脉冲星毛刺的流体动力学触发机制
A hydrodynamical trigger mechanism for pulsar glitches
摘要：
对脉冲星大故障的标准解释涉及角动量从内部超流成分到恒星地壳的转移。这个模型需要一个不稳定性来触发涡的突然脱钉，超流就是通过这种脱钉来旋转的。这封信描述了一种新的不稳定性，它可能起到这种作用。这种不稳定性与超流中子星的惯性r模有关，一旦系统中的旋转滞后达到临界水平，这种不稳定性就会开始。我们表明，我们的模型是在良好的协议与观测到的毛刺数据，这表明超流r-模式的不稳定性可能确实是触发大脉冲星毛刺的机制。
英文摘要：
The standard explanation for large pulsar glitches involves transfer of angular momentum from an internal superfluid component to the star's crust. This model requires an instability to trigger the sudden unpinning of the vortices by means of which the superfluid rotates. This Letter describes a new instability that may play this role. The instability, which is associated with the inertial r-modes of a superfluid neutron star, sets in once the rotational lag in the system reaches a critical level. We demonstrate that our model is in good agreement with observed glitch data, suggesting that the superfluid r-mode instability may indeed be the mechanism that triggers large pulsar glitches.
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。
