色超导夸克星中的迈斯纳效应和涡旋驱逐及其对磁星再加热的作用
The Meissner Effect and Vortex Expulsion in Color-Superconducting Quark stars, and its Role for Re-heating of Magnetars
摘要：
由夸克物质而不是强子物质组成的致密恒星有望形成颜色超导体。这种超导体应该是由旋转的涡旋线穿成的，恒星内部的磁场至少部分地被限制在涡旋线内。这些涡旋（以及由此产生的磁通量）会在恒星向下旋转的过程中从恒星中排出，导致恒星表面的磁重联和大量的热能产生。在本文中，我们表明，这种能量释放可以重新加热夸克星异常高的温度，如观察到的软伽马重复（SGR），异常X射线散射（AXP），和X射线昏暗孤立中子星（XDIN）。此外，我们的数值研究的温度演化，自旋下降率，和磁场行为的超导夸克星表明，SGRs，AXP，和XDIN可能是联系在一起的祖先。最后，我们讨论了在恒星进入色超导相之前存在时间延迟的可能性，这可以用来估计夸克去精细的密度。根据观测，我们发现这个密度是核饱和度的五倍。
英文摘要：
Compact stars made of quark matter rather than confined hadronic matter, are expected to form a color superconductor. This superconductor ought to be threaded with rotational vortex lines, within which the star's interior magnetic field is at least partially confined. The vortices (and thus magnetic flux) would be expelled from the star during stellar spin-down, leading to magnetic reconnection at the surface of the star and the prolific production of thermal energy. In this paper, we show that this energy release can re-heat quark stars to exceptionally high temperatures, such as observed for Soft Gamma Repeaters (SGRs), Anomalous X-Ray pulsars (AXPs), and X-ray dim isolated neutron stars (XDINs). Moreover, our numerical investigations of the temperature evolution, spin-down rate, and magnetic field behavior of such superconducting quark stars suggest that SGRs, AXPs, and XDINs may be linked ancestrally. Finally, we discuss the possibility of a time delay before the star enters the color superconducting phase, which can be used to estimate the density at which quarks deconfine. From observations, we find this density to be of the order of five times that of nuclear saturation.
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。
