Pan、Atlas和Daphnis上的观赏赤道脊的增生
Accretion of Ornamental Equatorial Ridges on Pan, Atlas and Daphnis
摘要：
我们探讨的方案，装饰脊土星的卫星潘，阿特拉斯和达夫尼从土星环的材料吸积。当来自增生物质的扭矩不超过通常维持潮汐锁的土星潮汐扭矩时，环物质的复杂形状的脊状隆起应该是可能的。这给出了最大吸积速率和赤道脊生长的最短持续时间的限制。我们探讨的经度分布的山脊增生环材料，最初在圆形轨道上，到一个月球上是一个圆形的，倾斜的或偏心的轨道。如果月球在吸积过程中由于其形状的变化或由于盘边缘表面密度分布允许来自不同初始半长轴的环材料在赤道脊的不同位置撞击月球，则倾斜和叶状脊可以被吸积。我们发现，吸积从一个不对称的差距可能会占一个低气压的阿特拉斯的赤道脊。从轨道偏心率类似于希尔偏心率的不对称间隙中吸积，可能允许多个裂片的吸积，如潘星上所见。两种可能相互关联的情景对观赏性赤道脊的生长是有希望的。月亮穿过光环，缩小了它的间隙，促进了吸积。由于与另一颗卫星的轨道共振，月球的轨道偏心率可能会增加，将其推入其间隙边缘并促进吸积。
英文摘要：
We explore scenarios for the accretion of ornamental ridges on Saturn's moons Pan, Atlas, and Daphnis from material in Saturn's rings. Accretion of complex shaped ridges from ring material should be possible when the torque from accreted material does not exceed the tidal torque from Saturn that ordinarily maintains tidal lock. This gives a limit on the maximum accretion rate and the minimum duration for equatorial ridge growth. We explore the longitude distribution of ridges accreted from ring material, initially in circular orbits, onto a moon that is on a circular, inclined or eccentric orbit. Sloped and lobed ridges can be accreted if the moon tidally realigns during accretion due to its change in shape or because the disk edge surface density profile allows ring material originating at different initial semi-major axes to impact the moon at different locations on its equatorial ridge. We find that accretion from an asymmetric gap might account for a depression on Atlas's equatorial ridge. Accretion from an asymmetric gap at orbital eccentricity similar to the Hill eccentricity, might allow accretion of multiple lobes, as seen on Pan. Two possibly connected scenarios are promising for growth of ornamental equatorial ridges. The moon migrates through the ring, narrowing its gap and facilitating accretion. The moon's orbital eccentricity could increase due to orbital resonance with another moon, pushing it into its gap edges and facilitating accretion.
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