中子星内壳层中涡旋钉扎能的微观计算
Microscopic calculation of the pinning energy of a vortex in the inner crust of a neutron star
AI总结：
本文采用轴向形变 Hartree-Fock-Bogolyubov 方法微观计算中子星内壳层涡旋结构，以核–涡旋结合能表征钉扎能，并得到与既往结果一致的介观钉扎力。
摘要：
本文在 Wigner-Seitz 胞近似下，对脉冲星内壳层中的涡旋结构进行了微观计算，模拟了冷的、非吸积中子星内壳层的条件；在该环境中，原子核晶格与超流中子海共存。该计算基于轴向形变的 Hartree-Fock-Bogolyubov 框架，并采用有效相互作用。本工作从四个方面扩展并改进了以往研究：i）考虑了涡旋出现导致中子产生大形变，进而诱导质子发生轴向形变；ii）纳入了 Coulomb 交换效应；iii）考虑了对相互作用屏蔽可能产生的影响；iv）改进了数值处理。我们还证明，原子核–涡旋体系的结合能可作为涡旋钉扎能的替代量，并讨论了其适用条件。根据所得结果，我们可以估算作用于涡旋上的每单位长度介观钉扎力。所得数值介于 10^14 至 10^16 dyn/cm 之间，与以往研究结果一致。
英文摘要：
The structure of a vortex in the inner crust of a pulsar is calculated microscopically in the Wigner-Seitz cell approximation, simulating the conditions of the inner crust of a cold, non-accreting neutron star, in which a lattice of nuclei coexists with a sea of superfluid neutrons. The calculation is based on the axially deformed Hartree-Fock-Bogolyubov framework, using effective interactions. The present work extends and improves previous studies in four ways: i) it allows for the axial deformation of protons induced by the large deformation of neutrons due to the appearance of vortices; ii) it includes the effect of Coulomb exchange; iii) considers the possible effects of the screening of the pairing interaction; and iv) it improves the numerical treatment. We also demonstrate that the binding energy of the nucleus-vortex system can be used as a proxy to the pinning energy of a vortex and discuss in which conditions this applies. From our results, we can estimate the mesoscopic pinning forces per unit length acting on vortices. We obtain values ranging between $10^{14}$ to $10^{16}$ dyn/cm, consistent with previous findings.
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。
