论文标题
量子涡流网络的脉冲星故障
Pulsar glitches from quantum vortex networks
论文作者
论文摘要
中子星或脉冲星是非常迅速的紧凑型恒星，密度极高。这些神秘的天体的未解决的长期问题之一是脉冲星故障的起源，即中子星的旋转速度突然快速减速。尽管已经报道了许多小故障事件，但在微观机制上尚无共识。小故障的重要特征之一是缩放定律$ p（e）\ sim e^{ - α} $的概率分布的概率分布，带有能量$ e $。在这里，我们重新分析了累积的最新观察数据，以获取缩放定律的指数$α\约0.88 $，并提出了一个简单的微观模型，该模型自然地推论了这种缩放定律而无需任何自由参数。我们的模型在中子星核心的两种不同种类的超氟中的界面上出现的量子涡流网络的存在来解释了这些故障的外观；内核中的A $ p $ - 波中子超级流体与外部核心的$ s $ - 波中子超级流体相结合，在$ s $ -wave超级流体中的每个整数涡流连接到两个半晶体的涡流中的$ p $ - p $ - p $ - p $ - 通过结构称为“ boojums”的结构。
Neutron stars or pulsars are very rapidly rotating compact stars with extremely high density. One of the unsolved long-standing problems of these enigmatic celestial bodies is the origin of pulsars' glitches, i.e., the sudden rapid deceleration in the rotation speed of neutron stars. Although many glitch events have been reported, there is no consensus on the microscopic mechanism responsible for them. One of the important characterizations of the glitches is the scaling law $P(E) \sim E^{-α}$ of the probability distribution for a glitch with energy $E$. Here, we reanalyse the accumulated up-to-date observation data to obtain the exponent $α\approx 0.88$ for the scaling law, and propose a simple microscopic model that naturally deduces this scaling law without any free parameters. Our model explains the appearance of these glitches in terms of the presence of quantum vortex networks arising at the interface of two different kinds of superfluids in the core of neutron stars; a $p$-wave neutron superfluid in the inner core which interfaces with the $s$-wave neutron superfluid in the outer core, where each integer vortex in the $s$-wave superfluid connects to two half-quantized vortices in the $p$-wave superfluid through structures called "boojums."
