标题： 中子星中相邻I型和II型超导体因磁耦合产生的通量管聚类：持续的引力辐射 显示英文标题

标题： Flux tube clustering from magnetic coupling of adjacent type-I and -II superconductors in a neutron star: persistent gravitational radiation

摘要： 在由旋转供能的脉冲星中，相邻的I型和II型质子超导体被认为存在于一种亚稳态中，分别包含宏观量子化的磁通管。 先前的研究表明，当宏观磁通管在I型-II型界面附近通过称为磁通分支的过程分裂为量子化磁通管时，I型和II型区域通过磁场耦合在一起。 这些研究假设正常-超导边界是清晰的，并且量子化磁通管之间没有相互排斥。 在这里，通过考虑磁斥力对清晰界面近似进行了细化。 发现同一磁通树中的磁通管以比孤立磁通管低两到七倍的最小能量分离聚集在一起。 中子涡旋钉扎并聚集在磁通树周围。 我们发现，由聚集体涡旋的直线阵列发射的当前四极引力波的最大特征波幅 $h_0$ 超过均匀分布涡旋所发射的波幅 $h_0 \sim 10^{-32}(f/30 {\rm Hz})^{5/2} (D/1 {\rm kpc})^{-1}$ 的 $(1+N_{\rm v,t})^{1/2}$倍，其中 $N_{\rm v,t}$ 是每个磁通树上钉扎涡旋的平均数量， $f$ 是恒星的自转频率， $D$ 是恒星与地球之间的距离。 因子 $(1 + N_{\rm v,t})^{1/2}$ 在某些情况下使 $h_0$ 接近当前一代干涉引力波探测器的灵敏度极限，具体是在流分支形成相对较少（因而相对较大的）流树时。 显示英文摘要

摘要： Adjacent type-I and -II proton superconductors in a rotation-powered pulsar are predicted to exist in a metastable state containing macroscopic and quantized flux tubes, respectively. Previous studies show that the type-I and -II regions are coupled magnetically, when macroscopic flux tubes divide dendritically into quantized flux tubes near the type-I-II interface, through a process known as flux branching. The studies assume that the normal-superconducting boundary is sharp, and the quantized flux tubes do not repel mutually. Here the sharp-interface approximation is refined by accounting for magnetic repulsion. It is found that flux tubes in the same flux tree cluster with a minimum-energy separation two to seven times less than that of isolated flux tubes. Neutron vortices pin and cluster about flux trees. We find that the maximum characteristic wave strain $h_0$ of the current quadrupole gravitational radiation emitted by a rectilinear array of clustered vortices exceeds by $(1+N_{\rm v,t})^{1/2}$ the strain $h_0 \sim 10^{-32}(f/30 {\rm Hz})^{5/2} (D/1 {\rm kpc})^{-1}$ emitted by uniformly distributed vortices, where $N_{\rm v,t}$ is the mean number of pinned vortices per flux tree, $f$ is the star's spin frequency, and $D$ is the star's distance from Earth. The factor $(1 + N_{\rm v,t})^{1/2}$ brings $h_0$ close to the sensitivity limit of the current generation of interferometric gravitational wave detectors under certain circumstances, specifically when flux branching forms relatively few (and hence relatively large) flux trees.