AI 中文总结
该研究通过构建双组分可压缩恒星模型，发现旋转中子星上由马格努斯力产生的质量四极矩可达~10^-5，为连续引力波探测提供了新的研究方向。
AI 中文摘要
我们研究中子星上“马格努斯山”的形成，该结构由被钉扎的超流体涡旋对弹性壳层施加的非轴对称马格努斯力产生。这种变形的恒星将成为连续引力波的源。我们考虑可压缩的双组分恒星模型，自洽求解流体与弹性组分的耦合运动方程，以确定恒星变形及由此产生的质量四极矩。为简化计算，我们将恒星建模为无限长圆柱，由带薄海洋和壳层的流体区域构成。我们发现电流四极矩为零，而马格努斯力足够强，可产生无量纲质量四极矩高达~10^-5，因此该值仅受限于涡旋钉扎的有限强度及恒星弹性壳层的断裂应变。如此大的变形从当前及未来探测器探测连续引力波的角度来看颇具前景，这推动了对更真实恒星模型的进一步研究。
英文摘要
We investigate the formation of a "Magnus mountain'' on a neutron star, arising from the non-axisymmetric Magnus force acting on the elastic crust by pinned superfluid vortices. Such a deformed star would act as a source of continuous gravitational waves. We consider a compressible two-component stellar model and solve the coupled equations of motion for the fluid and elastic components self-consistently, allowing the stellar deformation and the resulting mass quadrupole to be determined. For simplicity, we model the star as an infinitely long cylinder, consisting of a fluid region with a thin ocean and crust. We find that the current quadrupole is zero, while the Magnus forces are strong enough to produce (dimensionless) mass quadrupoles as large as $\sim 10^{-5}$, and so would be limited only by the finite strength of the vortex pinning and the breaking strain of the star's elastic crust. Such large deformations are promising from the point of view of the detection of continuous gravitational waves by current and future detectors, and motivate further work on more realistic stellar models.
Comments19 pages, 12 Figures. Comments welcome
