进行建模，并采用基于统一SLy处方的冷态现实状态方程描述恒星物质。我们提供的证据表明，快速和差分旋转的恒星，低于预期的阈值的动力学棒模不稳定性，β_c = T/ |W| ~ 0.25，但发展剪切不稳定性的动态时间尺度和广泛的β值。这类不稳定性，到目前为止只发现了小的β值和非常小的增长率，因此比以前发现的更普遍，可能更有效地产生强的引力波源。总体而言，我们的研究结果支持Watts，Andersson和Jones对低T/ |W|性质的现象学预测。
英文摘要：
We present new results on instabilities in rapidly and differentially rotating neutron stars. We model the stars in full general relativity and describe the stellar matter adopting a cold realistic equation of state based on the unified SLy prescription. We provide evidence that rapidly and differentially rotating stars that are below the expected threshold for the dynamical bar-mode instability, beta_c = T/|W| ~ 0.25, do nevertheless develop a shear instability on a dynamical timescale and for a wide range of values of beta. This class of instability, which has so far been found only for small values of beta and with very small growth rates, is therefore more generic than previously found and potentially more effective in producing strong sources of gravitational waves. Overall, our findings support the phenomenological predictions made by Watts, Andersson and Jones on the nature of the low-T/|W|.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
