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

A'Hearn, Joseph; Hedman, M. M.; Moutamid, Maryame El

doi:10.3847/1538-4357/ab31af

Cited by 6 publications

(2 citation statements)

References 22 publications

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“…The ring arcs in the Adams ring comprise the most studied part of Neptune's rings (see for example Porco et al 1995;de Pater et al 2018). Ring arcs in the Saturnian system are confined longitudinally by orbital resonances with moons (Spitale et al 2006;Hedman et al 2007;Hedman et al 2009bHedman et al , 2010Cooper et al 2008;A'Hearn et al 2019). Although several ideas have been proposed about the particular resonance of Neptune's ring arcs, consensus has not been reached.…”

Section: Neptune's Le Verrier and Adams Ringsmentioning

confidence: 99%

Ring Seismology of the Ice Giants Uranus and Neptune

A'Hearn¹,

Hedman²,

Mankovich³

et al. 2022

Preprint

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We assess the prospect of using ring seismology to probe the interiors of the ice giants Uranus and Neptune. We do this by calculating normal mode spectra for different interior models of Uranus and Neptune using the stellar oscillation code GYRE. These spectra provide predictions of where in these planets' ring systems the effects of interior oscillations might be detected. We find that f-mode resonances with azimuthal order m = 2 or 7 ≤ m ≤ 19 fall among the inner rings (6, 5, 4, α, and β) of Uranus, while f-mode resonances with 2 ≤ m ≤ 12 fall in the tenuous ζ ring region. In addition, f-mode resonances with m = 2 or 6 ≤ m ≤ 13 may give azimuthal structure to Neptune's tenuous Galle ring. We also find that g-mode resonances may fall in the middle to outer rings of these planets. Although an orbiter is most likely required to confirm the association between any waves in the rings and planetary normal modes, the diversity of normal mode spectra implies that identification of just one or two modes in the rings of Uranus or Neptune would eliminate a variety of interior models, and thus aid in the interpretation of Voyager observations and future spacecraft measurements.

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Section: Neptune's Le Verrier and Adams Ringsmentioning

confidence: 99%

Ring Seismology of the Ice Giants Uranus and Neptune

A'Hearn¹,

Hedman²,

Mankovich³

et al. 2022

Preprint

Self Cite

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“…It is important to mention that there is possible to make theoretical predictions about the widths of the corotation resonances (e.g. El Moutamid et al 2014;A'Hearn et al 2019). Thus, we compute the widths of the three CERs by using the equation (7) of A'Hearn et al ( 2019), obtaining ≃ 112 km, 97 km and 59 km for Methone, Anthe and Aegaeon, respectively.…”

Section: Remarksmentioning

confidence: 99%

Dynamical stability in the vicinity of Saturnian small moons. The cases of Aegaeon, Methone, Anthe and Pallene

Rodríguez,

Callegari

2021

Preprint

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In this work we analyze the orbital evolution and the dynamical stability in the vicinity of the small saturnian moons Aegaeon, Methone, Anthe and Pallene. We numerically resolve the exact equations of motions to investigate the orbital motion of thousands of test particles within and near to the domain of the 7/6, 14/15, 10/11 mean motion resonances of Aegaeon, Methone and Anthe with Mimas, respectively. We show that, for massless small moons, the orbits of particles initially restricted to the resonant domains remain stable for at least 10 4 yr. We also conduct numerical simulations considering Aegaeon, Methone, Anthe and Pallene as massive bodies. The results show that most particles undergo significant perturbations in their orbital motions, ultimately destabilizing in timescales of a few hundreds of years or even less through collisions with the four small moons. In addition, we also simulate the orbital evolution of test particles initially distributed in form of arc around Aegaeon, Methone and Anthe. We show that the initial arcs are dynamically eroded on timescales of hundreds of years, allowing us to constraint the timescales for which gravitational forces operate to remove particles from the observed arcs.

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Neptune’s ring arcs confined by coorbital satellites: dust orbital evolution through solar radiation

Winter

Madeira

Sfair

2020

Monthly Notices of the Royal Astronomical Society

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Here, we report the results of a set of numerical simulations of the system formed by Neptune, Galatea, dust ring particles, and hypothetical co-orbital satellites. This dynamical system depicts a recent confinement mechanism formed by four co-orbital satellites being responsible for the azimuthal confinement of the arcs. After the numerical simulations, the particles were divided into four groups: particles that stay in the arcs, transient particles, particles that leave the arcs, and particles that collide with the co-orbital satellites. Our results showed that the lifetime of the smaller particles is 50 yr at most. After 100 yr, about $20{{\ \rm per\ cent}}$ of the total amount of larger particles are still present in the arcs. From our numerical simulations, the particles should be present in all arcs after 30 yr. Analysis of the dust production ruled out the hypothesis that small satellites close to or in the arc structure could be its source.

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

Cited by 6 publications

References 22 publications

Ring Seismology of the Ice Giants Uranus and Neptune

Ring Seismology of the Ice Giants Uranus and Neptune

Dynamical stability in the vicinity of Saturnian small moons. The cases of Aegaeon, Methone, Anthe and Pallene

Neptune’s ring arcs confined by coorbital satellites: dust orbital evolution through solar radiation

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