Three tenuous rings/arcs for three tiny moons

Hedman, M. M.; Murray, C. D.; Cooper, Nicholas J.; Tiscareno, Matthew S.; Beurle, K.; Evans, Michael; Burns, Joseph A.

doi:10.1016/j.icarus.2008.11.001

Cited by 55 publications

(94 citation statements)

References 23 publications

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“…[7] All moons are known to be sources of micron-or submicron-sized grains to their environment. This dust is assumed to be the product of collisional ejecta from interplanetary meteor impacts [Grün et al, 1998;Burns et al, 1999;Krivov et al, 2003;Krüger et al, 2003;Jones et al, 2008;Hedman et al, 2009;Krüger et al, 2009]. Such ejecta are commonly detected in close vicinity to large moons (e.g., Callisto and Rhea), trapped by the moons' gravity on ballistic trajectories.…”

Section: Introductionmentioning

confidence: 99%

Surface charging of Saturn's plasma‐absorbing moons

et al. 2010

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[1] Recent results from the study of the interaction of Earth's moon with the solar wind have highlighted lunar surface charging as an important physical process not only for the local interaction of the surface and the impinging plasma but also for charged dust ejection and transport. Excluding Earth's moon, however, such studies have been limited to very few solar system bodies. Here we assess the importance of surface charging for the Saturnian plasma-absorbing moons. In this initial study, we focus on the various moons' trailing hemispheres and their variable charging patterns as a function of their magnetospheric local time. With only a few exceptions, our results indicate negative potentials for all moons, with the most extreme values predicted for Rhea. When the leading hemisphere is partially sunlit, the surface potential profile can be quite complex with many different transition regions. We also find that electrostatic acceleration of dust is at least equally as (if not more) important as it is for Earth's moon for the submicron grains, but it is probably not sufficient to explain the detection of the larger micron-sized grains in the vicinity of the large moons of the outer planets. Regarding Saturn's asteroid-sized moons, we predict that electrostatic forces can accelerate grains above the escape velocity and populate the Saturnian system and/or contribute to dust transport across those moons' surfaces. On the basis of these results, we also propose several methods by which Cassini's instruments could be used to directly observe the effects of surface charging.

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Section: Introductionmentioning

confidence: 99%

Surface charging of Saturn's plasma‐absorbing moons

et al. 2010

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“…The orbit of Methone is farther away from the chaotic zone than Anthe, with an amplitude of libration of ±20 km and a corotation width of 55.36 km. The case of Aegaeon (inside the orbit of Mimas) is slightly different, its orbit seems to be more stable than those of Anthe and Methone, as it is far enough from the chaotic region, the width of the corotation site is 31.62 km, and the magnitude of libration in terms of semi-major axis is ±4 km (Hedman et al (2009(Hedman et al ( , 2010). We notice that the chaotic region is surrounding by many regular trajectories, this behavior means that the corotation stability is not affected, this result will be investigated in future works by analysis of capture probability of this structures inside CER site.…”

Section: Real Applicationsmentioning

confidence: 93%

“…We apply the CoraLin model to several recently discovered small satellites dynamically linked to Mimas through first mean motion resonances : Anthe, Methone and Aegaeon (Cooper et al (2008);Hedman et al (2009Hedman et al ( , 2010), all associated with arc of material. The presence of these structures are consistent with their confinement by CER with Mimas : Aegaeon is trapped in an inner 7:6 CER with Mimas, while Anthe and Methone are respectively near the outer 10:11 and a 14:15 CER resonances.…”

Section: Real Applicationsmentioning

confidence: 99%

“…This extends for instance the approach of Goldreich et al (1986) and Porco (1991), who proposed a model to explain the stability of Neptune's incomplete rings (arcs) under the combined effects of Lindblad and corotation resonances. More recently, Cooper et al (2008) and Hedman et al (2009Hedman et al ( , 2010 have studied the motion of the small Saturnian satellites Anthe, Aegaeon and Methone that are trapped in corotation resonances with Mimas, while being perturbed by nearby Lindblad resonances.…”

Section: Introductionmentioning

confidence: 99%

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Coupling between corotation and Lindblad resonances in the presence of secular precession rates

Moutamid

Sicardy

Renner³

2014

Celest Mech Dyn Astr

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We investigate the dynamics of two satellites with masses µ s and µ s orbiting a massive central planet in a common plane, near a first order mean motion resonance m+1:m (m integer). We consider only the resonant terms of first order in eccentricity in the disturbing potential of the satellites, plus the secular terms causing the orbital apsidal precessions. We obtain a two-degree of freedom system, associated with the two critical resonant angles φ = (m + 1)λ − mλ − and φ = (m + 1)λ − mλ − , where λ and are the mean longitude and longitude of periapsis of µ s , respectively, and where the primed quantities apply to µ s . We consider the special case where µ s → 0 (restricted problem). The symmetry between the two angles φ and φ is then broken, leading to two different kinds of resonances, classically referred to as Corotation Eccentric resonance (CER) and Lindblad Eccentric Resonance (LER), respectively. We write the four reduced equations of motion near the CER and LER, that form what we call the CoraLin model. This model depends upon only two dimensionless parameters that control the dynamics of the system: the distance D between the CER and LER, and a forcing parameter L that includes both the mass and the orbital eccentricity of the disturbing satellite. Three regimes are found: for D = 0 the system is integrable, for D of order unity, it exhibits prominent chaotic regions, while for D large compared to 2, the behavior of the system is regular and can be qualitatively described using simple adiabatic invariant arguments. We apply this model to three recently discovered small Saturnian satellites dynamically linked to Mimas through first order mean motion resonances : Aegaeon, Methone and Anthe. Poincaré surfaces of section reveal the dynamical structure of each orbit, and their proximity to chaotic regions. This work may be useful to explore various scenarii of resonant capture for those satellites.

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“…In our solar system, both Saturn and Neptune have ring arcs. Saturn's ring arcs are confined longitudinally due to corotation eccentricity resonances with Saturn's moon Mimas: Aegaeon and its ring arc are in a 7:6 corotation resonance with Mimas (Hedman et al 2007(Hedman et al , 2010) (see Figure 1), Anthe and its ring arc are in a 10:11 corotation resonance with Mimas (Cooper et al 2008;Hedman et al 2009), while Methone and its ring arc are in a 14:15 corotation resonance with Mimas (Spitale et al 2006;Hedman et al 2009). Neptune's ring arcs are also confined longitudinally (Smith et al 1989) and move at rates close to a 42:43 corotation resonance with Galatea, which may be the explanation for their confinement (Goldreich et al 1986;Porco 1991;Namouni & Porco 2002).…”

Section: Introductionmentioning

confidence: 99%

Dynamics of Multiple Bodies in a Corotation Resonance: Conserved Quantities and Relevance to Ring Arcs

A'Hearn

Hedman

Moutamid

2019

ApJ

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The interactions among objects in a mean motion resonance are important for the orbital evolution of satellites and rings, especially Saturn's ring arcs and associated moons. In this work, we examine interactions among massive bodies in the same corotation eccentricity resonance site that affect the orbital evolution of those bodies using numerical simulations. During these simulations, the bodies exchange angular momentum and energy during close encounters, altering their orbits. This energy exchange, however, does not mean that one body necessarily moves closer to exact corotation when the other moves away from it. Indeed, if one object moves towards one of these sites, the other object is equally likely to move towards or away from it. This happens because the timescale of these close encounters is short compared to the synodic period between these particles and the secondary mass (i.e., the timescale where corotation sites can be treated as potential maxima). Because the timescale of a gravitational encounter is comparable to the timescale of a collision, we could expect energy to be exchanged in a similar way for collisional interactions. In that case, these findings could be relevant for denser systems like the arcs in Neptune's Adams ring and how they can be maintained in the face of frequent inelastic collisions.

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Three tenuous rings/arcs for three tiny moons

Cited by 55 publications

References 23 publications

Surface charging of Saturn's plasma‐absorbing moons

Surface charging of Saturn's plasma‐absorbing moons

Coupling between corotation and Lindblad resonances in the presence of secular precession rates

Dynamics of Multiple Bodies in a Corotation Resonance: Conserved Quantities and Relevance to Ring Arcs

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