The role of diamagnetism in the separation of particles and sharp edges of the Saturn's ring

Contribution of magnetism to the Saturn rings origin

The magnetization relationships for magnetically uniform spherical particles of the Saturn rings are derived. The problem of a solitary magnetized sphere and spherical particle among identical particles scattered in a disk-like structure is solved. The differential equations of motion of particles in the gravitational and magnetic field are derived. Special cases of these equations are solved exactly, and their solutions suggest that the superposition of the gravitational attraction and repulsion by a magnetic field of the iced particles which possess diamagnetism can account for the stability…

双曲扩散能否帮助解释土星环缝隙中的锐利边缘？

Can Hyperbolic Diffusion Help Explain Sharp Edges in the Gaps in Saturn's Rings?

研究探讨双曲扩散能否增强土星环缝隙锐利边缘的形成，通过引入弛豫时间的径向扩散模型，发现其能产生密度骤降的锐利边缘及尖峰，与N体模拟结果一致。

土星环中嵌入小卫星扰动产生的环缝边缘结构的全局N体模拟

Global N-body Simulation of Gap Edge Structures Created by Perturbations from a Small Satellite Embedded in Saturn's Rings

本文用高分辨率全局全N体模拟固定圆轨道嵌入小卫星在土星环中开缝的过程，解释密度波、锐边和垂直壁如何由引力与非弹性碰撞共同形成。

土星环III中的弹道输运不稳定性：数值模拟

The ballistic transport instability in Saturn's rings III: numerical simulations

土星内部的B环和C环支持着振幅不同但长度相似的波列，都是100-1000公里。此外，内部B环被两个有趣的“平坦”区域打断，半径为93，000公里和98，000公里，其中波消失，而C环波与高原森林，狭窄的小环和间隙共存。在这两个区域中，波可能是由大尺度的线性不稳定性产生的，这种不稳定性的起源在于环的陨石撞击：弹道输运不稳定性。在本文中，在一系列的第三，我们数值模拟的长期非线性演化的这种不稳定性在一个方便的本地模型。我们的C环模拟证实，不稳定的系统形成低振幅的波列拥有一个首选的波段。另一方面，B环模拟显示出由线性稳定平坦区域分隔的局部非线性波“包”。波包传播缓慢，同时在时间上传播，这一结果表明，在土星B环中观察到的平坦区域正在缩小。最后，我们提出了探索运行的内部B-环边缘再现早期的数值结果：弹道输运可以保持一个扩展的边缘的锐度，同时建立一个“斜坡”结构在其基础上。此外，弹道输运不稳定性可影响斜坡区域，但仅在低粘度运行中。

氦雨层的稳定分层导致木星和土星具有截然不同的内部结构与磁场

Stable stratification of the helium rain layer yields vastly different interiors and magnetic fields for Jupiter and Saturn

本研究基于氢氦相图发现木星和土星内部均存在稳定的氦雨层，但两者的内部结构、演化特征及磁场差异显著，土星可能具有更广阔的氦雨区域并依靠下沉氦滴传输绝大部分内禀热通量。

A simple model for the location of Saturn's F ring

In this paper, we introduce a simplified model to understand the location of Saturn's F ring. The model is a planar restricted five-body problem defined by the gravitational field of Saturn, including its second zonal harmonic $J_2$, the shepherd moons Prometheus and Pandora, and Titan. We compute accurate long-time numerical integrations of (about 2.5 million) non-interacting test-particles initially located in the region between the orbits of Prometheus and Pandora, and address whether they escape or remain trapped in this region. We obtain a wide region of initial conditions of the test par…