Numerical simulation of satellite-ring interactions: Resonances and satellite-ring torques

Brophy, T. G.; Esposito, L. W.; Stewart, G. R.; Rosen, P. A.

doi:10.1016/0019-1035(92)90108-j

Cited by 5 publications

(3 citation statements)

References 27 publications

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“…This, combined with the fact that Prometheus is closer of the rings, ensures the orbital converging. As suggested in the introduction, the standard torque could be less efficient than estimated by the linear theory either because of the formation of gaps at resonant locations (Goldreich & Tremaine 1982) or because of non‐linear effects (Brophy et al 1992). However, no gap was detected, while the second suggestion remains unproven.…”

Section: Prometheus and Pandora: An Unusual Pair Of Satellitesmentioning

confidence: 99%

Dynamical evolution of the Prometheus--Pandora system

Poulet

Sicardy

2001

Monthly Notices of the Royal Astronomical Society

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A B S T R A C TThe system of Saturn's inner satellites is saturated with many resonances. Its structure should be strongly affected by tidal forces driving the satellites through several orbit±orbit resonances. The evolution of these satellites is investigated using analytic and numerical methods. We show that the pair of satellites Prometheus and Pandora has a particularly short lifetime (,20 Myr) if the orbits of the satellites converge without capture into a resonance. The capture of Pandora into a resonance with Prometheus increases the lifetime of the couple by a few tens of Myr. However, resonances of the system are not well separated, and capture results in a chaotic motion. Secondary resonances also disrupt the resonant configurations. In all cases, the converging orbits of these two satellites result in a close encounter. The implications for the origin of Saturn's rings are discussed.

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Section: Prometheus and Pandora: An Unusual Pair Of Satellitesmentioning

confidence: 99%

Dynamical evolution of the Prometheus--Pandora system

Poulet

Sicardy

2001

Monthly Notices of the Royal Astronomical Society

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“…In other words, encounters with a satellite increase radial motions, while collisions circularize the orbits. A balance is achieved in which the particle orbits accommodate to the perturbing influence (Brophy et al 1992). The net effect is thus a repulsion of the orbits due to the gravitational attraction between the ring and moon (see Greenberg (1983))!…”

Section: Mechanisms For Ring Confinementmentioning

confidence: 99%

Planetary rings

Esposito

2002

Rep. Prog. Phys.

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In our solar system, planetary rings are found around all the giant planets, showing spectacular variety. Jupiter's thin ring system is composed mostly of dust. Saturn's rings are the largest and best studied, and the target of the NASA/ESA Cassini space mission that will begin orbiting Saturn in 2004. Its ring system consists of the broad A and B rings (separated by the Cassini Division) and the optically thinner C and D rings. Outside the main rings are the narrow 'braided' F ring and rings E and G. Uranus has ten narrow, sometimes eccentric rings and a family of dust bands. Neptune has three distinct rings (Galle, LeVervier, and Adams); the outermost Adams ring is patchy, with the thicker segments termed 'arcs.' All the ring systems have moons interspersed, which sculpt, collect, and release ring material. Moons are the likely parents of the present rings, ground down by meteorites and destroyed randomly to produce the relatively short-lived ring systems. Thus, we observe the natural stochastic results of birth and death processes when we examine the rings closely. Ring systems are relatively nearby and provide a natural laboratory for phenomena in flattened disks, including the nebula around our Sun that gave rise to the planets. Cassini will observe Saturn's rings and the numerous physical phenomena occurring within them close-up from 2004 to 2008, refining and possibly redefining our view of ring physics.

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“…One significant advance of this paper was the use of guiding center coordinates to simplify the description of the particle motion. These analytic papers paved the way for some of the first numerical work on these systems (Brophy et al, 1992). Given the computational power available at the time, this work used a statistical approach to modeling the system solving the kinetic equations of motion while using the Krook equation to statistically model interparticle collisions.…”

Section: Introductionmentioning

confidence: 99%